SkyView Surveys

Frequency vs Data Pixel Resolution plot of all SkyView Surveys

Plot of all surveys by resolution/frequency resolution

Click image to add survey names.

The diversity of SkyView surveys is shown here. Data ranges over about 18 orders of magnitude in energy and about 5 orders of magnitude in resolution. See our SkyView Blog post for more information.

Introduction

This document gives a short overview of each of the surveys included in SkyView. The descriptions include textual description which describe special properties of these surveys and a short table giving basic information for the survey.

The table includes:

The provenance of the data.
The copyright status of the data.
The spectral regime of the data.
Number of surveys, i.e., typically the number of separate frequency bands in SkyView.
The approximate frequency of the data. In addition to the frequency other indicators of the spectral range may be included (e.g., photon energy, wavelength, band).
The coverage of the survey on the sky. All-sky indicates that the survey covers substantially the entire sky although there may be small patches not covered.
Pixel scale. The angular size of the pixels. If only a single value is given then the pixels are assumed square.
Pixel units. The units in which the intensity at the pixel is given.
Resolution. A measure of the intrinsic resolution of the image. It may be greater or less than the pixel scale.
Coordinate system. The native coordinate system of the survey as used in SkyView.
Equinox. For data in Equatorial or Ecliptic coordinates, the equinox year of the coordinates.
Projection. The native projection of the data.
Reference. Reference to material giving further information on the survey.

Radio surveys
GTEE 0035 MHz Radio Survey
GMRT 150 MHz All-sky Radio Survey
Bonn 1420 MHz Survey
Effelsberg-Bonn HI Survey
HI All-Sky Continuum Survey
4850 MHz Survey/GB6
CO Galactic Plane Survey
FIRST
Dickey and Lockman HI map
NVSS
Sydney University Molonglo Sky Survey
VLA Low-frequency Sky Survey
Westerbork Northern Sky Survey
GOODS North Observations with the VLA

Millimeter surveys
Planck 030 GHz Survey
Planck 044 GHz Survey
Planck 070 GHz Survey
Planck 100 GHz Survey
Planck 143 GHz Survey
Planck 217 GHz Survey
Planck 353 GHz Survey
Planck 545 GHz Survey
Planck 857 GHz Survey
LABOCA Extended Chandra Deep Field South Submillimetre Survey

Infrared surveys
Two Micron All Sky Survey (H-Band)
Two Micron All Sky Survey (J-Band)
Two Micron All Sky Survey (K-Band)
WISE 3.4 All-Sky Release Survey
WISE 4.6 All-Sky Release Survey
WISE 12 Micron All-Sky Survey
WISE 22 Micron All-Sky Survey
AKARI WIDE-S
AKARI N160
Cosmic Background Explorer DIRBE Annual Average Map
Cosmic Background Explorer DIRBE Zodi-Subtracted Mission Average
IRAS Sky Survey Atlas: 100 micron
IRAS Sky Survey Atlas: 12 micron
IRAS Sky Survey Atlas: 25 micron
IRAS Sky Survey Atlas: 60 micron
Improved Reprocessing of the IRAS Survey: 100
Improved Reprocessing of the IRAS Survey: 12
Improved Reprocessing of the IRAS Survey: 25
Improved Reprocessing of the IRAS Survey: 60
Schlegel, Finkbeiner and Davis 100 micron survey
Schlegel, Finkbeiner and Davis Dust Survey
UKIRT Infrared Deep Survey H-band
UKIRT Infrared Deep Survey J-band
UKIRT Infrared Deep Survey K-band
UKIRT Infrared Deep Survey Y-band
WMAP Five Year Galaxy Removed
WMAP Five Year Ka-Band
WMAP Five Year K-Band
WMAP Five Year Q-Band
WMAP Five Year V-Band
WMAP Five Year W-band

Optical surveys
Original Digitized Sky Survey
First Digitized Sky Survey: Blue Plates
First Digitized Sky Survey: Red Plates
2nd Digitized Sky Survey (Blue)
2nd Digitized Sky Survey (Infrared)
2nd Digitized Sky Survey (Red)
Mellinger All Sky Mosaic: Blue
Mellinger All Sky Mosaic: Green
Mellinger All Sky Mosaic: Red
H-alpha Full Sky Map
Near-Earth Asteriod Tracking System Archive
Sloan Digitized Sky Survey G-band
Sloan Digitzed Sky Survey I-band
Sloan Digitzed Sky Survey R-band
Sloan Digitzed Sky Survey U-band
Sloan Digitzed Sky Survey Z-band
The Southern H-Alpha Sky Survey Atlas: Continuum
The Southern H-Alpha Sky Survey Atlas: Continuum-Corrected
The Southern H-Alpha Sky Survey Atlas: H-alpha
The Southern H-Alpha Sky Survey Atlas: Smoothed
GOODS HST ACS V Filter
GOODS HST ACS I Filter
GOODS HST ACS B Filter
GOODS HST ACS Z Filter

Ultraviolet surveys
Extreme Ultraviolet Explorer: 83 A
Extreme Ultraviolet Explorer: 171 A
Extreme Ultraviolet Explorer: 405 A
Extreme Ultraviolet Explorer: 555 A
Galaxy Explorer All Sky Survey: Far UV
Galaxy Explorer All Sky Survey: Near UV
ROSAT Wide Field Camera: F1
ROSAT Wide Field Camera: F2

Gamma ray surveys
CGRO Compton Telescope: 3 channel data
Energetic Gamma-Ray Event Telescope: 10 channel data
Energetic Gamma-Ray Event Telescope: Hard
Energetic Gamma-Ray Event Telescope: Soft
Fermi Map: Band 1
Fermi Map: Band 2
Fermi Map: Band 3
Fermi Map: Band 4
Fermi Map: Band 5

Radio surveys
4850 MHz Survey - GB6/PMN
Bonn 1420 MHz Survey
CO Galactic Plane Survey
Dickey and Lockman HI map
Effelsberg-Bonn HI Survey
FIRST
GLEAM 103-134: GaLactic and Extragalactic Allsky MWA Survey
GLEAM 139-170: GaLactic and Extragalactic Allsky MWA Survey
GLEAM 170-231: GaLactic and Extragalactic Allsky MWA Survey
GLEAM 72-103: GaLactic and Extragalactic Allsky MWA Survey
GMRT 150 MHz All-sky Radio Survey: First Alternative Data Release
GOODS North Observations with the VLA
GTEE 0035 MHz Radio survey
HI All-Sky Continuum Survey
LABOCA Extended Chandra Deep Field South Submillimetre Survey
NRA) VLA Sky Survey
Sydney University Molonglo Sky Survey
The HI 4-PI Survey
VLA Low-frequency Sky Survey
VLA Survey of SDSS Stripe 82
Westerbork Northern Sky Survey

Infrared surveys
2nd Digitized Sky Survey-Near Infrared
AKARI N160
AKARI N60
AKARI WIDE-L
AKARI WIDE-S
Cosmic Background Explorer DIRBE Annual Average Map
Cosmic Background Explorer DIRBE Zodi-Subtracted Mission Average
GOODS Herschel 100 micron, DR1 data release
GOODS Herschel 160 micron, DR1 data release
GOODS Herschel 250 micron, DR1 data release
GOODS Herschel 350 micron, DR1 data release
GOODS Herschel 500 micron, DR1 data release
GOODS NICMOS Survey
HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band H
HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band J
HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band Ks
HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band NB118
HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band Y
IRAS Sky Survey Atlas: 100 micron
IRAS Sky Survey Atlas: 12 micron
IRAS Sky Survey Atlas: 25 micron
IRAS Sky Survey Atlas: 60 micron
Improved Reprocessing of the IRAS Survey: 100
Improved Reprocessing of the IRAS Survey: 12
Improved Reprocessing of the IRAS Survey: 25
Improved Reprocessing of the IRAS Survey: 60
Schlegel, Finkbeiner and Davis 100 Micron survey
Schlegel, Finkbeiner and Davis dust map survey
Southern GOODS Field: VLT ISAAC Observations, H band
Southern GOODS Field: VLT ISAAC Observations, J band
Southern GOODS Field: VLT ISAAC Observations, KS band
Spitzer IRAC GOODS 3.6 micron data, channel 1
Spitzer IRAC GOODS 4.5 micron data, channel 2
Spitzer IRAC GOODS 5.8 micron data, channel 3
Spitzer IRAC GOODS 8.0 micron data, channel 4
Spitzer MIPS GOODS 24 Micron Data
The Hawaii Hubble Deep Field North: Band I
The Hawaii Hubble Deep Field North: Band Z
Two Micron All Sky Survey (H-Band)
Two Micron All Sky Survey (J-Band)
Two Micron All Sky Survey (K-Band)
UKIRT Infrared Deep Survey H-band
UKIRT Infrared Deep Survey J-band
UKIRT Infrared Deep Survey K-band
UKIRT Infrared Deep Survey Y-band
VLT ISAAC Ks Observations of the Southern Hubble Ultradeep Field
WISE 12 Micron All-Sky Survey>: All-WISE data release
WISE 22 Micron All-Sky Survey>: All-WISE data release
WISE 3.4 Micron All-Sky Survey>: All-WISE data release
WISE 4.6 Micron All-Sky Survey>: All-WISE data release
WMAP Nine Year Galaxy Removed
WMAP Nine Year K-Band
WMAP Nine Year Ka-Band
WMAP Nine Year Q-Band
WMAP Nine Year V-Band
WMAP Nine Year W-Band

Radio surveys

Bonn 1420 MHz Survey

Short name[s] used to specify survey: 1420MHz, 1420MHz (Bonn)

Description
This survey was taken with the Bonn Stockert 25m telescope. It was distributed on the NRAO Images from the Radio Sky CD-ROM. This image was delivered as a four map mosaic but was combined into a single map before being included in SkyView.

Provenance	Max Planck Institute for Radio Astronomy, generated by P. Reich and W. Reich
Copyright	Max-Planck-Institut fur Radioastronomie (permission for educational and private non-commercial use granted without further request)
Regime	Radio
NSurvey	1
Frequency	1420 MHz
Bandpass	1418.8-1421.2 MHz
Coverage	Declination > -16
PixelScale	0.25 deg/pixel
PixelUnits	millikelvins
Resolution	34'
CoordinateSystem	Equatorial
Equinox	1950
Projection	Rectangular (CAR)
Epoch	1972-09 to 1973-05, 1973-08 to 1974-04
Reference	Reich, 1982, A&AS48, 219. Reich and Reich, 1986, A&AS63, 205 (ADS)

HI All-Sky Continuum Survey

Short name[s] used to specify survey: 408MHz,0408MHz

Description
This survey is a mosaic of data taken at Jodrell Bank, Effelsberg and Parkes telescopes. The data was distributed in the NRAO Images from the Radio Sky CD ROM.

Provenance	Max Planck Institute for Radio Astronomy, generated by Glyn Haslam
Copyright	Max-Planck-Institut fur Radioastronomie (permission for educational and private non-commercial use granted without further request)
Regime	Radio
NSurvey	1
Frequency	408 MHz
Bandpass	406.25-409.75 MHz
Coverage	All-sky
PixelScale	0.3515 degrees/pixel
PixelUnits	Kelvins
Resolution	0.85 degrees
CoordinateSystem	Galactic
Projection	Rectangular (CAR)
Epoch	Jodrell Bank: 1965-11 to 1966-02 and 1978-08 to 1979-09 MPI: 1971-07 to 1972-02 PKS: 1973-12 to 1975-05
Reference	Haslam et al., 1982,A&AS47, 1 (ADS).

4850 MHz Survey - GB6/PMN

Short name[s] used to specify survey: 4850MHz,GB6/PMN,PMN,GB6,GB6 (4850MHz)

Description
The 4850MHz data is a combination of data from three different surveys: Parkes-MIT-NRAO (PMN) Southern (-88° to -37° declination) and tropical surveys (-29° to -9° declination, and (86+87) Green Bank survey (0° to +75° declination). The data contains gaps between -27° to -39°, -9° to 0°, and +77° to +90° declination. The 4850MHz survey data were obtained by tape from J.J. Condon and are comprised of 576 images and are used by permission. Full information pertaining to these surveys are found in the references.

Provenance	NRAO, generated by J.J. Condon, J.J. Broderick and G.A. Seielstad, Douglas, K., and Gregory, P.C.
Copyright	Used by permission of J.J. Condon
Regime	Radio
NSurvey	2
Frequency	4850 MHz continuum
Bandpass	4550 - 5150 MHz
Coverage	RA: 0d - 360d, DEC: -88d to +75d
PixelScale	1'/pixel (PMN), and 0.66' /pixel ((86+87) GB)
PixelUnits	janskies/beam (ca. 200,000 beams/steradian)
Resolution	3.5' FWHM
CoordinateSystem	Equatorial
Equinox	1950
Epoch	Greenbank: 1986-11,1987-10 PMN: 1990
Projection	Orthographic (SIN)
Reference	Condon, et al., 1991; 1993, 1994

LABOCA Extended Chandra Deep Field South Submillimetre Survey

Short name[s] used to specify survey:CDFS LESS, CDFS: LESS

Description
The LABOCA Extended Chandra Deep Field South (ECDFS) Submillimetre Survey (LESS) is a public legacy survey of the ECDFS at 870 ??m using the LABOCA camera (Siringo et al. 2009) on the APEX telescope.

The LABOCA data presented here were obtained between 2007 May and 2008 November in excellent conditions using time from both ESO and Max Planck allocations. The mapping pattern was designed to uniformly cover the 30'x30' extent of the ECDFS, centered on 03:32:29.0, -27:48:47.0 (J2000). The project used a total of 310 hrs of observations to achieve a beam-smoothed noise of 1.2 mJy/beam over 900 sq. arcmin (and <1.6mJy/beam over 1260 sq. arcmin). The flux calibration of the map came from observations of Mars, Uranus and Neptune (as well as secondary calibrators) and is accurate to within 8.5%.

Regime	Radio
Frequency	345 GHz
Bandwidth	315-375 GHz
Provenance	Data downloaded from ESO archive
Copyright	Data freely available from ESO archive. When using data products provided in this release, it is requested that authors refer to the publication Weiss et al. 2009, ApJ, 707, 1201 In addition, please also use the following statement in articles using these data: "Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, under programmes 078.F-9028(A), 079.F-9500(A), 080.A-3023(A), and 081.F-9500(A)."
NSurvey	1
Coverage	30'x30' in Chandra deep field south.
Resolution	19.2"
PixelSize	6"
CoordinateSystem	J2000
Projection	Gnomonic
PixelUnits	Jy/beam
Epoch	2007-07-12/2008-10-04
Reference	Paper and web site.>

CO Galactic Plane Survey

Short name[s] used to specify survey: CO2D,CO

Description
New large-scale CO surveys of the first and second Galactic quadrants and the nearby molecular cloud complexes in Orion and Taurus, obtained with the Harvard-Smithsonian Center for Astrophysics 1.2 m telescope, have been combined with 31 other surveys obtained over the past two decades with that instrument and a similar telescope on Cerro Tololo in Chile, to produce a new composite CO survey of the entire Milky Way. The survey consists of 488,000 spectra that Nyquist or beamwidth (1/8 deg) sample the entire Galactic plane over a strip 4 deg-10 deg wide in latitude, and beamwidth or 1/4 deg sample nearly all large local clouds at higher latitudes. Compared with the previous composite CO survey of Dame et al. (1987), the new survey has 16 times more spectra, up to 3.4 times higher angular resolution, and up to 10 times higher sensitivity per unit solid angle.

Users should be aware that both the angular resolution and the sensitivity varies from region to region in the velocity-integrated map. The component surveys were integrated individually using clipping or moment masking in order to display nearly all statistically significant emission but little noise above a level of ~1.5 K km/s. See the reference below and the Millimeter-Wave Group site for more details

Provenance	Data taken by two nearly-identical 1.2 m telescopes in Cambridge, MA and on Cerro Tololo, Chile combined into a complete survey of the Milky Way with CO integrated over all velocities.
Copyright	Permission is granted for publication and reproduction of this material for research or educational purposes so long as the reference (see below) is included.
Regime	Radio
NSurvey	1
Frequency	115 GHz
Bandpass	114.89 - 115.12 GHz
Coverage	9,853 sq. deg; All galactic longitudes, irregular bands between -35 and +35 latitudes
PixelScale	0.125d/pixel
Resolution	9-18'
PixelUnits	Pixel values are velocity-integrated main beam brightness temperature, in units of K km/s
CoordinateSystem	Galactic
Projection	Rectangular
Epoch	1980 to 2000
Reference	Dame, T. M., Hartmann, Dap, Thaddeus, P., ApJ, 2001 (ADS)

Effelsberg-Bonn HI Survey

Short name[s] used to specify survey:EBHIS, EBHIS(NHI)

Description
The Effelsberg-Bonn HI Survey (EBHIS) is a 21-cm survey performed with the 100-m telescope at Effelsberg. It covers the whole northern sky out to a redshift of z ~ 0.07 and comprises HI line emission from the Milky Way and the Local Volume. This dataset is the atomic neutral hydrogen (HI) column density map derived from the Milky-Way part of EBHIS (|Vlsr| < 600 km/s).

Provenance	Argelander-Institut für Astronomie (AIfA) and Max-Planck-Institut für Radioastronomie (MPIfR); data provided by B. Winkel
Regime	Radio
Copyright	Permission is granted for publication and reproduction of this material for scientific, scholarly, educational, and private non-commercial use by the Argelander-Institut für Astronomie (AIfA) and the Max-Planck-Institut für Radioastronomie (MPIfR), Germany. In addition, please also use the following statement in articles using the data: "The EBHIS data are based on observations performed with the 100-m telescope of the MPIfR at Effelsberg. EBHIS was funded by the Deutsche Forschungsgemeinschaft (DFG) under the grants KE757/7-1 to 7-3."
Frequency	1420 MHz
Coverage	All sky where δ > -5
Bandpass	1417.5 - 1423.5 MHz
PixelScale	1.5'
PixelUnit	atoms/cm²
Sensitivity	4.7 x 10¹⁸ cm^-2
Resolution	10.8'
Coordinates	Equatorial
Projection	Gnomonic
Epoch	2009-2013
Reference	Winkel et al., AA 585, A41, 2016; Kerp et al., 2011, AN 332, 637.

FIRST

Short name[s] used to specify survey:FIRST, VLA FIRST (1.4 GHz)

Description
The VLA FIRST (Faint Images of the Radio Sky at Twenty-centimeters) is a project designed to produce the radio equivalent of the Palomar Observatory Sky Survey over 10,000 square degrees of the North Galactic Cap. The FIRST home page has details of the instrumentation, status of the project, and data available. Currently about 5000 images of approximately .775x.58 degrees are available.

These FIRST data have been retrieved from the FIRST FTP archive at the Space Telescope Science Institute.

The FIRST survey is included on the SkyView High Resolution Radio Coverage map. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates.

Provenance	The FIRST project team: R.J. Becker, D.H. Helfand, R.L. White M.D. Gregg. S.A. Laurent-Muehleisen.
Copyright	1994, University of California. Permission is granted for publication and reproduction of this material for scholarly, educational, and private non-commercial use. Inquiries for potential commercial uses should be addressed to: Robert Becker, Physics Dept, University of California, Davis, CA 95616
Regime	Radio
NSurvey	1
Frequency	1.4 GHz Continuum
Bandpass	1.3635 - 1.4365 GHz
Coverage	Eventually will cover entire North Galactic Polar region (about 10,000 square degrees). See Status of FIRST Survey Observations
PixelScale	1.8"/pixel
PixelUnits	Janskies/beam
Resolution	5"
Coordinates	Equatorial
Equinox	2000
Projection	Orthographic
Epoch	1993-2004, 2009-2011
Reference	FIRST home page Becker et al., 1995 (ADS)

GLEAM 103-134: GaLactic and Extragalactic Allsky MWA Survey

Short name[s] used to specify survey: GLEAM103-134, GLEAM 103-134,GLEAM 103-134 MHz, GLEAM2, GLEAM 2

Description
GLEAM, the GaLactic and Extragalactic All-sky MWA survey, is a survey of the entire radio sky south of declination 30 degrees at frequencies between 72 and 231 MHz. It was made with the Murchison Widefield Array (MWA) using a drift scan method that makes efficient use of the MWA's very large field-of-view. The survey is described in Wayth et al. (2015) and the website at http://mwatelescope.org/science/gleam-survey.

The data presented here are from the first year of GLEAM observing, published in Hurley-Walker et al. (2017). The 25,000 square degrees of available sky excludes the Galactic Plane, the Magellanic Clouds, Centaurus A, and a few other small regions described in the catalogue paper.

The most sensitive and highest-resolution image is the 170-231MHz image which was used for all source-finding in generating the catalogue. It has a resolution of approximately 2.2 x 2.2/cos (dec + 26.7) arcmin at this frequency. However, due to ionospheric distortions, the final resolution of the survey varies by ~10% over the sky, with a direction-dependent PSF.

The SkyView data for the GLEAM surveys was extracted using the team's cutout server, into small (3 degree) raw cutouts over the region covered by the GLEAM survey. These cutouts have somewhat variable size and resolution. The default scale (i.e., pixel size) used for SkyView images is given in the table below.

SkyView resamples the cutouts retreived from the GLEAM web site into the image geometry requested by the user. Only four wide-band datasets are included here. The table below gives the frequency range, central frequency and a typical pixel scale for each of these bands.

GLEAM Bands In SkyView

Band f_min (MHz) f_max (MHz) f_C (MHz) Pixel scale (")

1 72 103 88 56

2 103 134 118 44

3 138 170 155 34

4 170 231 200 28

These data and 20 narrower bands are available through the team web site.

GLEAM Bands In SkyView
Band	f_min (MHz)	f_max (MHz)	f_C (MHz)	Pixel scale (")
1	72	103	88	56
2	103	134	118	44
3	138	170	155	34
4	170	231	200	28

To minimize resampling artifacts, this survey defaults to the Lanczos third order resampler.

Provenance	Source data extracted as cutouts from GLEAM cutout server.
Copyright	Natasha Hurley-Walker for the GLEAM teeam. Permission is granted for publication and reproduction of this material for scientific and educational purposes. When using data products provided in this release, it is requested that authors refer to the publications Wayth et al. (2015) and Hurley-Walker et al. (2017).
Regime	Radio
NSurvey	4
Frequency	118 MHz
Bandpass	103-134 MHz
Coverage	Declination < +25 excluding the Galactic plane
PixelScale	~ 44
PixelUnits	Jy/beam
Resolution	> 4' but varies with declination and frequency. See references.
CoordinateSystem	Equatorial
Equinox	ICRS
Projection	Zenital Equal Area (ZEA)
Epoch	2013-08-09 to 2014-06-18
Reference	Wayth et al. (2015), GLEAM: The GaLactic and Extragalactic All-Sky MWA Survey and Hurley-Walker, et al. (2017), GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey - I. A low-frequency extragalactic catalogue and GLEAM web site

GLEAM 139-170: GaLactic and Extragalactic Allsky MWA Survey

Short name[s] used to specify survey: GLEAM139-170, GLEAM 139-170,GLEAM 139-170 MHz, GLEAM3, GLEAM 3

GLEAM Bands In SkyView
Band	f_min (MHz)	f_max (MHz)	f_C (MHz)	Pixel scale (")
1	72	103	88	56
2	103	134	118	44
3	138	170	155	34
4	170	231	200	28

To minimize resampling artifacts, this survey defaults to the Lanczos third order resampler.

Provenance	Source data extracted as cutouts from GLEAM cutout server.
Copyright	Natasha Hurley-Walker for the GLEAM teeam. Permission is granted for publication and reproduction of this material for scientific and educational purposes. When using data products provided in this release, it is requested that authors refer to the publications Wayth et al. (2015) and Hurley-Walker et al. (2017).
Regime	Radio
NSurvey	4
Frequency	155 MHz
Bandpass	139-170 MHz
Coverage	Declination < +25 excluding the Galactic plane
PixelScale	~ 34
PixelUnits	Jy/beam
Resolution	> 4' but varies with declination and frequency. See references.
CoordinateSystem	Equatorial
Equinox	ICRS
Projection	Zenital Equal Area (ZEA)
Epoch	2013-08-09 to 2014-06-18
Reference	Wayth et al. (2015), GLEAM: The GaLactic and Extragalactic All-Sky MWA Survey and Hurley-Walker, et al. (2017), GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey - I. A low-frequency extragalactic catalogue and GLEAM web site

GLEAM 170-231: GaLactic and Extragalactic Allsky MWA Survey

Short name[s] used to specify survey: GLEAM170-231, GLEAM 170-231,GLEAM 170-231 MHz, GLEAM4, GLEAM 4

GLEAM Bands In SkyView
Band	f_min (MHz)	f_max (MHz)	f_C (MHz)	Pixel scale (")
1	72	103	88	56
2	103	134	118	44
3	138	170	155	34
4	170	231	200	28

To minimize resampling artifacts, this survey defaults to the Lanczos third order resampler.

Provenance	Source data extracted as cutouts from GLEAM cutout server.
Copyright	Natasha Hurley-Walker for the GLEAM teeam. Permission is granted for publication and reproduction of this material for scientific and educational purposes. When using data products provided in this release, it is requested that authors refer to the publications Wayth et al. (2015) and Hurley-Walker et al. (2017).
Regime	Radio
NSurvey	4
Frequency	200 MHz
Bandpass	170-231 MHz
Coverage	Declination < +25 excluding the Galactic plane
PixelScale	~ 28
PixelUnits	Jy/beam
Resolution	> 4' but varies with declination and frequency. See references.
CoordinateSystem	Equatorial
Equinox	ICRS
Projection	Zenital Equal Area (ZEA)
Epoch	2013-08-09 to 2014-06-18
Reference	Wayth et al. (2015), GLEAM: The GaLactic and Extragalactic All-Sky MWA Survey and Hurley-Walker, et al. (2017), GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey - I. A low-frequency extragalactic catalogue and GLEAM web site

GLEAM 72-103: GaLactic and Extragalactic Allsky MWA Survey

Short name[s] used to specify survey: GLEAM72-103, GLEAM 72-103,GLEAM 72-103 MHz, GLEAM1, GLEAM 1

GLEAM Bands In SkyView
Band	f_min (MHz)	f_max (MHz)	f_C (MHz)	Pixel scale (")
1	72	103	88	56
2	103	134	118	44
3	138	170	155	34
4	170	231	200	28

To minimize resampling artifacts, this survey defaults to the Lanczos third order resampler.

Provenance	Source data extracted as cutouts from GLEAM cutout server.
Copyright	Natasha Hurley-Walker for the GLEAM teeam. Permission is granted for publication and reproduction of this material for scientific and educational purposes. When using data products provided in this release, it is requested that authors refer to the publications Wayth et al. (2015) and Hurley-Walker et al. (2017).
Regime	Radio
NSurvey	4
Frequency	88 MHz
Bandpass	72-103 MHz
Coverage	Declination < +25 excluding the Galactic plane
PixelScale	~ 56
PixelUnits	Jy/beam
Resolution	> 4' but varies with declination and frequency. See references.
CoordinateSystem	Equatorial
Equinox	ICRS
Projection	Zenital Equal Area (ZEA)
Epoch	2013-08-09 to 2014-06-18
Reference	Wayth et al. (2015), GLEAM: The GaLactic and Extragalactic All-Sky MWA Survey and Hurley-Walker, et al. (2017), GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey - I. A low-frequency extragalactic catalogue and GLEAM web site

GOODS North Observations with the VLA

Short name[s] used to specify survey:GOODSNVLA,GOODS: VLA North,GOODS N VLA

Description
A combination of VLA measurements in all four configurations combined to generate a very deep image of the GOODS North region. A total of about 150 hours of VLA time was used. Data are sensitive to about 5 microJanskies in the central region. A total of 1230 discrete sources where found in the 40'x40' region.

Provenance	VLA Observations taken by Morrison et al. as provided through their web site.
Copyright	Public domain
Regime	Radio
Frequency	1.4 GHz
Bandpass	1.365-1.435 GHz
PixelScale	0.5"
PixelUnits	Jy/beam
NSurvey	1
Resolution	1.7"
Coverage	North GOODS field ~0.01% of sky
Projection	Sin
Coordinates	ICRS
Epoch	1996-11/1996-12, 2005-2,2005-8,2005-12
Reference	Morrison, et al, 2010

GTEE 0035 MHz Radio survey

Short name[s] used to specify survey:0035MHz,35MHz,GTEE,GEETEE,GTEE 35MHz

Description
This survey is a mosaic of data taken at the low frequency T-array near Gauribidanur, India. The data was distributed in the NRAO Images from the Radio Sky CD ROM.

The original 287x101 tiles had only 1 pixel overlap. To allow higher order resampling, the data were retiled into two hemisphere files of 1726x600 pixels with an overlap of 10 pixels.

The southernmost tiles were only 287x100 pixels. We assumed that bottom row of these tiles (as compared with the others) was truncated.

Copyright	Public domain
Regime	Radio
Frequency	34.5 MHz
Bandpass	34.3 - 34.7 MHz
Coverage	Complete between -50 and +70 degrees
PixelScale	0.105 x 0.20 degrees
PixelUnits	Kelvins
Resolution	26' x 42'/cos(dec-14)
Coordinates	Equatorial
Equinox	1950
Projection	Rectangular
Epoch	January 1987
Reference	K.S. Dwarakanath and N. Udaya Shankar 1990, J. Astrophys. Astr., 11 323. (ADS)

The HI 4-PI Survey

Short name[s] used to specify survey:HI4PI,HI4PI(NHI)

Description
The HI 4-PI Survey (HI4PI) is a 21-cm all-sky survey of neutral atomic hydrogen. It is constructed from the Effelsberg-Bonn HI Survey (EBHIS), made with the 100-m radio telescope at Effelsberg/Germany, and the Galactic All-Sky Survey (GASS), observed with the Parkes 64-m dish in Australia. HI4PI comprises HI line emission from the Milky Way. This dataset is the atomic neutral hydrogen (HI) column density map derived from HI4PI (|Vlsr| < 600 km/s).

Provenance	Argelander-Institut f??r Astronomie (AIfA), Max-Planck-Institut f??r Radioastronomie (MPIfR), and CSIRO/Australia; data provided by B. Winkel
Regime	Radio
Copyright	Permission is granted for publication and reproduction of this material for scientific and educational purposes. When using data products provided in this release, it is requested that authors refer to the HI4PI publication. We also ask that publications making use of these data include the following acknowledgement: "The Parkes Radio Telescope is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by CSIRO. The EBHIS data are based on observations performed with the 100-m telescope of the MPIfR at Effelsberg. EBHIS was funded by the Deutsche Forschungsgemeinschaft (DFG) under the grants KE757/7-1 to 7-3.
Frequency	1420 MHz
Coverage	All sky
Bandpass	1417.5 - 1423.5 MHz
PixelScale	1.5'
PixelUnit	atoms/cm²
Sensitivity	2.3 x 10¹⁸ cm^-2
Resolution	16.2'
Coordinates	Equatorial
Projection	Gnomonic
Epoch	2005-2013
Reference	HI4PI Collaboration, AA 594, 116, 2016

Dickey and Lockman HI map

Short name[s] used to specify survey:nH,HI map

Description
This survey is derived from the 21cm maps presented by Dickey and Lockman in the ARAA 28, p215. The nH is derived assuming optically thin emission. The nH given should be considered a lower limit when the nH is greater than several times 10²⁰.

Provenance	provided by S. Snowden from data by Dickey and Lockman
Regime	Radio
Copyright	Public domain
Frequency	1420 MHz line survey
Bandpass	1418.8 - 1421.2 MHz
PixelScale	40'
PixelUnit	atoms/cm^2
Resolution	1 degree
Coordinates	Galactic
Projection	Aitoff
Epoch	1980 to 1990
Reference	Dickey and Lockman, ARAA 28, 1990, 215 (ADS)

NRA) VLA Sky Survey

Short name[s] used to specify survey: NVSS,N-VSS

Description
SkyView has copied the NVSS intensity data from the NRAO FTP site. The full NVSS survey data includes information on other Stokes parameters.

Observations for the 1.4 GHz NRAO VLA Sky Survey (NVSS) began in 1993 September and should cover the sky north of -40 deg declination (82% of the celestial sphere) before the end of 1996. The principal data products are:

A set of 2326 continuum map "cubes," each covering 4 deg X 4 deg with three planes containing Stokes I, Q, and U images. These maps were made with a relatively large restoring beam (45 arcsec FWHM) to yield the high surface-brightness sensitivity needed for completeness and photometric accuracy. Their rms brightness fluctuations are about 0.45 mJy/beam = 0.14 K (Stokes I) and 0.29 mJy/beam = 0.09 K (Stokes Q and U). The rms uncertainties in right ascension and declination vary from 0.3 arcsec for strong (S > 30 mJy) point sources to 5 arcsec for the faintest (S = 2.5 mJy) detectable sources.
Lists of discrete sources.

The NVSS is being made as a service to the astronomical community, and the data products are being released as soon as they are produced and verified.

The NVSS survey is included on the SkyView High Resolution Radio Coverage map. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates.

Provenance	National Radio Astronomy Observatory. The NVSS project includes J. J. Condon, W. D. Cotton, E. W. Greisen, Q. F. Yin, R. A. Perley (NRAO), and J. J. Broderick (VPI).
Copyright	Copyright 1994, Associated Universities, Inc., National Radio Astronomy Observatory Permission is granted for publication and reproduction of this material for scholarly, educational, and private non-commerical use. 1994 Associated Universities, Inc. Inquiries for potential commercial uses should be addressed to: NRAO 520 Edgemont Road Charlottesville, VA 22903-2475
Regime	Radio
NSurvey	1
Frequency	1.4 GHz Continuum
Bandpass	1.3628 - 1.4472 GHz
Coverage	Declinations @gt; -40
PixelScale	15"/pixel
PixelUnits	Janskies/beam
Resolution	45"
Coordinates	Equatorial
Equinox	2000
Projection	Orthographic
Epoch	1993-1997
Reference	NVSS home page Condon et al. 1998 (ADS)

VLA Survey of SDSS Stripe 82

Short name[s] used to specify survey:Stripe82VLA,Stripe 82 VLA

Description
This survey is a deep, high resolution radio survey of a relatively small region that has particularly deep coverage in the Sloan Digital Sky Survey. As described in the reference abstract: This is a high-resolution radio survey of the Sloan Digital Sky Survey (SDSS) Southern Equatorial Stripe, a.k.a., Stripe 82. This 1.4 GHz survey was conducted from 2007 to 2009 with the Very Large Array primarily in the A-configuration, with supplemental B-configuration data to increase sensitivity to extended structure. The survey has an angular resolution of 1.8" and achieves a median rms noise of 53 microJy/beam over 92 square degrees. This is the deepest 1.4 GHz survey to achieve this large of an area filling in the phase space between small&deep and large&shallow surveys.

The astrometric accuracy of the data is excellent with errors in observed sources of 0.10" in both RA and declination. A comparison with the SDSS DR7 Quasar Catalog confirms that the astrometry is well tied to the optical reference frame with mean offsets of 0.02+/-0.01" in RA and 0.01+/-0.02 in declination.

Provenance	TBD
Regime	Radio
NSurvey	1
Frequency	1.4 GHz Continuum
Bandpass	1.3635 - 1.4365 GHz
Coverage	92 square degrees (0.23%)
PixelScale	0.6"
PixelUnits	Janskies/beam
Sensitivity	0.52 microJy/beam
Resolution	1.8"
Coordinates	Equatorial
Equinox	2000
Projection	Orthographic
Epoch	2007-2009
Reference	Survey paper: Hodge et al., AJ 142, 3, 2011

Sydney University Molonglo Sky Survey

Short name[s] used to specify survey: SUMSS, SUMSS 843 MHz

Description
The Sydney University Molonglo Sky Survey (SUMSS) is a deep radio survey at 843 MHz of the entire sky south of declination -30°, made using the Molonglo Observatory Synthesis Telescope ( MOST ), located near Canberra, Australia. The images from the SUMSS are produced as 4 x 4 degree mosaics of up to seventeen individual observations, to ensure even sensitivity across the sky. The mosaics slightly overlap each other. Data were last updated on January 28, 2015.

Images can also be obtained from the SUMSS Postage Stamp Server.

The SUMSS is intended to complement the NRAO-VLA Sky Survey (NVSS) which covered the sky between +90 and -40 deg declination, at a frequency of 1400MHz.

Provenance	The SUMSS project team, University of Sydney
Copyright	1997-2000 School of Physics, The University of Sydney. Permission is granted for publication and reproduction of this material for scholarly, educational, and private non-commerical use. Inquiries for potential commercial uses should be addressed to: Dr. R.W. Hunstead or Dr. E.M. Sadler Astrophysics Department, A29 University of Sydney Sydney, NSW 2006 Australia email: sumss@physics.usyd.edu.au
Regime	Radio
NSurvey	1
Frequency	843 MHz
Bandpass	841.5 - 844.5 MhZ
Coverage	Declination < -30°.
PixelScale	11" x 11" cosec (\|Dec\|). Default scale for retrieval is 11" x 11"
PixelUnits	Janskys/beam
Resolution	45" (RA) x 45" cosec (\|Dec\|)
Coordinates	Equatorial
Equinox	2000
Projection	Orthographic (SIN) representation of the NCP projection plane
Epoch	1997 to 2007
Reference	ADS SUMSS home page

GMRT 150 MHz All-sky Radio Survey: First Alternative Data Release

Short name[s] used to specify survey:TGSS, TGSS ADR1, TGSS_ADR1

Description
The first full release of a survey of the 150 MHz radio sky observed with the Giant Metrewave Radio Telescope between April 2010 and March 2012 as part of the TGSS project. Aimed at producing a reliable compact source survey, the automated data reduction pipeline efficiently processed more than 2000 hours of observations with minimal human interaction. Through application of innovative techniques such as image-based flagging, direction-dependent calibration of ionospheric phase errors, correcting for systematic offsets in antenna pointing, and improving the primary beam model, good quality images were created for over 95 percent of the 5336 pointings. This data release covers 36,900 square degrees (or 3.6 pi steradians) of the sky between -53 deg and +90 deg DEC, which is 90 percent of the total sky. The majority of pointing images have a background RMS noise below 5 mJy/beam with an approximate resolution of 25" x 25" (or 25" x 25" / cos (DEC - 19 deg) for pointings south of 19 deg DEC). The associated catalog has 640 thousand radio sources derived from an initial, high reliability source extraction at the 7 sigma level. The measured overall astrometric accuracy is better than 2" in RA and DEC, while the flux density accuracy is estimated at ~10 percent. Data is stored as 5336 mosaic images (5 deg x 5 deg).

SkyView uses Lanczos resampling and Sqrt image scaling by default for this survey.

Provenance	TGS ADR Team
Copyright	© Public Domain. If you are using the TGSS ADR survey products for your research, please add this reference (Intema et al. 2016) in your publication. Please also add the standard GMRT acknowledgement: "We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research."
Regime	Radio
NSurvey	1
Frequency	150 MHz (2 meters)
Bandpass	140-156 MHz
Coverage	All sky north of declination -53. (0.9 of all sky)
PixelScale	6.2"
PixelUnits	μJy
Resolution	25"
Coordinates	Equatorial
Projection	Sine
Epoch	April 2010 to March 2012
Reference	Intema, et al., 2016, or TGSS web site.

VLA Low-frequency Sky Survey

Short name[s] used to specify survey:VLSSr,4MASS,VLSS

Description
The VLA Low-Frequency Sky Survey (VLSS) is a 74 MHz continuum survey covering the entire sky north of -30 degrees declination. Using the VLA in BnA and B-configurations, it will map the entire survey region at a resolution of 80" and with an average rms noise of 0.1 Jy/beam.

This version include the data from the VLSS redux which increased the coverage region slightly and substantially improved the data reduction. Details are in the Lane et al. (2012) reference.

Provenance	VLSS Team: R.A. Perley, J.J. Condon, W.D. Cotton (NRAO); A.S. Cohen, W.M. Lane (NRC/NRL), N.E. Kassim, T.J.W. Lazio (NRL), W.C. Erickson (UMd)
Copyright
Regime	Radio
NSurvey	1
Frequency	74 MHz
Bandpass	73.02-74.58 MHz
Coverage	Declinations above -30 degrees
PixelScale	25"/pixel
PixelUnits	Janskies/beam
Resolution	75"
Coordinates	Equatorial
Equinox	2000
Projection	Orthographic (Sin)
Epoch	ca. 2006
Reference	VLSS download page . Details of the VLSSr reduction including comparisons with the original VLSS data are given in Lane et al. (2012)

Westerbork Northern Sky Survey

Short name[s] used to specify survey: WENSS,W-NSS

Description
The Westerbork Northern Sky Survey (WENSS) is a low-frequency radio survey that covers the whole sky north of delta=30 degree at a wavelength of 92 cm to a limiting flux density of approximately 18 mJy (5 sigma). This survey has a resolution of 54" x 54" cosec (delta) and a positional accuracy for strong sources of 1.5''.

Further information on the survey including links to catalogs derived from the survey is available at the WENSS web site.

The WENSS survey is included on the SkyView High Resolution Radio Coverage map. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates.

Provenance	WENSS Team. Data downloaded from WENSS FTP site 1999-03-18. The WENSS project is a collaboration between the Netherlands Foundation for Research in Astronomy (NFRA/ASTRON) and the Leiden Observatory.
Copyright	WENSS team. Anyone using data from the WENSS database in publications is asked to acknowledge this.
Regime	Radio
NSurvey	1
Frequency	325 MHz Continuum
Bandpass	322.5 - 327.5 MHz
Coverage	North of declination +30.
PixelScale	21"/pixel
PixelUnits	Janskies/beam
Resolution	54" cosec(declination)
Coordinates	Equatorial
Equinox	1950
Projection	Orthographic
Epoch	ca. 1991-1996
Reference	Rengelink et al., 1997, A&A Supp. 124, p 259. ADS

Millimeter surveys

Planck 353 GHz Survey

Short name[s] used to specify survey:Planck353,Planck 353,Planck-353

Description
Planck is ESA's third generation space based cosmic microwave background experiment, operating at nine frequencies between 30 and 857 GHz and was launched May 2009. Planck provides all-sky survey data at all nine frequencies with higher resolution at the 6 higher frequencies. It provides substantially higher resolution and sensitivity than WMAP. Planck orbits in the L2 Lagrange point. These data come from Release 1 of the Planck mission.

The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the HEALPix data. Users of the SkyView Jar will be able to access this survey through the web but performance may be poor since the FITS files are 150 to 600 MB in size and must be completely read in. SkyView will not automatically cache these files on the user machine as is done for non-HEALPix surveys.

Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

Provenance	Planck Team
Copyright
Regime	Millimeter
NSurvey	9
Frequency	353 GHz
Bandpass	310-410 GHz
Coverage	AllSky
PixelScale	1.7'
PixelUnits	K
Resolution	5.0'
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2009-2013
Reference	Planck Release 1 results

Planck 217 GHz Survey

Short name[s] used to specify survey:Planck217,Planck 217,Planck-217

Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

Provenance	Planck Team
Copyright
Regime	Millimeter
NSurvey	9
Frequency	217 GHz
Bandpass	190-250 GHz
Coverage	AllSky
PixelScale	1.7'
PixelUnits	K
Resolution	5.5'
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2009-2013
Reference	Planck Release 1 results

Planck 143 GHz Survey

Short name[s] used to specify survey:Planck143,Planck 143,Planck-143

Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

Provenance	Planck Team
Copyright
Regime	Millimeter
NSurvey	9
Frequency	143 GHz
Bandpass	130-160 GHz
Coverage	AllSky
PixelScale	1.7'
PixelUnits	K
Resolution	7.1'
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2009-2013
Reference	Planck Release 1 results

Planck 545 GHz Survey

Short name[s] used to specify survey:Planck545,Planck 545,Planck-545

Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

Provenance	Planck Team
Copyright
Regime	Millimeter
NSurvey	9
Frequency	545 GHz
Bandpass	450-650 GHz
Coverage	AllSky
PixelScale	1.7'
PixelUnits	MJy/sr
Resolution	5.0'
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2009-2013
Reference	Planck Release 1 results

Planck 030 GHz Survey

Short name[s] used to specify survey:Planck030,Planck 030,Planck-030

Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

Provenance	Planck Team
Copyright
Regime	Millimeter
NSurvey	9
Frequency	030 GHz
Bandpass	20-33 GHz
Coverage	AllSky
PixelScale	3.4'
PixelUnits	K
Resolution	33'
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2009-2013
Reference	Planck Release 1 results

Planck 100 GHz Survey

Short name[s] used to specify survey:Planck100,Planck 100,Planck-100

Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

Provenance	Planck Team
Copyright
Regime	Millimeter
NSurvey	9
Frequency	100 GHz
Bandpass	85-130 GHz
Coverage	AllSky
PixelScale	1.7'
PixelUnits	K
Resolution	10'
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2009-2013
Reference	Planck Release 1 results

Planck 070 GHz Survey

Short name[s] used to specify survey:Planck070,Planck 070,Planck-070

Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

Provenance	Planck Team
Copyright
Regime	Millimeter
NSurvey	9
Frequency	070 GHz
Bandpass	60-80 GHz
Coverage	AllSky
PixelScale	3.4'
PixelUnits	K
Resolution	14'
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2009-2013
Reference	Planck Release 1 results

Planck 857 GHz Survey

Short name[s] used to specify survey:Planck857,Planck 857,Planck-857

Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

Provenance	Planck Team
Copyright
Regime	Millimeter
NSurvey	9
Frequency	857 GHz
Bandpass	750-1000 GHz
Coverage	AllSky
PixelScale	1.7'
PixelUnits	MJy/sr
Resolution	5.0'
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2009-2013
Reference	Planck Release 1 results

Planck 044 GHz Survey

Short name[s] used to specify survey:Planck044,Planck 044,Planck-044

Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

Provenance	Planck Team
Copyright
Regime	Millimeter
NSurvey	9
Frequency	044 GHz
Bandpass	39-58 GHz
Coverage	AllSky
PixelScale	3.4'
PixelUnits	K
Resolution	24'
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2009-2013
Reference	Planck Release 1 results

Infrared surveys

Two Micron All Sky Survey (H-Band)

Short name[s] used to specify survey:2MASSH,2MASS-H

Description
2MASS data were collected by uniformly scanning the entire sky in three near-infrared bands to detect and characterize point sources brighter than about 1 mJy in each band, with signal-to-noise ratio (SNR) greater than 10, using a pixel size of 2.0". This achieves an 80,000-fold improvement in sensitivity relative to earlier surveys. 2MASS used two new, highly-automated 1.3-m telescopes, one at Mt. Hopkins, AZ, and one at CTIO, Chile. Each telescope is equipped with a three-channel camera, each channel consisting of a 256 by 256 array of HgCdTe detectors, capable of observing the sky simultaneously at J (1.25 microns), H (1.65 microns), and K_s (2.17 microns).

2MASS images and other data products can be obtained at the NASA/IPAC Infrared Science Archive

Provenance	The Two Micron All Sky Survey is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation.
Copyright	Researchers are asked to include the following acknowledgment in any published material that makes use of data products from the Two Micron All Sky Survey (2MASS): "This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation."
Regime	Infrared
NSurvey	3
Frequency	180 THz (1.65 microns)
Bandpass	167-197 THz
Coverage	All sky
PixelScale	1"/pixel
PixelUnits
Resolution	4"
Coordinates	Equatorial
Equinox	2000
Projection	Orthographic (SIN)
Epoch	1997 - 2002
Reference	2MASS web site

Two Micron All Sky Survey (J-Band)

Short name[s] used to specify survey:2MASSJ,2MASS-J

2MASS images and other data products can be obtained at the NASA/IPAC Infrared Science Archive

Provenance	The Two Micron All Sky Survey is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation.
Copyright	Researchers are asked to include the following acknowledgment in any published material that makes use of data products from the Two Micron All Sky Survey (2MASS): "This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation."
Regime	Infrared
NSurvey	3
Frequency	240 THz (1.25 microns)
Bandpass	222-375 THz
Coverage	All sky
PixelScale	1"/pixel
PixelUnits
Resolution	4"
Coordinates	Equatorial
Equinox	2000
Projection	Orthographic (SIN)
Epoch	1997 - 2002
Reference	2MASS web site

Two Micron All Sky Survey (K-Band)

Short name[s] used to specify survey:2MASSK,2MASS-K

2MASS images and other data products can be obtained at the NASA/IPAC Infrared Science Archive

Provenance	The Two Micron All Sky Survey is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation.
Copyright	Researchers are asked to include the following acknowledgment in any published material that makes use of data products from the Two Micron All Sky Survey (2MASS): "This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation."
Regime	Infrared
NSurvey	3
Frequency	137 THz (2.17 microns)
Bandpass	129-222 THz
Coverage	All sky
PixelScale	1"/pixel
PixelUnits
Resolution	4"
Coordinates	Equatorial
Equinox	2000
Projection	Orthographic (SIN)
Epoch	1997 - 2002
Reference	2MASS web site

AKARI N160

Short name[s] used to specify survey:AKARI N160, AKARI-N160, AKARI_N160

Description
The AKARI (formerly Astro-F) mission is a Japanese second generation all-sky infrared survey mission. SkyView currently includes surveys from the four bands of the FIS instrument: N60, WIDE-S, WIDE-L and N160.

These surveys cover 99% of the sky in four photometric bands centred at 65??m, 90??m, 140??m, and 160??m, with spatial resolutions ranging from 1-1.5'.

These data provide crucial information on the investigation and characterisation of the proper- ties of dusty material in the interstellar medium (ISM), since a significant portion of its energy is emitted between ???50 and 200 ??m. The large-scale distribution of interstellar clouds, their thermal dust temperatures, and their column densities can be investigated with the improved spatial resolution compared to earlier all-sky survey observations. In addition to the point source distribution, the large-scale distribution of ISM cirrus emis- sion, and its filamentary structure, are well traced.

Data are obtained using using the JVO AKARI Simple Image Access Service.

Provenance	AKARI FIS map making team [Univ of Tokyo, ISAS/JAXA, Tohoku Univ, Tsukuba Univ, The Rutherford Appleton Laboratory, The Open Univ]
Copyright
Regime	Infrared
NSurvey	4
Frequency	1.7 x 10¹²
Bandpass	1.3-2.1 x 10¹²
Coverage	All Sky
PixelScale	44.2"
PixelUnits	MJy/sr
Resolution	88"
Coordinates	Ecliptic
Projection	Tangent plane
Epoch	2006-2007
Reference	Doi, et al., 2016 and Takita, et al. 2015

AKARI N60

Short name[s] used to specify survey:AKARI N60, AKARI-N60, AKARI_N60

These surveys cover 99% of the sky in four photometric bands centred at 65??m, 90??m, 140??m, and 160??m, with spatial resolutions ranging from 1-1.5'.

Data are obtained using using the JVO AKARI Simple Image Access Service.

Provenance	AKARI FIS map making team [Univ of Tokyo, ISAS/JAXA, Tohoku Univ, Tsukuba Univ, The Rutherford Appleton Laboratory, The Open Univ]
Copyright
Regime	Infrared
NSurvey	4
Frequency	5 x 10¹²
Bandpass	3.7-6.0 x 10¹²
Coverage	All Sky
PixelScale	26.8"
PixelUnits	MJy/sr
Resolution	63"
Coordinates	Ecliptic
Projection	Tangent plane
Epoch	2006-2007
Reference	Doi, et al., 2016 and Takita, et al. 2015

AKARI WIDE-L

Short name[s] used to specify survey:AKARI WIDE-L, AKARI-WIDE-L, AKARI_WIDE-L

These surveys cover 99% of the sky in four photometric bands centred at 65??m, 90??m, 140??m, and 160??m, with spatial resolutions ranging from 1-1.5'.

Data are obtained using using the JVO AKARI Simple Image Access Service.

Provenance	AKARI FIS map making team [Univ of Tokyo, ISAS/JAXA, Tohoku Univ, Tsukuba Univ, The Rutherford Appleton Laboratory, The Open Univ]
Copyright
Regime	Infrared
NSurvey	4
Frequency	2.14 x 10¹²
Bandpass	1.7-2.7 x 10¹²
Coverage	All Sky
PixelScale	44.2"
PixelUnits	MJy/sr
Resolution	88"
Coordinates	Ecliptic
Projection	Tangent plane
Epoch	2006-2007
Reference	Doi, et al., 2016 and Takita, et al. 2015

AKARI WIDE-S

Short name[s] used to specify survey:AKARI WIDE-S, AKARI-WIDE-S, AKARI_WIDE-S

These surveys cover 99% of the sky in four photometric bands centred at 65??m, 90??m, 140??m, and 160??m, with spatial resolutions ranging from 1-1.5'.

Data are obtained using using the JVO AKARI Simple Image Access Service.

Provenance	AKARI FIS map making team [Univ of Tokyo, ISAS/JAXA, Tohoku Univ, Tsukuba Univ, The Rutherford Appleton Laboratory, The Open Univ]
Copyright
Regime	Infrared
NSurvey	4
Frequency	3.3 x 10¹²
Bandpass	2.7-5.0 x 10¹²
Coverage	All Sky
PixelScale	26.8"
PixelUnits	MJy/sr
Resolution	78"
Coordinates	Ecliptic
Projection	Tangent plane
Epoch	2006-2007
Reference	Doi, et al., 2016 and Takita, et al. 2015

Cosmic Background Explorer DIRBE Annual Average Map

Short name[s] used to specify survey: COBEAAM, COBE DIRBE/AAM

Description
The DIRBE Project Data Sets cover the whole sky and provide photometric data in 10 bands ranging in wavelength from 1.25 to 240 microns. SkyView has supported three maps: an early averaged map including including zodiacal and Galactic components (COBE DIRBE (OLD)), a more recent cleaner version of that data (COBE DIRBE/AAM) and a map with the zodaical light subtracted out (COBE DIRBE/ZSMA). The early data is no longer supported. Please contact us if you want access to these data.

Detailed descriptions of the DIRBE, the data processing, and the data products are given in an Explanatory Supplement. A Small Source Spectral Energy Distribution Browser can be used to assess the visibility of an unresolved or small extended source in the DIRBE data and see its spectral energy distribution. As noted in section 5.6.6 of the Explanatory Supplement, the DIRBE Time-ordered Data are required to derive definitive point source fluxes.

These maps provide an estimate of the infrared intensity at each pixel and wavelength band based on an interpolation of the observations made at various times at solar elongations close to 90°.

These COBE DIRBE maps are a combination original ten band passes with the following wavelengths:

Band 1 - 1.25 µm
Band 2 - 2.2 µm
Band 3 - 3.5 µm
Band 4 - 4.9 µm
Band 5 - 12 µm
Band 6 - 25 µm
Band 7 - 60 µm
Band 8 - 100 µm
Band 9 - 140 µm
Band 10 - 240 µm

The default two dimensional array uses Band 8 (100 µm).

The COBE DIRBE/Annual Average Maps (AAM) is the cumulative weighted average of the photometry. This average is calculated using the weighted number of observations from each Weekly Averaged Map ( WtNumObs from the Weekly Averaged Map) as the weight, such that annual_average =sum( weekly_average * weekly_weight )/ sum( weekly_weight )

COBE DIRBE/Zodi-Subtracted Mission Average (ZSMA) Skymap represents the extra-Solar system sky brightness. It is the average residual map that results after the modelled interplanetary dust (IPD) signal is subtracted from each of the DIRBE Weekly Skymaps from the cryogenic mission. Individual weekly residual maps can be reconstructed from the data supplied in the DIRBE Sky and Zodi Atlas (DSZA).

Provenance

COBE Team

Public Domain

Regime

Infrared

NSurvey

2 (10 bands)

Frequency

1.25-240 THz

Frequency Bands
Band	Central	Min
10		1.2491 THz	1.0016 THz	1.4966 THz
9		2.1414 THz	1.8394 THz	2.1717 THz
8		2.9979 THz	2.5159 THz	3.4799 THz
7		4.9965 THz	3.8365 THz	6.1565 THz
6		11.992 THz	9.9270 THz	14.057 THz
5		24.983 THz	18.333 THz	31.633 THz
4		61.182 THz	57.087 THz	65.277 THz
3		85.655 THz	74.655 THz	96.655 THz
2		136.70 THz	1.2550 THz	147.90 THz
1		239.83 THz	210.08 THz	269.58 THz

Coverage

All-sky

Scale

0.32 deg/pix

Units

MJy/sr

Resolution

ca. .75 deg

Coordinates

Ecliptic

Projection

CobeCube (CSC)

Equinox

2000

Epoch

1989-1990

Reference

COBE Diffuse Infrared Background Experiment (DIRBE) Explanatory Supplement ed. M.G. Hauser, T. Kelsall, D. Leisawitz, and J. Weiland COBE Ref. Pub. No. 97-A (Greenbelt, MD: NASA/GSFC) available in electronic form (in a slightly more up-to-date version) from the COBE Web page. Specific DIRBE information is available including an instrument description (PostScript).

Cosmic Background Explorer DIRBE Zodi-Subtracted Mission Average

Short name[s] used to specify survey: COBEZSMA, COBE DIRBE/ZSMA

These maps provide an estimate of the infrared intensity at each pixel and wavelength band based on an interpolation of the observations made at various times at solar elongations close to 90°.

These COBE DIRBE maps are a combination original ten band passes with the following wavelengths:

Band 1 - 1.25 µm
Band 2 - 2.2 µm
Band 3 - 3.5 µm
Band 4 - 4.9 µm
Band 5 - 12 µm
Band 6 - 25 µm
Band 7 - 60 µm
Band 8 - 100 µm
Band 9 - 140 µm
Band 10 - 240 µm

The default two dimensional array uses Band 8 (100 µm).

Provenance

COBE Team

Public Domain

Regime

Infrared

NSurvey

2 (10 bands)

Frequency

1.25-240 THz

Frequency Bands
Band	Central	Min
10		1.2491 THz	1.0016 THz	1.4966 THz
9		2.1414 THz	1.8394 THz	2.1717 THz
8		2.9979 THz	2.5159 THz	3.4799 THz
7		4.9965 THz	3.8365 THz	6.1565 THz
6		11.992 THz	9.9270 THz	14.057 THz
5		24.983 THz	18.333 THz	31.633 THz
4		61.182 THz	57.087 THz	65.277 THz
3		85.655 THz	74.655 THz	96.655 THz
2		136.70 THz	1.2550 THz	147.90 THz
1		239.83 THz	210.08 THz	269.58 THz

Coverage

All-sky

Scale

0.32 deg/pix

Units

MJy/sr

Resolution

ca. .75 deg

Coordinates

Ecliptic

Projection

CobeCube (CSC)

Equinox

2000

Epoch

1989-1990

Reference

2nd Digitized Sky Survey-Near Infrared

Short name[s] used to specify survey:DSS2IR, DSS2 IR

Description
This survey was generated by scanning Schmidt near-IR plates of the sky at 1" resolution. Scanning and compression was performed at the Space Telescope Science Institute. See the ST DSS site for further details.

The native projection of these data is described as a high-order polynomial distortion of a gnomonic projection using the same terms as the DSS.

SkyView has a copy of the compressed images which cover the entire sky. In previous versions of SkyView (prior to July 2007), this survey was served as a remote survey and data was retrieved in tiles from the ST ScI web site. Image generation using the local copy should be much faster at the SkyView web site. However data from this survey is not currently cached when it is used in the SkyView-in-a-Jar application so that data will be downloaded from the SkyView web site whenever an image is requested. Future updates to SkyView-in-a-Jar should address this caching issue.

Provenance	Data taken by ROE, AAO, and CalTech, Compression and distribution by Space Telescope Science Institute.
Copyright	There are multiple copyright holders depending upon the source plate or plates. See full copyright notices The coverage link below describes the coverage for each element of the surveys when the original plate used is not included in the SkyView files.
Regime	Infrared
NSurvey	1
Frequency	353 THz
Bandpass	327-422 THz
Coverage	All-sky
PixelScale	1"
PixelUnits	Pixel values are given as scaled densities
Resolution	Depends on plate. Typically 2-3".
Coordinates	Equatorial
Projection	Schmidt
Equinox	2000
Epoch	1987-2002
Reference	Some information on the DSS2 is given in McLean, 2000, The Second Generation Guide Star Catalog. Characteristics of the DSS surveys are summarized in this document.

GOODS Herschel 100 micron, DR1 data release

Short name[s] used to specify survey:GOODSHerschel1, GOODS Herschel 100, GOODS: Herschel 100

Description
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.

North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).

Note that the scale and resolution of the underlying pixels is different in each band.

Regime	Infrared
Frequency	3 THz
Bandpass	2.5-3.5 THz
Provenance	Downloaded from the Herschel Database in Marseille. Release DR1.
Copyright	All papers using GOODS-Herschel data downloaded from HeDaM should include the following acknowledgements: The GOODS-Herschel data was accessed through the Herschel Database in Marseille (HeDaM) - http://hedam.lam.fr - operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille.
NSurvey	5
PixelScale	1.2"
Resolution	6.7"
PixelUnits	Jy/pixel
Coverage	North and South GOODS Fields. 1.5e-6
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2009/2011
Reference	Elbaz, et al 2011

GOODS Herschel 160 micron, DR1 data release

Short name[s] used to specify survey:GOODSHerschel2, GOODS Herschel 160, GOODS: Herschel 160

Description
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.

North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).

Note that the scale and resolution of the underlying pixels is different in each band.

Regime	Infrared
Frequency	1.9 THz
Bandpass	1.6-2.2 THz
Provenance	Downloaded from the Herschel Database in Marseille. Release DR1.
Copyright	All papers using GOODS-Herschel data downloaded from HeDaM should include the following acknowledgements: The GOODS-Herschel data was accessed through the Herschel Database in Marseille (HeDaM) - http://hedam.lam.fr - operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille.
NSurvey	5
PixelScale	2.4"
Resolution	11.0"
PixelUnits	Jy/pixel
CoordinateSystem	ICRS
Projection	Gnomonic
Coverage	North and South GOODS fields: 1.e-5
Epoch	2009/2011
Reference	Elbaz, et al 2011

GOODS Herschel 250 micron, DR1 data release

Short name[s] used to specify survey:GOODSHerschel3, GOODS Herschel 250, GOODS: Herschel 250

Description
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.

North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).

Note that the scale and resolution of the underlying pixels is different in each band.

Regime	Infrared
Frequency	1.2 THz
Bandpass	1.0-1.4 THz
Provenance	Downloaded from the Herschel Database in Marseille. Release DR1.
Copyright	All papers using GOODS-Herschel data downloaded from HeDaM should include the following acknowledgements: The GOODS-Herschel data was accessed through the Herschel Database in Marseille (HeDaM) - http://hedam.lam.fr - operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille.
NSurvey	5
PixelScale	3.6"
Resolution	18.1"
PixelUnits	Jy/pixel
Coverage	Extended North GOODS Fields. 1.6e-5
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2009/2011
Reference	Elbaz, et al 2011

GOODS Herschel 350 micron, DR1 data release

Short name[s] used to specify survey:GOODSHerschel4, GOODS Herschel 350, GOODS: Herschel 350

Description
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.

North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).

Note that the scale and resolution of the underlying pixels is different in each band.

Regime	Infrared
Frequency	860 MHz
Bandpass	740-1000 MHz
Provenance	Downloaded from the Herschel Database in Marseille. Release DR1.
Copyright	All papers using GOODS-Herschel data downloaded from HeDaM should include the following acknowledgements: The GOODS-Herschel data was accessed through the Herschel Database in Marseille (HeDaM) - http://hedam.lam.fr - operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille.
NSurvey	5
PixelScale	4.8"
Resolution	24.9"
PixelUnits	Jy/pixel
Coverage	Extended North GOODS Fields. 1.6e-5
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2009/2011
Reference	Elbaz, et al 2011

GOODS Herschel 500 micron, DR1 data release

Short name[s] used to specify survey:GOODSHerschel5, GOODS Herschel 500, GOODS: Herschel 500

Description
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.

North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).

Note that the scale and resolution of the underlying pixels is different in each band.

Regime	Infrared
Frequency	600 MHz
Bandpass	510-700 MHz
Provenance	Downloaded from the Herschel Database in Marseille. Release DR1.
Copyright	All papers using GOODS-Herschel data downloaded from HeDaM should include the following acknowledgements: The GOODS-Herschel data was accessed through the Herschel Database in Marseille (HeDaM) - http://hedam.lam.fr - operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille.
NSurvey	5
PixelScale	7.2"
Resolution	36.6"
PixelUnits	Jy/pixel
Coverage	Extended North GOODS Fields. 1.6e-5
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2009/2011
Reference	Elbaz, et al 2011

Spitzer IRAC GOODS 3.6 micron data, channel 1

Short name[s] used to specify survey:GOODSIRAC 1, GOODS IRAC 1, GOODS IRAC 3.6, GOODS: Spitzer IRAC 3.6

Description
Spitzer IRAC medium infrared observations taken in all four IRAC channels in both the north and south GOODS fields.

Provenance	IRAC Goods Team, IRSA data center
Copyright	Public Domain
Regime	Infrared
NSurvey	4
Frequency	8.33 THz
Bandpass	7.58-9.43 THz
Coverage	GOODS North and South (approximately 0.01% of sky).
PixelScale	0.5"
PixelUnits	DN/s
Resolution	1.7" in bands 1-3, 1.9" in band 4
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2004-02-08/2004-05-26
Reference	The IRAC observation characteristics are summarized in this analysis paper while the discussion of how the data are archived are found in data release documentation.

Spitzer IRAC GOODS 4.5 micron data, channel 2

Short name[s] used to specify survey:GOODSIRAC 2, GOODS IRAC 2, GOODS IRAC 4.5, GOODS: Spitzer IRAC 4.5

Description
Spitzer IRAC medium infrared observations taken in all four IRAC channels in both the north and south GOODS fields.

Provenance	IRAC Goods Team, IRSA data center
Copyright	Public Domain
Regime	Infrared
NSurvey	4
Frequency	6.66 THz
Bandpass	5.98-7.59 THz
Coverage	GOODS North and South (approximately 0.01% of sky).
PixelScale	0.5"
PixelUnits	DN/s
Resolution	1.7" in bands 1-3, 1.9" in band 4
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2004-02-08/2004-05-26
Reference	The IRAC observation characteristics are summarized in this analysis paper while the discussion of how the data are archived are found in data release documentation.

Spitzer IRAC GOODS 5.8 micron data, channel 3

Short name[s] used to specify survey:GOODSIRAC 3, GOODS IRAC 3, GOODS IRAC 5.8, GOODS: Spitzer IRAC 5.8

Description
Spitzer IRAC medium infrared observations taken in all four IRAC channels in both the north and south GOODS fields.

Provenance	IRAC Goods Team, IRSA data center
Copyright	Public Domain
Regime	Infrared
NSurvey	4
Frequency	5.17 THz
Bandpass	4.65-5.98 THz
Coverage	GOODS North and South (approximately 0.01% of sky).
PixelScale	0.5"
PixelUnits	DN/s
Resolution	1.7" in bands 1-3, 1.9" in band 4
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2004-02-08/2004-05-26
Reference	The IRAC observation characteristics are summarized in this analysis paper while the discussion of how the data are archived are found in data release documentation.

Spitzer IRAC GOODS 8.0 micron data, channel 4

Short name[s] used to specify survey:GOODSIRAC 4, GOODS IRAC 4, GOODS IRAC 8.0, GOODS: Spitzer IRAC 8.0

Description
Spitzer IRAC medium infrared observations taken in all four IRAC channels in both the north and south GOODS fields.

Provenance	IRAC Goods Team, IRSA data center
Copyright	Public Domain
Regime	Infrared
NSurvey	4
Frequency	3.75 THz
Bandpass	3.21-4.65 THz
Coverage	GOODS North and South (approximately 0.01% of sky).
PixelScale	0.5"
PixelUnits	DN/s
Resolution	1.7" in bands 1-3, 1.9" in band 4
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2004-02-08/2004-05-26
Reference	The IRAC observation characteristics are summarized in this analysis paper while the discussion of how the data are archived are found in data release documentation.

Southern GOODS Field: VLT ISAAC Observations, H band

Short name[s] used to specify survey:GOODS ISAAC H, GOODS: VLT ISAAC H

Description
As part of the Great Observatories Origins Deep Survey (GOODS), near-infrared imaging observations of the Chandra Deep Field South (CDF-S) were carried out in J, H, Ks bands, using the ISAAC instrument mounted at the Antu Unit Telescope of the VLT at ESO's Cerro Paranal Observatory, Chile.

These data were obtained as part of the ESO Large Programme 168.A-0485 (PI: C. Cesarsky). Data covering four ISAAC fields in J and Ks bands were also drawn from the ESO programmes 64.O-0643, 66.A-0572 and 68.A-0544 (PI: E.Giallongo), which were part of the previous data releases.

This data release covers 172.4, 159.6, and 173.1 arcmin2 of the GOODS/CDF-S region in J, H and Ks respectively. More than 50% of the images reach a 5-sigma depth for point sources of at least 25.2 mag (J), 24.7 mag (H and Ks) in the AB system ("median depth").

This final GOODS/ISAAC data release accumulates observational data which have been acquired in 12814 science integrations between October 1999 and January 2007 totaling 1.3 Msec integration time. [Above adapted from reference Web site.]

SkyView uses the mosaic files provided in this delivery. The Version 1.5 mosaic is used for the KS band.

Regime	Infrared
Frequency	183 THz
Bandwidth	168-202 THz
Provenance	Data downloaded from VLT archive
Copyright	Data freely available
NSurvey	3
Resolution	0.3-0.6"
PixelSize	0.15"
CoordinateSystem	ICRS
Projection	Gnomonic
PixelUnits	ADU/s
Epoch	October 1999 to January 2007
Reference	Paper and web site.

Southern GOODS Field: VLT ISAAC Observations, J band

Short name[s] used to specify survey:GOODS ISAAC J, GOODS: VLT ISAAC J

SkyView uses the mosaic files provided in this delivery. The Version 1.5 mosaic is used for the KS band.

Regime	Infrared
Frequency	245 THz
Bandwidth	225-270 THz
Provenance	Data downloaded from VLT archive
Copyright	Data freely available
NSurvey	3
Resolution	0.3-0.6"
PixelSize	0.15"
CoordinateSystem	ICRS
Projection	Gnomonic
PixelUnits	ADU/s
Epoch	October 1999 to January 2007
Reference	Paper and web site.

Southern GOODS Field: VLT ISAAC Observations, KS band

Short name[s] used to specify survey:GOODS ISAAC KS, GOODS: VLT ISAAC KS

SkyView uses the mosaic files provided in this delivery. The Version 1.5 mosaic is used for the KS band.

Regime	Infrared
Frequency	137 THz
Bandwidth	125-150 THz
Provenance	Data downloaded from VLT archive
Copyright	Data freely available
NSurvey	3
Resolution	0.3-0.6"
PixelSize	0.15"
CoordinateSystem	ICRS
Projection	Gnomonic
PixelUnits	ADU/s
Epoch	October 1999 to January 2007
Reference	Paper and web site.

Spitzer MIPS GOODS 24 Micron Data

Short name[s] used to specify survey:GOODSMIPS, GOODS MIPS, GOODS: Spitzer MIPS, GOODS: Spitzer MIPS 24

Description
Spitzer MIPS observations of the GOODS North and South fields in the 24 micron channel.

Provenance	IRSA, GOODS team
Copyright	Public domain
Regime	Infrared
NSurvey	1
Frequency	12.5 THz (24 microns)
Bandpass	10.2-14.7 THz
Coverage	GOODS regions, 0.01% of sky
PixelScale	1.2"
PixelUnits	DN/s
Resolution	5"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2004-5/2004-8
Reference	See release documentation for data.

GOODS NICMOS Survey

Short name[s] used to specify survey:GOODSNICMOS, GNS, GOODS: HST NICMOS

Description
The GOODS NICMOS Survey (GNS) is a 180 orbit Hubble Space Telescope survey consisting of 60 pointings with the NICMOS-3 near-infrared camera. Each pointing is centred on a massive galaxy (M_* > 1011 M_sun) in the redshift range 1.7 < z < 3, selected by their optical-to-infrared colours (Papovich+06,Yan+04,Daddi+07) from the GOODS (Great Observatories Origins Deep Survey) fields.

The positions of the 60 GNS pointings were optimised to contain as many massive galaxies as possible and are partly overlapping, covering a total area of about 45 arcmin2. The field of view of the NICMOS-3 camera is 51.2 ?? 51.2 arcsec with a resolution of about 0.1 arcsec/pixel. The PSF has a width of about 0.3 arcsec FWHM. The limiting magnitude in H band reached at 5?? is HAB = 26.8, about 2 magnitudes fainter than in available ground based data of the GOODS fields. [Taken from reference web site.]

Provenance	University of Nottingham, GNS group.
Copyright	Public Domain
Regime	Infrared
NSurvey	1
Frequency	187 THz
Bandpass	167-214 THz
Coverage	About 10% of the GOODS fields or about 3 x 10^-7 of the sky
Resolution	0.3"
PixelScale	0.1"
CoordinateSystem	J2000
Projection	Gnomonic
Epoch	2007-02-14/2008-04-27
Reference	Web site and reference paper

The Hawaii Hubble Deep Field North: Band I

Short name[s] used to specify survey:Hawaii HDF I, Hawaii: HDF I

Description
The Hawaii-HDF-N is an intensive multi-color imaging survey of 0.2 sq. degrees centered on the HDF-N. Data were collected on the NOAO 4m Mayall telescope, the National Astronomical Observatory of Japan 8.2m Subaru telescope and the University of Hawaii 2.2m telescope. Deep U, B, V, R, I, and z' data were obtained over the whole field and deep HK' data over the Chandra Deep Field North. Details are available in the references. [Adapted from reference web site.]

Two different images are given in the V band (V0201 and V0401) from observations separated by about a month that had substantial differences in seeing.

Provenance	Data downloaded from the reference web site. A formatting error in the FITS files was corrected.
Copyright	Public Domain. Users are requested to include a reference to Capak, et al. 2004 when using these data.
Regime	Infrared
NSurvey	8
Frequency	375 THz
Bandpass	358-395 THz
Coverage	0.000005
Resolution	0.67-1.26"
PixelScale	0.3"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	1999/2002
Reference	2004AJ....127..180C or the web site.

The Hawaii Hubble Deep Field North: Band Z

Short name[s] used to specify survey:Hawaii HDF Z, Hawaii: HDF Z

Two different images are given in the V band (V0201 and V0401) from observations separated by about a month that had substantial differences in seeing.

Provenance	Data downloaded from the reference web site. A formatting error in the FITS files was corrected.
Copyright	Public Domain. Users are requested to include a reference to Capak, et al. 2004 when using these data.
Regime	Infrared
NSurvey	8
Frequency	330 THz
Bandpass	317-345 THz
Coverage	0.000005
Resolution	0.67-1.26"
PixelScale	0.3"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	1999/2002
Reference	2004AJ....127..180C or the web site.

VLT ISAAC Ks Observations of the Southern Hubble Ultradeep Field

Short name[s] used to specify survey:HUDFISAAC, HUDF: VLT ISAAC Ks

Description
A very deep Ks observation of the Hubble Ultradeep Field. This observation is approximately 0.6 magnitudes deeper than the GOODS ISAAC Ks image but covers only small fraction of the area.

Regime	Infrared
Frequency	137 THz
Bandwidth	125-150 THz
Provenance	Data downloaded from VLT archive
Copyright	Data freely available
NSurvey	1
Resolution	0.3-0.6"
PixelSize	0.15"
CoordinateSystem	ICRS
Projection	Gnomonic
PixelUnits	ADU/s
Reference	Paper and Web site

IRAS Sky Survey Atlas: 100 micron

Short name[s] used to specify survey: IRAS100, IRAS 100 micron, IRAS 100, IRAS 100

Description
The IRAS data include all data distributed as part of the IRAS Sky Survey Atlas. Data from the four IRAS bands are shown as individual surveys in SkyView. Users should be aware that IPAC does not encourage the use of data near the ecliptic plane as they feel that contribution from local cirrus emission is significant.

The data are distributed in sets of 430 maps. Each map covers approximately 12.5x12.5 degrees, and the map centers are offset by 5 degrees so that there is a 2.5 degree overlap. IPAC has processed to a uniform standard so that excellent mosaics of the maps can be made. Users should be cautious of data in saturated regions. Known problems in the analysis mean that data values are unlikely to be correct. Note that IPAC has optimized the processing of these data for features of 5' or more although the resolution of the data is closer to the 1.5' pixel size.

There are occasional pixels in the IRAS maps which are given as NULL values. Unless these are explicitly trapped by user software, these data will appear as large negative values. SkyView ignores these pixels when determining the color scale to display an image.

Essentially the entire sky is covered by the survey. However there are a few regions not surveyed and the data values in these regions are suspect. These are given to users as delivered from IPAC.

Provenance	NASA IPAC/Jet Propulsion Laboratory
Copyright	Public Domain
Regime	Infrared
NSurvey	4
Frequency	3 THz
Bandpass	2.5-3.6 THz
Coverage	All-sky
PixelScale	0.025 deg/pix
Units	MJy/sr
Resolution	2'
Coordinates	Equatorial
Projection	Gnomonic(TAN)
Equinox	1950
Epoch	1983
Reference	Infrared Astronomical Satellite (IRAS) Explanatory Supplement

IRAS Sky Survey Atlas: 12 micron

Short name[s] used to specify survey: IRAS12, IRAS 12 micron, IRAS 12, IRAS 12

Essentially the entire sky is covered by the survey. However there are a few regions not surveyed and the data values in these regions are suspect. These are given to users as delivered from IPAC.

Provenance	NASA IPAC/Jet Propulsion Laboratory
Copyright	Public Domain
Regime	Infrared
NSurvey	4
Frequency	25 THz
Bandpass	20-35 THz
Coverage	All-sky
PixelScale	0.025 deg/pix
Units	MJy/sr
Resolution	2'
Coordinates	Equatorial
Projection	Gnomonic(TAN)
Equinox	1950
Epoch	1983
Reference	Infrared Astronomical Satellite (IRAS) Explanatory Supplement

IRAS Sky Survey Atlas: 25 micron

Short name[s] used to specify survey: IRAS25, IRAS 25 micron, IRAS 25, IRAS 25

Essentially the entire sky is covered by the survey. However there are a few regions not surveyed and the data values in these regions are suspect. These are given to users as delivered from IPAC.

Provenance	NASA IPAC/Jet Propulsion Laboratory
Copyright	Public Domain
Regime	Infrared
NSurvey	4
Frequency	12 THz
Bandpass	10-15.8 THz
Coverage	All-sky
PixelScale	0.025 deg/pix
Units	MJy/sr
Resolution	2'
Coordinates	Equatorial
Projection	Gnomonic(TAN)
Equinox	1950
Epoch	1983
Reference	Infrared Astronomical Satellite (IRAS) Explanatory Supplement

IRAS Sky Survey Atlas: 60 micron

Short name[s] used to specify survey: IRAS60, IRAS 60 micron, IRAS 60, IRAS 60

Essentially the entire sky is covered by the survey. However there are a few regions not surveyed and the data values in these regions are suspect. These are given to users as delivered from IPAC.

Provenance	NASA IPAC/Jet Propulsion Laboratory
Copyright	Public Domain
Regime	Infrared
NSurvey	4
Frequency	5 THz
Bandpass	3.75-6.5 THz
Coverage	All-sky
PixelScale	0.025 deg/pix
Units	MJy/sr
Resolution	2'
Coordinates	Equatorial
Projection	Gnomonic(TAN)
Equinox	1950
Epoch	1983
Reference	Infrared Astronomical Satellite (IRAS) Explanatory Supplement

Improved Reprocessing of the IRAS Survey: 100

Short name[s] used to specify survey: IRIS100, IRIS 100 micron,IRIS 100, IRIS 100

Description
The IRIS data is a reprocessing of the IRAS data set and has the same geometry as the IRAS Sky Survey Atlas (ISSA, labeled as IRAS nnn micron in SkyView) surveys. This new generation of IRAS images, called IRIS, benefits from a better zodiacal light subtraction, from a calibration and zero level compatible with DIRBE, and from a better destriping. At 100 micron the IRIS product is also a significant improvement from the Schlegel et al. (1998) maps. IRIS keeps the full ISSA resolution, it includes well calibrated point sources and the diffuse emission calibration at scales smaller than 1 degree was corrected for the variation of the IRAS detector responsivity with scale and brightness. The uncertainty on the IRIS calibration and zero level are dominated by the uncertainty on the DIRBE calibration and on the accuracy of the zodiacal light model.

More information about the IRIS dataset is available at the IRIS Web site whence most of the preceding description came.

Provenance	Original IRAS data: NASA/JPL IPAC, IRIS Reprocessing: Canadian Institute for Theoretical Astrophysics/Institut d'Astrophysique Spatiale See the IRIS Web site.
Copyright	Public
Regime	Infrared
NSurvey	4
Frequency	3 THz
Bandpass	2.5-3.6 THz
Coverage	All-sky
PixelScale	0.025 deg/pix
Units	MJy/sr
Resolution	2'
Coordinates	Equatorial
Projection	Gnomonic(TAN)
Equinox	1950
Epoch	1983
Reference	M. Miville-Deschenes and G. Lagache, IRIS: A New Generation of IRAS Maps, Ap.J.Supplement 157, 302, 2005

Improved Reprocessing of the IRAS Survey: 12

Short name[s] used to specify survey: IRIS12, IRIS 12 micron,IRIS 12, IRIS 12

More information about the IRIS dataset is available at the IRIS Web site whence most of the preceding description came.

Provenance	Original IRAS data: NASA/JPL IPAC, IRIS Reprocessing: Canadian Institute for Theoretical Astrophysics/Institut d'Astrophysique Spatiale See the IRIS Web site.
Copyright	Public
Regime	Infrared
NSurvey	4
Frequency	25 THz
Bandpass	20-35 THz
Coverage	All-sky
PixelScale	0.025 deg/pix
Units	MJy/sr
Resolution	2'
Coordinates	Equatorial
Projection	Gnomonic(TAN)
Equinox	1950
Epoch	1983
Reference	M. Miville-Deschenes and G. Lagache, IRIS: A New Generation of IRAS Maps, Ap.J.Supplement 157, 302, 2005

Improved Reprocessing of the IRAS Survey: 25

Short name[s] used to specify survey: IRIS25, IRIS 25 micron,IRIS 25, IRIS 25

More information about the IRIS dataset is available at the IRIS Web site whence most of the preceding description came.

Provenance	Original IRAS data: NASA/JPL IPAC, IRIS Reprocessing: Canadian Institute for Theoretical Astrophysics/Institut d'Astrophysique Spatiale See the IRIS Web site.
Copyright	Public
Regime	Infrared
NSurvey	4
Frequency	12 THz
Bandpass	10-15.8 THz
Coverage	All-sky
PixelScale	0.025 deg/pix
Units	MJy/sr
Resolution	2'
Coordinates	Equatorial
Projection	Gnomonic(TAN)
Equinox	1950
Epoch	1983
Reference	M. Miville-Deschenes and G. Lagache, IRIS: A New Generation of IRAS Maps, Ap.J.Supplement 157, 302, 2005

Improved Reprocessing of the IRAS Survey: 60

Short name[s] used to specify survey: IRIS60, IRIS 60 micron,IRIS 60, IRIS 60

More information about the IRIS dataset is available at the IRIS Web site whence most of the preceding description came.

Provenance	Original IRAS data: NASA/JPL IPAC, IRIS Reprocessing: Canadian Institute for Theoretical Astrophysics/Institut d'Astrophysique Spatiale See the IRIS Web site.
Copyright	Public
Regime	Infrared
NSurvey	4
Frequency	5 THz
Bandpass	3.75-6.5 THz
Coverage	All-sky
PixelScale	0.025 deg/pix
Units	MJy/sr
Resolution	2'
Coordinates	Equatorial
Projection	Gnomonic(TAN)
Equinox	1950
Epoch	1983
Reference	M. Miville-Deschenes and G. Lagache, IRIS: A New Generation of IRAS Maps, Ap.J.Supplement 157, 302, 2005

Schlegel, Finkbeiner and Davis 100 Micron survey

Short name[s] used to specify survey: SFD100m,SFD 100m, SFD 100 Micron

Description
The full sky 100 micron map is a reprocessed composite of the COBE/DIRBE and IRAS/ISSA maps, with the zodiacal foreground and confirmed point sources removed. Artifacts from the IRAS scan pattern were removed. The result of these manipulations is a map with DIRBE-quality calibration and IR AS resolution.

Provenance	David J. Schlegel, Douglas P. Finkbeiner and Marc Davis, Princeton University and University of California, Berkeley
Copyright	Public domain
Regime	Infrared
Frequency	3 THz
Bandpass	2.519 - 3.612 THz
Coverage	All-sky
PixelScale	2.4'/pixel
PixelUnits	MJy/sr MegaJanskies per steradian (100 micron map) and E(B-V) reddening (Dust map)
Resolution	6' full-width half-maximum
Coordinates	Galactic
Projection	Zenith Equal Area
Equinox	2000
Epoch	1983
Reference	David J. Schlegel, Douglas P. Finkbeiner, & Marc Davis , 1998, Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds (ADS). See also Dirbe/IRAS Dust Maps

Schlegel, Finkbeiner and Davis dust map survey

Short name[s] used to specify survey: SFDdust,SFD dust, SFD dust map

Provenance	David J. Schlegel, Douglas P. Finkbeiner and Marc Davis, Princeton University and University of California, Berkeley
Copyright	Public domain
Regime	Infrared
Frequency	3 THz
Bandpass	2.519 - 3.612 THz
Coverage	All-sky
PixelScale	2.4'/pixel
PixelUnits	E(B-V) MegaJanskies per steradian (100 micron map) and E(B-V) reddening (Dust map)
Resolution	6' full-width half-maximum
Coordinates	Galactic
Projection	Zenith Equal Area
Equinox	2000
Epoch	1983
Reference	David J. Schlegel, Douglas P. Finkbeiner, & Marc Davis , 1998, Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds (ADS). See also Dirbe/IRAS Dust Maps

UKIRT Infrared Deep Survey H-band

Short name[s] used to specify survey:UKIDSS-H,UKIDSSH,UKIDSS H

Description
The UKIDSS survey is the next generation infrared survey, a successor to 2MASS. It will ultimately cover 7000 square degrees in the northern sky at both high and low Galactic latitudes and goes about three magnitudes deeper than 2MASS in the coverage area. Most data is taken in the J, H and K bands. A Y band is available in some regions.

UKIDSS is comprised of several distinct surveys in different regions of the sky. Of primary interest to SkyView users (since they have the largest sky coverage) are the Large Area Survey, the Galactic Plane Survey, and the Galactic Clusters Survey. There are deep and ultadeep surveys which cover much smaller fractions of the sky. The planned coverage for the UKIDSS surveys may be seen at the UKIDSS survey page. All UKIDSS data products are published by the Wide-Field Astronomy Unit (WFAU) at the University of Edinburgh through the WFCAM Science Archive (WSA) which includes more detailed coverage information for each data release.

SkyView currently uses the DR8 data release except for the Galactic Plane Survey region where the DR7 is the latest public release. Many thanks to the WSA team at WFAU for providing an interface to make all the latest data easily accessed. Note that coverage is not uniform across the different bands so that at a given point there might be H and K band data, but nothing in the J band.

Provenance	UKIDSS Project
Copyright	The UKIDSS team requests that text similar to the following be included when UKIDSS data is used: The UKIDSS project is defined in Lawrence et al (2007). UKIDSS uses the UKIRT Wide Field Camera (WFCAM; Hewett et al (2006), and the calibration is described in Hodgkin et al. (2009). The pipeline processing and science archive are described in Irwin et al (2009, in prep) and Hambly et al (2008).
Regime	Infrared
NSurvey	4
Frequency	184 THz
Bandpass	168-201 THz
Coverage	0.17 (7000 square degrees
PixelScale	0.4"
PixelUnits
Resolution	1"
Coordinates	Equatorial
Projection	Zenithal Polynomial
Epoch	2005-2012
Reference	See the UKIDSS web site or Lawrence et al (2007).

UKIRT Infrared Deep Survey J-band

Short name[s] used to specify survey:UKIDSS-J,UKIDSSJ,UKIDSS J

Provenance	UKIDSS Project
Copyright	The UKIDSS team requests that text similar to the following be included when UKIDSS data is used: The UKIDSS project is defined in Lawrence et al (2007). UKIDSS uses the UKIRT Wide Field Camera (WFCAM; Hewett et al (2006), and the calibration is described in Hodgkin et al. (2009). The pipeline processing and science archive are described in Irwin et al (2009, in prep) and Hambly et al (2008).
Regime	Infrared
NSurvey	4
Frequency	240 THz
Bandpass	225-260 THz
Coverage	0.17 (7000 square degrees
PixelScale	0.4"
PixelUnits
Resolution	1"
Coordinates	Equatorial
Projection	Zenithal Polynomial
Epoch	2005-2012
Reference	See the UKIDSS web site or Lawrence et al (2007).

UKIRT Infrared Deep Survey K-band

Short name[s] used to specify survey:UKIDSS-K,UKIDSSK,UKIDSS K

Provenance	UKIDSS Project
Copyright	The UKIDSS team requests that text similar to the following be included when UKIDSS data is used: The UKIDSS project is defined in Lawrence et al (2007). UKIDSS uses the UKIRT Wide Field Camera (WFCAM; Hewett et al (2006), and the calibration is described in Hodgkin et al. (2009). The pipeline processing and science archive are described in Irwin et al (2009, in prep) and Hambly et al (2008).
Regime	Infrared
NSurvey	4
Frequency	136 THz
Bandpass	126-148 THz
Coverage	0.17 (7000 square degrees
PixelScale	0.4"
PixelUnits
Resolution	1"
Coordinates	Equatorial
Projection	Zenithal Polynomial
Epoch	2005-2012
Reference	See the UKIDSS web site or Lawrence et al (2007).

UKIRT Infrared Deep Survey Y-band

Short name[s] used to specify survey:UKIDSS-Y,UKIDSSY,UKIDSS Y

Provenance	UKIDSS Project
Copyright	The UKIDSS team requests that text similar to the following be included when UKIDSS data is used: The UKIDSS project is defined in Lawrence et al (2007). UKIDSS uses the UKIRT Wide Field Camera (WFCAM; Hewett et al (2006), and the calibration is described in Hodgkin et al. (2009). The pipeline processing and science archive are described in Irwin et al (2009, in prep) and Hambly et al (2008).
Regime	Infrared
NSurvey	4
Frequency	290 THz
Bandpass	280-310 THz
Coverage	0.17 (7000 square degrees
PixelScale	0.4"
PixelUnits
Resolution	1"
Coordinates	Equatorial
Projection	Zenithal Polynomial
Epoch	2005-2012
Reference	See the UKIDSS web site or Lawrence et al (2007).

HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band H

Short name[s] used to specify survey:UltraVista-H

Description
UltraVISTA is an Ultra Deep, near-infrared survey with the new VISTA surveys telescope of the European Southern Observatory (ESO). Over the course of 5 years, UltraVISTA will repeatedly image the COSMOS field in 5 bands covering a 1.5deg^2 field.\n \nESO acknowledgment: Data products from observations made with ESO Telescopes at the La Silla Paranal Observatories under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.

This survey description was generated automatically from the HiPS property file

Provenance	Origin unknown
Copyright	ULTRAVISTA consortium -
Regime	Infrared
NSurvey	5
Coverage	4.527 x 10^-5 (near J2000 coordinates: [150., 1.58])
Resolution
PixelScale	Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	see McCracken et al. 2012A&A...544A.156M
Epoch

HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band J

Short name[s] used to specify survey:UltraVista-J

This survey description was generated automatically from the HiPS property file

Provenance	Origin unknown
Copyright	ULTRAVISTA consortium -
Regime	Infrared
NSurvey	5
Coverage	4.516 x 10^-5 (near J2000 coordinates: [150., 1.58])
Resolution
PixelScale	Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	see McCracken et al. 2012A&A...544A.156M
Epoch

HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band Ks

Short name[s] used to specify survey:UltraVista-Ks

This survey description was generated automatically from the HiPS property file

Provenance	Origin unknown
Copyright	ULTRAVISTA consortium -
Regime	Infrared
NSurvey	5
Coverage	4.523 x 10^-5 (near J2000 coordinates: [150., 1.58])
Resolution
PixelScale	Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	see McCracken et al. 2012A&A...544A.156M
Epoch

HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band NB118

Short name[s] used to specify survey:UltraVista-NB118

This survey description was generated automatically from the HiPS property file

Provenance	Origin unknown
Copyright	ULTRAVISTA consortium -
Regime	Infrared
NSurvey	5
Coverage	2.891 x 10^-5 (near J2000 coordinates: [150., 1.58])
Resolution
PixelScale	Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	see McCracken et al. 2012A&A...544A.156M
Epoch

HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band Y

Short name[s] used to specify survey:UltraVista-Y

This survey description was generated automatically from the HiPS property file

Provenance	Origin unknown
Copyright	ULTRAVISTA consortium -
Regime	Infrared
NSurvey	5
Coverage	4.513 x 10^-5 (near J2000 coordinates: [150., 1.58])
Resolution
PixelScale	Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	see McCracken et al. 2012A&A...544A.156M
Epoch

WISE 3.4 Micron All-Sky Survey>: All-WISE data release

Short name[s] used to specify survey:Wise W1,Wise 3.4, WiseW1, Wise3.4

Description
From the WISE mission site:.

NASA's Wide-field Infrared Survey Explorer (WISE) mapped the sky at 3.4, 4.6, 12 and 22 micrometers in 2010 with an angular resolution of 6.1", 6.4", 6.5" and 12.0" in the four bands. WISE achieved a 5 sigma point source sensitivities better and 0.08, 0.11 1 and 6 mJy in unconfused regions on the ecliptic in the four bands. Sensitivity improves toward the ecliptic poles due to denser coverage and lower zodaical background.

The WISE All-WISE includes all data taking during the WISE full cryogenic phase, from January 7, 2010 to August 6, 2010, that were processed with improved calibrations and reduction algorithms and combines this with the NEOWISE postcryogenic survey to form the most comprehensive view of the full mid-infrared sky. bibcode=1995ApJ...451..564V,2010ApJ...713..912W

SkyView includes the four WISE bands as separate surveys. Many non-image data products are available at the WISE site. Note that WISE data is distributed in relatively large (>50 MB) image files. When SkyView generates an image for a part of the sky where it has not yet cached the data from the IPAC server there may be a delay as full tiles are downloaded even when only a small fraction of a tile is needed. Images in cached regions, are generated much faster. Access to the WISE data uses the VO SIA interface maintained at IPAC. Even when data is cached, the SIA service must still be available for successful queries.

Provenance	WISE Archive (IRSA/IPAC)
Copyright	WISE data is in the public domain but publications are requested to include the statment: This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.
Regime	Infrared
NSurvey	4
Frequency	88 THz (3.4 micrometers)
Bandpass	78-107 THz
Coverage	All sky
PixelScale	1.375"
PixelUnits	DN
Resolution	6.1"
Coordinates	Equatorial
Projection	Sine
Epoch	January 2010 to February 2011
Reference	The main All-Sky survey is described in Wright et al (2010) The NEOWISE data is discussed in Mainzer et al.

WISE 4.6 Micron All-Sky Survey>: All-WISE data release

Short name[s] used to specify survey:Wise W2,Wise 4.6, WiseW2, Wise4.6

Description
From the WISE mission site:.

Provenance	WISE Archive (IRSA/IPAC)
Copyright	WISE data is in the public domain but publications are requested to include the statment: This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.
Regime	Infrared
NSurvey	4
Frequency	65 THz (4.6 micrometers)
Bandpass	58-74 THz
Coverage	All sky
PixelScale	1.375"
PixelUnits	DN
Resolution	6.4"
Coordinates	Equatorial
Projection	Sine
Epoch	January 2010 to February 2011
Reference	The main All-Sky survey is described in Wright et al (2010) The NEOWISE data is discussed in Mainzer et al.

WISE 12 Micron All-Sky Survey>: All-WISE data release

Short name[s] used to specify survey:Wise W3,Wise 12, WiseW3, Wise12

Description
From the WISE mission site:.

Provenance	WISE Archive (IRSA/IPAC)
Copyright	WISE data is in the public domain but publications are requested to include the statment: This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.
Regime	Infrared
NSurvey	4
Frequency	25 THz (12 micrometers)
Bandpass	18-40 THz
Coverage	All sky
PixelScale	1.375"
PixelUnits	DN
Resolution	6.5"
Coordinates	Equatorial
Projection	Sine
Epoch	January 2010 to February 2011
Reference	The main All-Sky survey is described in Wright et al (2010) The NEOWISE data is discussed in Mainzer et al.

WISE 22 Micron All-Sky Survey>: All-WISE data release

Short name[s] used to specify survey:Wise W4,Wise 22, WiseW4, Wise22

Description
From the WISE mission site:.

Provenance	WISE Archive (IRSA/IPAC)
Copyright	WISE data is in the public domain but publications are requested to include the statment: This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.
Regime	Infrared
NSurvey	4
Frequency	14 THz (22 micrometers)
Bandpass	12-15 THz
Coverage	All sky
PixelScale	1.375"
PixelUnits	DN
Resolution	12"
Coordinates	Equatorial
Projection	Sine
Epoch	January 2010 to February 2011
Reference	The main All-Sky survey is described in Wright et al (2010) The NEOWISE data is discussed in Mainzer et al.

WMAP Nine Year K-Band

Short name[s] used to specify survey:WMAPK,WMAP K,WMAP-K

Description
These data represent the 9 year co-added maps for each of the five frequency bands in the WMAP dataset. The original data are available at the LAMBDA archive.

Provenance	WMAP Mission/LAMBDA archive
Copyright	Public Domain
Regime	Infrared
NSurvey	1
Frequency	23 GHz
Bandpass	19-25 GHz
Coverage	AllSky
PixelScale	7.5'
PixelUnits	millikelvins
Resolution	0.91 degrees
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2000-2009
Reference	LAMBDA archive or Nine year results

WMAP Nine Year Ka-Band

Short name[s] used to specify survey:WMAPKa,WMAP Ka,WMAP-Ka

Description
These data represent the 9 year co-added maps for each of the five frequency bands in the WMAP dataset. The original data are available at the LAMBDA archive.

Provenance	WMAP Mission/LAMBDA archive
Copyright	Public Domain
Regime	Infrared
NSurvey	1
Frequency	33 GHz
Bandpass	29-37 GHz
Coverage	AllSky
PixelScale	7.5'
PixelUnits	millikelvins
Resolution	0.69 degrees
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2000-2009
Reference	LAMBDA archive or Nine year results

WMAP Nine Year Q-Band

Short name[s] used to specify survey:WMAPQ,WMAP Q,WMAP-Q

Description
These data represent the 9 year co-added maps for each of the five frequency bands in the WMAP dataset. The original data are available at the LAMBDA archive.

Provenance	WMAP Mission/LAMBDA archive
Copyright	Public Domain
Regime	Infrared
NSurvey	1
Frequency	40 GHz
Bandpass	35-45 GHz
Coverage	AllSky
PixelScale	7.5'
PixelUnits	millikelvins
Resolution	0.54 degrees
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2000-2009
Reference	LAMBDA archive or Nine year results

WMAP Nine Year V-Band

Short name[s] used to specify survey:WMAPV,WMAP V,WMAP-V

Description
These data represent the 9 year co-added maps for each of the five frequency bands in the WMAP dataset. The original data are available at the LAMBDA archive.

Provenance	WMAP Mission/LAMBDA archive
Copyright	Public Domain
Regime	Infrared
NSurvey	1
Frequency	61 GHz
Bandpass	54-68 GHz
Coverage	AllSky
PixelScale	7.5'
PixelUnits	millikelvins
Resolution	0.37 degrees
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2000-2009
Reference	LAMBDA archive or Nine year results

WMAP Nine Year W-Band

Short name[s] used to specify survey:WMAPW,WMAP W,WMAP-W

Description
These data represent the 9 year co-added maps for each of the five frequency bands in the WMAP dataset. The original data are available at the LAMBDA archive.

Provenance	WMAP Mission/LAMBDA archive
Copyright	Public Domain
Regime	Infrared
NSurvey	1
Frequency	94 GHz
Bandpass	84-104 GHz
Coverage	AllSky
PixelScale	7.5'
PixelUnits	millikelvins
Resolution	0.26 degrees
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2000-2009
Reference	LAMBDA archive or Nine year results

WMAP Nine Year Galaxy Removed

Short name[s] used to specify survey:WMAPILC,WMAP ILC,WMAP

Description
These survey represents a combination of the 9-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body.

The original data are available at the LAMBDA archive.

Provenance	WMAP Mission/LAMBDA archive
Copyright	Public Domain
Regime	Infrared
NSurvey	1
Frequency	23-200 GHz
Coverage	AllSky
PixelScale	7.5'
PixelUnits	millikelvins
Resolution	0.88 degree beam size
CoordinateSystem	Galactic
Projection	HEALPix
Epoch	2000-2009
Reference	LAMBDA archive or Seven year results

Optical surveys

HIPS Survey:CFHTLS D g

Short name[s] used to specify survey:CFHTLS-D-g

Description
The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at prime focus of the 3.6m CFH telescope during the period 2003-2008. The Deep survey concerns 4 patchsof 1 square-degree. All will be observed in u,g,r,i and z, with very lon gexposure time

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	647.3 THz
Coverage	1.044E-4
Resolution
PixelScale	2.795E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

HIPS Survey:CFHTLS D i

Short name[s] used to specify survey:CFHTLS-D-i

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	401.5 THz
Coverage	1.044E-4
Resolution
PixelScale	2.795E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

HIPS Survey:CFHTLS D r

Short name[s] used to specify survey:CFHTLS-D-r

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	486.7 THz
Coverage	1.044E-4
Resolution
PixelScale	2.795E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

HIPS Survey:CFHTLS D u

Short name[s] used to specify survey:CFHTLS-D-u

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	803.0 THz
Coverage	1.044E-4
Resolution
PixelScale	2.795E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

HIPS Survey:CFHTLS D z

Short name[s] used to specify survey:CFHTLS-D-z

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	337.3 THz
Coverage	1.044E-4
Resolution
PixelScale	2.795E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

HIPS Survey:CFHTLS W g

Short name[s] used to specify survey:CFHTLS-W-g

Description
The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at prime focus of the 3.6m CFH telescope during the period 2003-2008. The WIDE survey concerns 4 patchs, 3 of about 7x7 square-degrees each and 1 of about 4x4 square-degrees. All will be observed in u,g,r,i and z, with about 1 hr exposure time per filter

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	647.3 THz
Coverage	0.003731
Resolution
PixelScale	5.591E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

HIPS Survey:CFHTLS W i

Short name[s] used to specify survey:CFHTLS-W-i

Description
The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at prime focus of the 3.6m CFH telescope during the period 2003-2008. The WIDE survey concerns 4 patchs, 3 of about 7x7 square-degrees each and 1 of about 4x4 square-degrees. All will be observed in u,g,r,i and z, with about 1 hr exposure time per filter

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	401.5 THz
Coverage	0.003731
Resolution
PixelScale	5.591E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

HIPS Survey:CFHTLS W r

Short name[s] used to specify survey:CFHTLS-W-r

Description
The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at prime focus of the 3.6m CFH telescope during the period 2003-2008. The WIDE survey concerns 4 patchs, 3 of about 7x7 square-degrees each and 1 of about 4x4 square-degrees. All will be observed in u,g,r,i and z, with about 1 hr exposure time per filter

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	486.7 THz
Coverage	0.003731
Resolution
PixelScale	5.591E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

HIPS Survey:CFHTLS W u

Short name[s] used to specify survey:CFHTLS-W-u

Description
The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at prime focus of the 3.6m CFH telescope during the period 2003-2008. The WIDE survey concerns 4 patchs, 3 of about 7x7 square-degrees each and 1 of about 4x4 square-degrees. All will be observed in u,g,r,i and z, with about 1 hr exposure time per filter

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	803.0 THz
Coverage	0.003731
Resolution
PixelScale	5.591E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

HIPS Survey:CFHTLS W z

Short name[s] used to specify survey:CFHTLS-W-z

Description
The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at prime focus of the 3.6m CFH telescope during the period 2003-2008. The WIDE survey concerns 4 patchs, 3 of about 7x7 square-degrees each and 1 of about 4x4 square-degrees. All will be observed in u,g,r,i and z, with about 1 hr exposure time per filter

This survey description was generated automatically from the HiPS property file

Provenance	CFHT HiPS generated by CDS
Copyright	(c) CFH - powered by Terapix - healpixed by CDS The CFHT Science Archive contains data and meta-data provided by the Canada-France-Hawaii Telescope
Regime	Optical
NSurvey	5
Frequency	337.3 THz
Coverage	0.003731
Resolution
PixelScale	5.591E-5 Hierarchical
PixelUnits
Coordinates	Equatorial
Projection	HEALPix/HiPS
Reference	2012yCat.2317....0H, Also
Epoch	2006-06-01 to 2009-01-01

Original Digitized Sky Survey

Short name[s] used to specify survey:DSSOld,Digitized Sky Survey,DSS

Description
This survey comprises the compressed digitization of the Southern Sky Survey and the Palomar Sky Survey E plates as distributed on CD ROM by the Space Telescope Science Institute. Coverage of the entire sky is included. This survey consists of the digititized Southern Sky Survey conducted at the UK Southern Schmidt Survey Group by the Royal Observatory, Edinburgh (prior to 1988) and the Anglo-Australian Observatory (since 1988) Additional plates covering regions with bright objects are also included. The plates were digitized at the Space Telescope Science Institute and compressed using algorithms developed by R.White. These data are distributed on a set of 101 CD-ROMs.

The following data are included:

Southern hemisphere: SERC Southern Sky Survey and the SERC J Equatorial extension. These are typically deep, 3600s, IIIa-J exposures with a GG395 filter. Also included are 94 short (1200s) V exposures typically at Galactic latitudes below 15°. Special exposures are included in the regions of the Magellenic clouds.
Northern hemisphere: The northern hemisphere is covered by 644 plates from the POSS E survey. A special exposure of the M31 region that is distributed on the CD ROMs is not used in SkyView .

Provenance	Data taken by ROE and AAO, CalTech, Compression and distribution by Space Telescope Science Institute.
Copyright	STScI, ROE, AAO, UK-PPARC, CalTech, National Geographic Society. Full copyright notice
Regime	Optical
NSurvey	1
Frequency	560 THz (Different plates have different bands: J or E with a few exceptions)
Bandpass	422-965 THz (individual plates have smaller bandpass)
Coverage	All-sky
PixelScale	1.7"
Units	Scaled densities
Resolution	Depends on plate. Typically 2"
Coordinates	Equatorial
Projection	Schmidt (distorted Tangent plane projection)
Equinox	2000
Epoch	1945-1958 north, 1980-1999 south
Reference	Lasker, et al., 1990, A.J. 99 Characteristics of the DSS surveys are summarized in this document.

First Digitized Sky Survey: Blue Plates

Short name[s] used to specify survey: DSS1B,DSS1 Blue

Description
This survey uses the POSS1 Blue plates.

Provenance	Data taken by CalTech, Compression and distribution by Space Telescope Science Institute.
Copyright	STScI, CalTech, National Geographic Society. Full copyright notice
Regime	Optical
NSurvey	1
Frequency	638 THz
Bandpass	517-967 THz
Coverage	North of -30 degrees declination
PixelScale	1.7"
Units	Scaled densities
Resolution	Depends on plate. Typically 2"
Coordinates	Equatorial
Projection	Schmidt (distorted Tangent plane projection)
Equinox	2000
Epoch	1975-1988
Reference	Lasker, et al., 1990, A.J. 99

First Digitized Sky Survey: Red Plates

Short name[s] used to specify survey:DSS1R,DSS1 Red

Description
This survey is the POSS1 Red plates from the original POSS survey. It covers the sky north of -30 degrees declination.

Provenance	Data taken by CalTech Compression and distribution by Space Telescope Science Institute.
Copyright	CalTech, National Geographic Society. Full copyright notice
Regime	Optical
NSurvey	1
Frequency	461 THz
Bandpass	437-491 THz
Coverage	North of -30 degrees declination
PixelScale	1.7"
Units	Scaled densities
Resolution	Depends on plate. Typically 2"
Coordinates	Equatorial
Projection	Schmidt (distorted Tangent plane projection)
Equinox	2000
Epoch	1945-1958
Reference	Lasker, et al., 1990, A.J. 99 Characteristics of the DSS surveys are summarized in this document.

2nd Digitized Sky Survey (Blue)

Short name[s] used to specify survey:DSS2B, DSS2 Blue

Description

The native projection of these data is described as a high-order polynomial distortion of a gnomonic projection using the same terms as the DSS.

Provenance	Data taken by ROE, AAO, and CalTech, Compression and distribution by Space Telescope Science Institute.
Copyright	There are multiple copyright holders depending upon the source plate or plates. See full copyright notices The coverage link below describes the coverage for each element of the surveys when the original plate used is not included in the SkyView files.
Regime	Optical
NSurvey	1
Frequency	637 THz
Bandpass	517-967 THz
Coverage	All-sky, but some data not yet be processed.
PixelScale	1" in the north 1.7" in the south
PixelUnits	Pixel values are given as scaled densities
Resolution	Depends on plate. Typically better than 2".
Coordinates	Equatorial
Projection	Schmidt
Equinox	2000
Epoch	1950-1998
Reference	Some information on the DSS2 is given in McLean, 2000, The Second Generation Guide Star Catalog. Characteristics of the DSS surveys are summarized in this document.

2nd Digitized Sky Survey (Red)

Short name[s] used to specify survey:DSS2R, DSS2 Red

Description
This survey comprises the POSS2 Red data from the north and rescanned 1" scans of UKSTU red data in the south.

The native projection of these data is described as a high-order polynomial distortion of a gnomonic projection using the same terms as the DSS.

Provenance	Data taken by ROE, AAO, and CalTech, Compression and distribution by Space Telescope Science Institute.
Copyright	There are multiple copyright holders depending upon the source plate or plates. See full copyright notices The coverage link below describes the coverage for each element of the surveys when the original plate used is not included in the SkyView files.
Regime	Optical
NSurvey	1
Frequency	445 THz
Bandpass	422-564 THz
Coverage	All-sky, but some data not yet be processed.
PixelScale	1"
PixelUnits	Pixel values are given as scaled densities
Resolution	Depends on plate. Typically 3".
Coordinates	Equatorial
Projection	Schmidt
Equinox	2000
Epoch	1984-1999
Reference	Some information on the DSS2 is given in McLean, 2000, The Second Generation Guide Star Catalog. Characteristics of the DSS surveys are summarized in this document.

GOODS HST ACS B Filter

Short name[s] used to specify survey:GOODS ACS B,GOODS: HST ACS B,GOODS_ACS_B

Description
This is a SkyView rendering of the HST ACS data as described in the release document. This comprises four bands of observations of each both the north and south GOODS regions.

These data are stored in SkyView as a hierarchical image with 7 levels of pixels, each with a factor of 2 change in scale. Thus the coarsest sampling using pixels 64 times larger than the finest. As we go to coarser pixels, 4 adjacent pixels forming a square are averaged to create the pixel in the next level. The coarsest pixel scale that is at least the resolution requested is used.

The exposure times are given as: 7200

GOODS ACS exposure (s)

Band North> South
z850 24760 18232

i775 8530 7028

V606 5650 5450

B435
7200

Provenance	Created by the GOODS team and distributed by MAST
Copyright	Public domain
Regime	Optical
NSurvey	4
Frequency	6.93 x 10¹⁴
Bandpass	6.70-7.17 x 10¹⁴
Coverage	GOODS regions (0.01% of sky)
PixelScale	0.03"
PixelUnits	Counts (of electrons)
Resolution	0.1"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2002-07-04/2005-04-14
Reference	GOODS Version 2.0 HST ACS Imaging Data

GOODS HST ACS I Filter

Short name[s] used to specify survey:GOODS ACS I,GOODS: HST ACS I,GOODS_ACS_I

Description
This is a SkyView rendering of the HST ACS data as described in the release document. This comprises four bands of observations of each both the north and south GOODS regions.

The exposure times are given as: 7200

GOODS ACS exposure (s)

Band North> South
z850 24760 18232

i775 8530 7028

V606 5650 5450

B435
7200

Provenance	Created by the GOODS team and distributed by MAST
Copyright	Public domain
Regime	Optical
NSurvey	4
Frequency	3.90 x 10¹⁴
Bandpass	3.79-4.01 x 10¹⁴
Coverage	GOODS regions (0.01% of sky)
PixelScale	0.03"
PixelUnits	Counts (of electrons)
Resolution	0.1"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2002-07-04/2005-04-14
Reference	GOODS Version 2.0 HST ACS Imaging Data

GOODS HST ACS V Filter

Short name[s] used to specify survey:GOODS ACS V,GOODS: HST ACS V,GOODS_ACS_V

Description
This is a SkyView rendering of the HST ACS data as described in the release document. This comprises four bands of observations of each both the north and south GOODS regions.

The exposure times are given as: 7200

GOODS ACS exposure (s)

Band North> South
z850 24760 18232

i775 8530 7028

V606 5650 5450

B435
7200

Provenance	Created by the GOODS team and distributed by MAST
Copyright	Public domain
Regime	Optical
NSurvey	4
Frequency	5.06 x 10¹⁴
Bandpass	4.79-5.37 x 10¹⁴
Coverage	GOODS regions (0.01% of sky)
PixelScale	0.03"
PixelUnits	Counts (of electrons)
Resolution	0.1"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2002-07-04/2005-04-14
Reference	GOODS Version 2.0 HST ACS Imaging Data

GOODS HST ACS Z Filter

Short name[s] used to specify survey:GOODS ACS Z,GOODS: HST ACS Z,GOODS_ACS_Z

Description
This is a SkyView rendering of the HST ACS data as described in the release document. This comprises four bands of observations of each both the north and south GOODS regions.

The exposure times are given as: 7200

GOODS ACS exposure (s)

Band North> South
z850 24760 18232

i775 8530 7028

V606 5650 5450

B435
7200

Provenance	Created by the GOODS team and distributed by MAST
Copyright	Public domain
Regime	Optical
NSurvey	4
Frequency	3.32 x 10¹⁴
Bandpass	3.22-3.42 x 10¹⁴
Coverage	GOODS regions (0.01% of sky)
PixelScale	0.03"
PixelUnits	Counts (of electrons)
Resolution	0.1"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	2002-07-04/2005-04-14
Reference	GOODS Version 2.0 HST ACS Imaging Data

Southern GOODS Field: VLT VIMOS Observations, R band

Short name[s] used to specify survey:GOODS VIMOS R, GOODS: VLT VIMOS R

Description
As part of the Great Observatories Origins Deep Survey (GOODS), deep imaging in the Chandra Deep Field South (CDF-S) has been carried out, using the VIMOS instrument mounted at the Melipal Unit Telescope of the VLT at ESO's Cerro Paranal Observatory, Chile.

This data release contains the coadded images in U band from the ESO large programme 168.A-0485 (P.I. C. Cesarsky) which have been obtained in service mode observations between August 2004 and fall 2006. The 1-sigma depth for VIMOS U band in the area covered by the GOODS-ACS observations is ~30 AB (within an aperture of 1" radius, ranging from 29.5 and 30.2 AB). The PSF of the VIMOS U band mosaic is ~0.8" FWHM, but varies over the field.

Also included in this data release is a coadded image in R band obtained from data retrieved from the ESO archive. Due to the different observing strategies adopted in the programmes the resulting coverage of the GOODS-ACS area is more complex than for the U band. The depth of the VIMOS R band mosaic over the ACS area ranges from ~28 AB to 29 AB (1-sigma, 1" aperture radius). The PSF of the VIMOS R band mosaic is ~0".7 FWHM and varies over the field. [Adapted from reference web site.]

Regime	Optical
Frequency	455 THz
Bandwidth	412-509 THz
Provenance	Data downloaded from VLT archive
Copyright	Data freely available from ESO archive. When using data products provided in this release, acknowledgement should be given in the text to the ESO/GOODS programme, referring to the publication Nonino et al. 2009. In addition, please also use the following statement in your articles when using these data: "Based on observations made with ESO Telescopes at the La Silla or Paranal Observatories under programme number 168.A-0485."
NSurvey	2
Resolution	0.7-0.8"
PixelSize	0.2"
CoordinateSystem	ICRS
Projection	Gnomonic
PixelUnits	ADU/s
Epoch	2004-8-11 to 2006-10-27
Reference	Paper and web site.>

H-alpha Full Sky Map

Short name[s] used to specify survey:HAlpha,HALPHA/Comp,H-Alpha Comp,H-Alpha Composite,H-alpha

Description
The full-sky H-alpha map (6' FWHM resolution) is a composite of the Virginia Tech Spectral line Survey (VTSS) in the north and the Southern H-Alpha Sky Survey Atlas (SHASSA) in the south. Stellar artifacts and bleed trails have been carefully removed from these maps. The Wisconsin H-Alpha Mapper (WHAM) survey provides a stable zero-point over 3/4 of the sky on a one degree scale. This composite map can be used to provide limits on thermal bremsstrahlung (free-free emission) from ionized gas known to contaminate microwave-background data. The map (in Rayleighs; 1R=10⁶/4pi photons/cm²/s/sr), an error map, and a bitmask are provided in 8640x4320 Cartesian projections as well as HEALPIX (Nside 256, 512, and 1024) projections on the H-Alpha Full-Sky Map web site.

Copyright	Public domain
Regime	Optical
Frequency	456.79 THz
Bandpass	456.2-457.38 THz
Coverage	All-sky
PixelScale	2.5'
PixelUnits	Rayleighs (R)
Resolution	6' FWHM
Coordinates	Galactic
Equinox	2000
Projection	Rectangular
Epoch	1997 to 2002
Reference	"A Full-Sky H-alpha Template for Microwave Foreground Prediction" Douglas P. Finkbeiner 2003. This paper may be downloaded from ADS.

The Hawaii Hubble Deep Field North: Band B

Short name[s] used to specify survey:Hawaii HDF B, Hawaii: HDF B

Two different images are given in the V band (V0201 and V0401) from observations separated by about a month that had substantial differences in seeing.

Provenance	Data downloaded from the reference web site. A formatting error in the FITS files was corrected.
Copyright	Public Domain. Users are requested to include a reference to Capak, et al. 2004 when using these data.
Regime	Optical
NSurvey	8
Frequency	677 THz
Bandpass	632-728 THz
Coverage	0.000005
Resolution	0.67-1.26"
PixelScale	0.3"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	1999/2002
Reference	2004AJ....127..180C or the web site.

The Hawaii Hubble Deep Field North: Band R

Short name[s] used to specify survey:Hawaii HDF R, Hawaii: HDF R

Two different images are given in the V band (V0201 and V0401) from observations separated by about a month that had substantial differences in seeing.

Provenance	Data downloaded from the reference web site. A formatting error in the FITS files was corrected.
Copyright	Public Domain. Users are requested to include a reference to Capak, et al. 2004 when using these data.
Regime	Optical
NSurvey	8
Frequency	458 THz
Bandpass	436-484 THz
Coverage	0.000005
Resolution	0.67-1.26"
PixelScale	0.3"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	1999/2002
Reference	2004AJ....127..180C or the web site.

The Hawaii Hubble Deep Field North: Band V0201

Short name[s] used to specify survey:Hawaii HDF V0201, Hawaii: HDF V0201

Two different images are given in the V band (V0201 and V0401) from observations separated by about a month that had substantial differences in seeing.

Provenance	Data downloaded from the reference web site. A formatting error in the FITS files was corrected.
Copyright	Public Domain. Users are requested to include a reference to Capak, et al. 2004 when using these data.
Regime	Optical
NSurvey	8
Frequency	547 THz
Bandpass	520-577 THz
Coverage	0.000005
Resolution	0.67-1.26"
PixelScale	0.3"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	1999/2002
Reference	2004AJ....127..180C or the web site.

The Hawaii Hubble Deep Field North: Band V0401

Short name[s] used to specify survey:Hawaii HDF V0401, Hawaii: HDF V0401

Two different images are given in the V band (V0201 and V0401) from observations separated by about a month that had substantial differences in seeing.

Provenance	Data downloaded from the reference web site. A formatting error in the FITS files was corrected.
Copyright	Public Domain. Users are requested to include a reference to Capak, et al. 2004 when using these data.
Regime	Optical
NSurvey	8
Frequency	547 THz
Bandpass	520-577 THz
Coverage	0.000005
Resolution	0.67-1.26"
PixelScale	0.3"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	1999/2002
Reference	2004AJ....127..180C or the web site.

Mellinger All Sky Mosaic: Blue

Short name[s] used to specify survey:Mellinger-B,Mell-B,Mellinger Blue

Description
This all sky mosaic was created by Axel Mellinger and is used in SkyView with his permission. A fuller description is available at the survey web site.

Between October 2007 and August 2009 a digital all-sky mosaic was assembled from more than 3000 individual CCD frames. Using an SBIG STL-11000 camera, 70 fields (each covering 40x27 degrees) were imaged from dark-sky locations in South Africa, Texas and Michigan. In order to increase the dynamic range beyond the 16 bits of the camera's analog-to-digital converter (of which approximately 12 bits provide data above the noise leve) three different exposure times (240s, 15s and 0.5 s) were used. Five frames were taken for each exposure time and filter setting. The frames were photometrically calibrated using standard catalog stars and sky background data from the Pioneer 10 and 11 space probes. the panorama has an image scale of 36"/pixel and a limiting magnitude of approximately 14. The survey has an 18 bit dynamic range.

The processing of these data used a custom data pipeline built using IRAF, Source Extractor and SWarp.

The data used here were converted to three independent RGB color planes of 8 bits each and provided to SkyView as a single 36000x18000x3 Cartesian projection cube. To allow users to efficiently sample data in a region of the sky, this cube was broken up into 2100x2100 pixel regions with a 50 pixel overlap between adjacent images. Tiles at the poles were 2100x2050.

In SkyView each color plane comprises a survey. The individual planes may be sampled as surveys independently as Mellinger-R, Mellinger-G and Mellinger-B. The color mosaics can be regenerated by creating an RGB image of all three surveys. Since SkyView may stretch the intensity values within each color, linear scaling and a minimum of 0 and maximum of 255 should be specified to keep the original intensity scalings.

The full spatial resolution data is used for images of less than 30 degrees on a side. If a user requests a larger region, data are sampled from a lower resolution 3600x1800x3 data cube. Please contact the survey author if you need to use the higher resolution data for larger regions. The Mellinger survey is only available in SkyView through the Web site. SkyView-in-a-Jar cannot access the underlying data.

Provenance	Axel Mellinger
Copyright	Axel Mellinger. Permission is granted for use in research and personal, non-commercial use. Please contact Axel Mellinger for permission for other use. Survey web site
Regime	Optical
NSurvey	3
Frequency	475 THz
Bandpass	446-535 THz
Coverage	All-sky
PixelSize	0.01 deg/pix
Units	Byte-scaled intensity
Resolution	0.02
Coordinates	Galactic
Projection	Cartesian
Equinox	2000
Epoch	2008-10 to 2009-04
Reference	PASP 121, 1180, 2009 Survey web site.

Mellinger All Sky Mosaic: Green

Short name[s] used to specify survey:Mellinger-G,Mell-G,Mellinger Green

Description
This all sky mosaic was created by Axel Mellinger and is used in SkyView with his permission. A fuller description is available at the survey web site.

The processing of these data used a custom data pipeline built using IRAF, Source Extractor and SWarp.

Provenance	Axel Mellinger
Copyright	Axel Mellinger. Permission is granted for use in research and personal, non-commercial use. Please contact Axel Mellinger for permission for other use. Survey web site
Regime	Optical
NSurvey	3
Frequency	566 THz
Bandpass	491-631 THz
Coverage	All-sky
PixelSize	0.01 deg/pix
Units	Byte-scaled intensity
Resolution	0.02
Coordinates	Galactic
Projection	Cartesian
Equinox	2000
Epoch	2008-10 to 2009-04
Reference	PASP 121, 1180, 2009 Survey web site.

Mellinger All Sky Mosaic: Red

Short name[s] used to specify survey:Mellinger-R,Mell-R,Mellinger Red

Description
This all sky mosaic was created by Axel Mellinger and is used in SkyView with his permission. A fuller description is available at the survey web site.

The processing of these data used a custom data pipeline built using IRAF, Source Extractor and SWarp.

Provenance	Axel Mellinger
Copyright	Axel Mellinger. Permission is granted for use in research and personal, non-commercial use. Please contact Axel Mellinger for permission for other use. Survey web site
Regime	Optical
NSurvey	3
Frequency	697 THz
Bandpass	576-788 THz
Coverage	All-sky
PixelSize	0.01 deg/pix
Units	Byte-scaled intensity
Resolution	0.02
Coordinates	Galactic
Projection	Cartesian
Equinox	2000
Epoch	2008-10 to 2009-04
Reference	PASP 121, 1180, 2009 Survey web site.

Near-Earth Asteriod Tracking System Archive

Short name[s] used to specify survey:NEAT, NEAT/SkyMorph

Description
The NEAT/SkyMorph survey provides access to the archives of the Near Earth Asteroid Tracking (NEAT) project. NEAT is designed to look for potentially hazardous asteroids, i.e., those whose orbits cross the Earth's. Over 200,000 images are available in the NEAT archive. SkyMorph provides a Web interface to the NEAT images and allows users to select all images in which a given fixed or moving object is found.

Unlike most SkyView surveys, the NEAT data are extremely irregular in their spatial distribution. SkyView's algorithms for mosaicking images together to form large images are not adequate for the NEAT data, so mosaicking is surpressed. Only data within a single NEAT image will be displayed. The system attempts to find the most recent image within which has a offset in both RA and Dec of less than 0.8 degrees. If no such image is found, then an image with the minimum offset is returned, or the search may fail altogether if there are no nearby plates. The NEAT telescope uses an array of 4 CCDs. The backgrounds of the CCDs may differ significantly.

The NEAT survey covers approximately 30% of the sky. Extreme southern and low-Galactic latitude regions are unsurveyed. Coverage is otherwise particularly dense in the ecliptic plane.

NEAT data consists primarily of groups of three images taken with separations of 20 minutes and almost identical positions. SkyView will normally return the last of a 'triplet'. The SkyMorph site can be used to display an overlay of triplets to look for targets which moved during the interval between images.

A catalog of objects detected in the NEAT/SkyMorph pages is accessible through the SkyMorph pages. 'Light-curves' from all images during which an object was in the NEAT field of view can also be generated.

The NEAT data values are in arbitrary density units. To enhance the display data are transformed such that all pixels below the median values are scaled linearly to values 0-20, while all pixels above the median are shifted (but not scaled) to values greater than 20.

Provenance	NEAT project
Copyright	See the JPL Image Use Policy
Regime	Optical
NSurvey	1
Frequency	500 THz
Bandpass	374-750 THz
Coverage	Patches of the sky, approximately 30% coverage
PixelScale	1.42"
PixelUnits
Resolution	Depends on image. Typically 3"
Coordinates	Equatorial
Equinox	2000
Projection	Radially distorted gnomonic
Epoch	1995-2006
Reference	href=http://adsabs.harvard.edu/abs/1999AJ...117.1616P> Pravdo, et al. 1999 (ADS)

Sloan Digital Sky Survey g-band

Short name[s] used to specify survey:SDSSg,SDSS g

Description
The Sloan Digital Sky Survey is the deepest large scale survey of the sky currently available. SkyView dynamically queries the SDSS archive (currently release DR9) to retrieve information and resample it into the user requested frame. Further information on the SDSS and many additional services are available at the SDSS Web site.

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	646 THz
Bandpass	567-750 THz
Coverage	14,555 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	1998 to 2011
Reference	Sloan Digital Sky Survey web site or ADS

Sloan Digital Sky Survey i-band

Short name[s] used to specify survey:SDSSi,SDSS i

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	403 THz
Bandpass	372-439 THz
Coverage	14,555 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	1998 to 2011
Reference	Sloan Digital Sky Survey web site or ADS

Sloan Digital Sky Survey r-band

Short name[s] used to specify survey:SDSSr,SDSS r

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	490 THz
Bandpass	448-540 THz
Coverage	14,555 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	1998 to 2011
Reference	Sloan Digital Sky Survey web site or ADS

Sloan Digital Sky Survey u-band

Short name[s] used to specify survey:SDSSu,SDSS u

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	834 THz
Bandpass	772-934 THz
Coverage	14,555 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	1998 to 2011
Reference	Sloan Digital Sky Survey web site or ADS

Sloan Digital Sky Survey z-band

Short name[s] used to specify survey:SDSSz,SDSS z

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	337 THz
Bandpass	327-348 THz
Coverage	14,555 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	1998 to 2011
Reference	Sloan Digital Sky Survey web site or ADS

Sloan Digital Sky Survey g-band DR7

Short name[s] used to specify survey:SDSSdr7g,SDSSdr7 g

Description
The Sloan Digital Sky Survey is the deepest large scale survey of the sky currently available. SkyView dynamically queries the SDSS archive to retrieve information and resample it into the user requested frame. Further information on the SDSS and many additional services are available at the SDSS Web site.

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	646 THz
Bandpass	567-750 THz
Coverage	9,583 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits	ADUs
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	ca. 2000
Reference	Sloan Digital Sky Survey web site

Sloan Digital Sky Survey i-band DR7

Short name[s] used to specify survey:SDSSdr7i,SDSSdr7 i

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	403 THz
Bandpass	372-439 THz
Coverage	9,583 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits	ADUs
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	ca. 2000
Reference	Sloan Digital Sky Survey web site

Sloan Digital Sky Survey r-band DR7

Short name[s] used to specify survey:SDSSdr7r,SDSSdr7 r

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	490 THz
Bandpass	448-540 THz
Coverage	9,583 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits	ADUs
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	ca. 2000
Reference	Sloan Digital Sky Survey web site

Sloan Digital Sky Survey u-band DR7

Short name[s] used to specify survey:SDSSdr7u,SDSSdr7 u

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	834 THz
Bandpass	772-934 THz
Coverage	9,583 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits	ADUs
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	ca. 2000
Reference	Sloan Digital Sky Survey web site

Sloan Digital Sky Survey z-band DR7

Short name[s] used to specify survey:SDSSdr7z,SDSSdr7 z

Provenance	Sloan Digital Sky Survey Team
Copyright	See Sloan usage document for distribution rights and acknowledgements.
Regime	Optical
NSurvey	5
Frequency	337 THz
Bandpass	327-348 THz
Coverage	9,583 square degrees. The SDDS site provides coverage maps
PixelScale	0.4"
PixelUnits	ADUs
Resolution	1"
Coordinates	Equatorial
Projection	Tangent
Epoch	ca. 2000
Reference	Sloan Digital Sky Survey web site

The Southern H-Alpha Sky Survey Atlas: Continuum

Short name[s] used to specify survey:SHASSA-C,SHASSA_C,SHASSA C

Description
The Southern H-Alpha Sky Survey Atlas is the product of a wide-angle digital imaging survey of the H-alpha emission from the warm ionized interstellar gas of our Galaxy. This atlas covers the southern hemisphere sky (declinations less than +15 degrees). The observations were taken with a robotic camera operating at Cerro Tololo Inter-American Observatory (CTIO) in Chile. The atlas consists of 2168 images covering 542 fields. There are four images available for each field: H-alpha, Continuum, Continuum-Corrected (the difference of the H-alpha and Continuum images), and Smoothed (median filtered to 5 pixel, or 4.0 arcminute, resolution to remove star residuals better). The SHASSA web site has more details of the data and the status of this and related projects. Images can also be obtained from the Download Images section at the SHASSA site.

Provenance	John E. Gaustad (Swarthmore College), Peter R. McCullough (University of Illinois), Wayne Rosing (Las Cumbres Observatory), and Dave Van Buren (Extrasolar Research Corporation)
Copyright	Las Cumbres Observatory, Inc. See the Acknowledgement/Guidelines for Use of Images
Regime	Optical
Frequency	457 THz
Bandpass	456-458 THz
Coverage	All-sky south of 15
Resolution	3.2'
PixelScale	0.79'
PixelUnits	decirayleighs (dR) or 10⁵/4pi photons/cm²/s/sr
CoordinateSystem	Equatorial
Projection	Gnomonic
Equinox	2000
Epoch	1997-2000
Reference	"A Robotic Wide-Angle H-alpha Survey of the Southern Sky" by J.E. Gaustad, P.R. McCullough, W. Rosing, and D. Van Buren 2001, PASP, 113, 1326. This paper may be downloaded in PDF (2.5 Mb) or Postscript (12.7 Mb) format. or ADS

The Southern H-Alpha Sky Survey Atlas: Continuum-Corrected

Short name[s] used to specify survey:SHASSA-CC,SHASSA_CC,SHASSA CC

Provenance	John E. Gaustad (Swarthmore College), Peter R. McCullough (University of Illinois), Wayne Rosing (Las Cumbres Observatory), and Dave Van Buren (Extrasolar Research Corporation)
Copyright	Las Cumbres Observatory, Inc. See the Acknowledgement/Guidelines for Use of Images
Regime	Optical
Frequency	457 THz
Bandpass	456-458 THz
Coverage	All-sky south of 15
Resolution	3.2'
PixelScale	0.79'
PixelUnits	decirayleighs (dR) or 10⁵/4pi photons/cm²/s/sr
CoordinateSystem	Equatorial
Projection	Gnomonic
Equinox	2000
Epoch	1997-2000
Reference	"A Robotic Wide-Angle H-alpha Survey of the Southern Sky" by J.E. Gaustad, P.R. McCullough, W. Rosing, and D. Van Buren 2001, PASP, 113, 1326. This paper may be downloaded in PDF (2.5 Mb) or Postscript (12.7 Mb) format. or ADS

The Southern H-Alpha Sky Survey Atlas: H-Alpha

Short name[s] used to specify survey:SHASSA-H,SHASSA_H,SHASSA H

Provenance	John E. Gaustad (Swarthmore College), Peter R. McCullough (University of Illinois), Wayne Rosing (Las Cumbres Observatory), and Dave Van Buren (Extrasolar Research Corporation)
Copyright	Las Cumbres Observatory, Inc. See the Acknowledgement/Guidelines for Use of Images
Regime	Optical
Frequency	457 THz
Bandpass	456-458 THz
Coverage	All-sky south of 15
Resolution	3.2'
PixelScale	0.79'
PixelUnits	decirayleighs (dR) or 10⁵/4pi photons/cm²/s/sr
CoordinateSystem	Equatorial
Projection	Gnomonic
Equinox	2000
Epoch	1997-2000
Reference	"A Robotic Wide-Angle H-alpha Survey of the Southern Sky" by J.E. Gaustad, P.R. McCullough, W. Rosing, and D. Van Buren 2001, PASP, 113, 1326. This paper may be downloaded in PDF (2.5 Mb) or Postscript (12.7 Mb) format. or ADS

The Southern H-Alpha Sky Survey Atlas: Smoothed

Short name[s] used to specify survey:SHASSA-Sm,SHASSA_Sm,SHASSA Sm

Provenance	John E. Gaustad (Swarthmore College), Peter R. McCullough (University of Illinois), Wayne Rosing (Las Cumbres Observatory), and Dave Van Buren (Extrasolar Research Corporation)
Copyright	Las Cumbres Observatory, Inc. See the Acknowledgement/Guidelines for Use of Images
Regime	Optical
Frequency	457 THz
Bandpass	456-458 THz
Coverage	All-sky south of 15
Resolution	3.2'
PixelScale	0.79'
PixelUnits	decirayleighs (dR) or 10⁵/4pi photons/cm²/s/sr
CoordinateSystem	Equatorial
Projection	Gnomonic
Equinox	2000
Epoch	1997-2000
Reference	"A Robotic Wide-Angle H-alpha Survey of the Southern Sky" by J.E. Gaustad, P.R. McCullough, W. Rosing, and D. Van Buren 2001, PASP, 113, 1326. This paper may be downloaded in PDF (2.5 Mb) or Postscript (12.7 Mb) format. or ADS

Ultraviolet surveys

Extreme Ultraviolet Explorer: 171 A

Short name[s] used to specify survey:euve171, EUVE 171 A

Description
The EUVE satellite surveyed the entire sky in the extreme ultraviolet through a set of four filters. The filters include:

Lexan/Boron filter: peak at 83A (full range 50-180)
Aluminium/Carbon/Titanium : 171A (160-240)
Aluminium/Titanium/Antimony: 405A (345-605)
Tin/SiO: 555A (500-740)

The data currently in SkyView is direct from the Center for EUVE.

Provenance	Center for Extreme UV Astronomy, UCB
Regime	Ultraviolet
Copyright	Public domain
Frequency	17.3 PHz
Bandpass	8.1-17.6 PHz
PixelScale	0.025 degrees/pixel
PixelUnits	counts
Resolution	ca. 3'
CoordinateSystem	Equatorial
Projection	Gnomonic/Tan
Equinox	2000
Epoch	1992-07 to 1993-01
Reference	Boywer et al 1996 (ADS)

Extreme Ultraviolet Explorer: 405 A

Short name[s] used to specify survey:euve405, EUVE 405 A

Description
The EUVE satellite surveyed the entire sky in the extreme ultraviolet through a set of four filters. The filters include:

Lexan/Boron filter: peak at 83A (full range 50-180)
Aluminium/Carbon/Titanium : 171A (160-240)
Aluminium/Titanium/Antimony: 405A (345-605)
Tin/SiO: 555A (500-740)

The data currently in SkyView is direct from the Center for EUVE.

Provenance	Center for Extreme UV Astronomy, UCB
Regime	Ultraviolet
Copyright	Public domain
Frequency	7.4 PHz
Bandpass	5.0-7.9 PHz
PixelScale	0.025 degrees/pixel
PixelUnits	counts
Resolution	ca. 3'
CoordinateSystem	Equatorial
Projection	Gnomonic/Tan
Equinox	2000
Epoch	1992-07 to 1993-01
Reference	Boywer et al 1996 (ADS)

Extreme Ultraviolet Explorer: 555 A

Short name[s] used to specify survey:euve555, EUVE 555 A

Description
The EUVE satellite surveyed the entire sky in the extreme ultraviolet through a set of four filters. The filters include:

Lexan/Boron filter: peak at 83A (full range 50-180)
Aluminium/Carbon/Titanium : 171A (160-240)
Aluminium/Titanium/Antimony: 405A (345-605)
Tin/SiO: 555A (500-740)

The data currently in SkyView is direct from the Center for EUVE.

Provenance	Center for Extreme UV Astronomy, UCB
Regime	Ultraviolet
Copyright	Public domain
Frequency	5.4 PHz
Bandpass	3.75-6 PHz
PixelScale	0.025 degrees/pixel
PixelUnits	counts
Resolution	ca. 3'
CoordinateSystem	Equatorial
Projection	Gnomonic/Tan
Equinox	2000
Epoch	1992-07 to 1993-01
Reference	Boywer et al 1996 (ADS)

Extreme Ultraviolet Explorer: 83 A

Short name[s] used to specify survey:euve83, EUVE 83 A

Description
The EUVE satellite surveyed the entire sky in the extreme ultraviolet through a set of four filters. The filters include:

Lexan/Boron filter: peak at 83A (full range 50-180)
Aluminium/Carbon/Titanium : 171A (160-240)
Aluminium/Titanium/Antimony: 405A (345-605)
Tin/SiO: 555A (500-740)

The data currently in SkyView is direct from the Center for EUVE.

Provenance	Center for Extreme UV Astronomy, UCB
Regime	Ultraviolet
Copyright	Public domain
Frequency	36 PHz
Bandpass	15-43 PHz
PixelScale	0.025 degrees/pixel
PixelUnits	counts
Resolution	ca. 3'
CoordinateSystem	Equatorial
Projection	Gnomonic/Tan
Equinox	2000
Epoch	1992-07 to 1993-01
Reference	Boywer et al 1996 (ADS)

Galaxy Explorer All Sky Survey: Far UV

Short name[s] used to specify survey:GalexFar,GALEX Far UV

Description
The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682.

The SkyView GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image.

As of February 10, 2011 SkyView uses the GR6 data release for the entire sky.

Provenance	All data is downloaded from the MAST GALEX archive.
Copyright	Public domain.
Regime	Ultraviolet
NSurvey	2
Frequency	1.96 PHz
Bandpass	1.68-2.23 PHz
Coverage	All sky/patchy
PixelScale	1.5"
PixelUnits	Intensity
Resolution	4.3"
Coordinates	Equatorial
Equinox	2000
Projection	Tangent
Epoch	2003 to 2009
Reference	The GALEX Guest Invesitigator and MAST Archive sites provide documentation and characteristics of the GALEX observatory and archive. The technical document provides instrument details.

Galaxy Explorer All Sky Survey: Near UV

Short name[s] used to specify survey: GalexNear,GALEX NEAR UV

As of February 10, 2011, SkyView uses the GALEX GR6 data release.

Provenance	All data is downloaded from the MAST GALEX archive.
Copyright	Public domain.
Regime	Ultraviolet
NSurvey	2
Frequency	1.32 PHz
Bandpass	1.05-1.69 PHz
Coverage	All sky/patchy
PixelScale	1.5"
PixelUnits	Intensity
Resolution	5.3"
Coordinates	Equatorial
Equinox	2000
Projection	Tangent
Epoch	2003 to 2009
Reference	The GALEX Guest Invesitigator and MAST Archive sites provide documentation and characteristics of the GALEX observatory and archive. The technical document provides instrument details.

Southern GOODS Field: VLT VIMOS Observations, U band

Short name[s] used to specify survey:GOODS VIMOS U, GOODS: VLT VIMOS U

Regime	Ultraviolet
Frequency	821 THz
Bandwidth	753-903 THz
Provenance	Data downloaded from VLT archive
Copyright	Data freely available from ESO archive. When using data products provided in this release, acknowledgement should be given in the text to the ESO/GOODS programme, referring to the publication Nonino et al. 2009. In addition, please also use the following statement in your articles when using these data: "Based on observations made with ESO Telescopes at the La Silla or Paranal Observatories under programme number 168.A-0485."
NSurvey	2
Resolution	0.7-0.8"
PixelSize	0.2"
CoordinateSystem	ICRS
Projection	Gnomonic
PixelUnits	ADU/s
Epoch	2004-8-11 to 2006-10-27
Reference	Paper and web site.>

The Hawaii Hubble Deep Field North: Band U

Short name[s] used to specify survey:Hawaii HDF U, Hawaii: HDF U

Two different images are given in the V band (V0201 and V0401) from observations separated by about a month that had substantial differences in seeing.

Provenance	Data downloaded from the reference web site. A formatting error in the FITS files was corrected.
Copyright	Public Domain. Users are requested to include a reference to Capak, et al. 2004 when using these data.
Regime	Ultraviolet
NSurvey	8
Frequency	822 THz
Bandpass	780-868 THz
Coverage	0.000005
Resolution	0.67-1.26"
PixelScale	0.3"
CoordinateSystem	ICRS
Projection	Gnomonic
Epoch	1999/2002
Reference	2004AJ....127..180C or the web site.

Swift UVOT Combined B Counts Images

Short name[s] used to specify survey:UVOTBcnt,UVOT B Counts, SwiftUVOTBcnt

Description
The Swift UVOT instrument is a 30 cm modified Ritchey-Chretien reflecting telescope launched on board the Swift satellite on November 20, 2004. The range of optical and UV filters can accomodate wavebands between 1700 and 6500 Angstroms. A full field image covers 17x17 arcminutes and at maximum spatial sampling is imaged onto 2048x2048 0.5" pixels. A 1000 second observation can detect point sources to m=22.3 when no filter is used. The Swift Serendipitous Source Catalog (Page et al., 2015) detects sources down to m=23-26 for the six filters in very deep observations, but the typical limits are substantially brighter (~20-23 magnitude).

These surveys are mosaics of all Swift UVOT observations released between the start of the mission and July 2017. Data were extracted from the HEASARC archive from the UVOT products directory. Mosaics are provided in six filters and also with no filter, i.e., WHITE. The table below gives the number of observations and bandpasses for each of the filters. For each UVOT observation standard processing generates a counts and exposure file as a single multi-extension FITS file with a separate extension for each filter. To aid processing, these extensions were copied into separate files in directory trees for each filter. Four observations in which the exposure and counts maps did not agree on the filters used were omitted from the processing.

Some observations were recorded with 0.5" pixels while others were binned to 1". All 0.5" observations (typically fewer than 10%) were rebinned to the larger pixels for the counts maps since the counts data scales with the pixel size. Since the exposure values are intensive and do not vary significantly based upon the resolution, these data were not generally rebinned unless it was needed to ensure that Order 9 Hips data were produced.

The CDS Hipsgen software was used to generate Order 9 HiPS data (~0.8" pixels) for both the Counts and Exposure images. The HiPS (Hierarchical Progressive Survey VO standard) supports multi-resolution mosaics. Any quantitative use of these images should note that the rebinning increases the total counts by a factor of ~(1.0/0.8)^2 ~ 1.56. This software uses a bilinear interpolation to generate HEALPix tiles of an appropriate order (18 in this case). SkyView developed software was used to divide the level 9 counts maps tiles by the corresponding exposure maps to create intensity tiles. Pixels where the exposure was less than 5 seconds were left as NaNs. The lower order (8 to 3) order intensity tiles were then generated by averaging 2x2 sets of the higher order maps treating any missing maps or pixels as NaNs. A HiPS all-sky image was generated by averaged the Order 3 tiles.

Only the Intensity HIPS files are presented in the SkyView web page directly, but intensity, counts and exposure maps are available for all seven filters. Note that unlike the XRT HiPS data, the exposure and counts maps have not been clipped. I.e., the source FITS files have been aligned with the coordinate system and thus contain large numbers of unexposed pixels with 0 values. These 0's are simply propogated to HiPS tiles. NaNs are returned in regions which lie outside any of the original source images. For the Intensity map, any pixel for which the exposure was less than 5s is returned as a NaN. < >td>0.0314

Filter Count Central Wavelength (Å) Bandpass (Å) Central Frequency(THz) Bandpass (THz) Coverage

WHITE 3,000 3600 1600-6000 832 500-1874 0.0017

V 30,557 5468 5083-5852 548 512-590 0.0171

B 28,347 4392 3904-4880 683 614-768 0.0112

U 49,954 3465 3072-3875 865 774-975 0.0287

UVW1 60,690 2600 2253-2946 1154 1017-1330 0.0277

UVM2 56,977 2246 1997-2495 1334 1201-1501

UVW2 54,590 1928 1600-2256 1554 1328-1874 0.0260

Observation counts and bandpasses for UVOT Filters

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	865 THz (4392 A)
Bandpass	774-975 THz (3904-4880 ?)
Coverage	Patches over ~0.0112 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined U Counts Images

Short name[s] used to specify survey:UVOTUcnt,UVOT U Counts, SwiftUVOTUcnt

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	865 THz (3465 A)
Bandpass	774-975 THz (3072-3875 ?)
Coverage	Patches over ~0.0287 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined UVM2 Counts Images

Short name[s] used to specify survey:UVOTUVM2cnt,UVOT UVM2 Counts, SwiftUVOTUVM2cnt

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	1334 THz (2246 A)
Bandpass	1200-1500 THz (1997-2495 ?)
Coverage	Patches over ~0.0314 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined UVW1 Counts Images

Short name[s] used to specify survey:UVOTUVW1cnt,UVOT UVW1 Counts, SwiftUVOTUVW1cnt

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	1154 THz (2600 A)
Bandpass	1017-1330 THz (2253-2946 ?)
Coverage	Patches over ~0.0277 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined UVW2 Counts Images

Short name[s] used to specify survey:UVOTUVW2cnt,UVOT UVW2 Counts, SwiftUVOTUVW2cnt

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	1554 THz (1928 A)
Bandpass	1328-1874 THz (1600-2256 ?)
Coverage	Patches over ~0.0260 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined V Counts Images

Short name[s] used to specify survey:UVOTVcnt,UVOT V Counts, SwiftUVOTVcnt

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	548 THz (5468 A)
Bandpass	512-590 THz (5083-5852 ?)
Coverage	Patches over ~0.0171 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined WHITE Counts Images

Short name[s] used to specify survey:UVOTWHITEcnt,UVOT WHITE Counts, SwiftUVOTWHITEcnt

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	832 THz (3600 A)
Bandpass	500-1874 THz (1600-6000 ?)
Coverage	Patches over ~0.0017 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined B Exposure Images

Short name[s] used to specify survey:UVOTBexp,UVOT B Exposure, SwiftUVOTBexp

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	865 THz (4392 A)
Coverage	Patches over ~0.0112 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined U Exposure Images

Short name[s] used to specify survey:UVOTUexp,UVOT U Exposure, SwiftUVOTUexp

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	865 THz (3465 A)
Coverage	Patches over ~0.0287 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined UVM2 Exposure Images

Short name[s] used to specify survey:UVOTUVM2exp,UVOT UVM2 Exposure, SwiftUVOTUVM2exp

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	1334 THz (2246 A)
Coverage	Patches over ~0.0314 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined UVW1 Exposure Images

Short name[s] used to specify survey:UVOTUVW1exp,UVOT UVW1 Exposure, SwiftUVOTUVW1exp

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	1154 THz (2600 A)
Coverage	Patches over ~0.0277 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined UVW2 Exposure Images

Short name[s] used to specify survey:UVOTUVW2exp,UVOT UVW2 Exposure, SwiftUVOTUVW2exp

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	1554 THz ( A)
Coverage	Patches over ~0.0260 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined V Exposure Images

Short name[s] used to specify survey:UVOTVexp,UVOT V Exposure, SwiftUVOTVexp

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	548 THz (5468 A)
Coverage	Patches over ~0.0171 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined WHITE Exposure Images

Short name[s] used to specify survey:UVOTWHITEexp,UVOT WHITE Exposure, SwiftUVOTWHITEexp

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	832 THz (3600 A)
Bandpass	500-1874 THz (1600-6000 ?)
Coverage	Patches over ~0.0017 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined B Intensity Images

Short name[s] used to specify survey:UVOTBint,UVOT B Intensity, SwiftUVOTBint

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	865 THz (4392 A)
Coverage	Patches over ~0.0112 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts/s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined U Intensity Images

Short name[s] used to specify survey:UVOTUint,UVOT U Intensity, SwiftUVOTUint

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	865 THz (3465 A)
Coverage	Patches over ~0.0287 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts/s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined UVM2 Intensity Images

Short name[s] used to specify survey:UVOTUVM2int,UVOT UVM2 Intensity, SwiftUVOTUVM2int

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	1334 THz (2246 A)
Coverage	Patches over ~0.0314 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts/s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined UVW1 Intensity Images

Short name[s] used to specify survey:UVOTUVW1int,UVOT UVW1 Intensity, SwiftUVOTUVW1int

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	1154 THz (2600 A)
Coverage	Patches over ~0.0277 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts/s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined UVW2 Intensity Images

Short name[s] used to specify survey:UVOTUVW2int,UVOT UVW2 Intensity, SwiftUVOTUVW2int

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	1554 THz (1928 A)
Coverage	Patches over ~0.0260 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts/s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined V Intensity Images

Short name[s] used to specify survey:UVOTVint,UVOT V Intensity, SwiftUVOTVint

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	548 THz (5468 A)
Bandpass	512-590 THz (5083-5852 ?)
Coverage	Patches over ~0.0171 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts/s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

Swift UVOT Combined WHITE Intensity Images

Short name[s] used to specify survey:UVOTWHITEint,UVOT WHITE Intensity, SwiftUVOTWHITEint

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	Ultraviolet
NSurvey	21
Frequency	832 THz (3600 A)
Bandpass	500-1874 THz (1600-6000 ?)
Coverage	Patches over ~0.0017 of the sky
PixelScale	0.8" (Highest resolution/Hierarchical)
PixelUnits	Counts/s
Resolution	2.5"
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to July 2017
Reference	Web site

ROSAT Wide Field Camera: F1

Short name[s] used to specify survey:wfcf1, ROSAT WFC F1

Description
This survey is a mosaic of images taken by the ROSAT Wide Field Camera and comprises of 12,743 seperates fields in each of two filters. Each field covers a region 2.6° x 2.6° with a 0.3° overlap. Currently, this data is not a complete coverage of the sky; regions near the northern ecliptic pole are currently not included.

Provenance	University of Leicester
Copyright	University of Leicester used by permission (no restrictions on not for profit use)
Regime	Ultraviolet
NSurvey	2
Frequency	19.3 PHz
Bandpass	15-27 PHz
Coverage	all-sky
PixelScale	1 arcminute/pixel
PixelUnit	Counts
Resolution	3'
Coordinates	Ecliptic
Projection	Gnomonic
Epoch	1990-07 to 1991-01
Reference	ADS

ROSAT Wide Field Camera: F2

Short name[s] used to specify survey:wfcf2, ROSAT WFC F2

Provenance	University of Leicester
Copyright	University of Leicester used by permission (no restrictions on not for profit use)
Regime	Ultraviolet
NSurvey	2
Frequency	30 PHz
Bandpass	21-50 PHz
Coverage	all-sky
PixelScale	1 arcminute/pixel
PixelUnit	Counts
Resolution	3'
Coordinates	Ecliptic
Projection	Gnomonic
Epoch	1990-07 to 1991-01
Reference	ADS

X-ray surveys

Swift BAT 70 Month All-Sky Survey: 14-20 keV: flux

Short name[s] used to specify survey:BAT-flux-1, BAT flux 1, BAT flux 14-20

Description
This BAT Hard X-ray Survey data is the 70-month survey product of the BAT instrument on the Swift observatory. Swift/BAT is a wide field-of-view (70x100 degrees) hard X-ray imager consisting of a coded mask and a large array of CdZnTe detectors (with an effective area of ~ 5000 cm²).

BAT is sensitive in the energy range 14-195 keV. The data are divided into 8 energy bands

Band Energy (keV) Frequency (EHz)

1 14-20 3.38-4.84

2 20-24 4.84-5.80

3 24-35 5.80-8.46

4 35-50 8.46-12.1

5 50-75 12.1-18.1

6 75-100 18.1-24.2

7 100-150 24.2-36.3

8 150-195 36.3-47.2

Sum (SNR only) 14-195 3.38-47.2

Each band is represented as as two separate surveys, a signal-to-noise (SNR) map and a flux map. (e.g., BAT-snr-1 or BAT SNR 1 or BAT SNR 14-20, or BAT-Flux-1, ...). An additional summed survey, BAT-SNR-SUM or BAT SNR SUM or BAT SNR 14-195, is also available, but there is no summed flux survey. In our Web interface only the SNR surveys are shown in the Web form. Users can get flux maps corresponding to a given SNR image from the results pages. The batch interfaces may directly query any of the surveys since the user chooses the names explicitly rather than from a selection box.

The values displayed in the significance maps are the local signal to noise ratio in each pixel. The noise in these coded-mask images follows a Gaussian distribution with center at zero and a characteristic width (sigma) of 1.0. The noise is calculated locally for each pixel by measuring the RMS value of all pixel values in an annulus around each pixel and hence includs both statistical and systematic components. Known sources are excluded from the annuli.

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

While the Swift mission is primarily designed to follow gamma-ray bursts, the random distribution of bursts in the sky means that these survey's sky coverage is relatively uniform with the exposure at any point varying between about 6 to 16 megaseconds. The survey limits for source detection are about 10^-11 ergs/s/cm² over about half the sky and 1.3x10^-11 ergs/s/cm² over 90%.

These data replace the 9-month BAT datasets which we have retired. If you wish access to the older data please let us know. Note that for the 9-month data we provided access through the web page to the flux data and gave links to the signal-to-noise maps. Since the existence of sources is most easily seen in the SNR maps, we decided to invert that for this release.

For the 8 band data, the source data were provided by the BAT team as 6 FITS files. Each of these contained the 8 bands in separate image extensions for a region centered at l=0,b=+/-90 or l=0,90,180,270,b=0, the centers of 6 cubic facets. However these data are not the classical cube-faced projections, e.g., as used in COBE data. The data on the facets overlap, so that this is just a convenient way to tile the sky. SkyView separated each of the FITS image extensions into a separate file, but no other modifications were made to the data. The summed image was provided as six separate files.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	4.04 EHz
Bandpass	3.38-4.84 EHz
Coverage	All-sky
PixelScale	2.8'
PixelUnits	cts/s/det
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 14-20 keV: snr

Short name[s] used to specify survey:BAT-snr-1, BAT snr 1, BAT snr 14-20

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	4.04 EHz
Bandpass	3.38-4.84 EHz
Coverage	All-sky
PixelScale	2.8'
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 20-24 keV: flux

Short name[s] used to specify survey:BAT-flux-2, BAT flux 2, BAT flux 20-24

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	5.29 EHz
Bandpass	4.84-5.80 EHz
Coverage	All-sky
PixelScale	2.8'
PixelUnits	cts/s/det
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 20-24 keV: snr

Short name[s] used to specify survey:BAT-snr-2, BAT snr 2, BAT snr 20-24

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	5.29 EHz
Bandpass	4.84-5.80 EHz
Coverage	All-sky
PixelScale	2.8'
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 24-35 keV: flux

Short name[s] used to specify survey:BAT-flux-3, BAT flux 3, BAT flux 24-35

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	7.00 EHz
Bandpass	5.80-8.46 EHz
Coverage	All-sky
PixelScale	2.8'
PixelUnits	cts/s/det
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 24-35 keV: snr

Short name[s] used to specify survey:BAT-snr-3, BAT snr 3, BAT snr 24-35

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	7.00 EHz
Bandpass	5.80-8.46 EHz
Coverage	All-sky
PixelScale	2.8'
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 35-50 keV: flux

Short name[s] used to specify survey:BAT-flux-4, BAT flux 4, BAT flux 35-50

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	10.1 EHz
Bandpass	8.46-12.1 EHz
Coverage	All-sky
PixelScale	2.8'
PixelUnits	cts/s/det
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 35-50 keV: snr

Short name[s] used to specify survey:BAT-snr-4, BAT snr 4, BAT snr 35-50

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	10.1 EHz
Bandpass	8.46-12.1 EHz
Coverage	All-sky
PixelScale	2.8'
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 50-75 keV: flux

Short name[s] used to specify survey:BAT-flux-5, BAT flux 5, BAT flux 50-75

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	14.8 EHz
Bandpass	12.1-18.1 EHz
Coverage	All-sky
PixelScale	2.8'
PixelUnits	cts/s/det
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 50-75 keV: snr

Short name[s] used to specify survey:BAT-snr-5, BAT snr 5, BAT snr 50-75

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	14.8 EHz
Bandpass	12.1-18.1 EHz
Coverage	All-sky
PixelScale	2.8'
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 75-100 keV: flux

Short name[s] used to specify survey:BAT-flux-6, BAT flux 6, BAT flux 75-100

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	20.9 EHz
Bandpass	18.1-24.2 EHz
Coverage	All-sky
PixelScale	2.8'
PixelUnits	cts/s/det
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 75-100 keV: snr

Short name[s] used to specify survey:BAT-snr-6, BAT snr 6, BAT snr 75-100

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	20.9 EHz
Bandpass	18.1-24.2 EHz
Coverage	All-sky
PixelScale	2.8'
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 100-150 keV: flux

Short name[s] used to specify survey:BAT-flux-7, BAT flux 7, BAT flux 100-150

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	29.6 EHz
Bandpass	24.2-36.3 EHz
Coverage	All-sky
PixelScale	2.8'
PixelUnits	cts/s/det
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 100-150 keV: snr

Short name[s] used to specify survey:BAT-snr-7, BAT snr 7, BAT snr 100-150

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	29.6 EHz
Bandpass	24.2-36.3 EHz
Coverage	All-sky
PixelScale	2.8'
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 150-195 keV: flux

Short name[s] used to specify survey:BAT-flux-8, BAT flux 8, BAT flux 150-195

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	41.4 EHz
Bandpass	36.3-48.2 EHz
Coverage	All-sky
PixelScale	2.8'
PixelUnits	cts/s/det
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 150-195 keV: snr

Short name[s] used to specify survey:BAT-snr-8, BAT snr 8, BAT snr 150-195

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	41.4 EHz
Bandpass	36.3-48.2 EHz
Coverage	All-sky
PixelScale	2.8'
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

Swift BAT 70 Month All-Sky Survey: 14-195 keV: snr

Short name[s] used to specify survey:BAT-snr-sum, BAT snr sum, BAT snr 14-195

The signal in each pixel is taken from the flux maps.

The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10^-7m^2.

Provenance	NASA BAT Team
Copyright	Public domain
Regime	X-ray
NSurvey	9
Frequency	12 EHz
Bandpass	3.38-47.2 EHz
Coverage	All-sky
PixelScale	2.8'
Resolution	20'
Coordinates	Galactic
Equinox
Projection	Zenithal Equal Area
Epoch	2005-2010
Reference	The 70-Month Swift-BAT Hard X-ray Survey, (Baumgartner et al 2013)

GOODS Chandra ACIS: Full band (0.5-8 keV)

Short name[s] used to specify survey:GOODSACISFB,GOODS: Chandra ACIS FB, GOODS ACIS FB

Description
This survey comprises the 2 Ms Chandra Deep Field North and 4 Ms Deep Field South ACIS observations. All observations are co-added into two fields in the north and south. Data are provided in three bands, the soft 0.5-2 keV band, the hard 2.0-8.0 keV and the full 0.5 to 8 keV band.

Provenance	Taken from the Neil Brandt's PSU web sites for the the north and south.
Copyright	Public domain
Regime	X-ray
Frequency	480 PHz
Bandpass	121-1900 PHz
Coverage	Approximately 10.e-5 around two goods regions (roughly 0.4 square degrees)
NSurvey	3
PixelScale	0.5"
PixelUnits	Counts
CoordinateSystem	ICRS
Resolution	1"
Projection	Gnomonic
Epoch	1999/2010
Reference	Published descriptions of the North and South field observations.

GOODS Chandra ACIS: Hard band (2-8 keV)

Short name[s] used to specify survey:GOODSACISHB,GOODS: Chandra ACIS HB, GOODS ACIS HB

Provenance	Taken from the Neil Brandt's PSU web sites for the the north and south.
Copyright	Public domain
Regime	X-ray
Frequency	960 PHz
Bandpass	480-1900 PHz
Coverage	Approximately 10.e-5 around two goods regions (roughly 0.4 square degrees)
NSurvey	3
PixelScale	0.5"
PixelUnits	Counts
CoordinateSystem	ICRS
Resolution	1"
Projection	Gnomonic
Epoch	1999/2010
Reference	Published descriptions of the North and South field observations.

GOODS Chandra ACIS: Soft band (0.5-2 keV)

Short name[s] used to specify survey:GOODSACISSB,GOODS: Chandra ACIS SB, GOODS ACIS SB

Provenance	Taken from the Neil Brandt's PSU web sites for the the north and south.
Copyright	Public domain
Regime	X-ray
Frequency	240 PHz
Bandpass	121-480 PHz
Coverage	Approximately 10.e-5 around two goods regions (roughly 0.4 square degrees)
NSurvey	3
PixelScale	0.5"
PixelUnits	Counts
CoordinateSystem	ICRS
Resolution	1"
Projection	Gnomonic
Epoch	1999/2010
Reference	Published descriptions of the North and South field observations.

GRANAT/SIGMA Flux

Short name[s] used to specify survey:GRANAT_SIGMA_Flux,GRANAT/SIGMA Flux,

Description
The Soviet orbital observatory GRANAT was launched in December 1989 and was operational till November 1998. One of the main instruments of the observatory was the French-Soviet hard X-ray coded mask telescope SIGMA (Paul et al.1 1991, Adv.Space Res., 11, 279). It was the first space telescope that used coded aperture technique for reconstruction of sky images in hard X-rays (35-1300 keV). The angular resolution of the telescope was approximately 12' and the accuracy of a source localization is approximately 2-3'.

SIGMA discovered numerous interesting hard X-ray sources including GRS 1758-258, which is located only 40' from bright soft X-ray source GX 5-1. It detected hard X-ray flux from X-ray burster A1742-294, which is very near to bright black hole binary 1E1740.7-2942. SIGMA set an upper limit on the hard X-ray flux of from the central supermassive black hole in our Galaxy.

During the period 1990-1998 SIGMA observed more that one quarter of the sky with sensitivity better than 100 mCrab. The Galactic Center region had the deepest exposure ( approximately 9 million sec), with the sensitivity to a source discovery (S/N > ~ 5) or approximately 10 mCrab.

A list of all detected sources with references to publications on them is presented in the paper of Revnivtsev et al. 2004, Astr. Lett. v.6. In these survey images (40-100 keV) all performed observations are averaged together. Transient sources that were discovered by SIGMA may not visible in the averaged image.

This survey has some features that users should keep in mind. The SIGMA telescope is a complicated instrument and is strongly dominated by the accuracy of the background subtraction. The presence of a very bright source in the field of view of the telescope sometimes cannot be fully accounted for and as a result of it some 'ghost' sources can appear. Such features can be seen in the regions near very bright sources like Crab Nebula, Cyg X-1, Nova Per 1992, Nova Mus 1991, Nova Oph 1993, and in the Galactic Center region. In addition to its nominal field of view (~17x17 deg) located around the optical axis of the telescope, SIGMA had another window of relatively high transparency of its shield, approximately 20-30° apart from the optical axis. Becuase of this a very bright sources like Cyg X-1 can cause non zero illumination of the SIGMA detector if they are located approximately 20-30° from the optical axis. The ring-like features caused by this effect, can be seen around Cyg X-1, and Nova Per 1992.

The count rate of detected sources (or upper limits) can be roughly translated into mCrab using the fact that that Crab nebula gives the count rate approximately 2.8e^-3 cnts/s in the units, provided in 'flux' maps

Provenance	High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; CEA, Centre d'Etudes de Saclay Orme des Merisiers, France; Centre d'Etude Spatiale des Rayonnements, Toulouse, France; Fédération de Recherche Astroparticule et Cosmologie Université de Paris, France
Copyright	Public Domain
Regime	X-ray
NSurvey	2 (significance and flux)
Frequency	16 EHz
Bandpass	10-24 EHz
Coverage	Approximately one quarter of the sky
PixelScale	3.24 arc minutes/pix
Units	Statistical significance, Flux
Resolution	12 arc minutes
Coordinates	Equatorial
Projection	Gnomonic
Equinox	1950
Epoch	1983-1989
Reference	Hard X-ray sky survey with the SIGMA telescope aboard GRANAT observatory, Revnivtsev M., Sunyaev R., Gilfanov M., Churazov E., Goldwurm A., Paul J., Mandrou P., Roques J.-P., Astronomy Letters 2004, v.30 (ADS)

GRANAT/SIGMA Significance

Short name[s] used to specify survey:GRANAT_SIGMA_Sig,GRANAT/SIGMA Sig, GRANAT/SIGMA

Provenance	High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; CEA, Centre d'Etudes de Saclay Orme des Merisiers, France; Centre d'Etude Spatiale des Rayonnements, Toulouse, France; Fédération de Recherche Astroparticule et Cosmologie Université de Paris, France
Copyright	Public Domain
Regime	X-ray
NSurvey	2 (significance and flux)
Frequency	16 EHz
Bandpass	10-24 EHz
Coverage	Approximately one quarter of the sky
PixelScale	3.24 arc minutes/pix
Units	Statistical significance, Flux
Resolution	12 arc minutes
Coordinates	Equatorial
Projection	Gnomonic
Equinox	1950
Epoch	1983-1989
Reference	Hard X-ray sky survey with the SIGMA telescope aboard GRANAT observatory, Revnivtsev M., Sunyaev R., Gilfanov M., Churazov E., Goldwurm A., Paul J., Mandrou P., Roques J.-P., Astronomy Letters 2004, v.30 (ADS)

HEAO 1A

Short name[s] used to specify survey:HEAO1A, HEAO 1 A-2

Description
These data were generated at the HEASARC in 1994. Certain gaps and streaks in the image have been fixed by interpolating over the the gap. Typically these gaps are no more than a pixel or two wide. A brief description of the satellite and the data analysis follows. The map used in SkyView is the map designated 322_15_tot_ecl_samp.img in the HEASARC FTP area. Many other maps are available. These differ in epoch, resolution, energy band, coordinate system and projection, and sampling methods. Details are given in the README file in the archive.

See Allen, Jahoda, and Whitlock (1994) for full details about the available maps, their processing, and methods for converting the map intensities into familiar physical units.

Provenance	NASA, HEASARC
Copyright	Public domain
Regime	X-ray
Frequency	2.4 EHz
Bandpass	0.48-14.5 EHz
CoordinateSystem	Ecliptic
Projection	Cartesion
PixelScale	0.5x0.25 degrees
Units	Counts/Secont
Coverage	All-sky
NSurvey	1
Resolution	Approxmately 2 degrees
Epoch	1978 to 1979
Reference	Shafer, R.A. 1983, Spatial Fluctuations in the Diffuse X-Ray Background, University of Maryland Ph.D. thesis. Allen, J., Jahoda, K., and Whitlock, L. 1994, HEAO-1 and the A2 experiment, Legacy, 5. also HEAO1

ROSAT High Resolution Image Pointed Observations Mosaic: Intensity

Short name[s] used to specify survey:HRIint, HRI

Description
This survey was generated from all available ROSAT HRI observations. Data were mosaicked into 1.1 degree tiles by SkyView. Exposure maps were generated for each HRI observation using the hriexpmap FTOOL. For each tile, all observations that might contribute to that tile were located and added to count and exposure map tiles. Exposures for each observation were calculated using a nearest neighbor interpolation of the center of the tile pixels to the exposure map pixels. Counts were computed by projecting the RA and Decs of each eligible photon into the appropriate tile pixel. Only photons with a PHA > 3 were included in the mosaic and within each observation only counts within the region where the exposure was greater than half the maximum exposure were included.

Provenance	Data from GSFC and MPE. SkyView mosaic generated by SkyView.
Copyright	Public Domain
Regime	X-ray
NSurvey	1
Frequency	260 PHz
Bandpass	24-480 PHz
Coverage	Observation patches covering ~1.8% of the sky.
PixelScale	5"
PixelUnits
Resolution	10"
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991 to 1999
Reference	The ROSAT High Resolution Imager (HRI) Calibration Report

INTEGRAL/Spectral Imager Galactic Center Survey

Short name[s] used to specify survey:INTEGRALSPI_gc, INTEGRAL/SPI GC

Description
The INTEGRAL observatory (Winkler et al. 2003, A&A, 411, L1) was launched in October 2002. The spectrograph SPI (Vedrenne et al. 2003, A&A, 411, L63) consists of 19 Germanium detectors and is capable of imaging in the 20 - 8000 keV band because of a coded mask. Part of the core program of the INTEGRAL mission is a study of the Galactic Centre, the Galactic Centre Deep Exposure (GCDE).

The SPI significance map is based on the public GCDE data and uses data in the 20 - 40 keV energy range. The analysis of the data was done using the SPIROS software (Skinner & Connell 2003, A&A, 411, L123). This software uses the 'Iterative Removal of Sources' technique in order to find the most significant sources. In the output significance map the sources found in this process are put on top of the residual map as points with a FWHM of 1 degree.

Current data respresent the combination of all public observations as of September 1, 2004.

Provenance	INTEGRAL Science Data Center, Geneva, Switzerland
Copyright	Public Domain
Regime	X-ray
NSurvey	1
Frequency	6.8 EHz
Bandpass	2.9-4.8 EHz
Coverage
PixelScale	6 arc minutes/pix
Units	Statistical significance
Resolution	approximately 1 degree
Coordinates	Galactic
Projection	Aitoff
Epoch	March 2002 - May 2003
Reference	INTEGRAL Guest Observer Facility SPI Reference at (ADS)

Nine Year INTEGRAL IBIS 17-35 keV Galactic Plane Survey: Exposure

Short name[s] used to specify survey:INT GAL 17-35 Exp, INTGAL1735E

Description
This survey combines 9 years of INTEGRAL IBIS observations from December 2002 through January 2011 into a single Galactic Plane image. A total of 135 megaseconds of exposure is included in the observations used. Survey data is generated for the Galactic plane in the region |b| <= 17.5. The original flux data has been convolved with 5' seeing kernel. To minimize loss of resolution in transformations, the Lanczos sampler is suggested as the default, but may be overriden by the user. Both the preconvolved and standard convolved maps are available at the Web site.

The exposure and sensitivity vary considerably over the coverage region, but 90% of the field has a limiting sensitivity better than 2.2 x 10^-11ergs s^-1cm^-2 or about 1.56 mCrab. Further details of the survey construction are given in the reference.

The flux and significance maps use the PSF convolved maps from the survey. The flux maps are in millicrab units. Exposure maps (with exposures in seconds) were from the exposure extension in the MAPDLD files and give the dead-time corrected exposure in seconds.

Links to the exposure and significance maps corresponding to the requested region will be given in the Web output. These maps can be generated directly in the CLI interface. For each waveband the flux, significance and exposure maps are available with just the end of the survey names distinguishing them (e.g., INT Gal 17-35 [Flux|Sig|Exp] or INTGal1735[F|S|E])

Provenance	Krivonos et al., 2012 Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.
Copyright	Space Research Institute (IKI), Moscow, Russia
Regime	X-ray
Frequency	6 EHz
Bandpass	4.4-8.5 EHz
CoordinateSystem	Galactic
Projection	Cartesian
PixelScale	4'
Units	Flux (milliCrabs), Exposure (s) and Significance
Coverage	Galactic plane, \|b\| < 17.5 (30% of the sky)
NSurvey	9 [(Flux,Significance,Exposure) x 3 bands]
Resolution	Gaussian 5'
Epoch	December 2002 to January 2011
Reference	Survey paper: Krivonos et al., 2012 Web site

Nine Year INTEGRAL IBIS 17-35 keV Galactic Plane Survey: Flux

Short name[s] used to specify survey:INT GAL 17-35 Flux, INTGAL1735F

Provenance	Krivonos et al., 2012 Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.
Copyright	Space Research Institute (IKI), Moscow, Russia
Regime	X-ray
Frequency	6 EHz
Bandpass	4.4-8.5 EHz
CoordinateSystem	Galactic
Projection	Cartesian
PixelScale	4'
Units	Flux (milliCrabs), Exposure (s) and Significance
Coverage	Galactic plane, \|b\| < 17.5 (30% of the sky)
NSurvey	9 [(Flux,Significance,Exposure) x 3 bands]
Resolution	Gaussian 5'
Epoch	December 2002 to January 2011
Reference	Survey paper: Krivonos et al., 2012 Web site

Nine Year INTEGRAL IBIS 17-35 keV Galactic Plane Survey: Significance

Short name[s] used to specify survey:INT GAL 17-35 Sig, INTGAL1735S

Provenance	Krivonos et al., 2012 Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.
Copyright	Space Research Institute (IKI), Moscow, Russia
Regime	X-ray
Frequency	6 EHz
Bandpass	4.4-8.5 EHz
CoordinateSystem	Galactic
Projection	Cartesian
PixelScale	4'
Units	Flux (milliCrabs), Exposure (s) and Significance
Coverage	Galactic plane, \|b\| < 17.5 (30% of the sky)
NSurvey	9 [(Flux,Significance,Exposure) x 3 bands]
Resolution	Gaussian 5'
Epoch	December 2002 to January 2011
Reference	Survey paper: Krivonos et al., 2012 Web site

Nine Year INTEGRAL IBIS 17-60 keV Galactic Plane Survey: Exposure

Short name[s] used to specify survey:INT GAL 17-60 Exp, INTGAL1760E

Provenance	Krivonos et al., 2012 Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.
Copyright	Space Research Institute (IKI), Moscow, Russia
Regime	X-ray
Frequency	8 EHz
Bandpass	4.4-14 EHz
CoordinateSystem	Galactic
Projection	Cartesian
PixelScale	4'
Units	Flux (milliCrabs), Exposure (s) and Significance
Coverage	Galactic plane, \|b\| < 17.5 (30% of the sky)
NSurvey	9 [(Flux,Significance,Exposure) x 3 bands]
Resolution	Gaussian 5'
Epoch	December 2002 to January 2011
Reference	Survey paper: Krivonos et al., 2012 Web site

Nine Year INTEGRAL IBIS 17-60 keV Galactic Plane Survey: Flux

Short name[s] used to specify survey:INT GAL 17-60 Flux, INTGAL1760F

Provenance	Krivonos et al., 2012 Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.
Copyright	Space Research Institute (IKI), Moscow, Russia
Regime	X-ray
Frequency	8 EHz
Bandpass	4.4-14 EHz
CoordinateSystem	Galactic
Projection	Cartesian
PixelScale	4'
Units	Flux (milliCrabs), Exposure (s) and Significance
Coverage	Galactic plane, \|b\| < 17.5 (30% of the sky)
NSurvey	9 [(Flux,Significance,Exposure) x 3 bands]
Resolution	Gaussian 5'
Epoch	December 2002 to January 2011
Reference	Survey paper: Krivonos et al., 2012 Web site

Nine Year INTEGRAL IBIS 17-60 keV Galactic Plane Survey: Significance

Short name[s] used to specify survey:INT GAL 17-60 Sig, INTGAL1760S

Provenance	Krivonos et al., 2012 Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.
Copyright	Space Research Institute (IKI), Moscow, Russia
Regime	X-ray
Frequency	8 EHz
Bandpass	4.4-14 EHz
CoordinateSystem	Galactic
Projection	Cartesian
PixelScale	4'
Units	Flux (milliCrabs), Exposure (s) and Significance
Coverage	Galactic plane, \|b\| < 17.5 (30% of the sky)
NSurvey	9 [(Flux,Significance,Exposure) x 3 bands]
Resolution	Gaussian 5'
Epoch	December 2002 to January 2011
Reference	Survey paper: Krivonos et al., 2012 Web site

Nine Year INTEGRAL IBIS 35-80 keV Galactic Plane Survey: Exposure

Short name[s] used to specify survey:INT GAL 35-80 Exp, INTGAL3580E

Provenance	Krivonos et al., 2012 Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.
Copyright	Space Research Institute (IKI), Moscow, Russia
Regime	X-ray
Frequency	12 EHz
Bandpass	7.2-20 EHz
CoordinateSystem	Galactic
Projection	Cartesian
PixelScale	4'
Units	Flux (milliCrabs), Exposure (s) and Significance
Coverage	Galactic plane, \|b\| < 17.5 (30% of the sky)
NSurvey	9 [(Flux,Significance,Exposure) x 3 bands]
Resolution	Gaussian 5'
Epoch	December 2002 to January 2011
Reference	Survey paper: Krivonos et al., 2012 Web site

Nine Year INTEGRAL IBIS 35-80 keV Galactic Plane Survey: Flux

Short name[s] used to specify survey:INT GAL 35-80 Flux, INTGAL3580F

Provenance	Krivonos et al., 2012 Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.
Copyright	Space Research Institute (IKI), Moscow, Russia
Regime	X-ray
Frequency	12 EHz
Bandpass	7.2-20 EHz
CoordinateSystem	Galactic
Projection	Cartesian
PixelScale	4'
Units	Flux (milliCrabs), Exposure (s) and Significance
Coverage	Galactic plane, \|b\| < 17.5 (30% of the sky)
NSurvey	9 [(Flux,Significance,Exposure) x 3 bands]
Resolution	Gaussian 5'
Epoch	December 2002 to January 2011
Reference	Survey paper: Krivonos et al., 2012 Web site

Nine Year INTEGRAL IBIS 35-80 keV Galactic Plane Survey: Significance

Short name[s] used to specify survey:INT GAL 35-80 Sig, INTGAL3580S

Provenance	Krivonos et al., 2012 Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.
Copyright	Space Research Institute (IKI), Moscow, Russia
Regime	X-ray
Frequency	12 EHz
Bandpass	7.2-20 EHz
CoordinateSystem	Galactic
Projection	Cartesian
PixelScale	4'
Units	Flux (milliCrabs), Exposure (s) and Significance
Coverage	Galactic plane, \|b\| < 17.5 (30% of the sky)
NSurvey	9 [(Flux,Significance,Exposure) x 3 bands]
Resolution	Gaussian 5'
Epoch	December 2002 to January 2011
Reference	Survey paper: Krivonos et al., 2012 Web site

PSPC summed pointed observations, 1 degree cutoff, Counts

Short name[s] used to specify survey:PSPC1Cnt, PSPC 1.0 Deg-Cnt, PSPC 1.0 Deg-Counts

Description
The ROSAT PSPC surveys were generated by SkyView as mosaics from publically available PSPC observations. The surveys include all data available through March 1, 1997. This includes the vast majority of ROSAT PSPC observations. Filter observations and observations taken during the verification phase in 1991 were not included in either set. The details of the generation of the surveys are discussed in a companion document. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two.

The smaller cut-offs allow users to distinguish point sources in fields where a bright source may have been towards the edge of one observation and near the center of another. In these cases the source appears fuzzy due to the poor resolution of ROSAT near the edge of the field of view. This comes at the cost of a substantial reduction in the fraction of the sky covered. Counts and exposure maps are included for users who may need this information (e.g., to do statistical analysis).

The global organization of the surveys is similar to the IRAS survey. Each map covers an area of 2.5°x2.5° with a minimum overlap of 0.25°. To cover the entire sky would require over 10,000 maps. However due to lack of coverage only approximately 4000-6000 maps are actually populated. Users asking for reqions where there is no ROSAT coverage may get a blank region returned.

Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document.

Provenance	Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.
Copyright	Public domain
Regime	X-ray
NSurvey	1
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	Isolated pointings in the sky. Total coverage < 14%
PixelScale	15"
PixelUnits	cts/s/pixel
Resolution	30" but variable across the field of view
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991-1994
Reference	ROSAT Mission Description and Data Products Guide, available through the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.

PSPC summed pointed observations, 1 degree cutoff, Exposure

Short name[s] used to specify survey:PSPC1Exp, PSPC 1.0 Deg-Exp, PSPC 1.0 Deg-Expos

Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document.

Provenance	Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.
Copyright	Public domain
Regime	X-ray
NSurvey	1
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	Isolated pointings in the sky. Total coverage < 14%
PixelScale	15"
PixelUnits	cts/s/pixel
Resolution	30" but variable across the field of view
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991-1994
Reference	ROSAT Mission Description and Data Products Guide, available through the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.

PSPC summed pointed observations, 1 degree cutoff, Intensity

Short name[s] used to specify survey:PSPC1Int, PSPC 1.0 Deg-Int, PSPC 1.0 Deg-Inten

Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document.

Provenance	Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.
Copyright	Public domain
Regime	X-ray
NSurvey	1
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	Isolated pointings in the sky. Total coverage < 14%
PixelScale	15"
PixelUnits	cts/s/pixel
Resolution	30" but variable across the field of view
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991-1994
Reference	ROSAT Mission Description and Data Products Guide, available through the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.

PSPC summed pointed observations, 2 degree cutoff, Counts

Short name[s] used to specify survey:PSPC2Cnt, PSPC 2.0 Deg-Cnt, PSPC 2.0 Deg-Counts

Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document.

Provenance	Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.
Copyright	Public domain
Regime	X-ray
NSurvey	1
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	Isolated pointings in the sky. Total coverage < 14%
PixelScale	15"
PixelUnits	cts/s/pixel
Resolution	30" but variable across the field of view
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991-1994
Reference	ROSAT Mission Description and Data Products Guide, available through the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.

PSPC summed pointed observations, 2 degree cutoff, Exposure

Short name[s] used to specify survey:PSPC2Exp, PSPC 2.0 Deg-Exp, PSPC 2.0 Deg-Expos

Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document.

Provenance	Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.
Copyright	Public domain
Regime	X-ray
NSurvey	1
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	Isolated pointings in the sky. Total coverage < 14%
PixelScale	15"
PixelUnits	cts/s/pixel
Resolution	30" but variable across the field of view
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991-1994
Reference	ROSAT Mission Description and Data Products Guide, available through the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.

PSPC summed pointed observations, 2 degree cutoff, Intensity

Short name[s] used to specify survey:PSPC2Int, PSPC 2.0 Deg-Int, PSPC 2.0 Deg-Inten

Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document.

Provenance	Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.
Copyright	Public domain
Regime	X-ray
NSurvey	1
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	Isolated pointings in the sky. Total coverage < 14%
PixelScale	15"
PixelUnits	cts/s/pixel
Resolution	30" but variable across the field of view
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991-1994
Reference	ROSAT Mission Description and Data Products Guide, available through the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.

PSPC summed pointed observations, 0.6 degree cutoff, Counts

Short name[s] used to specify survey:PSPC0.6Cnt, PSPC 0.6 Deg-Cnt, PSPC 0.6 Deg-Counts

Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document.

Provenance	Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.
Copyright	Public domain
Regime	X-ray
NSurvey	1
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	Isolated pointings in the sky. Total coverage < 14%
PixelScale	15"
PixelUnits	cts/s/pixel
Resolution	30" but variable across the field of view
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991-1994
Reference	ROSAT Mission Description and Data Products Guide, available through the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.

PSPC summed pointed observations, 0.6 degree cutoff, Exposure

Short name[s] used to specify survey:PSPC0.6Exp, PSPC 0.6 Deg-Exp, PSPC 0.6 Deg-Expos

Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document.

Provenance	Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.
Copyright	Public domain
Regime	X-ray
NSurvey	1
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	Isolated pointings in the sky. Total coverage < 14%
PixelScale	15"
PixelUnits	cts/s/pixel
Resolution	30" but variable across the field of view
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991-1994
Reference	ROSAT Mission Description and Data Products Guide, available through the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.

PSPC summed pointed observations, 0.6 degree cutoff, Intensity

Short name[s] used to specify survey:PSPC0.6Int, PSPC 0.6 Deg-Int, PSPC 0.6 Deg-Inten

Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document.

Provenance	Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.
Copyright	Public domain
Regime	X-ray
NSurvey	1
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	Isolated pointings in the sky. Total coverage < 14%
PixelScale	15"
PixelUnits	cts/s/pixel
Resolution	30" but variable across the field of view
Coordinates	Equatorial
Equinox	2000
Projection	Gnomonic
Epoch	1991-1994
Reference	ROSAT Mission Description and Data Products Guide, available through the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.

ROSAT All-Sky X-ray Survey Hard Band: Counts

Short name[s] used to specify survey:RASShbC, RASSCnt hb, RASS-Cnt Hard ,RASS Hard, RASS3hb, RASShb

Description
The ROSAT All-Sky X-ray Survey was obtained during 1990/1991 using the ROSAT Position Sensitive Proportional Counter (PSPC) in combination with the ROSAT X-ray Telescope (XRT). More than 60,000 X-ray sources were detected during this time.

SkyView has multiple surveys derived from the RASS data. The surveys whose RASS are counts and exposure maps from the survey. Previously The RASSBCK maps have had the point sources removed to show the diffuse X-ray background and are presended at lower resolution.

The full-resolution RASS surveys data are organized in 1378 fields each 6.4° x 6.4° covering the whole sky. Neighboring fields overlap by at least 0.23°.

Three bands are available through SkyView

broad band (0.1-2.4 keV)
hard band (0.5-2.0 keV)
soft band (0.1-0.4 keV)

Data was dowloaded from the MPE FTP site.

The intensity maps are created from the exposure maps using the single exposure map available which is appropriate for the broad band images, so the intensities of the hard and soft bands are only approximate.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPE but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	240 PHz
Bandpass	120-480 PHz
Coverage	All-sky
PixelScale	45"
PixelUnits	Counts,Flux
Resolution
Coordinates	Equatorial
Equinox
Projection	Gnomonic
Epoch	1990-07 to 1991-02, 1991-98
Reference	The ROSAT All-Sky Survey (ADS)

ROSAT All-Sky X-ray Survey Broad Band: Counts

Short name[s] used to specify survey:RASSbbC, RASSCnt bb, RASS-Cnt Broad ,RASS Broad, RASS3bb, RASSbb ,RASS

The full-resolution RASS surveys data are organized in 1378 fields each 6.4° x 6.4° covering the whole sky. Neighboring fields overlap by at least 0.23°.

Three bands are available through SkyView

broad band (0.1-2.4 keV)
hard band (0.5-2.0 keV)
soft band (0.1-0.4 keV)

Data was dowloaded from the MPE FTP site.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPE but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	All-sky
PixelScale	45"
PixelUnits	Counts,Flux
Resolution
Coordinates	Equatorial
Equinox
Projection	Gnomonic
Epoch	1990-07 to 1991-02, 1991-98
Reference	The ROSAT All-Sky Survey (ADS)

ROSAT All-Sky X-ray Survey Soft Band: Counts

Short name[s] used to specify survey:RASSsbC, RASSCnt sb, RASS-Cnt Soft ,RASS Soft, RASS3sb, RASSsb

The full-resolution RASS surveys data are organized in 1378 fields each 6.4° x 6.4° covering the whole sky. Neighboring fields overlap by at least 0.23°.

Three bands are available through SkyView

broad band (0.1-2.4 keV)
hard band (0.5-2.0 keV)
soft band (0.1-0.4 keV)

Data was dowloaded from the MPE FTP site.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPE but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	73 PHz
Bandpass	24-120 PHz
Coverage	All-sky
PixelScale	45"
PixelUnits	Counts,Flux
Resolution
Coordinates	Equatorial
Equinox
Projection	Gnomonic
Epoch	1990-07 to 1991-02, 1991-98
Reference	The ROSAT All-Sky Survey (ADS)

ROSAT All-Sky X-ray Survey Hard Band: Intensity

Short name[s] used to specify survey:RASShbI, RASSInt hb, RASS-Int Hard

The full-resolution RASS surveys data are organized in 1378 fields each 6.4° x 6.4° covering the whole sky. Neighboring fields overlap by at least 0.23°.

Three bands are available through SkyView

broad band (0.1-2.4 keV)
hard band (0.5-2.0 keV)
soft band (0.1-0.4 keV)

Data was dowloaded from the MPE FTP site.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPE but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	240 PHz
Bandpass	120-480 PHz
Coverage	All-sky
PixelScale	45"
PixelUnits	Counts,Flux
Resolution
Coordinates	Equatorial
Equinox
Projection	Gnomonic
Epoch	1990-07 to 1991-02, 1991-98
Reference	The ROSAT All-Sky Survey (ADS)

ROSAT All-Sky X-ray Survey Broad Band: Intensity

Short name[s] used to specify survey:RASSbbI, RASSInt bb, RASS-Int Broad

The full-resolution RASS surveys data are organized in 1378 fields each 6.4° x 6.4° covering the whole sky. Neighboring fields overlap by at least 0.23°.

Three bands are available through SkyView

broad band (0.1-2.4 keV)
hard band (0.5-2.0 keV)
soft band (0.1-0.4 keV)

Data was dowloaded from the MPE FTP site.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPE but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	240 PHz
Bandpass	24-580 PHz
Coverage	All-sky
PixelScale	45"
PixelUnits	Counts,Flux
Resolution
Coordinates	Equatorial
Equinox
Projection	Gnomonic
Epoch	1990-07 to 1991-02, 1991-98
Reference	The ROSAT All-Sky Survey (ADS)

ROSAT All-Sky X-ray Survey Soft Band: Intensity

Short name[s] used to specify survey:RASSsbI, RASSInt sb, RASS-Int Soft

The full-resolution RASS surveys data are organized in 1378 fields each 6.4° x 6.4° covering the whole sky. Neighboring fields overlap by at least 0.23°.

Three bands are available through SkyView

broad band (0.1-2.4 keV)
hard band (0.5-2.0 keV)
soft band (0.1-0.4 keV)

Data was dowloaded from the MPE FTP site.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPE but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	73 PHz
Bandpass	24-120 PHz
Coverage	All-sky
PixelScale	45"
PixelUnits	Counts,Flux
Resolution
Coordinates	Equatorial
Equinox
Projection	Gnomonic
Epoch	1990-07 to 1991-02, 1991-98
Reference	The ROSAT All-Sky Survey (ADS)

ROSAT All-Sky X-ray Background Survey: Band 1

Short name[s] used to specify survey:RASSBck1,rassback1,RASS Background 1

Description
These maps present maps of ROSAT soft X-ray all-sky survey as presented in Snowden et al, ApJ 485, 125 (1997). The maps cover approximately 98% of the sky. These maps have had all point sources removed These surveys supercede the RASS0.25, RASS0.75 and RASS1.5 Kev surveys previously provided. Those surveys may still be invoked in SkyView using batch and jar tools but are not accessible on the Web page.

The seven maps correspond to ranges in the pulse height analysis of the photons detected. Since the energy resolution of the PSPC is poor, there is consider overlap between adjacent bands.

The energy range for the bands corresponds to:
Band Energy range (keV)

Band 1 0.11 - 0.284

Band 2 0.14 - 0.284

Band 3 0.2 - 0.83

Band 4 0.44 - 1.01

Band 5 0.56 - 1.21

Band 6 0.73 - 1.56

Band 7 1.05 - 2.04

Note the substantial overlap between bands. Each photon detected is assigned to a band based on the pulse height analysis for that photon, but the energy resolution of the detectors is relatively poor. Also note that Band 3 was not included in the reference paper due to poor statistics and background modeling.

SkyView has several other sets of surveys derived from ROSAT data with substantially higher resolution and which include point sources. The RASS surveys are derived from the RASS all sky survey. These include count and intensity maps. The PSPC maps are dervived from the PSPC pointed observations which were combined by SkyView. The HRI survey is derived from a similar mosaicking of all HRI observations.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPI but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	41 PHz
Coverage	All-sky
PixelScale	0.2
PixelUnits	10^-6counts/s
Resolution	ca. 2°
Coordinates	Galactic
Projection	Zenithal Equal Area
Epoch	1990-07 to 1991-02, 1991-8
Reference	S.L. Snowden, et al., Ap,J, Vol.485 (1997), pp.125

ROSAT All-Sky X-ray Background Survey: Band 2

Short name[s] used to specify survey:RASSBck2,rassback2,RASS Background 2

The seven maps correspond to ranges in the pulse height analysis of the photons detected. Since the energy resolution of the PSPC is poor, there is consider overlap between adjacent bands.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPI but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	51 PHz
Coverage	All-sky
PixelScale	0.2
PixelUnits	10^-6counts/s
Resolution	ca. 2°
Coordinates	Galactic
Projection	Zenithal Equal Area
Epoch	1990-07 to 1991-02, 1991-8
Reference	S.L. Snowden, et al., Ap,J, Vol.485 (1997), pp.125

ROSAT All-Sky X-ray Background Survey: Band 3

Short name[s] used to specify survey:RASSBck3,rassback3,RASS Background 3

The seven maps correspond to ranges in the pulse height analysis of the photons detected. Since the energy resolution of the PSPC is poor, there is consider overlap between adjacent bands.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPI but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	100 PHz
Coverage	All-sky
PixelScale	0.2
PixelUnits	10^-6counts/s
Resolution	ca. 2°
Coordinates	Galactic
Projection	Zenithal Equal Area
Epoch	1990-07 to 1991-02, 1991-8
Reference	S.L. Snowden, et al., Ap,J, Vol.485 (1997), pp.125

ROSAT All-Sky X-ray Background Survey: Band 4

Short name[s] used to specify survey:RASSBck4,rassback4,RASS Background 4

The seven maps correspond to ranges in the pulse height analysis of the photons detected. Since the energy resolution of the PSPC is poor, there is consider overlap between adjacent bands.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPI but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	170 PHz
Coverage	All-sky
PixelScale	0.2
PixelUnits	10^-6counts/s
Resolution	ca. 2°
Coordinates	Galactic
Projection	Zenithal Equal Area
Epoch	1990-07 to 1991-02, 1991-8
Reference	S.L. Snowden, et al., Ap,J, Vol.485 (1997), pp.125

ROSAT All-Sky X-ray Background Survey: Band 5

Short name[s] used to specify survey:RASSBck5,rassback5,RASS Background 5

The seven maps correspond to ranges in the pulse height analysis of the photons detected. Since the energy resolution of the PSPC is poor, there is consider overlap between adjacent bands.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPI but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	190 PHz
Coverage	All-sky
PixelScale	0.2
PixelUnits	10^-6counts/s
Resolution	ca. 2°
Coordinates	Galactic
Projection	Zenithal Equal Area
Epoch	1990-07 to 1991-02, 1991-8
Reference	S.L. Snowden, et al., Ap,J, Vol.485 (1997), pp.125

ROSAT All-Sky X-ray Background Survey: Band 6

Short name[s] used to specify survey:RASSBck6,rassback6,RASS Background 6

The seven maps correspond to ranges in the pulse height analysis of the photons detected. Since the energy resolution of the PSPC is poor, there is consider overlap between adjacent bands.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPI but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	250 PHz
Coverage	All-sky
PixelScale	0.2
PixelUnits	10^-6counts/s
Resolution	ca. 2°
Coordinates	Galactic
Projection	Zenithal Equal Area
Epoch	1990-07 to 1991-02, 1991-8
Reference	S.L. Snowden, et al., Ap,J, Vol.485 (1997), pp.125

ROSAT All-Sky X-ray Background Survey: Band 7

Short name[s] used to specify survey:RASSBck7,rassback7,RASS Background 7

The seven maps correspond to ranges in the pulse height analysis of the photons detected. Since the energy resolution of the PSPC is poor, there is consider overlap between adjacent bands.

Provenance	Max Planck Institute for Exterrestrial Physics (Garching FRG)
Copyright	MPI but data may be used for scientific purposes so long as appropriate reference is included.
Regime	X-ray
NSurvey	6
Frequency	370 PHz
Coverage	All-sky
PixelScale	0.2
PixelUnits	10^-6counts/s
Resolution	ca. 2°
Coordinates	Galactic
Projection	Zenithal Equal Area
Epoch	1990-07 to 1991-02, 1991-8
Reference	S.L. Snowden, et al., Ap,J, Vol.485 (1997), pp.125

RXTE Allsky 3-8 keV Flux

Short name[s] used to specify survey:RXTE3_8k_flux, RXTE AllSky 3-8keV flux

Description
Rossi X-ray Timing Explorer was launched at the end of 1995 and up to now (2004) it has been successfully operating for more than 7 years. The mission was primarily designed to study the variability of X-ray sources on time scales from sub-milliseconds to years. The maneuvering capability of the satellite combined with the high photon throughput of its main detector (PCA) and high quality of background prediction (thanks to PCA intrumental group of LHEA, GSFC) has also made it possible to construct maps of the sky in energy band 3-20 keV. During its life time RXTE/PCA has collected a large amount of data from slew observations covering almost the entire sky.

We have utilized the slew parts of all RXTE/PCA observations performed from April 15, 1996-July 16, 2002 which amounts in total to approximately 50,000 observations. The exposure time at a given point in the map is typically between 200-500 seconds. The observational period before April 15, 1996 (High Voltage Epochs 1 and 2) was excluded from the analysis because during that time the PCA had significantly different gain and dependence of the effective area on energy. The data reduction was done using standard tools of the LHEASOFT with a set of packages written by M. Revnivtsev (HEAD/IKI, Moscow; MPA, Garching).

The survey has several features. It has strongly different exposure times at different points on the sky that lead to strong variability of the statistical noise on images. Because of that the only meaningful representation of images is the map in units of statistical significance. After the detection of a source flux can be determined from the map in the 'flux' units. Map resolution is determined mainly by the slew rate of the RXTE (<0.05-0.1°/sec) and the time resolution of used data (16 sec, Std2 mode of the PCA). Sources can be detected down to the level of ~6e^-12 erg/s/cm², but at this level the confusion starts to play an important role. Details of the survey are presented in the paper of Revnivtsev et al. (2004).

Provenance	High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M PA, Garching, Germany
Copyright	Public domain
Regime	X-ray
NSurvey	3
Frequency	1.2 EHz
Bandpass	0.72-1.9 EHz
Coverage	All-sky \|b\| > 3
PixelScale	.5x.5° pixel
PixelUnits	Flux
Resolution	1°
Coordinates	Galactic
Equinox
Projection	Gnomonic
Epoch	1996-2002
Reference	RXTE all-sky slew survey. Catalog of X-ray sources at \|b\|>10 &# 176;, M. Revnivtsev, S. Sazonov, M. Gilfanov, K. Jahoda 2004, A&A, 418, 92 7

RXTE Allsky 3-8 keV Significance

Short name[s] used to specify survey:RXTE3_8k_sig, RXTE AllSky 3-8keV sig ,RXTE AllSky 3-8keV

Provenance	High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M PA, Garching, Germany
Copyright	Public domain
Regime	X-ray
NSurvey	3
Frequency	1.2 EHz
Bandpass	0.72-1.9 EHz
Coverage	All-sky \|b\| > 3
PixelScale	.5x.5° pixel
PixelUnits	Significance
Resolution	1°
Coordinates	Galactic
Equinox
Projection	Gnomonic
Epoch	1996-2002
Reference	RXTE all-sky slew survey. Catalog of X-ray sources at \|b\|>10 &# 176;, M. Revnivtsev, S. Sazonov, M. Gilfanov, K. Jahoda 2004, A&A, 418, 92 7

RXTE Allsky 8-20 keV Flux

Short name[s] used to specify survey:RXTE8_20k_flux, RXTE AllSky 8-20keV flux

Provenance	High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M PA, Garching, Germany
Copyright	Public domain
Regime	X-ray
NSurvey	3
Frequency	2.9 EHz
Bandpass	1.9-4.8 EHz
Coverage	All-sky \|b\| > 3
PixelScale	.5x.5° pixel
PixelUnits	Flux
Resolution	1°
Coordinates	Galactic
Equinox
Projection	Gnomonic
Epoch	1996-2002
Reference	RXTE all-sky slew survey. Catalog of X-ray sources at \|b\|>10 &# 176;, M. Revnivtsev, S. Sazonov, M. Gilfanov, K. Jahoda 2004, A&A, 418, 92 7

RXTE Allsky 8-20 keV Significance

Short name[s] used to specify survey:RXTE8_20k_sig, RXTE AllSky 8-20keV sig ,RXTE AllSky 8-20keV

Provenance	High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M PA, Garching, Germany
Copyright	Public domain
Regime	X-ray
NSurvey	3
Frequency	2.9 EHz
Bandpass	1.9-4.8 EHz
Coverage	All-sky \|b\| > 3
PixelScale	.5x.5° pixel
PixelUnits	Significance
Resolution	1°
Coordinates	Galactic
Equinox
Projection	Gnomonic
Epoch	1996-2002
Reference	RXTE all-sky slew survey. Catalog of X-ray sources at \|b\|>10 &# 176;, M. Revnivtsev, S. Sazonov, M. Gilfanov, K. Jahoda 2004, A&A, 418, 92 7

RXTE Allsky 3-20 keV Flux

Short name[s] used to specify survey:RXTE3_20k_flux, RXTE AllSky 3-20keV flux

Provenance	High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M PA, Garching, Germany
Copyright	Public domain
Regime	X-ray
NSurvey	3
Frequency	1.9 EHz
Bandpass	0.72-4.8 EHz
Coverage	All-sky \|b\| > 3
PixelScale	.5x.5° pixel
PixelUnits	Flux
Resolution	1°
Coordinates	Galactic
Equinox
Projection	Gnomonic
Epoch	1996-2002
Reference	RXTE all-sky slew survey. Catalog of X-ray sources at \|b\|>10 &# 176;, M. Revnivtsev, S. Sazonov, M. Gilfanov, K. Jahoda 2004, A&A, 418, 92 7

RXTE Allsky 3-20 keV Significance

Short name[s] used to specify survey:RXTE3_20k_sig, RXTE AllSky 3-20keV sig ,RXTE AllSky 3-20keV

Provenance	High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M PA, Garching, Germany
Copyright	Public domain
Regime	X-ray
NSurvey	3
Frequency	1.9 EHz
Bandpass	0.72-4.8 EHz
Coverage	All-sky \|b\| > 3
PixelScale	.5x.5° pixel
PixelUnits	Significance
Resolution	1°
Coordinates	Galactic
Equinox
Projection	Gnomonic
Epoch	1996-2002
Reference	RXTE all-sky slew survey. Catalog of X-ray sources at \|b\|>10 &# 176;, M. Revnivtsev, S. Sazonov, M. Gilfanov, K. Jahoda 2004, A&A, 418, 92 7

Swift XRT Combined Counts Images

Short name[s] used to specify survey:XRTCnt, Swift XRT Counts, SwiftXRTCnt

Description
The Swift XRT (Burrows et al 2005, SSRv, 120, 165) is a sensitive, broad-band (0.2 - 10 keV) X-ray imager with an effective area of about 125 cm**2 at 1.5 keV. The 600 x 600 pixel CCD at the focus provides a 23.6' x 23.6' field of view with a pixel scale of 2.36". The point spread function is 18" (HPD) at 1.5 keV.

These XRT surveys represent the data from the first 12.5 years of Swift X-ray observations. They include all data taken in photon counting mode. A total of just over 8% of the sky has some non-zero exposure. The fraction of sky exposed as a function of the exposure is given in the following table:

Exposure >0 10 30 100 300 1000 3000 1000 30000 100000 300000

Coverage 8.42 8.37 8.29 7.67 7.29 5.68 3.40 1.26 0.35 0.044 0.00118
The individual exposure and counts maps have been combined into a Hierarchical Progressive Survey (HiPS) where the data are stored in tiles in the HEALPix projection at a number of different resulutions. The highest resolution pixels (HEALPix order 17) have a size of roughly 1.6". Data are also stored at lower resolutions at factors of 1/2, 1/4, 1/8, 1/16, and 1/32, and in an all sky image with a resolution 1/256 of the higest resolution. An intensity map has been created as the ratio of the counts and exposure maps.

These surveys combine the basic count and exposure maps provided as standard products in the Swift XRT archive in obsid/xrt/products/*xpc_(sk|ex).img.gz. The surveys were created as follows:

All of the exposure maps available in the archive in mid-May 2017 were combined using the CDS-developed Hipsgen tool. This includes 129,063 observations for which both count and exposure files were found in PC mode. Three exposures where there was a counts map but no exposure map were ignored. A few exposure files had more than one exposure extension. 1,082 files had two extensions and 1 file had 3 extensions. The 1084 HDUs in extensions were extracted as separate files and included in the total exposure. The value of 0 was given to the Hipsgen software as the null value for the FITS files. This caused the CDS software to treat such pixels as missing rather than 0 exposure.
The counts data was extracted from the counts maps for each observation using SkyView developed software. For any pixel in which a count was recorded, the corresponding exposure file was checked and if there was any exposure (in any of the associated extensions), then the count was retained. If there was no exposure in any of the extensions of the corresponding exposure file, the counts in the pixel were omitted. Once a count was accepted, the overlap between the counts map pixel and the pixels of the corresponding HiPS tile (or tiles) was computed. Each count was then assigned entirely to a single pixel in the HiPS tile randomly but with the destination pixel probabilities weighted by area of the overlap. Thus if several pixels were found in a given counts map pixel they might be assigned to different pixels in the output image. The HiPS pixels (~1.6") used were of substantially higher resolution than the XRT resolution of 18" and somewhat higher than the counts map resolution of 2.36".
A total of 183,750,428 photons were extracted from the counts maps while 15,226 were rejected as being from pixels with 0 exposure. There were 501 pixels which required special treatment as straddling the boundaries of the HEALPix projection.
The resulting counts tiles were then clipped using the exposure tiles that had been previously generated. Basically this transferred the coverage of the exposure tiles to the counts tiles. Any counts pixel where the corresponding exposure pixel was a NaN was changed to a NaN to indicate that there was no coverage in this region.
During the clipping process 137,730 HiPS level 8 were clipped (of 786,432 over the entire sky). There were 12,236 tiles for which there was some exposure but no counts found. During the clipping process 2 photons were found on pixels where there was no corresponding exposure in the exposure tiles. This can happen when the pixel assignment process noted above shifts a photon just outside the exposed region but should be -- as it was -- rare. These photons were deleted.
After creating the clipped level 8 counts maps, level 7 to 3 tiles and an all sky map where generated by averaging pixels 2x2 to decrease each level. When adding the four pixels in the level N map together only pixels whose value was not NaN were considered.
Finally an intensity map was created by dividing the counts tiles by the exposure tiles. To eliminate gross fluctuations due to rare counts in regions with very low exposure, only regions with exposure > 1 second were retained. A total of 30 photons were deleted due to this criterion.

Note that while any sampler may in principle be used with these data, the Spline sampler may give unexpected results. The spline computation propogates NaNs thought the image and means that even occasional NaNs can corrupt the output image completely. NaNs are very common in this dataset. Also, if the region straddles a boundary in the HEALPix projection, the size of the requested input region is likely to exceed memory limits since the HiPS data are considered a single very large image.

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	X-ray
NSurvey	3
Frequency	360 PHz (1.5 keV)
Bandpass	48 PHz - 2,400 PHz (0.2-10 keV)
Coverage	Patches over ~6% of the sky
PixelScale	1.6" (Highest resolution/Hierarchical)
PixelUnits	Counts
Resolution	18" (HPD)
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to May 2017
Reference	The XRT Web Site or Burrows et al 2005, instrument reference

Swift XRT Combined Exposure Images

Short name[s] used to specify survey:XRTExp, Swift XRT Exposure, SwiftXRTExp

These surveys combine the basic count and exposure maps provided as standard products in the Swift XRT archive in obsid/xrt/products/*xpc_(sk|ex).img.gz. The surveys were created as follows:

All of the exposure maps available in the archive in mid-May 2017 were combined using the CDS-developed Hipsgen tool. This includes 129,063 observations for which both count and exposure files were found in PC mode. Three exposures where there was a counts map but no exposure map were ignored. A few exposure files had more than one exposure extension. 1,082 files had two extensions and 1 file had 3 extensions. The 1084 HDUs in extensions were extracted as separate files and included in the total exposure. The value of 0 was given to the Hipsgen software as the null value for the FITS files. This caused the CDS software to treat such pixels as missing rather than 0 exposure.
The counts data was extracted from the counts maps for each observation using SkyView developed software. For any pixel in which a count was recorded, the corresponding exposure file was checked and if there was any exposure (in any of the associated extensions), then the count was retained. If there was no exposure in any of the extensions of the corresponding exposure file, the counts in the pixel were omitted. Once a count was accepted, the overlap between the counts map pixel and the pixels of the corresponding HiPS tile (or tiles) was computed. Each count was then assigned entirely to a single pixel in the HiPS tile randomly but with the destination pixel probabilities weighted by area of the overlap. Thus if several pixels were found in a given counts map pixel they might be assigned to different pixels in the output image. The HiPS pixels (~1.6") used were of substantially higher resolution than the XRT resolution of 18" and somewhat higher than the counts map resolution of 2.36".
A total of 183,750,428 photons were extracted from the counts maps while 15,226 were rejected as being from pixels with 0 exposure. There were 501 pixels which required special treatment as straddling the boundaries of the HEALPix projection.
The resulting counts tiles were then clipped using the exposure tiles that had been previously generated. Basically this transferred the coverage of the exposure tiles to the counts tiles. Any counts pixel where the corresponding exposure pixel was a NaN was changed to a NaN to indicate that there was no coverage in this region.
During the clipping process 137,730 HiPS level 8 were clipped (of 786,432 over the entire sky). There were 12,236 tiles for which there was some exposure but no counts found. During the clipping process 2 photons were found on pixels where there was no corresponding exposure in the exposure tiles. This can happen when the pixel assignment process noted above shifts a photon just outside the exposed region but should be -- as it was -- rare. These photons were deleted.
After creating the clipped level 8 counts maps, level 7 to 3 tiles and an all sky map where generated by averaging pixels 2x2 to decrease each level. When adding the four pixels in the level N map together only pixels whose value was not NaN were considered.
Finally an intensity map was created by dividing the counts tiles by the exposure tiles. To eliminate gross fluctuations due to rare counts in regions with very low exposure, only regions with exposure > 1 second were retained. A total of 30 photons were deleted due to this criterion.

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	X-ray
NSurvey	3
Frequency	360 PHz (1.5 keV)
Bandpass	48 PHz - 2,400 PHz (0.2-10 keV)
Coverage	Patches over ~6% of the sky
PixelScale	1.6" (Highest resolution/Hierarchical)
PixelUnits	s
Resolution	18" (HPD)
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to May 2017
Reference	The XRT Web Site or Burrows et al 2005, instrument reference

Swift XRT Combined Intensity Images

Short name[s] used to specify survey:XRTInt, Swift XRT Intensity, SwiftXRTInt

These surveys combine the basic count and exposure maps provided as standard products in the Swift XRT archive in obsid/xrt/products/*xpc_(sk|ex).img.gz. The surveys were created as follows:

All of the exposure maps available in the archive in mid-May 2017 were combined using the CDS-developed Hipsgen tool. This includes 129,063 observations for which both count and exposure files were found in PC mode. Three exposures where there was a counts map but no exposure map were ignored. A few exposure files had more than one exposure extension. 1,082 files had two extensions and 1 file had 3 extensions. The 1084 HDUs in extensions were extracted as separate files and included in the total exposure. The value of 0 was given to the Hipsgen software as the null value for the FITS files. This caused the CDS software to treat such pixels as missing rather than 0 exposure.
The counts data was extracted from the counts maps for each observation using SkyView developed software. For any pixel in which a count was recorded, the corresponding exposure file was checked and if there was any exposure (in any of the associated extensions), then the count was retained. If there was no exposure in any of the extensions of the corresponding exposure file, the counts in the pixel were omitted. Once a count was accepted, the overlap between the counts map pixel and the pixels of the corresponding HiPS tile (or tiles) was computed. Each count was then assigned entirely to a single pixel in the HiPS tile randomly but with the destination pixel probabilities weighted by area of the overlap. Thus if several pixels were found in a given counts map pixel they might be assigned to different pixels in the output image. The HiPS pixels (~1.6") used were of substantially higher resolution than the XRT resolution of 18" and somewhat higher than the counts map resolution of 2.36".
A total of 183,750,428 photons were extracted from the counts maps while 15,226 were rejected as being from pixels with 0 exposure. There were 501 pixels which required special treatment as straddling the boundaries of the HEALPix projection.
The resulting counts tiles were then clipped using the exposure tiles that had been previously generated. Basically this transferred the coverage of the exposure tiles to the counts tiles. Any counts pixel where the corresponding exposure pixel was a NaN was changed to a NaN to indicate that there was no coverage in this region.
During the clipping process 137,730 HiPS level 8 were clipped (of 786,432 over the entire sky). There were 12,236 tiles for which there was some exposure but no counts found. During the clipping process 2 photons were found on pixels where there was no corresponding exposure in the exposure tiles. This can happen when the pixel assignment process noted above shifts a photon just outside the exposed region but should be -- as it was -- rare. These photons were deleted.
After creating the clipped level 8 counts maps, level 7 to 3 tiles and an all sky map where generated by averaging pixels 2x2 to decrease each level. When adding the four pixels in the level N map together only pixels whose value was not NaN were considered.
Finally an intensity map was created by dividing the counts tiles by the exposure tiles. To eliminate gross fluctuations due to rare counts in regions with very low exposure, only regions with exposure > 1 second were retained. A total of 30 photons were deleted due to this criterion.

Provenance	Data generated from public images at HEASARC archive
Copyright	Public Domain
Regime	X-ray
NSurvey	3
Frequency	360 PHz (1.5 keV)
Bandpass	48 PHz - 2,400 PHz (0.2-10 keV)
Coverage	Patches over ~6% of the sky
PixelScale	1.6" (Highest resolution/Hierarchical)
PixelUnits	Counts/s
Resolution	18" (HPD)
Coordinates	Equatorial
Projection	HEALPix/HIPS
Epoch	January 2005 to May 2017
Reference	The XRT Web Site or Burrows et al 2005, instrument reference

Gamma ray surveys

CGRO Compton Telescope: 3 channel data

Short name[s] used to specify survey:Comptel,CGRO Comptel

Description
This survey is a maximum entropy solution to the data taken by the CompTel instrument on the Compton Gamma Ray Observatory. The data in this survey are intended only to give the general appearance of the MeV gamma-ray sky. Fluxes, flux limits and spectra should be derived using the Compass system for the analysis of CompTel data. Compass is available at the Compton Observatory Science Support Center .

The maps were originally generated by the CompTel Instrument Team as three separate maps in the bands:

1-3 MeV
3-10 MeV
10-30 MeV

All CompTel observations from phases 1, 2 and 3 were included in the maps (May 1991 through October 1994). These maps were combined into a single 3-D map at SkyView

Provenance	CompTel Instrument Team. Maps generated by Andrew Strong, Max-Planck Institute for Extraterrestrial Physics (Garching).
Copyright	Public domain
Regime	Gamma Ray
NSurvey	1 survey with 3 bands
Frequency	2.4 ZHz
Bandpass	0.24-7.2 ZHz
Coverage	All-sky
PixelScale	1d
PixelUnits	cts/s/cm2/steradian
Resolution	~3d
Epoch	May 1991 to October 1994
CoordinateSystem	Galactic
Projection	Rectangular (CAR)
Reference	Comptel Instrument Team Home Page

Energetic Gamma-Ray Event Telescope: Hard

Short name[s] used to specify survey:EGRETHard, EGRET1000, EGRET >100 MeV

Description
These data are from the Compton GRO EGRET team. Data are from all pointings of the EGRET instrument in the verification phase and phase 1-4 of the Compton mission. The maps exist in energies 30-100 MeV, 100-100000 MeV, and as a multi-dimensional, 10 channel survey. For the multi-dimensional survey, channels 1-3 comprise energies less than 100 MeV, and channels 4-10 comprise energies greater than 100 MeV. Note that the energies are not uniformly split among the channels.

The EGRET 3D map is comprised of ten channels with the following energy ranges:

Channel 1 30-50 MeV
Channel 2 50-70 MeV
Channel 3 70-100 MeV
Channel 4 100-150 MeV
Channel 5 150-300 MeV
Channel 6 300-500 MeV
Channel 7 500-1000 MeV
Channel 8 1000-2000 MeV
Channel 9 2000-4000 MeV
Channel 10 4000-10000 MeV

The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV).

Provenance	EGRET Instrument team, NASA Goddard Space Flight Center
Copyright	Public domain
Regime	Gamma Ray
NSurveys	3
Frequency	72 ZHz
Bandpass	24-2400 ZHz
Coverage	All-sky
Resolution	ca. 5d below 100 MeV, ca. 2d above 100 MeV
PixelScale	0.5 degrees/pixel
PixelUnits	cts/s/cm2/steradian
Coordinates	Galactic
Projection	Rectangular
Epoch	1992-1995
Reference	Hartman, et al., 1999, The Third EGRET Source Catalog, ApJ Supplement, 123, 79-202

Energetic Gamma-Ray Event Telescope: Soft

Short name[s] used to specify survey:EGRETSoft, EGRET30, EGRET <100 MeV

The EGRET 3D map is comprised of ten channels with the following energy ranges:

Channel 1 30-50 MeV
Channel 2 50-70 MeV
Channel 3 70-100 MeV
Channel 4 100-150 MeV
Channel 5 150-300 MeV
Channel 6 300-500 MeV
Channel 7 500-1000 MeV
Channel 8 1000-2000 MeV
Channel 9 2000-4000 MeV
Channel 10 4000-10000 MeV

The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV).

Provenance	EGRET Instrument team, NASA Goddard Space Flight Center
Copyright	Public domain
Regime	Gamma Ray
NSurveys	3
Frequency	15 ZHz
Bandpass	7.2-24 ZHz
Coverage	All-sky
Resolution	ca. 5d below 100 MeV, ca. 2d above 100 MeV
PixelScale	0.5 degrees/pixel
PixelUnits	cts/s/cm2/steradian
Coordinates	Galactic
Projection	Rectangular
Epoch	1992-1995
Reference	Hartman, et al., 1999, The Third EGRET Source Catalog, ApJ Supplement, 123, 79-202

Energetic Gamma-Ray Event Telescope: 10 channel data

Short name[s] used to specify survey:EGRET3D,EGRET(3D), EGRET (3D)

Description
These data are from the Compton GRO EGRET team. Data are from all pointings of the EGRET instrument in the verification phase and phase 1-4 of the Compton mission. The maps exist in energies 30-100 MeV, 100-10000 MeV, and as a multi-dimensional, 10 channel survey. For the multi-dimensional survey, channels 1-3 comprise energies less than 100 MeV, and channels 4-10 comprise energies greater than 100 MeV. Note that the energies are not uniformly split among the channels.

The EGRET 3D map is comprised of ten channels with the following energy ranges:

Channel 1 30-50 MeV
Channel 2 50-70 MeV
Channel 3 70-100 MeV
Channel 4 100-150 MeV
Channel 5 150-300 MeV
Channel 6 300-500 MeV
Channel 7 500-1000 MeV
Channel 8 1000-2000 MeV
Channel 9 2000-4000 MeV
Channel 10 4000-10000 MeV

The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV).

Provenance	EGRET Instrument team, NASA Goddard Space Flight Center
Copyright	Public domain
Regime	Gamma Ray
NSurveys	3
Frequency	24 ZHz
Bandpass	.24-2400 ZHz
Coverage	All-sky
Resolution	ca. 5d below 100 MeV, ca. 2d above 100 MeV
PixelScale	0.5 degrees/pixel
PixelUnits	cts/s/cm2/steradian
Coordinates	Galactic
Projection	Rectangular
Epoch	1992-1995
Reference	Hartman, et al., 1999, The Third EGRET Source Catalog, ApJ Supplement, 123, 79-202

Fermi Map: Band 1

Short name[s] used to specify survey:Fermi 1, Fermi1, Fermi band 1

Description
This survey sums all data observed by the Fermi mission up to week 396. This version of the Fermi survey are intensity maps where the summed counts data are divided by the exposure for each pixel (in cm^2 s) and the area of the pixel. Data is broken into 5 energy bands

30-100 MeV Band 1
100-300 MeV Band 2
300-1000 MeV Band 3
1-3 GeV Band 4
3-300 GeV Band 5

The SkyView data are based upon a Cartesian projection of the counts divided by the exposure maps. In the Cartesian projection pixels near the pole have a much smaller area than pixels on the equator, so these pixels have smaller integrated flux. When creating large scale images in other projections users may wish to make sure to compensate for this effect the flux conserving clip-resampling option.

Provenance	Fermi LAT instrument team, NASA Goddard Space Flight Center
Copyright	Public domain
Regime	Gamma Ray
NSurveys	5
Frequency	12 ZHz
Bandwidth	7-24 ZHz (30-100 MeV)
Coverage	All-sky
Resolution	3 degrees.
PixelScale	0.1 degrees/pixel
PixelUnits	cnts/s/cm^2/sr
Coordinates	Equatorial
Equinox	2000
Projection	Rectangular
Epoch	2008-2012
Reference	Data and survey paper (ADS)

Fermi Map: Band 2

Short name[s] used to specify survey:Fermi 2, Fermi2, Fermi band 2

30-100 MeV Band 1
100-300 MeV Band 2
300-1000 MeV Band 3
1-3 GeV Band 4
3-300 GeV Band 5

Provenance	Fermi LAT instrument team, NASA Goddard Space Flight Center
Copyright	Public domain
Regime	Gamma Ray
NSurveys	5
Frequency	40 ZHz
Bandwidth	24-70 ZHz (100-300 MeV)
Coverage	All-sky
Resolution	2 degrees.
PixelScale	0.1 degrees/pixel
PixelUnits	cnts/s/cm^2/sr
Coordinates	Equatorial
Equinox	2000
Projection	Rectangular
Epoch	2008-2012
Reference	Data and survey paper (ADS)

Fermi Map: Band 3

Short name[s] used to specify survey:Fermi 3, Fermi3, Fermi band 3

30-100 MeV Band 1
100-300 MeV Band 2
300-1000 MeV Band 3
1-3 GeV Band 4
3-300 GeV Band 5

Provenance	Fermi LAT instrument team, NASA Goddard Space Flight Center
Copyright	Public domain
Regime	Gamma Ray
NSurveys	5
Frequency	150 ZHz
Bandwidth	70-240 ZHz (300-1000 MeV)
Coverage	All-sky
Resolution	1 degrees.
PixelScale	0.1 degrees/pixel
PixelUnits	cnts/s/cm^2/sr
Coordinates	Equatorial
Equinox	2000
Projection	Rectangular
Epoch	2008-2012
Reference	Data and survey paper (ADS)

Fermi Map: Band 4

Short name[s] used to specify survey:Fermi 4, Fermi4, Fermi band 4

30-100 MeV Band 1
100-300 MeV Band 2
300-1000 MeV Band 3
1-3 GeV Band 4
3-300 GeV Band 5

Provenance	Fermi LAT instrument team, NASA Goddard Space Flight Center
Copyright	Public domain
Regime	Gamma Ray
NSurveys	5
Frequency	400 ZHz
Bandwidth	240-700 ZHz (1-3 GeV)
Coverage	All-sky
Resolution	0.4 degrees.
PixelScale	0.1 degrees/pixel
PixelUnits	cnts/s/cm^2/sr
Coordinates	Equatorial
Equinox	2000
Projection	Rectangular
Epoch	2008-2012
Reference	Data and survey paper (ADS)

Fermi Map: Band 5

Short name[s] used to specify survey:Fermi 5, Fermi5, Fermi band 5

30-100 MeV Band 1
100-300 MeV Band 2
300-1000 MeV Band 3
1-3 GeV Band 4
3-300 GeV Band 5

Provenance	Fermi LAT instrument team, NASA Goddard Space Flight Center
Copyright	Public domain
Regime	Gamma Ray
NSurveys	5
Frequency	1400 ZHz
Bandwidth	700-70000 ZHz (3-300 GeV)
Coverage	All-sky
Resolution	0.2 degrees.
PixelScale	0.1 degrees/pixel
PixelUnits	cnts/s/cm^2/sr
Coordinates	Equatorial
Equinox	2000
Projection	Rectangular
Epoch	2008-2012
Reference	Data and survey paper (ADS)

GOODS ACS exposure (s)
Band	North>	South
z850	24760	18232
i775	8530	7028
V606	5650	5450
B435
7200

Filter	Count	Central Wavelength (Å)	Bandpass (Å)	Central Frequency(THz)	Bandpass (THz)	Coverage
WHITE	3,000	3600	1600-6000	832	500-1874	0.0017
V	30,557	5468	5083-5852	548	512-590	0.0171
B	28,347	4392	3904-4880	683	614-768	0.0112
U	49,954	3465	3072-3875	865	774-975	0.0287
UVW1	60,690	2600	2253-2946	1154	1017-1330	0.0277
UVM2	56,977	2246	1997-2495	1334	1201-1501
UVW2	54,590	1928	1600-2256	1554	1328-1874	0.0260

Band	Energy (keV)	Frequency (EHz)
1	14-20	3.38-4.84
2	20-24	4.84-5.80
3	24-35	5.80-8.46
4	35-50	8.46-12.1
5	50-75	12.1-18.1
6	75-100	18.1-24.2
7	100-150	24.2-36.3
8	150-195	36.3-47.2
Sum (SNR only)	14-195	3.38-47.2

Band	Energy range (keV)
Band 1	0.11 - 0.284
Band 2	0.14 - 0.284
Band 3	0.2 - 0.83
Band 4	0.44 - 1.01
Band 5	0.56 - 1.21
Band 6	0.73 - 1.56
Band 7	1.05 - 2.04

Exposure	>0	10	30	100	300	1000	3000	1000	30000	100000	300000
Coverage	8.42	8.37	8.29	7.67	7.29	5.68	3.40	1.26	0.35	0.044	0.00118