SkyView Surveys
Energy vs Data Pixel Resolution plot of all SkyView Surveys
(Click for larger image)
The diversity of SkyView surveys is shown here. Data ranges over about 16 orders of magnitude in energy and about 5 orders of magnitude in resolution.
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
Bonn 1420 MHz 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
Infrared surveys
Two Micron All Sky Survey (H-Band)
Two Micron All Sky Survey (J-Band)
Two Micron All Sky Survey (K-Band)
Cosmic Background Explorer DIRBE
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
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)
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
Ultraviolet surveys
Extreme Ultraviolet Explorer: 83 A
Extreme Ultraviolet Explorer: 171 A
Extreme Ultraviolet Explorer: 405 A
Extreme Ultraviolet Explorer: 555 A
ROSAT Wide Field Camera: F1
ROSAT Wide Field Camera: F2
X-ray surveys
Swift BAT All-Sky Survey: Flux and Significance
GRANAT/SIGMA Flux
GRANAT/SIGMA
HEAO 1A
ROSAT High Resolution Image Pointed Observations Mosaic: Intensity
INTEGRAL/Spectral Imager Galactic Center Survey
PSPC summed pointed observations, 1 degree cutoff, intensity
PSPC summed pointed observations, 2 degree cutoff, counts
PSPC summed pointed observations, 2 degree cutoff, exposure
PSPC summed pointed observations, 2 degree cutoff, intensity
ROSAT All-Sky X-ray Survey Broad Band
ROSAT All-Sky X-ray Survey Hard Band
ROSAT All-Sky X-ray Survey Soft Band
ROSAT All-Sky X-ray Background Survey: Bands 1
ROSAT All-Sky X-ray Background Survey: Bands 2
ROSAT All-Sky X-ray Background Survey: Bands 3
ROSAT All-Sky X-ray Background Survey: Bands 4
ROSAT All-Sky X-ray Background Survey: Bands 5
ROSAT All-Sky X-ray Background Survey: Bands 6
ROSAT All-Sky X-ray Background Survey: Bands 7
ROSAT All-Sky Broad Band Intensity
ROSAT All-Sky Hard Band Intensity
ROSAT All-Sky Broad Band Intensity
RXTE Allsky 3-20keV Significance
RXTE Allsky 3-8keV Significance
RXTE Allsky 8-20keV Significance
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
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 Continuum |
Coverage | Complete above 16 degrees south Equatorial latitude |
PixelScale | 0.25 deg/pixel |
PixelUnits | millikelvins |
Resolution | 34' |
CoordinateSystem | Equatorial |
Equinox | 1950 |
Projection | Rectangular (CAR) |
Epoch | ca. 1980 |
Reference |
Reich, 1982, A&AS48, 219. Reich and Reich, 1986, A&AS63, 205.
|
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 |
Coverage | All-sky |
PixelScale | 0.3515 degrees/pixel |
PixelUnits | Kelvins |
Resolution | 0.85 degrees |
CoordinateSystem | Galactic |
Projection | Rectangular (CAR) |
Reference |
Haslam et al., 1982,A&AS47, 1.
|
4850 MHz Survey/GB6
Short name[s] used to specify survey: 4850MHz,4850mhz,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 |
Coverage | RA: 0d - 360d, DEC: -88d to +75d |
PixelScale | 0.0167deg/pixel (PMN), and 0.0111 deg/pixel ((86+87) GB) |
PixelUnits | janskies/beam (ca. 200,000 beams/steradian) |
Resolution | 7' FWHM |
CoordinateSystem | Equatorial |
Equinox | 1950 |
Epoch | ca. 1990 |
Projection | Orthographic (SIN) |
Reference |
Condon, et al., 1991, AJ 102, 2041; 1993, AJ 106, 1095; 1994, AJ 107, 1829
|
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 |
Coverage | All galactic longitudes, irregular bands between -35 and +35 latitudes
|
PixelScale | 0.125d/pixel |
PixelUnits | intensities are velocity-integrated main beam brightness temperature, in units of K km/s |
CoordinateSystem | Galactic |
Projection | Rectangular |
Epoch | 2001 |
Reference |
Dame, T. M., Hartmann, Dap, Thaddeus, P., ApJ, 2001
|
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 (January 1997) 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 |
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 | 1994 - 1996 |
Reference |
FIRST home page
|
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 |
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 | 1990 |
Reference |
K.S. Dwarakanath and N. Udaya Shankar 1990, J. Astrophys. Astr., 11 323.
|
Dickey and Lockman HI map
Short name[s] used to specify survey:nh,nH
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 |
PixelScale | 40' |
PixelUnit | atoms/cm^2 |
Resolution | 1 degree |
Coordinates | Galactic |
Projection | Aitoff |
Epoch | ca. 1980 |
Reference | Dickey and Lockman, ARAA 28, 1990, p215. |
NVSS
Short name[s] used to specify survey: NVSS
Description
The NRAO VLA Sky Survey is currently underway at the VLA and data is
made available to the public as soon as processed. SkyView
has copied the NVSS intensity data from the NRAO FTP site. The full
NVSS survey data includes information on other Stokes parameters.
Note that SkyView may be slightly out of date with regard
to the latest releases of NVSS data. The current information was
copied in November 1997.
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 will be:
- 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 |
Coverage | Declinations above -40 degrees |
PixelScale | 15"/pixel |
PixelUnits | Janskies/beam |
Resolution | 45" |
Coordinates | Equatorial |
Equinox | 2000 |
Projection | Orthographic |
Epoch | ca. 1994-1996 |
Reference |
NVSS home page
or the NVSS preprint
|
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.
The survey was completed in 2007. Please note that the images still
contain some telescope artifacts. 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 |
Coverage | Covers mostly the entire sky south of
declination -30°. See the coverage map
for current status. |
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 | ca. 1997 - present |
Reference |
SUMSS home page
|
VLA Low-frequency Sky Survey
Short name[s] used to specify survey:VLSS,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.
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 |
Coverage | Declinations above -30 degrees |
PixelScale | 25"/pixel |
PixelUnits | Janskies/beam |
Resolution | 80" |
Coordinates | Equatorial |
Equinox | 2000 |
Projection | Orthographic (Sin) |
Epoch | ca. 2006 |
Reference |
VLSS home page
or the VLSS proposal
|
Westerbork Northern Sky Survey
Short name[s] used to specify survey: WENSS
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.
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 Ks (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 | K=138 THz (2.17 microns), H=180 THz (1.65 microns), J=240 THz (1.25 microns) |
Coverage | Allsky |
PixelScale | 1"/pixel |
PixelUnits | |
Resolution | 1" |
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
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 Ks (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 | K=138 THz (2.17 microns), H=180 THz (1.65 microns), J=240 THz (1.25 microns) |
Coverage | Allsky |
PixelScale | 1"/pixel |
PixelUnits | |
Resolution | 1" |
CoordinateSystem | 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
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 Ks (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 | K=138 THz (2.17 microns), H=180 THz (1.65 microns), J=240 THz (1.25 microns) |
Coverage | Allsky |
PixelScale | 1"/pixel |
PixelUnits | |
Resolution | 1" |
CoordinateSystem | Equatorial |
Equinox | 2000 |
Projection | Orthographic (SIN) |
Epoch | 1997 - 2002 |
Reference |
2MASS web site
|
Cosmic Background Explorer DIRBE
Short name[s] used to specify survey:COBE, COBE DIRBE(OLD), COBE DIRBE (OLD)
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 currently
provides 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). We do not recommend use of the first map, but it is
retained for compability with earlier investigations.
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
|
Copyright | Public Domain |
Regime | Infrared |
NSurvey | 1 (10 bands) |
Frequency | 1.25-240 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.
|
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 currently
provides 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). We do not recommend use of the first map, but it is
retained for compability with earlier investigations.
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
|
Copyright | Public Domain |
Regime | Infrared |
NSurvey | 1 (10 bands) |
Frequency | 1.25-240 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.
|
Cosmic Background Explorer DIRBE Zodi-Subtracted Mission Average
Short name[s] used to specify survey: COBEZSMA, COBE DIRBE/ZSMA
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 currently
provides 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). We do not recommend use of the first map, but it is
retained for compability with earlier investigations.
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
|
Copyright | Public Domain |
Regime | Infrared |
NSurvey | 1 (10 bands) |
Frequency | 1.25-240 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.
|
IRAS Sky Survey Atlas: 100 micron
Short name[s] used to specify survey: IRAS100, IRAS 100 micron, 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 | 3-30 THz |
Coverage | All-sky |
Scale | 0.025 deg/pix |
Units | MJy/sr |
Resolution | 2' |
Coordinates | Equatorial |
Projection | Gnomonic(TAN) |
Equinox | 1950 |
Epoch | 1983 |
Reference |
Wheelock, et al., 1991, IRAS Sky Survey Atlas Explanatory Supplement..
|
IRAS Sky Survey Atlas: 12 micron
Short name[s] used to specify survey: IRAS12, IRAS 12 micron,IRAS 12
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 | 3-30 THz |
Coverage | All-sky |
Scale | 0.025 deg/pix |
Units | MJy/sr |
Resolution | 2' |
Coordinates | Equatorial |
Projection | Gnomonic(TAN) |
Equinox | 1950 |
Epoch | 1983 |
Reference |
Wheelock, et al., 1991, IRAS Sky Survey Atlas Explanatory Supplement..
|
IRAS Sky Survey Atlas: 25 micron
Short name[s] used to specify survey: IRAS25, IRAS 25 micron,IRAS 25
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 | 3-30 THz |
Coverage | All-sky |
Scale | 0.025 deg/pix |
Units | MJy/sr |
Resolution | 2' |
Coordinates | Equatorial |
Projection | Gnomonic(TAN) |
Equinox | 1950 |
Epoch | 1983 |
Reference |
Wheelock, et al., 1991, IRAS Sky Survey Atlas Explanatory Supplement..
|
IRAS Sky Survey Atlas: 60 micron
Short name[s] used to specify survey: IRAS60, IRAS 60 micron,IRAS 60
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 | 3-30 THz |
Coverage | All-sky |
Scale | 0.025 deg/pix |
Units | MJy/sr |
Resolution | 2' |
Coordinates | Equatorial |
Projection | Gnomonic(TAN) |
Equinox | 1950 |
Epoch | 1983 |
Reference |
Wheelock, et al., 1991, IRAS Sky Survey Atlas Explanatory Supplement..
|
Improved Reprocessing of the IRAS Survey: 100
Short name[s] used to specify survey: IRIS100, IRIS 100 micron,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 | 3-30 THz |
Coverage | All-sky |
Scale | 0.025 deg/pix |
Units | MJy/sr |
Resolution | 2' |
Coordinates | Equatorial |
Projection | Gnomonic(TAN) |
Equinox | 1950 |
Epoch | 1983 |
Reference |
2005ApJS..157..302M
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,IRIS 12 micron,IRIS 12
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 | 3-30 THz |
Coverage | All-sky |
Scale | 0.025 deg/pix |
Units | MJy/sr |
Resolution | 2' |
Coordinates | Equatorial |
Projection | Gnomonic(TAN) |
Equinox | 1950 |
Epoch | 1983 |
Reference |
2005ApJS..157..302M
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,IRIS 25 micron,IRIS 25
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 | 3-30 THz |
Coverage | All-sky |
Scale | 0.025 deg/pix |
Units | MJy/sr |
Resolution | 2' |
Coordinates | Equatorial |
Projection | Gnomonic(TAN) |
Equinox | 1950 |
Epoch | 1983 |
Reference |
2005ApJS..157..302M
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,IRIS 60 micron, IRIS 60
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 | 3-30 THz |
Coverage | All-sky |
Scale | 0.025 deg/pix |
Units | MJy/sr |
Resolution | 2' |
Coordinates | Equatorial |
Projection | Gnomonic(TAN) |
Equinox | 1950 |
Epoch | 1983 |
Reference |
2005ApJS..157..302M
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 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.
Schlegel, Finkbeiner and Davis Dust Survey
Short name[s] used to specify survey: SFD Dust,SFDdust, SFD Dust Map
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.
WMAP Five Year Galaxy Removed
Short name[s] used to specify survey:WMAPILC,WMAP ILC,WMAP
Description
These survey represents a combination of the 5-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.
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 WMAP data.
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 | 2000-2005 |
Reference |
LAMBDA archive
|
WMAP Five Year K-Band
Short name[s] used to specify survey:WMAPK,WMAP K,WMAP-K
Description
These data represent the 5 year co-added maps for each of the five frequency bands
in the WMAP dataset. These energies of the bands and their widths are:
Band | Frequency (GHz) | Bandwidth (GHz) |
K | 23 | 5.5 |
Ka | 33 | 7.0 |
Q | 41 | 8.3 |
V | 61 | 14.0 |
W | 94 | 20.5 |
The original data are available at the LAMBDA archive.
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 WMAP data.
Provenance | WMAP Mission/LAMBDA archive |
Copyright | Public Domain |
Regime | Infrared |
NSurvey | 1 |
Frequency | 23 GHz |
Coverage | AllSky |
PixelScale | 7.5' |
PixelUnits | millikelvins |
Resolution | 0.88 degree beam size |
CoordinateSystem | Galactic |
Projection | HEALPix |
Epoch | 2000-2005 |
Reference |
LAMBDA archive
|
WMAP Five Year Ka-Band
Short name[s] used to specify survey:WMAPKa,WMAP Ka,WMAP-Ka
Description
These data represent the 5 year co-added maps for each of the five frequency bands
in the WMAP dataset. These energies of the bands and their widths are:
Band | Frequency (GHz) | Bandwidth (GHz) |
K | 23 | 5.5 |
Ka | 33 | 7.0 |
Q | 41 | 8.3 |
V | 61 | 14.0 |
W | 94 | 20.5 |
The original data are available at the LAMBDA archive.
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 WMAP data.
Provenance | WMAP Mission/LAMBDA archive |
Copyright | Public Domain |
Regime | Infrared |
NSurvey | 1 |
Frequency | 33 GHz |
Coverage | AllSky |
PixelScale | 7.5' |
PixelUnits | millikelvins |
Resolution | 0.66 degree beam size |
CoordinateSystem | Galactic |
Projection | HEALPix |
Epoch | 2000-2005 |
Reference |
LAMBDA archive
|
WMAP Five Year Q-Band
Short name[s] used to specify survey:WMAPQ,WMAP Q,WMAP-Q
Description
These data represent the 5 year co-added maps for each of the five frequency bands
in the WMAP dataset. These energies of the bands and their widths are:
Band | Frequency (GHz) | Bandwidth (GHz) |
K | 23 | 5.5 |
Ka | 33 | 7.0 |
Q | 41 | 8.3 |
V | 61 | 14.0 |
W | 94 | 20.5 |
The original data are available at the LAMBDA archive.
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 WMAP data.
Provenance | WMAP Mission/LAMBDA archive |
Copyright | Public Domain |
Regime | Infrared |
NSurvey | 1 |
Frequency | 41 GHz |
Coverage | AllSky |
PixelScale | 7.5' |
PixelUnits | millikelvins |
Resolution | 0.51 degree beam size |
CoordinateSystem | Galactic |
Projection | HEALPix |
Epoch | 2000-2005 |
Reference |
LAMBDA archive
|
WMAP Five Year V-Band
Short name[s] used to specify survey:WMAPV,WMAP V,WMAP-v
Description
These data represent the 5 year co-added maps for each of the five frequency bands
in the WMAP dataset. These energies of the bands and their widths are:
Band | Frequency (GHz) | Bandwidth (GHz) |
K | 23 | 5.5 |
Ka | 33 | 7.0 |
Q | 41 | 8.3 |
V | 61 | 14.0 |
W | 94 | 20.5 |
The original data are available at the LAMBDA archive.
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 WMAP data.
Provenance | WMAP Mission/LAMBDA archive |
Copyright | Public Domain |
Regime | Infrared |
NSurvey | 1 |
Frequency | 61 GHz |
Coverage | AllSky |
PixelScale | 7.5' |
PixelUnits | millikelvins |
Resolution | 0.35 degree beam size |
CoordinateSystem | Galactic |
Projection | HEALPix |
Epoch | 2000-2005 |
Reference |
LAMBDA archive
|
WMAP Five Year W-band
Short name[s] used to specify survey:WMAPW,WMAP W,WMAP-W
Description
These data represent the 5 year co-added maps for each of the five frequency bands
in the WMAP dataset. These energies of the bands and their widths are:
Band | Frequency (GHz) | Bandwidth (GHz) |
K | 23 | 5.5 |
Ka | 33 | 7.0 |
Q | 41 | 8.3 |
V | 61 | 14.0 |
W | 94 | 20.5 |
The original data are available at the LAMBDA archive.
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 WMAP data.
Provenance | WMAP Mission/LAMBDA archive |
Copyright | Public Domain |
Regime | Infrared |
NSurvey | 1 |
Frequency | 94 GHz |
Coverage | AllSky |
PixelScale | 7.5' |
PixelUnits | millikelvins |
Resolution | 0.22 degree beam size |
CoordinateSystem | Galactic |
Projection | HEALPix |
Epoch | 2000-2005 |
Reference |
LAMBDA archive
|
Optical surveys
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 | 600 THz (J or E band images with a few exceptions) |
Coverage | All-sky |
Scale | 1.7" |
Units | Scaled densities |
Resolution | Depends on plate. Typically 2" |
Coordinates | Equatorial |
Projection | Schmidt (distorted Tangent plane projection) |
Equinox | 2000 |
Epoch | 1945-1955 north, 1980-1990 south |
Reference |
Lasker, et al., 1990, A.J. 99
|
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 | 600 THz |
Coverage | North of -30 degrees declination |
Scale | 1.7" |
Units | Scaled densities |
Resolution | Depends on plate. Typically 2" |
Coordinates | Equatorial |
Projection | Schmidt (distorted Tangent plane projection) |
Equinox | 2000 |
Epoch | 1950-1955 |
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 | 600 THz |
Coverage | North of -30 degrees declination |
Scale | 1.7" |
Units | Scaled densities |
Resolution | Depends on plate. Typically 2" |
Coordinates | Equatorial |
Projection | Schmidt (distorted Tangent plane projection) |
Equinox | 2000 |
Epoch | 1945-1955 |
Reference |
Lasker, et al., 1990, A.J. 99
|
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 | 2 |
Frequency | 450-600 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 | 1984-1999 |
Reference |
Some information on the DSS2 is given in
McLean, 2000, The Second Generation Guide Star Catalog.
|
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 | Optical |
NSurvey | 2 |
Frequency | 450-600 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 better than 2". |
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.
|
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 | 2 |
Frequency | 450-600 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 better than 2". |
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.
|
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 | 6563 ? |
Coverage | All-sky |
PixelScale | 2.5' |
PixelUnits | Rayleighs (R) |
Resolution | 6' FWHM |
Coordinates | Galactic |
Equinox | 2000 |
Projection | Rectangular |
Epoch | 1997-2000 |
Reference |
"A Full-Sky H-alpha Template for Microwave Foreground Prediction" Douglas P. Finkbeiner 2003. This paper may be downloaded from
astro-ph.
|
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 | 600 THz |
Coverage | Patches of the sky, approximately 30% coverage |
PixelScale | 1.42" |
PixelUnits | |
Resolution | Depends on image. Typically 1.5" |
Coordinates | Equatorial |
Equinox | 2000 |
Projection | Radially distorted gnomonic |
Epoch | 1997-1999 |
Reference |
href=http://www.sdss.org> SDSS Web site
|
Sloan Digitized 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
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 | 300-750 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 Digitzed Sky Survey I-band
Short name[s] used to specify survey:SDSSi,SDSS i
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 | 300-750 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 Digitzed Sky Survey R-band
Short name[s] used to specify survey:SDSSr,SDSS r
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 | 300-750 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 Digitzed Sky Survey U-band
Short name[s] used to specify survey:SDSSu,SDSS u
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 | 300-750 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 Digitzed Sky Survey Z-band
Short name[s] used to specify survey:SDSSz,SDSS z
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 | 300-750 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
|
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 | 6563 ? |
Coverage | All-sky south of 15 |
PixelScale | 0.79'/pixel |
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. |
The Southern H-Alpha Sky Survey Atlas: Continuum-Corrected
Short name[s] used to specify survey:SHASSA-CC,SHASSA_CC,SHASSA CC
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 | 6563 ? |
Coverage | All-sky south of 15 |
PixelScale | 0.79'/pixel |
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. |
The Southern H-Alpha Sky Survey Atlas: H-alpha
Short name[s] used to specify survey:SHASSA-H,SHASSA_H,SHASSA H
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 | 6563 ? |
Coverage | All-sky south of 15 |
PixelScale | 0.79'/pixel |
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. |
The Southern H-Alpha Sky Survey Atlas: Smoothed
Short name[s] used to specify survey:SHASSA-SM,SHASSA Smoothed,SHASSA_Sm,SHASSA Sm
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 | 6563 ? |
Coverage | All-sky south of 15 |
PixelScale | 0.79'/pixel |
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. |
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 | 5 to 50 PHz (83, 171, 405, 555 Angstroms) |
PixelScale | 0.025 degrees/pixel |
PixelUnits | counts |
Resolution | ca. 2' |
CoordinateSystem | Equatorial |
Projection | Gnomonic/Tan |
Equinox | 2000 |
Epoch | 1991-1993 |
Reference |
Welsh et al, 1990, Opt.Eng. 29, 752. Bowyer and
Malina, 1991, in Extreme Ultraviolet Astronomy, 397.
|
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 | 5 to 50 PHz (83, 171, 405, 555 Angstroms) |
PixelScale | 0.025 degrees/pixel |
PixelUnits | counts |
Resolution | ca. 2' |
CoordinateSystem | Equatorial |
Projection | Gnomonic/Tan |
Equinox | 2000 |
Epoch | 1991-1993 |
Reference |
Welsh et al, 1990, Opt.Eng. 29, 752. Bowyer and
Malina, 1991, in Extreme Ultraviolet Astronomy, 397.
|
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 to 50 PHz (83, 171, 405, 555 Angstroms) |
PixelScale | 0.025 degrees/pixel |
PixelUnits | counts |
Resolution | ca. 2' |
CoordinateSystem | Equatorial |
Projection | Gnomonic/Tan |
Equinox | 2000 |
Epoch | 1991-1993 |
Reference |
Welsh et al, 1990, Opt.Eng. 29, 752. Bowyer and
Malina, 1991, in Extreme Ultraviolet Astronomy, 397.
|
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 | 5 to 50 PHz (83, 171, 405, 555 Angstroms) |
PixelScale | 0.025 degrees/pixel |
PixelUnits | counts |
Resolution | ca. 2' |
CoordinateSystem | Equatorial |
Projection | Gnomonic/Tan |
Equinox | 2000 |
Epoch | 1991-1993 |
Reference |
Welsh et al, 1990, Opt.Eng. 29, 752. Bowyer and
Malina, 1991, in Extreme Ultraviolet Astronomy, 397.
|
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 | 20 and 30 PHz (100 and 130 Angstroms) |
Coverage | all-sky |
PixelScale | 1 arcminute/pixel |
PixelUnit | Counts |
Resolution | 30 arcminutes |
Coordinates | Ecliptic |
Projection | Gnomonic |
Reference | |
ROSAT Wide Field Camera: F2
Short name[s] used to specify survey:wfcf2, ROSAT WFC F2
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 | 20 and 30 PHz (100 and 130 Angstroms) |
Coverage | all-sky |
PixelScale | 1 arcminute/pixel |
PixelUnit | Counts |
Resolution | 30 arcminutes |
Coordinates | Ecliptic |
Projection | Gnomonic (Tan) |
Reference | |
X-ray surveys
Swift BAT All-Sky Survey: Flux 14-195 keV
Short name[s] used to specify survey:BATFlux14-195,BATFlux0,BAT Flux 14-195,BATFlux
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
Swift BAT All-Sky Survey: Flux 14-24 keV
Short name[s] used to specify survey:BATFlux14-24,BATFlux1,BAT Flux 14-24
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
Swift BAT All-Sky Survey: Flux 24-50 keV
Short name[s] used to specify survey:BATFlux24-50,BATFlux2,BAT Flux 24-50
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
Swift BAT All-Sky Survey: Flux 50-100 keV
Short name[s] used to specify survey:BATFlux50-100,BATFlux3,BAT Flux 50-100
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
Swift BAT All-Sky Survey: Flux 100-195 keV
Short name[s] used to specify survey:BATFlux100-195,BATFlux4,BAT Flux 100-195
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
Swift BAT All-Sky Survey: Significance 14-195 keV
Short name[s] used to specify survey:BATSig14-195,BATSig0,BAT Sig 14-195,BATSig
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
Swift BAT All-Sky Survey: Significance 14-24 keV
Short name[s] used to specify survey:BATSig14-24,BATSig1,BAT Sig 14-24
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
Swift BAT All-Sky Survey: Significance 24-50 keV
Short name[s] used to specify survey:BATSig24-50,BATSig2,BAT Sig 24-50
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
Swift BAT All-Sky Survey: Significance 50-100 keV
Short name[s] used to specify survey:BATsig50-100,BATsig3,BAT sig 50-100
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
Swift BAT All-Sky Survey: Significance 100-195 keV
Short name[s] used to specify survey:BATsig100-195,BATsig4,BAT sig 100-195
Description
The BAT Hard X-ray Survey data is a 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 large array
of CdZnTe detectors (5000 cm2). The primary purpose of BAT is the
detection gamma-ray bursts and the BAT survey data is collected during
the search for gamma-ray bursts.
BAT is sensitive in the energy range 14-195 keV. The data from the
first 9 months of the survey is divided into 4 energy channels: 14-24,
24-50, 50-100, and 100-195 keV. Each of these is represented as separate
survey, and an averaged survey over all bands is also given.
The all sky maps are presented in two forms, the significance maps and
the flux maps. The significance maps are the count rate divided by
the noise (sigma RMS) in a region of the map around the position. The
noise is variable across the sky due to variable exposure and
systematic noise. The noise is Gaussian and and the significances can
be interpreted with the usual Gaussian probabilities. A threshold of
4.8 sigma for the blind detection of sources in the BAT survey
corresponds to about 1 false detection on the whole sky.
The BAT flux map is scaled from the Crab rate in the survey and
normalized to an assumed Crab spectrum of 10.4 E-2.15
photons.cm2/sec/keV. Due to the large number of randomly distributed
gamma-ray burst pointings that contribute to any point in the image,
this is an accurate characterization for the whole sky. The 4.8 sigma
threshold in the 9-month survey covers 80% of the sky at flux
threshold of 3.5x10-11 ergs/cm2/s in the 14-195 keV band and covers 1/3
of the sky near the ecliptic poles at 2.5x10-11 ergs/cm2/s.
Provenance |
NASA BAT Team
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 10 |
Frequency | 14-24, 24-50, 50-100m 100-195 keV |
Coverage | All-sky |
PixelScale | 5' |
PixelUnits | Statistical significance or Flux |
Resolution | 10' |
Coordinates | Galactic |
Equinox | |
Projection | Zenital Equal Area |
Epoch | 2007 |
Reference |
Tueller et al, 2008
|
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 numerious 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 can not 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 | 40-100 keV |
Coverage | Approximately one quarter of the sky |
Scale | 3.24 arc minutes/pix |
Units | Statistical significance, Flux |
Resolution | 12 arc minutes |
Coordinates | Equatorial |
Projection | Gnomonic |
Equinox | 1950 |
Epoch | 1989-1998 |
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
|
GRANAT/SIGMA
Short name[s] used to specify survey:GRANAT_SIGMA_sig, GRANAT/SIGMA
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 numerious 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 can not 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 | 40-100 keV |
Coverage | Approximately one quarter of the sky |
Scale | 3.24 arc minutes/pix |
Units | Statistical significance, Flux |
Resolution | 12 arc minutes |
Coordinates | Equatorial |
Projection | Gnomonic |
Equinox | 1950 |
Epoch | 1989-1998 |
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
|
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 EHz 2-20 keV |
CoordinateSystem | Ecliptic |
Projection | Cartesion |
Scale | 0.5x0.25 degrees |
Units | Counts/Secont |
Coverage | All-sky |
NSurvey | 1 |
Resolution | Approxmately 2 degrees |
Epoch | ca. 1978 |
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.
|
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 | 1 keV |
Coverage | Observation patches covering ~1.8% of the sky. |
PixelScale | 5" |
PixelUnits | |
Resolution | 1" |
Coordinates | Equatorial |
Equinox | 2000 |
Projection | Gnomonic |
Epoch | |
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 (significance and flux) |
Frequency | 20-40 keV |
Coverage | |
Scale | 6 arc minutes/pix |
Units | Statistical significance, Flux |
Resolution | approximately 1 degree |
Coordinates | Galactic |
Projection | Aitoff |
Epoch | March 2002 - May 2003 |
Reference |
INTEGRAL Guest Observer Facility
|
PSPC summed pointed observations, 1 degree cutoff, intensity
Short name[s] used to specify survey:PSPC1, PSPC1int, PSPC 1.0 Deg-Inten
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 | 0.3 EHz (.1-2.4 keV) |
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-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 | 0.3 EHz (.1-2.4 keV) |
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 | 1992-1994 |
Reference |
|
PSPC summed pointed observations, 2 degree cutoff, exposure
Short name[s] used to specify survey:PSPC2exp,PSPC 2.0 Deg-Expos
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 | 0.3 EHz (.1-2.4 keV) |
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 |
|
PSPC summed pointed observations, 2 degree cutoff, intensity
Short name[s] used to specify survey:PSPC2, PSPC2int, PSPC 2.0 Deg-Inten
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 | 0.3 EHz (.1-2.4 keV) |
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 thr
ough the ROSAT Guest Observer Facility, NASA GSFC. SkyView Rosat Survey Generation description.
|
ROSAT All-Sky X-ray Survey
Short name[s] used to specify survey:RASS.25keV, RASS 1/4 keV,RASS 0.25 keV
Description
The following is adapted from the MPI FTP site information: 7/16/97
These maps present the initial version of the results from the
ROSAT soft X-ray all-sky survey as presented in ApJ 454, 643.
The maps cover approximately 98% of the sky in the 1/4 keV, 3/4 keV,
and 1.5 keV bands, with about 2° angular resolution and high
sensitivity for low surface brightness extended features.
The effects of non-X-ray contamination and X-rays of solar system
origin have been eliminated to the greatest possible extent, but
discrete X-ray sources have not been removed.
The much improved angular resolution, statistical precision, and
completeness of coverage of these maps reveals considerable structure
over the entire 0.1-2.0 keV energy range that was not observed
previously. The data compare well with previous all-sky surveys in
terms of absolute normalization and zero point.
SkyView also has two other sets of surveys derived from the RASS data
with substantially higher resolution.
The surveys whose
names begin with RASS3 are counts maps with 45" pixels. The
RASS or RASSInt surveys are intensity maps generated by dividing
the counts maps with the exposure maps provided by MPE.
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 | 3 |
Frequency | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 40.5' |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Aitoff |
Epoch | ca. 1991 |
Reference |
S.L. Snowden, M.J. Freyberg, P.P. Plucinsky, J.H.M.M. Schmitt,
J. Trümper, W. Voges, R.J. Edgar, D. McCammon, W.T. Sanders:
Astrophysical Journal, Vol.454 (1995), pp.643-653
|
ROSAT All-Sky X-ray Survey 3/4 keV
Short name[s] used to specify survey:RASS.75keV, RASS 3/4 keV,RASS 0.75 keV
Description
The following is adapted from the MPI FTP site information: 7/16/97
These maps present the initial version of the results from the
ROSAT soft X-ray all-sky survey as presented in ApJ 454, 643.
The maps cover approximately 98% of the sky in the 1/4 keV, 3/4 keV,
and 1.5 keV bands, with about 2° angular resolution and high
sensitivity for low surface brightness extended features.
The effects of non-X-ray contamination and X-rays of solar system
origin have been eliminated to the greatest possible extent, but
discrete X-ray sources have not been removed.
The much improved angular resolution, statistical precision, and
completeness of coverage of these maps reveals considerable structure
over the entire 0.1-2.0 keV energy range that was not observed
previously. The data compare well with previous all-sky surveys in
terms of absolute normalization and zero point.
SkyView also has two other sets of surveys derived from the RASS data
with substantially higher resolution.
The surveys whose
names begin with RASS3 are counts maps with 45" pixels. The
RASS or RASSInt surveys are intensity maps generated by dividing
the counts maps with the exposure maps provided by MPE.
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 | 3 |
Frequency | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 40.5' |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Aitoff |
Epoch | ca. 1991 |
Reference |
S.L. Snowden, M.J. Freyberg, P.P. Plucinsky, J.H.M.M. Schmitt,
J. Trümper, W. Voges, R.J. Edgar, D. McCammon, W.T. Sanders:
Astrophysical Journal, Vol.454 (1995), pp.643-653
|
ROSAT All-Sky X-ray Survey 1.5 keV
Short name[s] used to specify survey:RASS1.5keV, RASS 1.5 keV
Description
The following is adapted from the MPI FTP site information: 7/16/97
These maps present the initial version of the results from the
ROSAT soft X-ray all-sky survey as presented in ApJ 454, 643.
The maps cover approximately 98% of the sky in the 1/4 keV, 3/4 keV,
and 1.5 keV bands, with about 2° angular resolution and high
sensitivity for low surface brightness extended features.
The effects of non-X-ray contamination and X-rays of solar system
origin have been eliminated to the greatest possible extent, but
discrete X-ray sources have not been removed.
The much improved angular resolution, statistical precision, and
completeness of coverage of these maps reveals considerable structure
over the entire 0.1-2.0 keV energy range that was not observed
previously. The data compare well with previous all-sky surveys in
terms of absolute normalization and zero point.
SkyView also has two other sets of surveys derived from the RASS data
with substantially higher resolution.
The surveys whose
names begin with RASS3 are counts maps with 45" pixels. The
RASS or RASSInt surveys are intensity maps generated by dividing
the counts maps with the exposure maps provided by MPE.
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 | 3 |
Frequency | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 40.5' |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Aitoff |
Epoch | ca. 1991 |
Reference |
S.L. Snowden, M.J. Freyberg, P.P. Plucinsky, J.H.M.M. Schmitt,
J. Trümper, W. Voges, R.J. Edgar, D. McCammon, W.T. Sanders:
Astrophysical Journal, Vol.454 (1995), pp.643-653
|
ROSAT All-Sky X-ray Survey Broad Band
Short name[s] used to specify survey:RASS3bb, RASS-Cnt Broad
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 three sets of surveys derived from the RASS data. The surveys whose
names begin with RASS3 are counts maps. The surveys with the names
RASS or RASSINT are intensity images. These are simply the ratios of the
counts maps and the exposure images produced by MPE. Both the counts maps and
the intensity images have 45" pixels. A third set of RASS surveys is available
int the surveys labeled RASS(.25|.75|1.5)keV. These are lower resolution
intensity surveys (40.5' pixels) wiprith where point sources have been removed.
They give the best sense of the background X-ray flux.
For the full-resolution RASS3 counts surveys
data are organized in 1378 RASS3 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 | 3 |
Frequency | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 45" |
PixelUnits | Counts |
Resolution | |
Coordinates | Equatorial |
Equinox | |
Projection | Gnomonic |
Epoch | |
Reference |
The ROSAT All-Sky Survey
|
ROSAT All-Sky X-ray Survey Hard Band
Short name[s] used to specify survey:RASS3hb, RASS-Cnt Hard
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 three sets of surveys derived from the RASS data. The surveys whose
names begin with RASS3 are counts maps. The surveys with the names
RASS or RASSINT are intensity images. These are simply the ratios of the
counts maps and the exposure images produced by MPE. Both the counts maps and
the intensity images have 45" pixels. A third set of RASS surveys is available
int the surveys labeled RASS(.25|.75|1.5)keV. These are lower resolution
intensity surveys (40.5' pixels) wiprith where point sources have been removed.
They give the best sense of the background X-ray flux.
For the full-resolution RASS3 counts surveys
data are organized in 1378 RASS3 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 | 3 |
Frequency | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 45" |
PixelUnits | Counts |
Resolution | |
Coordinates | Equatorial |
Equinox | |
Projection | Gnomonic |
Epoch | |
Reference |
The ROSAT All-Sky Survey
|
ROSAT All-Sky X-ray Survey Soft Band
Short name[s] used to specify survey:RASS3sb,RASS-Cnt Soft
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 three sets of surveys derived from the RASS data. The surveys whose
names begin with RASS3 are counts maps. The surveys with the names
RASS or RASSINT are intensity images. These are simply the ratios of the
counts maps and the exposure images produced by MPE. Both the counts maps and
the intensity images have 45" pixels. A third set of RASS surveys is available
int the surveys labeled RASS(.25|.75|1.5)keV. These are lower resolution
intensity surveys (40.5' pixels) wiprith where point sources have been removed.
They give the best sense of the background X-ray flux.
For the full-resolution RASS3 counts surveys
data are organized in 1378 RASS3 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 | 3 |
Frequency | 0.5-2 KeV |
Coverage | All-sky |
PixelScale | 45" |
PixelUnits | Counts |
Resolution | |
Coordinates | Equatorial |
Equinox | |
Projection | Gnomonic |
Epoch | |
Reference |
The ROSAT All-Sky Survey
|
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 | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 0.2 |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Zenithal Equal Area |
Epoch | ca. 1991 |
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
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 | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 0.2 |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Zenithal Equal Area |
Epoch | ca. 1991 |
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
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 | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 0.2 |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Zenithal Equal Area |
Epoch | ca. 1991 |
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
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 | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 0.2 |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Zenithal Equal Area |
Epoch | ca. 1991 |
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
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 | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 0.2 |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Zenithal Equal Area |
Epoch | ca. 1991 |
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
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 | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 0.2 |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Zenithal Equal Area |
Epoch | ca. 1991 |
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
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 | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 0.2 |
PixelUnits | 10-6counts/s |
Resolution | ca. 2° |
Coordinates | Galactic |
Projection | Zenithal Equal Area |
Epoch | ca. 1991 |
Reference |
S.L. Snowden, et al.,
Ap,J, Vol.485 (1997), pp.125
|
ROSAT All-Sky Broad Band Intenstiy
Short name[s] used to specify survey:RASS, RASS Broad
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 three sets of surveys derived from the RASS data. The surveys whose
names begin with RASS3 are counts maps. The surveys with the names
RASS or RASSINT are intensity images. These are simply the ratios of the
counts maps and the exposure images produced by MPE. Both the counts maps and
the intensity images have 45" pixels. A third set of RASS surveys is available
int the surveys labeled RASS(.25|.75|1.5)keV. These are lower resolution
intensity surveys (40.5' pixels) wiprith where point sources have been removed.
They give the best sense of the background X-ray flux.
For the full-resolution RASS intensity surveys
data are organized in 1378 RASS 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)
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 | 3 |
Frequency | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 45" |
PixelUnits | Counts/S |
Resolution | |
Coordinates | Equatorial |
Equinox | |
Projection | Gnomonic |
Epoch | |
Reference |
The ROSAT All-Sky Survey
|
ROSAT All-Sky Hard Band Intensity
Short name[s] used to specify survey:RASSHB, RASS-HB, RASS Hard
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 three sets of surveys derived from the RASS data. The surveys whose
names begin with RASS3 are counts maps. The surveys with the names
RASS or RASSINT are intensity images. These are simply the ratios of the
counts maps and the exposure images produced by MPE. Both the counts maps and
the intensity images have 45" pixels. A third set of RASS surveys is available
int the surveys labeled RASS(.25|.75|1.5)keV. These are lower resolution
intensity surveys (40.5' pixels) wiprith where point sources have been removed.
They give the best sense of the background X-ray flux.
For the full-resolution RASS intensity surveys
data are organized in 1378 RASS 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)
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 | 3 |
Frequency | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 45" |
PixelUnits | Counts/S |
Resolution | |
Coordinates | Equatorial |
Equinox | |
Projection | Gnomonic |
Epoch | |
Reference |
The ROSAT All-Sky Survey
|
ROSAT All-Sky Broad Band Intensity
Short name[s] used to specify survey:RASSSB, RASS Soft
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 three sets of surveys derived from the RASS data. The surveys whose
names begin with RASS3 are counts maps. The surveys with the names
RASS or RASSINT are intensity images. These are simply the ratios of the
counts maps and the exposure images produced by MPE. Both the counts maps and
the intensity images have 45" pixels. A third set of RASS surveys is available
int the surveys labeled RASS(.25|.75|1.5)keV. These are lower resolution
intensity surveys (40.5' pixels) wiprith where point sources have been removed.
They give the best sense of the background X-ray flux.
For the full-resolution RASS intensity surveys
data are organized in 1378 RASS 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)
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 | 3 |
Frequency | 0.1-2 KeV |
Coverage | All-sky |
PixelScale | 45" |
PixelUnits | Counts/S |
Resolution | |
Coordinates | Equatorial |
Equinox | |
Projection | Gnomonic |
Epoch | |
Reference |
The ROSAT All-Sky Survey
|
RXTE Allsky 3-20keV Significance
Short name[s] used to specify survey:RXTE3_20k_sig, RXTE AllSky 3-20keV
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; MPA, Garching, Germany
|
Copyright |
Public domain
|
Regime | X-ray |
NSurvey | 6 |
Frequency | 3-20keV, 3-8keV, 8-20keV |
Coverage | All-sky |b| > 3 |
PixelScale | .5x.5° pixel |
PixelUnits | Statistical significance, 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 °, M. Revnivtsev, S. Sazonov, M. Gilfanov, K. Jahoda 2004, A&A, 418, 927
|
RXTE Allsky 3-8keV Significance
Short name[s] used to specify survey:RXTE3_8k_sig, RXTE AllSky 3-8keV
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 | 6 |
Frequency | 3-20keV, 3-8keV, 8-20keV |
Coverage | All-sky |b| > 3 |
PixelScale | .5x.5° pixel |
PixelUnits | Statistical significance, 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 8-20keV Significance
Short name[s] used to specify survey:RXTE8_20k_sig, RXTE AllSky 8-20keV
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 | 6 |
Frequency | 8-20keV |
Coverage | All-sky |b| > 3 |
PixelScale | .5x.5° pixel |
PixelUnits | Statistical significance, 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
|
Gamma ray surveys
CGRO Compton Telescope: 3 channel data
Short name[s] used to specify survey: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 | 1-3 MeV, 3-10 MeV, 10-30 MeV |
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: 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, 100-100000 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 | 6 ZHz to 1 YHz (30-100 MeV, 100-10000 MeV) |
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: 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 | 6 ZHz to 1 YHz (30-100 MeV, 100-10000 MeV) |
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
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 | 6 ZHz to 1 YHz (30-100 MeV, 100-10000 MeV) |
Coverage | All-sky |
Resolution | ca. 5 degrees below 100 MeV, ca. 2 degrees above 100 MeV
|
PixelScale | 0.5 d/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
|
-------------- Other surveys --------------
Galaxy Explorer All Sky Survey: Near UV
Short name[s] used to specify survey: GalexNear,GALEX NEAR 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 October 8, 2008, SkyView uses the GALEX GR4 data release.
Provenance |
All data is downloaded from the
MAST GALEX archive.
|
Copyright |
Public domain.
|
Regime | UV |
NSurvey | 2 |
Frequency | Near UV: 1-1.7 PHz (2831-1771A), Far UV: 1.7-2.4 PHz (1786-1344A)
|
Coverage | All sky/patchy |
PixelScale | 1.5" |
PixelUnits | Intensity |
Resolution | 5" |
Coordinates | Equatorial |
Equinox | 2000 |
Projection | Tangent |
Epoch | ca. 2007 |
Reference |
The GALEX Guest Invesitigator and
MAST Archive sites provide documentation and
characteristics of the GALEX observatory and archive.
|
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 October 8, 2008 SkyView uses the GR4 data release for the entire sky.
Provenance |
All data is downloaded from the
MAST GALEX archive.
|
Copyright |
Public domain.
|
Regime | UV |
NSurvey | 2 |
Frequency | Near UV: 1-1.7 PHz (2831-1771A), Far UV: 1.7-2.4 PHz (1786-1344A)
|
Coverage | All sky/patchy |
PixelScale | 1.5" |
PixelUnits | Intensity |
Resolution | 5" |
Coordinates | Equatorial |
Equinox | 2000 |
Projection | Tangent |
Epoch | ca. 2007 |
Reference |
The GALEX Guest Invesitigator and
MAST Archive sites provide documentation and
characteristics of the GALEX observatory and archive.
|