| Name | Spectral Coverage | Description | Compliant? | Service URL |
|---|---|---|---|---|
| Digitized Sky Survey | Optical/Infrared | The Online Digitized Sky Surveys (DSS1 & 2) server at the ESO/ST-ECF Archive provides access to the CD-ROM set produced by the Space Telescope Science Institute through its Guide Star Survey group. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. The photographic plates were scanned to a pixel scale of about 1.7 arcseconds per pixel for the POSS, SERC, and Palomar Quick-V surveys, and to about 1.0 arcseconds per pixel for the POSS-II surveys. Images of any part of the sky may be extracted from the DSS, in either FITS or GIF format. | Yes (Details) |
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| Hubble Space Telescope Press Release Image Archive | Optical/Infrared/UV | The Hubble Space Telescope Press Release Image Archive is a pointed image archive of press release images from the Hubble Space Telescope. The resource provides a conditionally compliant simple image access (SIA) interface to access the image archive. SIA 1.0 compliance is conditional because press release images, in general, do not retain specific observation parameters like observation date and spectral bandpass. The TIFF or JPEG format images are highly processed (i.e., unsuited for astronomical analysis), and may contain annotations on top of the astronomical image. All images have associated valid world coordinate system metadata. Identical images may be available in the archive with different access identifiers, different image formats, or different pixel resolutions. | No (Details) Could not find metadata |
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| SIA Service for ROSAT Archive | X-ray | ROSAT image service for both all sky survey and all the pointed observations. | Yes (Details) |
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| MITVLA Gravitational Lens Snapshot Survey | not specified | The 19 year MITVLA gravitational survey contains over 5000 images. | No (Details) |
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| VO-Paris Southern ATlas SRC-J | Optical | This the second step in VO-Comlpiant publication of schmidt surveys of the southern sky digitized with MAMA microdensitometer at the Observatoire de Paris Image Analysis Centre (CAI). The pixel size is 10 micrometers (0,7 arc-sec). The SRC-J atlas will be followed by the southern part of POSS1 E | No (Details) |
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| VO-Paris MAMA ESO R Atlas | Optical | une proposition: This is the first step in a VO-compliant publication of Schmidt surveys of the southern sky digitized with the MAMA microdensitometer at the Observatoire de Paris Image Analysis Centre (CAI). The pixel size is 10 micrometers (0.7 arc-sec). The ESO-R atlas will be followed by the SRC-J and the southern part of the POSS1_E atlases. Catalogs of the detected objects will also be available. The bandpass is : close to R (combination: IIIaF + RG 630) | No (Details) |
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| Sloan Digitized Sky Survey G-band | Optical | 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 http://www.sdss.org SDSS Web site/a. | Yes (Details) |
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| First Digitized Sky Survey: Blue Plates | Optical | This survey uses the POSS1 Blue plates. | Yes (Details) |
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| First Digitized Sky Survey: Red Plates | Optical | This survey is the POSS1 Red plates from the original POSS survey. It covers the sky north of -30 degrees declination. | Yes (Details) |
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| 2nd Digitized Sky Survey (Blue) | Optical | P 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. | Yes (Details) |
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| HI All-Sky Continuum Survey | Radio | This survey is a mosaic of data taken at Jodrell Bank, Effelsberg and Parkes telescopes. The data was distributed in the NRAO iImages from the Radio Sky/i CD ROM. | Yes (Details) |
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| Bonn 1420 MHz Survey | Radio | This survey was taken with the Bonn Stockert 25m telescope. It was distributed on the NRAO iImages from the Radio Sky/i CD-ROM. This image was delivered as a four map mosaic but was combined into a single map before being included in iSkyView/i. | Yes (Details) |
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| VLA Low-frequency Sky Survey | Radio | 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. | Yes (Details) |
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| Dickey and Lockman HI map | Radio | This survey is derived from the 21cm maps presented by Dickey and Lockman in the iARAA/i 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 10sup20/sup. | Yes (Details) |
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| Schlegel, Finkbeiner and Davis 100 micron survey | Infrared | 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. | Yes (Details) |
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| Schlegel, Finkbeiner and Davis Dust Survey | Infrared | 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. | Yes (Details) |
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| SkyView Virtual Observatory | Radio/Infrared/Optical/UV/X-ray/Gamma-ray | SkyView is a Virtual Observatory on the Net. Astronomers can generate images of any portion of the sky at wavelengths in all regimes from radio to gamma-ray. Users tell SkyView the position, scale and orientation desired, and SkyView gives users an image made to their specification. The user need not worry about transforming between equinoxes or coordinate systesm, mosaicking submaps, rotating the image,.... SkyView handles these geometric issues and lets the user get started on astronomy. | Yes (Details) |
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| ROSAT Wide Field Camera: F1 | UV | 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. | Yes (Details) |
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| Improved Reprocessing of the IRAS Survey: 12 | Infrared | 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 iSkyView/i) 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. p More information about the IRIS dataset is available at http://www.cita.utoronto.ca/~mamd/IRIS the IRIS Web site/a whence most of the preceding description came. | Yes (Details) |
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| Westerbork Northern Sky Survey | Radio | The Westerbork Northern Sky Survey (iWENSS/i) 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''. p Further information on the survey including links to catalogs derived from the survey is available at the "http://www.strw.leidenuniv.nl/wenss" iWENSS/i web site/a. p The iWENSS/i survey is included on the bSkyView High Resolution Radio Coverage /b"http://skyview.gsfc.nasa.gov/images/high_res_radio.jpg" map/a. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates. p | Yes (Details) |
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| IRAS Sky Survey Atlas: 12 micron | Infrared | 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. p 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. p 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. p 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. | Yes (Details) |
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| The Southern H-Alpha Sky Survey Atlas: Continuum | Optical | 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: bH-alpha/b, bContinuum/b, bContinuum-Corrected/b (the difference of the H-alpha and Continuum images), and bSmoothed/b (median filtered to 5 pixel, or 4.0 arcminute, resolution to remove star residuals better). The "http://amundsen.swarthmore.edu/SHASSA"SHASSA web site/a has more details of the data and the status of this and related projects. Images can also be obtained from the "http://amundsen.astro.swarthmore.edu/SHASSA/#Images"Download Images/a section at the SHASSA site. | Yes (Details) |
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| Sydney University Molonglo Sky Survey | Radio | 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 ("http://www.physics.usyd.edu.au/astrop/most/" MOST /a), 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. p The survey was completed in 2007. Please note that the images still contain some telescope artifacts. Images can also be obtained from the "http://www.astrop.physics.usyd.edu.au/cgi-bin/postage.pl"SUMSS Postage Stamp Server/a. p 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. p | Yes (Details) |
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| ROSAT All-Sky X-ray Survey 3/4 keV | X-ray | i The following is adapted from the MPI FTP site information: 7/16/97 /ibr 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. p 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. | Yes (Details) |
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| ROSAT All-Sky Broad Band Intenstiy | X-ray | 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. p 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. p 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°.p Three bands are available through iSkyView/i UL LI broad band (0.1-2.4 keV) LI hard band (0.5-2.0 keV) LI soft band (0.1-0.4 keV) /ul | Yes (Details) |
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| ROSAT All-Sky X-ray Survey | X-ray | i The following is adapted from the MPI FTP site information: 7/16/97 /ibr 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. p 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. | Yes (Details) |
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| 4850 MHz Survey/GB6 | Radio | 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.P | Yes (Details) |
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| Two Micron All Sky Survey (H-Band) | Infrared | 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 Ksubs/sub (2.17 microns). p2MASS images and other data products can be obtained at the "http://irsa.ipac.caltech.edu/applications/2MASS/QL/"NASA/IPAC Infrared Science Archive/a | Yes (Details) |
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| ROSAT High Resolution Image Pointed Observations Mosaic: Intensity | X-ray | 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. | Yes (Details) |
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| Energetic Gamma-Ray Event Telescope: 10 channel data | Gamma-ray | 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. P The EGRET 3D map is comprised of ten channels with the following energy ranges: UL LIChannel 1 30-50 MeV LIChannel 2 50-70 MeV LIChannel 3 70-100 MeV LIChannel 4 100-150 MeV LIChannel 5 150-300 MeV LIChannel 6 300-500 MeV LIChannel 7 500-1000 MeV LIChannel 8 1000-2000 MeV LIChannel 9 2000-4000 MeV LIChannel 10 4000-10000 MeV /ul p The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV). | Yes (Details) |
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| H-alpha Full Sky Map | Optical | 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=10sup6/sup/4pi photons/cmsup2/sup/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 "http://astro.princeton.edu/~dfink/halpha/" H-Alpha Full-Sky Map web site/a. | Yes (Details) |
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| HEAO 1A | X-ray | 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 i SkyView /i is the map designated tt 322_15_tot_ecl_samp.img/tt in the ftp://legacy.gsfc.nasa.gov/heao1/data/a2/maps/heasarc_med_hed HEASARC FTP area/a. 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. p 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. | Yes (Details) |
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| INTEGRAL/Spectral Imager Galactic Center Survey | X-ray | 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).p 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. p Current data respresent the combination of all public observations as of September 1, 2004. | Yes (Details) |
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| GTEE 0035 MHz Radio survey | Radio | 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. p 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. p The southernmost tiles were only 287x100 pixels. We assumed that bottom row of these tiles (as compared with the others) was truncated. | Yes (Details) |
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| Energetic Gamma-Ray Event Telescope: Hard | Gamma-ray | 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. P The EGRET 3D map is comprised of ten channels with the following energy ranges: UL LIChannel 1 30-50 MeV LIChannel 2 50-70 MeV LIChannel 3 70-100 MeV LIChannel 4 100-150 MeV LIChannel 5 150-300 MeV LIChannel 6 300-500 MeV LIChannel 7 500-1000 MeV LIChannel 8 1000-2000 MeV LIChannel 9 2000-4000 MeV LIChannel 10 4000-10000 MeV /ul p The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV). | Yes (Details) |
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| Original Digitized Sky Survey | Optical | 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. P The following data are included: DL DTSouthern hemisphere DD 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. DTNorthern hemisphere dd 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 i SkyView /i. /DL | Yes (Details) |
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| Extreme Ultraviolet Explorer: 83 A | UV | The EUVE satellite surveyed the entire sky in the extreme ultraviolet through a set of four filters. The filters include: UL LILexan/Boron filter: peak at 83A (full range 50-180) LIAluminium/Carbon/Titanium : 171A (160-240) LIAluminium/Titanium/Antimony: 405A (345-605) LITin/SiO: 555A (500-740) /UL P The data currently in iSkyView/i is direct from the Center for EUVE. | Yes (Details) |
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| FIRST | Radio | 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 "http://sundog.stsci.edu/top.html" FIRST home page /a 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. P These FIRST data have been retrieved from the "ftp://archive.stsci.edu/pub/vla_first/data/" FIRST FTP archive /a at the "http://www.stsci.edu/resources" Space Telescope Science Institute/a. p The FIRST survey is included on the bSkyView High Resolution Radio Coverage /b"/images/high_res_radio.jpg" map/a. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates. | Yes (Details) |
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| CO Galactic Plane Survey | Radio | 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. P 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 "http://cfa-www.harvard.edu/cfa/mmw/MilkyWayinMolClouds.html" Millimeter-Wave Group site/a for more details | Yes (Details) |
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| CGRO Compton Telescope: 3 channel data | Gamma-ray | This survey is a maximum entropy solution to the data taken by the CompTel instrument on the i Compton /i 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 "http://cossc.gsfc.nasa.gov/cossc/cossc.html" Compton Observatory Science Support Center /a. P The maps were originally generated by the CompTel Instrument Team as three separate maps in the bands: UL LI1-3 MeV LI3-10 MeV LI10-30 MeV /ul P 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 i SkyView /i P | Yes (Details) |
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| Galaxy Explorer All Sky Survey: Far UV | UV | 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. p The iSkyView/i 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. p As of October 8, 2008 SkyView uses the GR4 data release for the entire sky. | Yes (Details) |
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| ROSAT All-Sky X-ray Survey 1.5 keV | X-ray | i The following is adapted from the MPI FTP site information: 7/16/97 /ibr 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. p 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. | Yes (Details) |
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| Galaxy Explorer All Sky Survey: Near UV | UV | 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. p The iSkyView/i 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. p As of October 8, 2008, SkyView uses the GALEX GR4 data release. | Yes (Details) |
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| CADC/HSTCA SIA service | Optical/UV | SIAP service for HST imaging data. This service currently queries and delivers new HST products originating from CADC such as ACS visit associations. | No (Details) Could not find metadata |
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| ROSAT All-Sky X-ray Survey 1.5 keV | X-ray | i The following is adapted from the MPI FTP site information: 7/16/97 /ibr 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. These maps may be used for scientific purposes as long as reference is made to the relevant publication | Yes (Details) |
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| IA2 Italian Center for Astronomical Archive: TNG | not specified | This SIAP service provides the public data from TNG (Telescopio Nazionale Galileo; Galileo Italian National Telescope) | No (Details) Could not find metadata |
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| Canadian Network for Observational Cosmology Image | Optical | The CNOC1 Cluster Survey targeted 16 rich X-ray selected galaxy clusters at 0.17 & z & 0.55. Observations were made from Jan 1993 to Mar 1995 using the CFHT Multi-Object-Spectrograph (MOS). Gunn g an | No (Details) Could not find metadata |
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| NRAO VLBA 2cm Survey | Radio | The VLBA 2cm Survey is an imaging survey of compact radio sources at 15 GHZ. The VLBA provides images having milliarcsecond resolution. The observations are performed in a "snapshot" observing mode (1 scan per hour of 4-5 minute duration, over a 8 hour period). We achieve a dynamic range of typically exceeding 1000:1, with a typical noise limit (rms) of 0.35 milli-Jansky. | No (Details) |
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| NRAO VLA Pipeline Images | Radio | The NRAO VLA Archive Survey is a collection of images that are being produced by an automated pipelined process. These images are constructed from archived VLA data taken from observations in all VLA array configurations, and all observing frequency bands above 1 GHz. The NVAS is an ongoing project. New images are added to the NRAO Archive on a weekly basis. As of this publication date, 2007-Nov-30, there are approximately 65000 NVAS images available. | No (Details) |
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| NRAO VLA Sky Survey at 1.4 GHz | not specified | The NRAO VLA Sky Survey (NVSS) is a 1.4 GHz continuum survey covering the entire sky north of -40 deg declination. A detailed description appears in the 1998 May issue of The Astronomical Journal (Condon, J. J., Cotton, W. D., Greisen, E. W., Yin, Q. F., Perley, R. A., Taylor, G. B., & Broderick, J. J. 1998, AJ, 115, 1693). | Yes (Details) |
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| Faint Images of the Radio Sky at Twenty-centimeters | not specified | FIRST -- Faint Images of the Radio Sky at Twenty-cm -- 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 survey uses the Very Large Array in "B" array. | Yes (Details) |
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| NRAO VLBA Calibrator Source Survey | Radio | A catalog containing milliarcsecond-accurate positions of 1332 extragalactic radio sources distributed over the northern sky is presented-the Very Long Baseline Array Calibrator Survey (VCS1). The positions have been derived from astrometric analysis of dual- frequency 2.3 and 8.4 GHz VLBA snapshot observations; in a majority of cases, images of the sources are also available. These radio sources are suitable for use in geodetic and astrometric experiments, and as phase-reference calibrators in high-sensitivity astronomical imaging. The VCS1 is the largest high-resolution radio survey ever undertaken and triples the number of sources available to the radio astronomy community for VLBI applications. In addition to the astrometric role, this survey can be used in active galactic nuclei, Galactic, gravitational lens, and cosmological studies. | Yes (Details) |
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| Cosmic Background Explorer DIRBE | Infrared | P 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. P 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. p 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°. P These COBE DIRBE maps are a combination original ten band passes with the following wavelengths: UL LIBand 1 - 1.25 µm LIBand 2 - 2.2 µm LIBand 3 - 3.5 µm LIBand 4 - 4.9 µm LIBand 5 - 12 µm LIBand 6 - 25 µm liBand 7 - 60 µm liBand 8 - 100 µm liBand 9 - 140 µm liBand 10 - 240 µm /ul p The default two dimensional array uses Band 8 (100 µm). P 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 ) p 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). | Yes (Details) |
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| PSPC summed pointed observations, 2 degree cutoff, counts | X-ray | The ROSAT PSPC surveys were generated by i SkyView /i 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 "http://skyview.gsfc.nasa.gov/help/pspc_generation.html" companion document/a. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two. p 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 (ie.g./i, to do statistical analysis). p 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. p Detailed information regarding the creation of the ROSAT suveys can be found in the "http://skyview.gsfc.nasa.gov/help/pspc_generation.html" ROSAT PSPC Generation Document/a. | Yes (Details) |
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| GRANAT/SIGMA | X-ray | 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'.p 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.p 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.p 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. p 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. p 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 2.8esup-3/sup cnts/s in the units, provided in 'flux' maps | Yes (Details) |
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| Near-Earth Asteriod Tracking System Archive | Optical | 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. http://skys.gsfc.nasa.gov/skymorph/skymorph.htmlSkyMorph/a 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. p Unlike most iSkyView/i surveys, the NEAT data are extremely irregular in their spatial distribution. iSkyView/i'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. p 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. p NEAT data consists primarily of groups of three images taken with separations of 20 minutes and almost identical positions. i SkyView /i 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. p 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. P 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. | Yes (Details) |
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| NVSS | Radio | The NRAO VLA Sky Survey is currently underway at the VLA and data is made available to the public as soon as processed. i SkyView /i has copied the NVSS intensity data from the NRAO FTP site. The full NVSS survey data includes information on other Stokes parameters. Note that i SkyView /i may be slightly out of date with regard to the latest releases of NVSS data. The current information was copied in November 1997. p 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: ol li 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. li Lists of discrete sources. /ol 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. P The NVSS survey is included on the bSkyView High Resolution Radio Coverage /b"http://skyview.gsfc.nasa.gov/images/high_res_radio.jpg" map/a. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates. p | Yes (Details) |
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| Swift BAT All-Sky Survey: Significance 14-195 keV | X-ray | 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 cmsup2/sup). 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. p 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. p 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. p The BAT flux map is scaled from the Crab rate in the survey and normalized to an assumed Crab spectrum of 10.4 Esup-2.15/sup photons.cmsup2/sup/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 3.5x10sup-11/sup ergs/cmsup2/sup/s in the 14-195 keV band and covers 1/3 of the sky near the ecliptic poles at 2.5x10sup-11/sup ergs/cmsup2/sup/s. | Yes (Details) |
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| Cosmic Background Explorer DIRBE | Infrared | 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. P 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. p 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°. P These COBE DIRBE maps are a combination original ten band passes with the following wavelengths: UL LIBand 1 - 1.25 µm LIBand 2 - 2.2 µm LIBand 3 - 3.5 µm LIBand 4 - 4.9 µm LIBand 5 - 12 µm LIBand 6 - 25 µm liBand 7 - 60 µm liBand 8 - 100 µm liBand 9 - 140 µm liBand 10 - 240 µm /ul p The default two dimensional array uses Band 8 (100 µm). P 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 ) p 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). | Yes (Details) |
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| Swift BAT All-Sky Survey: Flux 14-195 keV | X-ray | 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 cmsup2/sup). 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. p 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. p 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. p The BAT flux map is scaled from the Crab rate in the survey and normalized to an assumed Crab spectrum of 10.4 Esup-2.15/sup photons.cmsup2/sup/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 3.5x10sup-11/sup ergs/cmsup2/sup/s in the 14-195 keV band and covers 1/3 of the sky near the ecliptic poles at 2.5x10sup-11/sup ergs/cmsup2/sup/s. | Yes (Details) |
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| PSPC summed pointed observations, 2 degree cutoff, intensity | X-ray | The ROSAT PSPC surveys were generated by i SkyView /i 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 "http://skyview.gsfc.nasa.gov/help/pspc_generation.html" companion document/a. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two. p 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 (ie.g./i, to do statistical analysis). p 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. p Detailed information regarding the creation of the ROSAT suveys can be found in the "http://skyview.gsfc.nasa.gov/help/pspc_generation.html" ROSAT PSPC Generation Document/a. | Yes (Details) |
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| ROSAT All-Sky X-ray Background Survey: Band 1 | X-ray | 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. p 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. p The energy range for the bands corresponds to: tabletrthBand/ththEnergy range (keV)/th/tr trtdBand 1/tdtd0.11 - 0.284/tdtr trtdBand 2/tdtd0.14 - 0.284/tdtr trtdBand 3/tdtd0.2 - 0.83/td/tr trtdBand 4/tdtd0.44 - 1.01/tdtr trtdBand 5/tdtd0.56 - 1.21/tdtr trtdBand 6/tdtd0.73 - 1.56/tdtr trtdBand 7/tdtd1.05 - 2.04/tdtr /table 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. p 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. | Yes (Details) |
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| ROSAT All-Sky X-ray Survey Broad Band | X-ray | 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. p 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. p 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°.p Three bands are available through iSkyView/i UL LI broad band (0.1-2.4 keV) LI hard band (0.5-2.0 keV) LI soft band (0.1-0.4 keV) /ul Data was dowloaded from the "http://www.xray.mpe.mpg.de/rosat/survey/rass-3/main/help.html#ftp"MPE FTP site/a. | Yes (Details) |
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| PSPC summed pointed observations, 1 degree cutoff, intensity | X-ray | The ROSAT PSPC surveys were generated by i SkyView /i 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 "http://skyview.gsfc.nasa.gov/help/pspc_generation.html" companion document/a. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two. p 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 (ie.g./i, to do statistical analysis). p 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. p Detailed information regarding the creation of the ROSAT suveys can be found in the "http://skyview.gsfc.nasa.gov/help/pspc_generation.html" ROSAT PSPC Generation Document/a. | Yes (Details) |
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| PSPC summed pointed observations, 2 degree cutoff, exposure | X-ray | The ROSAT PSPC surveys were generated by i SkyView /i 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 "http://skyview.gsfc.nasa.gov/help/pspc_generation.html" companion document/a. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two. p 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 (ie.g./i, to do statistical analysis). p 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. p Detailed information regarding the creation of the ROSAT suveys can be found in the "http://skyview.gsfc.nasa.gov/help/pspc_generation.html" ROSAT PSPC Generation Document/a. | Yes (Details) |
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| RXTE Allsky 3-20keV Significance | X-ray | 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. p 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).p p 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 ~6esup-12/sup erg/s/cmsup2/sup, 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). | Yes (Details) |
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| Cosmic Lens All-Sky Survey | not specified | The Cosmic Lens All-Sky Survey (CLASS) is an international collaborative program which has obtained high-resolution radio images of over 10000 flat-spectrum radio sources in order to create the largest and best studied statistical sample of radio-loud gravitationally lensed systems. With this survey, combined with detailed studies of the lenses found therein, constraints can be placed on the expansion rate, matter density, and dark energy (e.g. cosmological constant, quintessence) content of the Universe that are complementary to and independent of those obtained through other methods. CLASS is aimed at identifying lenses where multiple images are formed from compact flat-spectrum radio sources, which should be easily identifiable in the radio maps. Because CLASS is radio-based, dust obscuration in lensing galaxies is not a factor, and the relative insensitivity of the instrument to environmental conditions leads to nearly uniform sensitivity and resolution over the entire survey. | No (Details) |
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| The ISO Data Archive InterOperability System | not specified | The Infrared Space Observatory (ISO) was the world's first true orbiting infrared observatory. Equipped with four highly-sophisticated and versatile scientific instruments, it was launched by Ariane in November 1995 and provided astronomers world-wide with a facility of unprecedented sensitivity and capabilities for a detailed exploration of the Universe at infrared wavelengths. The two spectrometers (SWS and LWS), a camera (ISOCAM) and an imaging photo-polarimeter (ISOPHOT) jointly covered wavelengths from 2.5 to around 240 microns with spatial resolutions ranging from 1.5 arcseconds (at the shortest wavelengths) to 90 arcseconds (at the longer wavelengths). Its 60 cm diameter telescope was cooled by superfluid liquid helium to temperatures of 2-4 K. | Yes (Details) |
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| Epic Image SIAP of the SSC Interface for the 2XMMi Catalogue | not specified | 2XMMi is the incremental second catalogue of serendipitous X-ray sources from the European Space Agency's (ESA) XMM-Newton observatory. The catalogue has been constructed by the XMM-Newton Survey Science Centre (SSC) on behalf of ESA. The collection contains 4119 images covering all XMMi pointing. Images are merged form pictures of the 3 XMM cameras (PN, MOS1 and MOS2). Image size matches the XMM field of view size (r~15arcmin) | No (Details) Could not find metadata Could not find data |
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| 2MASS All-Sky Atlas Image Service | Infrared | This service provides access to and information about the 2MASS All- Sky Atlas Images. Atlas Images delivered by this service are in FITS format and contain full WCS information in their headers. Additionally, the image headers contain photometric zero point information. 2MASS Atlas Images are suitable for quantitative photometric measurements. | Mostly (Details) |
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| HST Cosmic Evolution Survey | Optical | COSMOS (P.I. Nicholas Scoville, California Institute of Technology, USA/CA) is an HST Treasury Program to survey a 2 square degree equatorial field, centered on RA=10:00:28.6 and DEC=+02:12:21.0 with the ACS in the I band of the VIMOS equatorial field. Parallel observations with WFPC2 and NICMOS were also obtained. | Mostly (Details) Could not find data |
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| HST WFPC2 Spiral Galaxies | Optical | Holwerda et al. examined 32 HST/WFPC2 archival fields of 29 spiral galaxies (Sab and later) for their paper The Opacity of Spiral Galaxy Disks. IV. Radial Extinction Profiles from Counts of Distant Galaxies Seen through Foreground Disks (2005, AJ,129:1396-1411). The majority of the data are from the Cepheid distance scale Key Project. The explicit goal was to provide deep mosaics in both V- and I-band with a better sampling in order to identify background galaxies through the foreground disk. | Mostly (Details) Could not find data |
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| HST Ultra Deep Field (UDF) Images | Optical | The ACS Ultra Deep Field (UDF) is a cycle 12 survey carried out using the Advanced Camera for Surveys (ACS) on HST and taking advantage of the Director's Discretionary time. The UDF consists of a single ultra- deep field (412 orbits in total taken in 4 bands) within the CDF-S GOODS area. It is the deepest image ever obtained with Hubble. This service also includes data from the UDF follow-Up program by PI Massimo Stiavelli and colleagues obtained under HST cycle 14 program 10632 titled Searching for galaxies at z6.5 in the Hubble Ultra Deep Field (also known as UDF05). | Mostly (Details) Could not find data |
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| Hubble Space Telescope gallery of Interacting and Merging Galaxies | Optical | A gallery of images of interacting and merging galaxies from Hubble Space Telescope press releases. These data were originally acquired under HST programs 6276, 10592, 11091, 11092, and 11095, and include WFPC2 images of Arp 87, NGC 6050, and Arp 148 (and two ACS images of Arp 148). | Mostly (Details) Could not find data |
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| CADC/CGPS Image Search | Radio | Image search and retrieval for Canadian Galactic Plane Survey (CGPS) HI continuum images. | Yes (Details) |
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| CADC/GEMINI Image Search | Infrared/Optical | Image Search and retrieval for Gemini imaging data. This service is quite new and contains a modest amount of content. | Yes (Details) |
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| CADC/IRIS Image Search | Infrared | The Improved Reprocessing of the IRAS Survey (IRIS) enhances significantly the general quality of the ISSA plates in the four bands (12, 25, 60 and 100 microns). 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. [from IRIS Overview at http://www.cita.utoronto.ca/~mamd/IRIS/IrisOverview.html] | Yes (Details) |
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| The IRAS Galaxy Atlas | Infrared | The IRAS Galaxy Atlas (IGA) is a high resolution image atlas of the Galactic plane at 60 and 100 microns, it has been produced using the IRAS satellite data. The HIRES program was developed by the Infrared Processing and Analysis Center (IPAC) to produce high resolution (~ 1 arcmin) images from IRAS data using the Maximum Correlation Method (H.H. Aumann, J.W. Fowler and M. Melnyk, 1990, Astronomical Journal, 99, 1674). | Mostly (Details) |
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| The MAST Image Scrapbook | Infrared/Optical/UV/EUV | The MAST Spectral/Image Scrapbook is designed to allow users to take a quick look at sample data in the MAST archive of a particular astronomical object of interest. It is set up here as an interoperability project between IRSA and MAST. | Mostly (Details) |
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| The Spitzer Wide-area InfraRed Extragalactic Survey | Optical | * A wide-area, high galactic latitude imaging survey conducted using the Spitzer MIPS far-infrared and IRAC mid-infrared cameras. The satellite data will be complemented by an extensive program of ground-based optical, near-infrared and radio observations. | Mostly (Details) |
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| Coma Legacy Survey SIAP | Optical | Simple Image Access Service for COMALS survey WARNING! This is a test for ComaLS data publishing. The official data release will be available at May 2008. | No (Details) |
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| Galaxy Evolution Explorer | UV | The Galaxy Evolution Explorer (GALEX), a NASA Small Explorer mission, is performing the first all-sky, deep imaging and spectroscopic ultraviolet surveys in space. The prime goal of GALEX is to study star formation in galaxies and its evolution with time. | Mostly (Details) |
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| HST ACS mosaic images of M51 | Optical | In January 2005, the Hubble Heritage Team obtained a large 4-color mosaic image of the Whirlpool Galaxy NGC 5194 (M51), and its companion NGC 5195, with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST observing program 10452, PI: Steven V. W. Beckwith). A six-pointing ACS WFC mosaic of the galaxy pair M51 was obtained in four filters: B, V, I, and H-alpha. | Mostly (Details) Could not find data |
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| HST Galaxy Evolution from Morphology and SEDs | Optical | GEMs is a large-area (800 arcmin 2) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the Hubble Space Telescope. Centered on the Chandra Deep Field-South, it covers an area of ~ 28'x28', or about 120 HDF areas, to a depth of MAB(F606W)=28.5(5s) for compact sources. Focusing on the redshift range ~ 0.2z1.1, GEMS provides morphologies and structural parameters for nearly 10,000 galaxies where redshift estimates, luminosities, and SEDs exist from COMBO-17. | Mostly (Details) Could not find data |
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| GALEX Atlas of Nearby Galaxies | UV | The GALEX Atlas of Nearby Galaxies contains images of 1034 nearby galaxies recently observed by the GALEX satellite in its far- ultraviolet (FUV; 1516A) and near-ultraviolet (NUV; 2267A) bands. The Atlas was prepared by A. Gil de Paz,S. Boissier, B.F. Madore, M. Seibert and associated members of the GALEX Team. The full paper is posted on astroph/0606440 and will be published in ApJS in 2007. | Mostly (Details) Could not find data |
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| Observations of neutron stars | Optical/Infrared | Broad-band photometry of the pulsars, images in FITS format | No (Details) Could not find metadata Could not find data |
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| Sloan Digital Sky Survey DR5 - Images | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) |
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| HST Archival Pure Parallels Project | Optical | The Archival Pure Parallel Project processed and combined about 2,000 WFPC2 images, primarily in the wide UBVI filters, obtained in parallel with other HST instruments. Combined, drizzled, cosmic-ray cleaned images were produced for each pointing. These data can be used to address a wide range of science topics: measuring the cosmic shear on scales from 20'' to 2'; discovering ~ 50 starforming galaxies at z ~ 4; finding optical counterparts to AGNs in wide-area radio and X-ray catalogs; improving the determination of the scale length of the Galactic disk; and studying stellar populations down to 1 solar mass for about 25 separate lines of sight in the Magellanic Clouds. | Mostly (Details) Could not find data |
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| HST-ACS GOODS data within Chandra Deep Field South (CDFS) | not specified | This SIAP service provides the public HST-ACS GOODS data within the VVDS-CDFS. | Mostly (Details) Could not find data |
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| Great Observatories Origins Deep Survey (GOODS) Cutout Service | Optical | GOODS aims to unite extremely deep observations from NASA's Great Observatories, the Spitzer Space Telescope, Hubble, and Chandra, ESA's XMM-Newton, and from the most powerful ground-based facilities, to survey the distant universe to the faintest flux limits across the broadest range of wavelengths. GOODS will survey a total of roughly 320 square arcminutes in two fields centered on the Hubble Deep Field North and the Chandra Deep Field South. | Yes (Details) |
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| Great Observatories Origins Deep Survey (GOODS) - | Optical | GOODS aims to unite extremely deep observations from NASA's Great Observatories, the Spitzer Space Telescope, Hubble, and Chandra, ESA's XMM-Newton, and from the most powerful ground-based facilities, to survey the distant universe to the faintest flux limits across the broadest range of wavelengths. GOODS will survey a total of roughly 320 square arcminutes in two fields centered on the Hubble Deep Field North and the Chandra Deep Field South. | Mostly (Details) Could not find data |
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| Digitized Sky Survey 2 - Infrared | Optical | The Digitized Sky Survey comprises a set of all-sky photographic surveys in E, V, J, R, and N bands conducted with the Palomar and UK Schmidt telescopes. The 6.5-degree x 6.5-degree plates are scanned using a modified PDS microdensitometer to a pixel scale of about 1.7 arcseconds per pixel for the POSS, SERC, and Palomar Quick-V surveys, and to about 1.0 arcseconds per pixel for the POSS-II surveys. Images of any part of the sky may be extracted from the DSS, in either FITS or GIF format. | No (Details) Could not find metadata |
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| Digitized Sky Survey 2 | Optical | The Digitized Sky Survey comprises a set of all-sky photographic surveys in E, V, J, R, and N bands conducted with the Palomar and UK Schmidt telescopes. The 6.5-degree x 6.5-degree plates are scanned using a modified PDS microdensitometer to a pixel scale of about 1.7 arcseconds per pixel for the POSS, SERC, and Palomar Quick-V surveys, and to about 1.0 arcseconds per pixel for the POSS-II surveys. Images of any part of the sky may be extracted from the DSS, in either FITS or GIF format. | No (Details) Could not find metadata |
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| Digitized Sky Survey 1 | Optical | The Digitized Sky Survey comprises a set of all-sky photographic surveys in E, V, J, R, and N bands conducted with the Palomar and UK Schmidt telescopes. The 6.5-degree x 6.5-degree plates are scanned using a modified PDS microdensitometer to a pixel scale of about 1.7 arcseconds per pixel for the POSS, SERC, and Palomar Quick-V surveys, and to about 1.0 arcseconds per pixel for the POSS-II surveys. Images of any part of the sky may be extracted from the DSS, in either FITS or GIF format. | No (Details) Could not find metadata |
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| Digitized Sky Survey 2 - Blue | Optical | The Digitized Sky Survey comprises a set of all-sky photographic surveys in E, V, J, R, and N bands conducted with the Palomar and UK Schmidt telescopes. The 6.5-degree x 6.5-degree plates are scanned using a modified PDS microdensitometer to a pixel scale of about 1.7 arcseconds per pixel for the POSS, SERC, and Palomar Quick-V surveys, and to about 1.0 arcseconds per pixel for the POSS-II surveys. Images of any part of the sky may be extracted from the DSS, in either FITS or GIF format. | No (Details) Could not find metadata |
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| Digitized Sky Survey 2 - Red | Optical | The Digitized Sky Survey comprises a set of all-sky photographic surveys in E, V, J, R, and N bands conducted with the Palomar and UK Schmidt telescopes. The 6.5-degree x 6.5-degree plates are scanned using a modified PDS microdensitometer to a pixel scale of about 1.7 arcseconds per pixel for the POSS, SERC, and Palomar Quick-V surveys, and to about 1.0 arcseconds per pixel for the POSS-II surveys. Images of any part of the sky may be extracted from the DSS, in either FITS or GIF format. | No (Details) Could not find metadata |
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| HST trans-Neptunian Objects Search field images | Optical | The "TNO Search Field" images are the sidereally summed images of a search for trans-Neptunian objects (TNOs) using the Wide Field Camera of the HST/ACS instrument. The observations were taken under Cycle 11 program GO-9433, "The Size Distribution of Kuiper Belt Bodies," with G. Bernstein as PI. The TNO search consisted of approximately 96x400 s exposures in the F606W filter for each of six contiguous ACS fields of view. The TNO search field is approximately 6'x10', centered near 14h 07M 53.3s -11d 21' 38'' (J2000). | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR2 - Filter z | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) |
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| Sloan Digital Sky Survey DR2 - Filter g | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) |
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| Hubble Space Telescope Preview Images | Optical | Quick-look preview images produced and processed by CADC. Data from the following HST instruments are included: WFPC, WFPC2, STIS, NICMOS, FOC, and ACS. | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR2 - Filter u | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) |
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| Sloan Digital Sky Survey DR2 - Filter r | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) |
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| Sloan Digital Sky Survey DR2 - Filter i | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) |
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| Sloan Digital Sky Survey DR1 - Filter u | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR1 - Filter r | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| VLA Faint Images of the Radio Sky at Twenty Centimeters (FIRST) | Radio | Faint Images of the Radio Sky at Twenty-cm (FIRST) is a systematic survey of the North and South Galactic caps begun in 1993, using the NRAO Very Large Array (VLA) . Typical images are comprised of 1150x1550 1.8" pixels with 5" resolution. Source catalogs are also available including peak and integrated flux densities generated from the high resolution coadded images. The survey yields very accurate (1 arcsec rms) radio positions of faint (1 mJy/beam) compact sources. The areas observed were chosen to coincide with the Sloan Digital Sky Survey. | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR1 - Filter g | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| Ultraviolet Imaging Telescope (UIT) | UV | The Ultraviolet Imaging Telescope UIT was one of three ultraviolet telescopes on the ASTRO-1 mission flown on the space shuttle Columbia during 2-10 December 1990. The same three instruments were later flown on the space shuttle Endeavour from 3-17 March 1995, as part of the ASTRO-2 mission. Exposures were obtained on 70-mm photographic film in the 1200-3300 Ã… range using broadband filters and later digitized using a Perkin-Elmer microdensitometer. Image resolution was 3'' over a 40' field of view. Overall, UIT-1 obtained 821 exposures of 66 targets, and UIT-2 obtained 758 images of 193 targets. | Mostly (Details) Could not find data |
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| HST Hubble Deep Field | Optical | The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image a typical field at high galactic latitude in four wavelength passbands as deeply as reasonably possible. In order to optimize observing in the time available, a field in the northern continuous viewing zone (CVZ) was selected and images were taken for 10 consecutive days, or approximately 150 orbits. Shorter 1-orbit images were also obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were carried out from 18-30 December 1995, and the data are available to the community for study. | Mostly (Details) Could not find data |
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| Digitized Sky Survey 1 - Blue | Optical | The Digitized Sky Survey comprises a set of all-sky photographic surveys in E, V, J, R, and N bands conducted with the Palomar and UK Schmidt telescopes. The 6.5-degree x 6.5-degree plates are scanned using a modified PDS microdensitometer to a pixel scale of about 1.7 arcseconds per pixel for the POSS, SERC, and Palomar Quick-V surveys, and to about 1.0 arcseconds per pixel for the POSS-II surveys. Images of any part of the sky may be extracted from the DSS, in either FITS or GIF format. | No (Details) Could not find metadata |
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| Chandra X-Ray Observatory Data Archive | X-ray | The Chandra X-ray Observatory is the U.S. follow-on to the Einstein Observatory. Chandra was formerly known as AXAF, the Advanced X-ray Astrophysics Facility, but renamed by NASA in December, 1998. Originally three instruments and a high-resolution mirror carried in one spacecraft, the project was reworked in 1992 and 1993. The Chandra spacecraft carries a high resolution mirror, two imaging detectors, and two sets of transmission gratings. Important Chandra features are: an order of magnitude improvement in spatial resolution, good sensitivity from 0.1 to 10 keV, and the capability for high spectral resolution observations over most of this range. | No (Details) |
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| HST Hubble HELIX Observations | Optical | For the 14 hours of peak Leonid meteoroid flux in November 2002, the Hubble Space Telescope was pointed away from the radiant, and the solar arrays were oriented to minimize their cross-section. By coincidence, one of the nearest and largest planetary nebulae, the Helix Nebula (NGC 7293), was nearly opposite the incoming Leonids and could be observed. A "Hubble Helix Team" (below) of volunteers led by Margaret Meixner (STScI) organized a nine-orbit campaign to observe the Helix with the ACS, WFPC2, NICMOS, and STIS. | Mostly (Details) Could not find data |
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| HST Hubble Deep Field South | Optical | A second Hubble Deep Field campaign was carried out between late September and October of 1998. The raw, pipeline calibrated and reprocessed data were released to the community on November 23, 1998. The rationale for undertaking a second deep field campaign followed from the wealth of information that has come out of HDF-N, and from the desire to provide a point of focus for similar studies of the distant universe from southern-hemisphere facilities. Simultaneous, parallel observations were made with the three HST instruments STIS, WFPC2 and NICMOS of separate, neighboring fields. As was the case for HDF-N, approximately 150 consecutive orbits were devoted to a single telescope pointing. | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR3 - Filter r | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| MAST Image Scrapbook | Optical/UV/Infrared | The MAST Spectral/Image Scrapbook is designed to allow users to take a quick look at sample data in the MAST archive of a particular astronomical object of interest. It is particularly useful if the user is not already familiar with the datasets involved. The imaging missions currently included in the scrapbook are: HST/WFPC2,HST/STIS,HST/FOC,Astro/UIT | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR3 - Filter g | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR3 - Filter i | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR4 - Images | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR1 - Filter i | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| NOAO Science Archive | Optical | The NOAO Science Archive has been developed to provide access to processed datasets from the NOAO Surveys Program. Future holdings will include many other scientifically interesting raw and processed NOAO data. | Yes (Details) |
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| Sloan Digital Sky Survey DR3 - Filter z | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR3 | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR1 | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR2 | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) |
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| Sloan Digital Sky Survey DR3 - Filter u | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| Sloan Digital Sky Survey DR4 | Optical | The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | Mostly (Details) Could not find data |
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| SAI Supernova light curve catalogue | not specified | Service allows to plot supernova light curves online, as well as various distributions of supernova. | No (Details) Could not find metadata Could not find data |
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| Hubble Space Telescope multi-color ACS mosaic of M82 | Optical | In March 2006, the Hubble Heritage Team obtained a large 4-color (B, V, I, and H-alpha) mosaic image of the M82 with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope. | Mostly (Details) Could not find data |
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| Hubble Ultra Deep Field Follow-Up (UDF05) | Optical | PI Massimo Stiavelli and colleagues obtained an HST cycle 14 program titled "Searching for galaxies at z6.5" in the Hubble Ultra Deep Field (also known as UDF05). The program was conceived as a follow-on program to the Hubble Ultra Deep Field (UDF) program and was designed to obtain deep ACS (F606W, F775W, F850LP) imaging in the area of the original UDF NICMOS parallel fields. | Mostly (Details) Could not find data |
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| Hubble Space Telescope Heritage Press Release Images | Optical | WFPC2 and ACS images used to create the Heritage project color composite press releases. The data has been expertly prepared, significantly beyond the standard pipeline processing. This usually involves careful image registration, combination, and cleaning via drizzling, making it ready for further scientific analysis and educational use. These data will typically be made available at the time of the associated press release. | Mostly (Details) Could not find data |
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| Hubble Space Telescope ACS Nearby Galaxy Survey (ANGST) | Optical | The ACS Nearby Galaxy Survey observed roughly 14 million stars in 69 galaxies. The survey explored a region called the "Local Volume," and the galaxy distances ranged from 6.5 million light-years to 13 million light-years from Earth. The Local Volume resides beyond the Local Group of galaxies, an even nearer collection of a few dozen galaxies within about 3 million light-years of our Milky Way Galaxy. The observations were made in November 2006 with Hubble's Advanced Camera for Surveysi (ACS). | Mostly (Details) Could not find data |
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| Space Telescope A901/902 Galaxy Evolution Survey (STAGES) | Optical | STAGES is a large area (0.5x0.5 degree) survey of the complex Abell 901(a,b)/902 multiple-cluster system at z=0.165. An 80-tile imaging mosaic in F606W was conducted in HST cycle 13 with the HST/ACS instrument. | Mostly (Details) Could not find data |
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| HST ACS Coma cluster (Abell 1656) Treasury Survey (COMA) | Optical | The HST ACS Coma cluster Treasury survey is a deep two-passband imaging survey of one of the nearest rich clusters of galaxies, the Coma cluster (Abell 1656). | Mostly (Details) Could not find data |
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| Hubble Space Telescope Snapshots of 3CR Radio Galaxies | Infrared | The revised 3C catalogue (3CR, Bennett 1962) forms a flux-limited sample of the most radio-powerful sources in the northern hemisphere. Over the decade and a half of HST operation we have performed "snapshot" imaging from the near-IR to the near-UV of a large number of these sources. Most recently we have completed a NICMOS 1.6 micron survey of low-redshift (z less than 0.3) 3CR sources (Madrid et al. 2006, Floyd et al 2008). The fully-reduced data for all 101 sources included in those papers are presented here in numerical order. | Mostly (Details) Could not find data |
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| Hubble Space Telescope Ultraviolet Images of the UDF and HDF | UV | Wavelength coverage of the Hubble Ultra Deep Field (UDF) has been extended to ultraviolet wavelength observations. Observations include ACS-SBC images in the Far-UV {1500 Angstrom} and WFPC2 images in the Near-UV {F300W} during excution of the HST Treasury program 10403 ( PI Harry Teplitz -- California Institute of Technology). Included with this set of data are ACS/SBC observations of the Hubble Deep Field (HDF) North. | Mostly (Details) Could not find data |
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| CADC/JCMT Image Search | Millimeter | Image search and retrieval of JCMT images. The collection e currently contains SCUBA products at 450 and 850um. | Yes (Details) |
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| The Extended IRAS Galaxy Atlas | Infrared | The Extended IRAS Galaxy Atlas (EIGA) is an extension of the original IRAS Galaxy Atlas (IGA) to b = 6.7 deg.. High resolution images at 60 microns and 100 microns have been produced to match the latitude coverage of radio continuum observations obtained as part of the Canadian Galactic Plane Survey (CGPS). Also associated with the EIGA and IGA is the Mid-Infrared Galaxy Atlas (MIGA). | Mostly (Details) |
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| Spitzer First Look Survey (FLS) -- NOAO ELAIS N1 -- R | Optical | The Spitzer First Look Survey has obtained several pointings with the NOAO MOSAIC camera on the Kitt Peak 4m telescope covering the ELAIS N1 region in the R-band. This region is also part of the SWIRE project. Available to the public are image FITS files, bad pixel maps, exposure maps and source catalogs of each pointing. | Mostly (Details) |
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| Spitzer First Look Survey (FLS) -- NOAO Extragalactic -- R | Optical | The Spitzer First Look Survey has obtained approximately 30 pointings with the NOAO MOSAIC camera on the Kitt Peak 4m telescope covering the entire extragalactic First Look Survey region in the R-band. Available to the public are image FITS files, bad pixel maps, exposure maps and source catalogs of each pointing. | Mostly (Details) |
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| The Surface Photometry Catalogue of the ESO-Uppsala Galaxies Simple Image Access | Optical | Simple Image Access Service for ESOLV catalog | No (Details) |
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| Cosmic Evolution Survey with HST | Radio | The COSMOS Archive serves data taken for the Cosmic Evolution Survey with HST (COSMOS) project, using IRSA's general search service, Atlas. COSMOS is an HST Treasury Project to survey a 2 square degree equatorial field with the ACS camera. | Mostly (Details) |
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| The Mid-Infrared Galaxy Atlas | Infrared | The Mid-Infrared Galaxy Atlas (MIGA) is a high resolution image atlas of the Galactic plane at 12 microns and 25 microns, it has been produced using the HIRES processed infrared data from the IRAS satellite. It is a counterpart to the far-infrared IRAS Galaxy Atlas (IGA) and the Extended IRAS Galaxy Atlas (EIGA). | Mostly (Details) |
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| SIAP Service Hubble Space Telescope preview images | Optical/UV | SIAP service for HST preview images. Supported instruments: WFPC2 ACS NICMOS FOC. | Yes (Details) |
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| CADC/HST Image Search | Optical/UV | Image search and retrieval for HST imaging data. The collection currently includes calibrated ACS observations and stacks (associations) and stacks from the WFPC2 Association project. | Yes (Details) |
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| Spitzer First Look Survey (FLS) -- Ancillary VLA Data | Radio | The Spitzer First Look Survey has obtained VLA radio data. Available to the public is a catalog of radio sources along with a mosaic of 35 VLA pointings taken during 2001 and 2002, representing 240 hours in B-array at 1.4 GHz. | Mostly (Details) |
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| 2MASS All-Sky Quicklook Image Service | Infrared | This service provides access to and information about the 2MASS All-Sky Quicklook Images. The Quicklook Images delivered by this service are restored from lossy-compressed files in FITS format with full WCS information contained in the image headers. These images are suitable for position measurements, finding charts and visual inspection of the near-infrared sky. | Mostly (Details) |
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| CADC Image Search | Millimeter/Infrared/Optical/UV | Image search and retrieval for all calibrated CADC images and advanced products. This service is based on the same content as the archive-specific image search services provided by CADC. | Yes (Details) |
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| INT-WFS: images | not specified | The INT Wide Field Survey (WFS) used the Wide Field Camera (~0.3 square degrees per exposure ) on the 2.5m Isaac Newton Telescope (INT). The project was initiated in August 1998 with a duration of up to five years. Multicolour data have been obtained over 200+ square degrees to a typical depth of ~25 mag (U through Z). This service provides whole-CCD images calibrated for photometry and astrometry. | No (Details) Could not find data |
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| The IRAS Sky Survey Atlas | Infrared | The IRAS Sky Survey Atlas (ISSA) is a survey of 98% of the sky in four bands with effective wavelengths of 12, 25, 60 and 100 microns, which was done during a ten month period from January to November, 1983. The ISSA covers the sky with 430 fields. Each field is a 12.5 deg. by 12.5 deg. region centered every 10 deg. along declination bands which are spaced 10 deg. apart. | Mostly (Details) |
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| 2MASS Large Galaxy Atlas | Infrared | The high sensitivity and angular resolution of the 2MASS Large Galaxy Atlas (LGA) images allows closer inspection of diverse stellar populations, large-scale structures such as spirals, bulges, warps and bars, star formation regions and evolution of galaxies. This image atlas represents the first uniform, all-sky, view of galaxies as seen in the near-infrared wavelength window that is most sensitive to the dominant mass component of galaxies. | Mostly (Details) |
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| CADC/CFHT Image Search | Optical | Image search and retrieval for CFHT imaging data. The current collection includes calibrated public data from CFHTLS and PI observing programs. | Yes (Details) |
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| The Midcourse Space Experiment Data Atlas | Infrared | The Midcourse Space Experiment (MSX), a Ballistic Missile Defense Organization satellite, was launched in April 1996. The first ten months of the mission were devoted to mid-infrared observations with a solid hydrogen-cooled telescope. This instrument had five line-scanned focal plane arrays that spanned the spectral region from 4.2 to 26 microns. | Mostly (Details) |
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| CADC/MACHO Image Search | Optical | Image search and retrieval for MACHO imaging data. | Yes (Details) |
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| The Infrared Telescope in Space Data Atlas | Infrared | The Infrared Telescope in Space (IRTS) is a cryogenically cooled, small infrared telescope that flew from March - April in 1995. It surveyed approximately 10% of the sky with a relatively wide beam during its 20 day mission. Four focal-plane instruments , the Near-Infrared Spectrometer (NIRS), the Mid-Infrared Spectrometer (MIRS), the Far-Infrared Line Mapper (FILM), and the Far-Infrared Photometer (FIRP) made simultaneous observations of the sky at wavelengths ranging from 1 to 1000 um. | Mostly (Details) |
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| 2MASS 6X Lockman Hole Ancillary Data Atlas | Infrared | These Lockman Hole (LH) data represent a preliminary analysis of the deep 2MASS observations of this region, and are not a product endorsed by the 2MASS project. These data are described in The Astronomical Journal, Volume 125, Issue 5, pp. 2521-2530 "A Deep 2MASS survey of the Lockman Hole" by Beichman et al. | Mostly (Details) |
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| The NASA/IPAC Extragalactic Database Image Data Atlas | Radio/Millimeter/Infrared/Optical/UV/EUV/X-ray/Gamma-ray | NED is built around a master list of extragalactic objects for which cross-identifications of names have been established, accurate positions and redshifts entered to the extent possible, and some basic data collected. Bibliographic references relevant to individual objects have been compiled, and abstracts of extragalactic interest are kept on line. Detailed and referenced photometry, position, and redshift data, have been taken from large compilations and from the literature. NED also includes images for over 773,000 extragalactic objects from 2MASS, from the literature, and from the Digitized Sky Survey. NED's data and references are being continually updated, with revised versions being put on-line every 2-3 months. | Mostly (Details) |
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| VLA-A Array AL218 Texas Survey Source Snapshots (AL218) | Radio | The VLA-A Texas Survey consists of a sample of objects extracted from the earlier Texas Interferometer 365 MHz Survey of radio sources covering a strip of sky from approximately -35.5 degrees declination to +71.5 degrees declination, and complete to flux densities of 0.25 Jy, with positional accuracies of ~1 arcsecond in RA and DEC. The sample is a subset of 71 sources drawn from the area of one optical Schmidt sky survey plate (covering ~6.5x6.5 degrees), Region S861, centered at approximately RA=190.640822109, DEC=-0.273834224277 (J2000), from the UK Schmidt SRC-J Survey. The Region S861 was initially chosen because it represented the combination of the deepest UK Schmidt plate material (the best optical survey material available at the time of the sample definition in 1989) and the highest galactic latitude, thereby emphasizing the extragalactic nature of the survey and also maximizing the likelihood of having more optical detections. Much more recently, the area of this plate has been covered by a number of important sky surveys including 2MASS, NRAO VLA FIRST, and the Sloan Digital Sky Survey (SDSS) which is now public. In particular, the availability of the Sloan Survey data provides 5-band ugriz color information at optical wavelengths, to depth of g,r=22.2. | Mostly (Details) Could not find data |
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| HST Ultraviolet Atlas of Nearby Galaxies | UV | A pictorial atlas of UV (2300 Å) images, obtained with the Hubble Space Telescope (HST) Faint Object Camera, of the central 22''× 22'' of 110 galaxies (Maoz, Filippenko, Ho, Macchetto, Rix, & Schneider 1996). The observed galaxies are an unbiased selection constituting about one half of a complete sample of all large (D6 arcmin) and nearby (V 2000 km/s ) galaxies. This is the first extensive UV imaging survey of normal galaxies. The data are useful for studying star formation, low-level nuclear activity, and UV emission by evolved stellar populations in galaxies. At the HST resolution (~ 0.05''), the images display an assortment of morphologies and UV brightnesses. These include bright nuclear point sources, compact young star clusters scattered in the field or arranged in circumnuclear rings, centrally-peaked diffuse light distributions, and galaxies with weak or undetected UV emission. We measure the integrated ~2300 Å flux in each image, and classify the UV morphology. | Mostly (Details) Could not find data |
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| The Integral Science Data Archive InterOperability System | not specified | INTEGRAL (The International Gamma-Ray Astrophysics Laboratory) is the second medium-sized mission of ESA's Horizon 2000 Science Programme. INTEGRAL is dedicated to the fine spectroscopy (E/deltaE = 500) and fine imaging (angular resolution: 12 arcmin FWHM) of celestial gamma-ray sources in the energy range 15 keV to 10 MeV with concurrent source monitoring in the X-ray (3-35 keV) and optical (V-band, 550 nm) energy ranges. The INTEGRAL payload consists of the two main gamma-ray instruments, the spectrometer SPI , the imager IBIS and two monitors, the X-ray monitor JEM-X and the optical monitor OMC . All instruments are coaligned, covering simultaneously a very broad energy range for the study of high energy astrophysical sources. The INTEGRAL Science Operations Centre (ISOC) is responsible for the definition of scientific operations including the instrument configuration for each observation, the mission planning and implementation of the observing programme. | No (Details) |
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| The XMM-Newton Science Archive InterOperability System | not specified | The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations. Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis. | Mostly (Details) |
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| The MACHO Project Image Archive SIAP Service | Optical | The MACHO Project was a collaboration between scientists at the Mt. Stromlo and Siding Spring Observatories, the Center for Particle Astrophysics at the Santa Barbara, San Diego, and Berkeley campuses of the University of California, and the Lawrence Livermore National Laboratory. Our primary aim was to test the hypothesis that a significant fraction of the dark matter in the halo of the Milky Way is made up of objects like brown dwarfs or planets: these objects have come to be known as MACHOs, for MAssive Compact Halo Objects. The signature of these objects is the occasional amplification of the light from extragalactic stars by the gravitational lens effect. The amplification can be large, but events are extremely rare: it was necessary to monitor photometrically several million stars for a period of 10 years in order to obtain a useful detection rate. For this purpose we built a two channel system that employed eight 2048*2048 CCDs, mounted on the 50 inch telescope at Mt. Stromlo. The MACHO project data archive consists of approximately 127,000 two-colour images of fields collected between 1992 and 2003 covering the large and small Magellanic clouds and the galactic bulge and two-colour light-curves for approximately 18 million stars in the LMC and galactic bulge. | No (Details) |
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| Maidanak Observatory SIAP Query | not specified | Observations of (mainly) lensed quasars from Maidanak Observatory, Uzbekhistan | Mostly (Details) Could not find data |
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| SIAP Interface to Heidelberg Digitized Astronomical Plates | not specified | Scans of plates obtained at Landessternwarte Heidelberg-Königstuhl and German-Spanish Astronomical Center (Calar Alto Observatory), Spain, 1900 through 1999. | Mostly (Details) Could not find data |
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| SFD IR | Infrared | 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. A map proportional to dust column density is also calculated using this information and data from 240 microns. | Mostly (Details) Could not find data |
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| WENSS | Radio | The Westerbork Northern Sky Survey (<i>WENSS</i>) 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''. <p> Further information on the survey including links to catalogs derived from the survey is available at the <a href="http://www.strw.leidenuniv.nl/wenss"> <i>WENSS</i> web site</a>. <p> The <i>WENSS</i> survey is included on the <b>SkyView High Resolution Radio Coverage </b><a href="http://skyview.gsfc.nasa.gov/images/high_res_radio.jpg"> map</a>. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates. <p> | Yes (Details) |
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| IRAS | Infrared | 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. <p> 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. <p> There are occasional pixels in the IRAS maps which are given as NULL values. Unless these are explicitly trapped by user software, thes | Yes (Details) |
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| SUMSS | Radio | 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 (<a href="http://www.physics.usyd.edu.au/astrop/most/"> MOST </a>), 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. <p> As of 3/19/2000 35% of the survey has been completed. This is an early release of the data. Please note that the images still contain some telescope artifacts. Images can also be obtained from the <a href="http://www.astrop.physics.usyd.edu.au/cgi-bin/postage.pl">SUMSS Postage Stamp Server</a>. <p> 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. <p> The SUMSS survey is included on the <b>SkyView High Resolution Radio Coverage </b><a | Yes (Details) |
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| FIRST | Radio | 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 <a href="http://sundog.stsci.edu/top.html"> FIRST home page </a> 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. <P> These FIRST data have been retrieved from the <a href="ftp://archive.stsci.edu/pub/vla_first/data/"> FIRST FTP archive </a> at the <a href="http://www.stsci.edu/resources"> Space Telescope Science Institute</a>. <p> The FIRST survey is included on the <b>SkyView High Resolution Radio Coverage </b><a href="/images/high_res_radio.jpg"> map</a>. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates. | Yes (Details) |
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| NVSS | Radio | The NRAO VLA Sky Survey is currently underway at the VLA and data is made available to the public as soon as processed. <i> SkyView </i> has copied the NVSS intensity data from the NRAO FTP site. The full NVSS survey data includes information on other Stokes parameters. Note that <i> SkyView </i> may be slightly out of date with regard to the latest releases of NVSS data. The current information was copied in November 1997. <P> The NVSS survey is included on the <b>SkyView High Resolution Radio Coverage </b><a href="http://skyview.gsfc.nasa.gov/images/high_res_radio.jpg"> map</a>. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates. <p> | Yes (Details) |
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| DSS1 | Optical | his 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. i | Mostly (Details) Could not find data |
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| GB6 | Radio | 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.<P> | Yes (Details) |
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| HAlpha | Optical | 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=10<sup>6</sup>/4pi photons/cm<sup>2</sup>/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 <a href="http://astro.princeton.edu/~dfink/halpha/"> H-Alpha Full-Sky Map web site</a>. | Yes (Details) |
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| ROSAT/PSPC | X-ray | The ROSAT PSPC surveys were generated by SkyView as mosaics from publically available PSPC observations. Approximately 15% of the sky is covered by one or more PSPC observation. These are scattered over the sky but concentrate on targets of interest. Note that a query to the SIA service will return a link regardless of whether there are any observations at the given region. A total of 9 maps were created with a count, exposure and intensity map for each of three different cutoff radii. Since the spatial resolution of the PSPC was a strong function of offset from the center of the field of view, use of the smaller cutoffs is recommended when looking for evidence of spatial extent. However, the small cutoff maps have much smaller total sky coverage. | Mostly (Details) Could not find data |
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| NEAT | Optical | 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. <a href=http://skys.gsfc.nasa.gov/skymorph/skymorph.html>SkyMorph</a> 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. <p> Unlike most <i>SkyView</i> surveys, the NEAT data are extremely irregular in their spatial distribution. <i>SkyView</i>'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 | Yes (Details) |
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| EGRET | Gamma Ray | <P> 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. <P> The EGRET 3D map is comprised of ten channels with the following energy ranges: <UL> <LI>Channel 1 30-50 MeV <LI>Channel 2 50-70 MeV <LI>Channel 3 70-100 MeV <LI>Channel 4 100-150 MeV <LI>Channel 5 150-300 MeV <LI>Channel 6 300-500 MeV <LI>Channel 7 500-1000 MeV <LI>Channel 8 1000-2000 MeV <LI>Channel 9 2000-4000 MeV <LI>Channel 10 4000-10000 MeV </ul> <p> The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV). | Yes (Details) |
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| EUVE | EUV | The EUVE satellite surveyed the entire sky in the extreme ultraviolet through a set of four filters. The filters include: <UL> <LI>Lexan/Boron filter: peak at 83A (full range 50-180) <LI>Aluminium/Carbon/Titanium : 171A (160-240) <LI>Aluminium/Titanium/Antimony: 405A (345-605) <LI>Tin/SiO: 555A (500-740) </UL> <P> The data currently in <i>SkyView</i> is direct from the Center for EUVE. | Yes (Details) |
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| HRI | X-ray | 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. | Yes (Details) |
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| FIRST | FIRST -- Faint Images of the Radio Sky at Twenty-cm -- 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 survey uses the Very Large Array in "B" array. | Yes (Details) |
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| CLASS | The Cosmic Lens All-Sky Survey (CLASS) is an international collaborative program which has obtained high-resolution radio images of over 10000 flat-spectrum radio sources in order to create the largest and best studied statistical sample of radio-loud gravitationally lensed systems. With this survey, combined with detailed studies of the lenses found therein, constraints can be placed on the expansion rate, matter density, and dark energy (e.g. cosmological constant, quintessence) content of the Universe that are complementary to and independent of those obtained through other methods. CLASS is aimed at identifying lenses where multiple images are formed from compact flat-spectrum radio sources, which should be easily identifiable in the radio maps. Because CLASS is radio-based, dust obscuration in lensing galaxies is not a factor, and the relative insensitivity of the instrument to environmental conditions leads to nearly uniform sensitivity and resolution over the entire survey. | Yes (Details) |
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| VCS | A catalog containing milliarcsecond-accurate positions of 1332 extragalactic radio sources distributed over the northern sky is presented-the Very Long Baseline Array Calibrator Survey (VCS1). The positions have been derived from astrometric analysis of dual-frequency 2.3 and 8.4 GHz VLBA snapshot observations; in a majority of cases, images of the sources are also available. These radio sources are suitable for use in geodetic and astrometric experiments, and as phase-reference calibrators in high-sensitivity astronomical imaging. The VCS1 is the largest high-resolution radio survey ever undertaken and triples the number of sources available to the radio astronomy community for VLBI applications. In addition to the astrometric role, this survey can be used in active galactic nuclei, Galactic, gravitational lens, and cosmological studies. | Yes (Details) |
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| SIA service | A Simple Image Access Protocol service for the reduced images of the Isaac Newton Telescope wide-field survey. | No (Details) Could not find metadata |
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| SIA service | Optical | A Simple Image Access Protocol service (pointed-observation type) giving access to the reduced images of the Isaac Newton Telescope Photometric Halpha Survey (IPHAS). | No (Details) Could not find data |
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| SIA service | A SIAP service for the SWIRE 1.0 images in the ELAIS N1 region. This is an atlas-image service. | No (Details) Could not find metadata |
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| SIA service | A SIAP service for the SWIRE 1.0 images in the ELAIS N1 region. This is an atlas-image service. | No (Details) Could not find metadata |
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| 2MASS | Infrared | A Simple Image Access protocol thjat gives access to the 2MASS images | No (Details) Could not find metadata |
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| SDSSDR4-Colour | Fixed. Seee ivo://roe.ac.uk/services/SIAPDR4-images for reasons why. Rest of description follows unchanged from ivo://sdss.jhu/services/SIAPDR4-CutOut. The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | No (Details) |
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| SDSSDR4 | The JHU registry entry ivo://sdss.jhu/services/SIAPDR4-images contains an accessURL which does not satisfy the SIAP standard since it includes FORMAT keyword. This is a (hopefully) temporary entry in which has this been corrected. The contact details above are for the author of this registry entry. Rest of description follows below, unaltered. The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey | No (Details) |
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| 1420MHz | Radio | This survey was taken with the Bonn Stockert 25m telescope. It was distributed on the NRAO <i>Images from the Radio Sky</i> CD-ROM. This image was delivered as a four map mosaic but was combined into a single map before being included in <i>SkyView</i>. | Yes (Details) |
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| 408MHz | Radio | This survey is a mosaic of data taken at Jodrell Bank, Effelsberg and Parkes telescopes. The data was distributed in the NRAO <i>Images from the Radio Sky</i> CD ROM. | Yes (Details) |
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| CO | Radio | <A NAME=CO> CO</A> <P> 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. <P> Users should be aware that both the angular resolution and the sensitivity varies from region to region in the velocity-integra | Yes (Details) |
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| Comptel | Gamma Ray | <P> This survey is a maximum entropy solution to the data taken by the CompTel instrument on the <i> Compton </i> 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 <a href="http://cossc.gsfc.nasa.gov/cossc/cossc.html"> Compton Observatory Science Support Center </a>. <P> The maps were originally generated by the CompTel Instrument Team as three separate maps in the bands: <UL> <LI>1-3 MeV <LI>3-10 MeV <LI>10-30 MeV </ul> <P> 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 <i> SkyView </i> <P> | Yes (Details) |
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| DSS | Optical | 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. <P> The following data are included: <DL> <DT>Southern hemisphere <DD> 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 th | Yes (Details) |
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| DSS2 | Optical | <A NAME=DSS2>Second Generation Digitized Sky Survey</A> This survey includes high-resolution all sky optical images in two colors. This survey is not local to <i>SkyView</i>, it is served remotely from the <a href=http://www-gsss.stsci.edu> ST ScI </a>. Processing of the survey is ongoing. The current state is of each of the elements is described in the <a href=http://www-gsss.stsci.edu/PlateMaterial/plateMaterial.htm#DSSIIPlates> plate status table </a> at the ST ScI. <P> Data are retrieved from the ST ScI site in 18' tiles that are cached at the <I>SkyView</i> server. Thus users may note that when multiple images are retrieved from near the same region, the first request takes substantially longer. <p> 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 This is not one of the standard projections offered as an output by<i> SkyView</i>. | Yes (Details) |
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| HEAO1A | X-ray | The HEAO-1 spacecraft was launched into low earth orbit on 12 August, 1977. Its orbit was very nearly circular with an apogee of 445 km, inclination of 22.75°, and orbital period of 93 minutes. During the bulk of the mission, the spacecraft operated in a scanning mode in which it rotated with a period of 35 minutes, scanning out great circles of constant ecliptic longitude. Every twelve hours, the spin axis would be realigned with the Sun, adjusting the longitude of the great circle by roughly half a degree. Thus, afte1r six months, the spacecraft would have scanned the entire sky. After the first 100 days, the scanning was interupted periodically to performed pointed observations. These pointings became more frequent until 9 January, 1979, when the attitude control gas supply ran out. The satellite re-entered the Earth's atmosphere on 14 March, 1979. <p> HEAO-1 was equipped with four instrument packages. This file contains an all-sky map made from roughly six months of scanning data from the A2 instrument. T | Yes (Details) |
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| INTEGRALSPI_gc | X-ray | 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).<p> 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. <p> Current data respresent the combination of all public observations as of September 1, 2004. | Yes (Details) |
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| PSPC1 | X-ray | <P> The ROSAT PSPC surveys were generated by <i> SkyView </i> as mosaics from publically available PSPC observations. The original survey included all data available before October 1, 1994. The revised 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 <a href="http://skyview.gsfc.nasa.gov/help/pspc_generation.html"> companion document</a>. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two. <p> The revised data generally should be used for all processing. The older survey is currently being retained for compatibility purposes but may be deleted if usage drops off. <p> Nine new <i> SkyView </i> surveys have actually been added. Only two of these are immediately visible within the Form inter | Yes (Details) |
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| PSPC2 | X-ray | <P> The ROSAT PSPC surveys were generated by <i> SkyView </i> as mosaics from publically available PSPC observations. The original survey included all data available before October 1, 1994. The revised 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 <a href="http://skyview.gsfc.nasa.gov/help/pspc_generation.html"> companion document</a>. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two. <p> The revised data generally should be used for all processing. The older survey is currently being retained for compatibility purposes but may be deleted if usage drops off. <p> Nine new <i> SkyView </i> surveys have actually been added. Only two of these are immediately visible within the Form inter | Yes (Details) |
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| RASS3 | X-ray | <P> <P> 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. Data are organized in 1378 RASS3 fields each 6.4° x 6.4° covering the whole sky. Neighboring fields are overlapping by at least 0.23°. Three bands are available through <i>SkyView</i> (dowloaded from the <a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-3/main/help.html#ftp">MPE FTP site</a>): <UL> <LI> broad band (0.1-2.4 keV) <LI> hard band (0.5-2.0 keV) <LI> soft band (0.1-0.4 keV) </ul> | Yes (Details) |
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| SFD100m | Infrared | <P> 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. | Yes (Details) |
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| SFDdust | Infrared | <P> 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. | Yes (Details) |
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| 2MASS | Infrared | 2MASS data were collected by uniformly scanning the entire sky in three near-infrared bands to detect and characterize point sources brighter than about 1 mJy in each band, with signal-to-noise ratio (SNR) greater than 10, using a pixel size of 2.0''. This achieves an 80,000-fold improvement in sensitivity relative to earlier surveys. 2MASS used two new, highly-automated 1.3-m telescopes, one at Mt. Hopkins, AZ, and one at CTIO, Chile. Each telescope is equipped with a three-channel camera, each channel consisting of a 256 by 256 array of HgCdTe detectors, capable of observing the sky simultaneously at J (1.25 microns), H (1.65 microns), and K<sub>s</sub> (2.17 microns). <p>2MASS images and other data products can be obtained at the <a href="http://irsa.ipac.caltech.edu/applications/2MASS/QL/">NASA/IPAC Infrared Science Archive</a> | Mostly (Details) Could not find data |
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| Granat/Sigma | X-ray | 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'.<p> 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.<p> During the period 1990-1998 SIGMA observed more that one quarter of the sky with sensitivity better than 100 mCrab. The Galact | Yes (Details) |
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| RXTE Slew | X-ray | 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 | Yes (Details) |
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| SDSS | Optical | 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 <a href=http://www.sdss.org> SDSS Web site</a>. | Yes (Details) |
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| SHASSA-C | Optical | 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: <b>H-alpha</b>, <b>Continuum</b>, <b>Continuum-Corrected</b> (the difference of the H-alpha and Continuum images), and <b>Smoothed</b> (median filtered to 5 pixel, or 4.0 arcminute, resolution to remove star residuals better). The <a href="http://amundsen.swarthmore.edu/SHASSA">SHASSA web site</a> has more details of the data and the status of this and related projects. Images can also be obtained from the <a href="http://amundsen.astro.swarthmore.edu/SHASSA/#Images">Download Images</a> section at the SHASSA site. | Yes (Details) |
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| FUSE | The Far Ultraviolet Spectroscopic Explorer (FUSE), launched on June 24, 1999, covers the 905-1187 Å spectral region and obtains high resolution spectra of hot and cool stars, AGNs, supernova remnants, planetary nebulae, solar system objects as well as perform detailed studies of the interstellar medium. This service allows access to the FUSE spectra reprocessed using CalFUSE 3.1 and reformatted to be VO-compatible. | No (Details) |
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| IUE | The International Ultraviolet Explorer (IUE) performed spectrophotometry at high (0.1-0.3 Å) and low (6-7 Å) resolution between 1150 Å and 3200 Å. This service currently provides access to the low dispersion "NEWSIPS" data, reformatted to be VO-compatible. | No (Details) |
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