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- ID:
- ivo://mast.stsci/phat
- Title:
- Panchromatic Hubble Andromeda Treasury (PHAT)
- Short Name:
- PHAT
- Date:
- 23 Jul 2020 19:28:22
- Publisher:
- Space Telescope Science Institute Archive
- Description:
- The Panchromatic Hubble Andromeda Treasury is a Hubble Space Telescope Multi-cycle program to map roughly a third of M31's star forming disk, using 6 filters covering from the ultraviolet through the near infrared. With HST's resolution and sensitivity, the disk of M31 will be resolved into more than 100 million stars, enabling a wide range of scientific endeavors.
203. P60 GRBCam
- ID:
- ivo://irsa.ipac/P60/Images/GRBCam
- Title:
- P60 GRBCam
- Short Name:
- GRBCam
- Date:
- 24 Aug 2023 19:31:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- During the years 2004 to 2017, the Palomar 60 inch telescope (P60) operated as a fully robotic facility to obtain targeted optical observations of gamma-ray burst (GRB) afterglows and other transient events. An automated pipeline reduced the data in real time. The raw, calibration, and pipeline-processed data are available here.
- ID:
- ivo://fai.kz/grb_photometry/q/i
- Title:
- Photometrical observations of GRB
- Short Name:
- grb siap
- Date:
- 10 Oct 2023 11:48:20
- Publisher:
- Fesenkov Astrophysical Institute
- Description:
- The database of Gamma Ray Burst (GRB) photometrical observations obtained on defferent telescopes at Fesenkov Astrophysical Institute, Almaty, Kazakhstan. Observations were carried out in the optical range.
- ID:
- ivo://nasa.heasarc/skyview/planck030
- Title:
- Planck 030 GHz Survey
- Short Name:
- Planck030
- Date:
- 03 Dec 2018
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Planck is ESA's third generation space based cosmic microwave background experiment, operating at nine frequencies between 30 and 857 GHz and was launched May 2009. Planck provides all-sky survey data at all nine frequencies with higher resolution at the 6 higher frequencies. It provides substantially higher resolution and sensitivity than WMAP. Planck orbits in the L2 Lagrange point. These data come from Release 1 of the Planck mission. <p> The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the HEALPix data. Users of the SkyView Jar will be able to access this survey through the web but performance may be poor since the FITS files are 150 to 600 MB in size and must be completely read in. SkyView will not automatically cache these files on the user machine as is done for non-HEALPix surveys. </p> Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.
- ID:
- ivo://nasa.heasarc/skyview/planck857i
- Title:
- Planck 857 GHz Survey: I
- Short Name:
- Planck857I
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Planck is ESA's third generation space based cosmic microwave background experiment, operating at nine frequencies between 30 and 857 GHz and was launched May 2009. Planck provides all-sky survey data at all nine frequencies with higher resolution at the 6 higher frequencies. It provides substantially higher resolution and sensitivity than WMAP. Planck orbits in the L2 Lagrange point. <p> These data come from the legacy Release 3 of the Planck mission. <p> These products include polarization information available to visualize in several ways. The data contain Stokes parameters I, Q, and U, and in addition to these, it is possible to visualize the polarized intensity PI=sqrt(Q^2+U^2) and the polarization angle PA=1/2atan(U/Q). Note that at their native resolution of a few arcmin (depending on the frequency), these polarization data will appear very noisy. In order to visualize the polarization information, it is highly recommended that the data be resampled with the "Clip (intensive)" sampler and the result smoothed. That sampler will average all the data points within a given output pixel rather than the more common nearest neighbor. It will do this averaging before computing either PI or PA to reduce the effects of the noise. This sampler is set as the default for this survey. If the output pixel resolution is not significantly larger than the resolution, a smoothing of the output pixels will also be necessary. <p> Note also that Q and U are defined relative to a given co-ordinate system, in this case Galactic, and following the CMB convention (not the IAU); see https://lambda.gsfc.nasa.gov/product/about/pol_convention.cfm. This means that they will appear to vary rapidly near the pole of that coordinate system. The PI and PA will be computed correctly for any position on the sky. <p> The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the HEALPix data. Users of the SkyView Jar will be able to access this survey through the web but performance may be poor since the FITS files are 150 to 600 MB in size and must be completely read in. SkyView will not automatically cache these files on the user machine as is done for non-HEALPix surveys. </p> Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'. Provenance: Data split using skyview.survey.HealPixSplitter from the PR3 distriuted by the Planck Science team.. This is a service of NASA HEASARC.
- ID:
- ivo://org.gavo.dc/flare_survey/q/data
- Title:
- Plates From Münster Flare Star Survey 1986-1991
- Short Name:
- flare_survey.dat
- Date:
- 23 Mar 2022 13:13:07
- Publisher:
- The GAVO DC team
- Description:
- From 1986 through 1991, the Astronomical Institute of Münster University performed a search for flare stars in several southern associations and open stellar clusters using the GPO telescope (d=40 cm, WFPDB identifier ESO040); the fields suveyed include Coalsack, M42, B228 Lup, the Chameleon T1 association, omicron Vel cluster, R CrA association, the Pipe nebula (B59 Oph), and the Sco-Oph association. This was done primarily through multiple exposures. The files published here are plate scans done in 2017. The obscore collection name for these files is Muenster Flare Survey.
- ID:
- ivo://org.gavo.dc/kapteyn/q/plates
- Title:
- Potsdam Kapteyn Series Plates
- Short Name:
- kapteyn.plates
- Date:
- 01 Dec 2022 00:50:28
- Publisher:
- The GAVO DC team
- Description:
- In the context of Kapteyn's plan to obtain a photometric standard, in Potsdam more than 400 photographic plates of several Selected Areas, Special Areas, and Kapteyn-Pritchard areas were obtained between 1910 and 1933, both as direct images and with an object prism. This service provides FITS images of the science area of the plates as well as images of the entire plates, including previous markings.
- ID:
- ivo://irsa.ipac/Herschel/Images/V838MON
- Title:
- Properties of the Dust and Gas in the Environs of V838 Monocerotis
- Short Name:
- V838MON
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- Herschel far-infrared imaging and spectroscopy were taken at several epochs to probe the central point source and the extended environment of the stellar outburst object V838 Monocerotis.
- ID:
- ivo://nasa.heasarc/skyview/pspc2
- Title:
- PSPC summed pointed observations, 2 degree cutoff, Intensity
- Short Name:
- PSPC2
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 <a href="https://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 (<i>e.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&#176;;x2.5&#176;; with a minimum overlap of 0.25&#176;;. 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 <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> ROSAT PSPC Generation Document</a>. Provenance: Observational data from NASA Goddard Space Flight Center, mosaicking of images done by <i>SkyView</i>.. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/pspc0.6int
- Title:
- PSPC summed pointed observations, 0.6 degree cutoff, Intensity
- Short Name:
- PSPC0.6Int
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 <a href="https://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 (<i>e.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&#176;;x2.5&#176;; with a minimum overlap of 0.25&#176;;. 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 <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> ROSAT PSPC Generation Document</a>. Provenance: Observational data from NASA Goddard Space Flight Center, mosaicking of images done by <i>SkyView</i>.. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/pspc1
- Title:
- PSPC summed pointed observations, 1 degree cutoff, Intensity
- Short Name:
- PSPC1
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 <a href="https://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 (<i>e.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&#176;;x2.5&#176;; with a minimum overlap of 0.25&#176;;. 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 <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> ROSAT PSPC Generation Document</a>. Provenance: Observational data from NASA Goddard Space Flight Center, mosaicking of images done by <i>SkyView</i>.. This is a service of NASA HEASARC.
- ID:
- ivo://iacvo/PSZ1y2
- Title:
- PSZ1 and PSZ2 Planck catalogs images
- Short Name:
- PSZ1y2
- Date:
- 23 May 2019 15:00:57
- Publisher:
- Instituto de Astrofísica de Canarias
- Description:
- PSZ1 and PSZ2 Planck images in optical wavelength
- ID:
- ivo://nasa.heasarc/rassmaster
- Title:
- ROSAT All-Sky Survey Archival Data
- Short Name:
- RASSMASTER
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table contains the list German ROSAT All-Sky Survey observations which were obtained during the ROSAT All-Sky Survey phase (1990 July 30 to 1991 Jan 25) and which have become available to the public. These data were obtained in scanning mode and therefore an individual dataset covers a much larger area of the sky than do pointed moded observations. In addition all these data were obtained with PSPC-C, while all pointed mode observations after the end of the All-Sky Survey were obtained with PSPC-B. For each observation listed in this database table, the instrument used, processing site, and coordinates of the field center are given, as well as the ROSAT observation request number (ROR), actual exposure time, date the observation took place, and more. For details about the ROSAT instruments, consult the ROSAT Mission Description (NASA Research Announcement for ROSAT, Appendix F and its addendum) and the ROSAT GSFC GOF website at <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rosgof.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rosgof.html</a> for more information. For more information about the ROSAT All Sky Survey, see the ROSAT All Sky Survey page at <a href="http://www.xray.mpe.mpg.de/cgi-bin/rosat/rosat-survey">http://www.xray.mpe.mpg.de/cgi-bin/rosat/rosat-survey</a>. This database table was created at the HEASARC in March 2002, based on information provided by Max-Planck-Institut fuer extraterrestrische Physik at <a href="http://wave.xray.mpe.mpg.de/">http://wave.xray.mpe.mpg.de/</a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/rassback
- Title:
- ROSAT All-Sky X-ray Background Survey: Band 1
- Short Name:
- RASSBACK
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- These maps present maps of ROSAT soft X-ray all-sky survey as presented in Snowden et al, ApJ 485, 125 (1997). The maps cover approximately 98% of the sky. These maps have had all point sources removed These surveys supercede the RASS0.25, RASS0.75 and RASS1.5 Kev surveys previously provided. Those surveys may still be invoked in SkyView using batch and jar tools but are not accessible on the Web page. <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: <table><tr><th>Band</th><th>Energy range (keV)</th></tr> <tr><td>Band 1</td><td>0.11 - 0.284</td><tr> <tr><td>Band 2</td><td>0.14 - 0.284</td><tr> <tr><td>Band 3</td><td>0.2 - 0.83</td></tr> <tr><td>Band 4</td><td>0.44 - 1.01</td><tr> <tr><td>Band 5</td><td>0.56 - 1.21</td><tr> <tr><td>Band 6</td><td>0.73 - 1.56</td><tr> <tr><td>Band 7</td><td>1.05 - 2.04</td><tr> </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. Provenance: Max Planck Institute for Exterrestrial Physics (Garching FRG). This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/rass3
- Title:
- ROSAT All-Sky X-ray Survey Broad Band: Intensity
- Short Name:
- RASS3
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ROSAT All-Sky X-ray Survey was obtained during 1990/1991 using the ROSAT Position Sensitive Proportional Counter (PSPC) in combination with the ROSAT X-ray Telescope (XRT). More than 60,000 X-ray sources were detected during this time. <p> SkyView has multiple surveys derived from the RASS data. The surveys whose RASS are counts and exposure maps from the survey. Previously The RASSBCK maps have had the point sources removed to show the diffuse X-ray background and are presended at lower resolution. <p> The full-resolution RASS surveys data are organized in 1378 fields each 6.4&#176;; x 6.4&#176;; covering the whole sky. Neighboring fields overlap by at least 0.23&#176;;.<p> Three bands are available through <i>SkyView</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 <a href="https://www.xray.mpe.mpg.de/rosat/survey/rass-3/main/help.html#ftp">MPE FTP site</a>. <p> The intensity maps are created from the exposure maps using the single exposure map available which is appropriate for the broad band images, so the intensities of the hard and soft bands are only approximate. Provenance: Max Planck Institute for Exterrestrial Physics (Garching FRG). This is a service of NASA HEASARC.
217. ROSAT Archival Data
- ID:
- ivo://nasa.heasarc/rosmaster
- Title:
- ROSAT Archival Data
- Short Name:
- ROSAT
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table contains the list of all Röntgen Satellite (ROSAT) X-Ray Telescope (XRT) pointing-mode observations for which data sets are available, i.e., it excludes the ROSAT All-Sky Survey observations. Users should consult the RASSMASTER database table for those XRT observations which were made in scanning mode during the ROSAT All-Sky Survey (RASS) phase (30 July 1990 to 25 January 1991, and 3 August 1991 to 13 August 1991). For each observation listed in this table, parameters such as the focal-plane instrument used, the data processing site, and the target name and coordinates are given, as well as the ROSAT Observation Request (ROR) number, the actual and requested exposure times, the date(s) on which the observation took place, etc. For details about the ROSAT instruments, consult the ROSAT Guest Observer Facility (GOF) website at <a href="https://heasarc.gsfc.nasa.gov/docs/rosat/">https://heasarc.gsfc.nasa.gov/docs/rosat/</a>. A list of the available online ROSAT documentation can be found at <a href="https://heasarc.gsfc.nasa.gov/docs/rosat/rosdocs.html">https://heasarc.gsfc.nasa.gov/docs/rosat/rosdocs.html</a>. This table was created by the HEASARC in July 2004 by combining the data from two long-standing HEASARC Browse tables into one master table. It was updated by the HEASARC in March 2022 to add start and end times for the 157 sequence IDs which did not already have start and end times. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/roshritotal
- Title:
- ROSAT Complete Results Archive Sources for the HRI
- Short Name:
- ROSAT/HRI
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ROSHRITOTAL data table contains a list of sources detected by the Standard Analysis Software System (SASS) in reprocessed, public HRI datasets. In addition to the parameters returned by SASS (like position, count rate, signal-to-noise, etc.) each source in the table has associated with it a set of source and sequence "flags." These flags are provided by the ROSAT data centers in the US, Germany and the UK to help the user of the ROSHRITOTAL database table quickly judge the reliability of a given source. The ROSHRITOTAL database table is a superset of the ROSHRI database table. The ROSHRI table excludes sources that meet the following parameter criteria: false_det = 'T' or deferred = 'T' or not_checked = 'T' or un_unique ='T'. See the documentation below for descriptions of these parameters. These data have been screened by ROSAT data centers in the US, Germany, and the UK as a step in the production of the ROSAT Results Archive. The RRA contains extracted source and associated products with an indication of reliability for the primary parameters. This database table was last updated in August 2001. More information about the ROSAT Results Archive for HRI sources can be obtained at the following web pages: <pre> <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html</a> <a href="http://hea-www.harvard.edu/rosat/rra.html">http://hea-www.harvard.edu/rosat/rra.html</a> <a href="http://www.aip.de/groups/xray/rosat/rra.html">http://www.aip.de/groups/xray/rosat/rra.html</a> <a href="http://ledas-www.star.le.ac.uk/rra">http://ledas-www.star.le.ac.uk/rra</a> </pre> This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/hri
- Title:
- ROSAT High Resolution Image Pointed Observations Mosaic: Intensity
- Short Name:
- HRI
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This survey was generated from all available ROSAT HRI observations. Data were mosaicked into 1.1 degree tiles by SkyView. Exposure maps were generated for each HRI observation using the hriexpmap FTOOL. For each tile, all observations that might contribute to that tile were located and added to count and exposure map tiles. Exposures for each observation were calculated using a nearest neighbor interpolation of the center of the tile pixels to the exposure map pixels. Counts were computed by projecting the RA and Decs of each eligible photon into the appropriate tile pixel. Only photons with a PHA > 3 were included in the mosaic and within each observation only counts within the region where the exposure was greater than half the maximum exposure were included. Provenance: Data from GSFC and MPE. <i>SkyView</i> mosaic generated by SkyView.. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/roshri
- Title:
- ROSAT Results Archive Sources for the HRI
- Short Name:
- ROSAT/HRI
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ROSHRI data table contains a list of sources detected by the Standard Analysis Software System (SASS) in reprocessed, public HRI datasets. In addition to the parameters returned by SASS (like position, count rate, signal-to-noise, etc.) each source in the table has associated with it a set of source and sequence "flags." These flags are provided by the ROSAT data centers in the US, Germany and the UK to help the user of the ROSHRI database table quickly judge the reliability of a given source. The ROSHRI table excludes sources that meet the following parameter criteria: false_det = 'T' or deferred = 'T' or not_checked = 'T' or un_unique ='T'. See the documentation below for descriptions of these parameters. These data have been screened by ROSAT data centers in the US, Germany, and the UK as a step in the production of the ROSAT Results Archive. The RRA contains extracted source and associated products with an indication of reliability for the primary parameters. This database table was last updated in August 2001. More information about the ROSAT Results Archive for HRI sources can be obtained at the following web pages: <pre> <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html</a> <a href="http://hea-www.harvard.edu/rosat/rra.html">http://hea-www.harvard.edu/rosat/rra.html</a> <a href="http://www.aip.de/groups/xray/rosat/rra.html">http://www.aip.de/groups/xray/rosat/rra.html</a> <a href="http://ledas-www.star.le.ac.uk/rra">http://ledas-www.star.le.ac.uk/rra</a> </pre> This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/rospspc
- Title:
- ROSAT Results Archive Sources for the PSPC
- Short Name:
- ROSAT/PSPC
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ROSPSPC database table contains a list of sources detected by the Standard Analysis Software System (SASS) in public, unfiltered, pointed PSPC datasets. In addition to the parameters returned by SASS (like position, count rate, likelihood, etc.) each source in the table has associated with it a set of source and sequence "flags." These flags are provided by the ROSAT data centers in the US, Germany and the UK to help the user of the ROSPSPC database table quickly judge the reliability of a given source. The ROSPSPC table excludes sources that meet the following parameter criteria: false_det = 'T' or deferred = 'T' or not_checked = 'T'. See the documentation below for descriptions of these parameters. The catalog consists of all primary source parameters from the automated detection algorithm employed by the SASS. In addition each observation has been quality checked, both by automatic algorithms and by detailed visual inspection. The results of this quality checking are contained as a set of logical-value flags for a set of principal source parameters. If a source parameter is suspect, the associated flag is set to "TRUE"; parameters with no obvious problems maintain the default, "FALSE", value. This database table was last updated in August 2001. More information about the ROSAT Results Archive for PSPC sources can be obtained at the following web pages: <pre> <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html</a> <a href="http://hea-www.harvard.edu/rosat/rra.html">http://hea-www.harvard.edu/rosat/rra.html</a> <a href="http://www.aip.de/groups/xray/rosat/rra.html">http://www.aip.de/groups/xray/rosat/rra.html</a> <a href="http://ledas-www.star.le.ac.uk/rra">http://ledas-www.star.le.ac.uk/rra</a> </pre> This is a service provided by NASA HEASARC .
- ID:
- ivo://org.gavo.dc/rosat/q/im
- Title:
- ROSAT Survey and Pointed Images
- Short Name:
- ROSAT images
- Date:
- 20 Apr 2023 00:06:45
- Publisher:
- The GAVO DC team
- Description:
- Images taken by the ROSAT x-ray observatory. This comprises both pointed observations and images taken within the all-sky survey.
- ID:
- ivo://nasa.heasarc/skyview/wfcf
- Title:
- ROSAT Wide Field Camera: F1
- Short Name:
- WFCF
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This survey is a mosaic of images taken by the ROSAT Wide Field Camera and comprises of 12,743 seperates fields in each of two filters. Each field covers a region 2.6&#176;; x 2.6&#176;; with a 0.3&#176;; overlap. Currently, this data is not a complete coverage of the sky; regions near the northern ecliptic pole are currently not included. Provenance: University of Leicester. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/rxte3_20k_flux
- Title:
- RXTE Allsky 3\-20 keV Flux
- Short Name:
- RXTE3_20k_flux
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Rossi X-ray Timing Explorer was launched at the end of 1995 and up to now (2004) it has been successfully operating for more than 7 years. The mission was primarily designed to study the variability of X-ray sources on time scales from sub-milliseconds to years. The maneuvering capability of the satellite combined with the high photon throughput of its main detector (PCA) and high quality of background prediction (thanks to PCA intrumental group of LHEA, GSFC) has also made it possible to construct maps of the sky in energy band 3-20 keV. During its life time RXTE/PCA has collected a large amount of data from slew observations covering almost the entire sky. <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&#176;;/sec) and the time resolution of used data (16 sec, Std2 mode of the PCA). Sources can be detected down to the level of ~6e<sup>-12</sup> erg/s/cm<sup>2</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). Provenance: High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M PA, Garching, Germany. This is a service of NASA HEASARC.
- ID:
- ivo://org.gavo.dc/sasmirala/q/im
- Title:
- Sasmirala Subarcsecond mid-infrared atlas of local AGN
- Short Name:
- sasmirala atlas
- Date:
- 23 Mar 2022 13:13:11
- Publisher:
- The GAVO DC team
- Description:
- These FITS images were generated with the IDL package MIRphot [Asmus2014]_ by extraction (and combination) of the sub-images from the chopped/nodded total images from COMICS, Michelle, T-ReCS and VISIR (see [Asmus2014]_ for details). The FITS images contain the central ~4 arcsec of each source centered on the (putative) nuclear position with North being up and East to the left. The WCS registration has been performed after extraction by using coordinates of the nucleus from other wavelengths (mostly 2MASS and NED). The uncertainty of these reference position is usually less than 1 arcsec. In addition, the imprecision of the assignment itself is ~1px ~ 0.1". The FITS images are flux calibrated (unit is mJy) using the Gaussian 2D fits to the corresponding STD observation (where available, otherwise using the median conversion factor for the used instrument/filter settings). Therefore, correction factors have to be applied in case other flux measurement methods are applied to the images. The flux values given in the FITS headers should be regarded as approximate values. In particular for the instruments, VISIR and COMICS, they are not necessarily exactly equal to the values provided in the photometry results table, because many flux measurements were performed during the process of combining individual subimages (all in MIRphot), instead of in the final combined image, provided here. The used total images are available upon request. Note, however, that these are just the products of the observatory-delivered pipelines with default parameters. .. [Asmus2014] Asmus D., Hoenig S.F., Gandhi P., Smette A., Duschl W.: The subarcsecond mid-infrared view of local active galactic nuclei: I. The N- and Q-band imaging atlas, `2014MNRAS.439.1648A <http://ads.ari.uni-heidelberg.de/abs/2014MNRAS.439.1648A>`_
- ID:
- ivo://org.gavo.dc/plts/q/data
- Title:
- Scans of the Palomar-Leiden Trojan Survey Plates
- Short Name:
- plts.data
- Date:
- 23 Mar 2022 13:13:18
- Publisher:
- The GAVO DC team
- Description:
- This service publishes plate scans of the Palomar-Leiden Troian surveys conducted between 1960 and 1977. The surveys led to the discovery of more than 2,000 asteroids (1,800 with orbital information), with another 2,400 asteroids, including 19 Trojans, found after further analysis of the plates. Note that because of the large size of the plates, in this service each original plate is contained in two parts, marked with "_1" and "_2", respectively. The central parts of the two parts overlap.
- ID:
- ivo://nasa.heasarc/skyview/sfd
- Title:
- Schlegel, Finkbeiner and Davis dust\ map survey
- Short Name:
- SFD
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The full sky 100 micron map is a reprocessed composite of the COBE/DIRBE and IRAS/ISSA maps, with the zodiacal foreground and confirmed point sources removed. Artifacts from the IRAS scan pattern were removed. The result of these manipulations is a map with DIRBE-quality calibration and IR AS resolution. Provenance: David J. Schlegel, Douglas P. Finkbeiner and Marc Davis, Princeton University and University of California, Berkeley. This is a service of NASA HEASARC.
- ID:
- ivo://chivo/alma_fits/q/siap-alma-fits
- Title:
- Simple Image Access for ALMA FITS
- Short Name:
- SIAP ALMA FITS
- Date:
- 06 Nov 2017 14:35:31
- Publisher:
- ChiVO
- Description:
- The resource contains the recommendations and requirements for ALMA FITS products of the Inter-ARC ALMA Science Archive Working Group (ASAWG) with the view to including a metadataset that is complete and easily accessible by the ChiVO Data Provider (CDP).
- ID:
- ivo://nasa.heasarc/skyview/skyview
- Title:
- SkyView Virtual Observatory
- Short Name:
- SkyView
- Date:
- 06 Apr 2021
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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.
- ID:
- ivo://sdss.jhu/services/SIAPDR4-Color
- Title:
- Sloan Digital Sky Survey DR4
- Short Name:
- SDSSDR4-Color
- Date:
- 14 Feb 2012 18:49:17
- Publisher:
- The Johns Hopkins Univer
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR3-Color
- Title:
- Sloan Digital Sky Survey DR3
- Short Name:
- SDSSDR3-Color
- Date:
- 14 Feb 2012 18:48:16
- Publisher:
- The Johns Hopkins Univer
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR3-G
- Title:
- Sloan Digital Sky Survey DR3 - Filter g
- Short Name:
- SDSSDR3-G
- Date:
- 14 Feb 2012 18:48:30
- Publisher:
- The Johns Hopkins Univer
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR3-I
- Title:
- Sloan Digital Sky Survey DR3 - Filter i
- Short Name:
- SDSSDR3-I
- Date:
- 14 Feb 2012 18:48:36
- Publisher:
- The Johns Hopkins Univer
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR3-R
- Title:
- Sloan Digital Sky Survey DR3 - Filter r
- Short Name:
- SDSSDR3-R
- Date:
- 14 Feb 2012 18:48:53
- Publisher:
- The Johns Hopkins Univer
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR3-U
- Title:
- Sloan Digital Sky Survey DR3 - Filter u
- Short Name:
- SDSSDR3-U
- Date:
- 14 Feb 2012 18:49:01
- Publisher:
- The Johns Hopkins University
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR3-Z
- Title:
- Sloan Digital Sky Survey DR3 - Filter z
- Short Name:
- SDSSDR3-Z
- Date:
- 14 Feb 2012 18:49:08
- Publisher:
- The Johns Hopkins Univer
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR4-images
- Title:
- Sloan Digital Sky Survey DR4 - Images
- Short Name:
- SDSSDR4
- Date:
- 14 Feb 2012 18:49:26
- Publisher:
- The Johns Hopkins Univer
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR5-images
- Title:
- Sloan Digital Sky Survey DR5 - Images
- Short Name:
- SDSSDR5
- Date:
- 14 Sep 2011 17:51:46
- Publisher:
- The Johns Hopkins University
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR1-images
- Title:
- Sloan Digital Sky Survey DR1 - Images
- Short Name:
- SDSSDR1
- Date:
- 23 Jun 2015 19:12:00
- Publisher:
- The Johns Hopkins University
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR2-images
- Title:
- Sloan Digital Sky Survey DR2 - Images
- Short Name:
- SDSSDR2
- Date:
- 23 Jun 2015 19:11:00
- Publisher:
- The Johns Hopkins University
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR9-images
- Title:
- Sloan Digital Sky Survey DR9 - Images
- Short Name:
- SDSSDR9
- Date:
- 05 Feb 2015 21:07:21
- Publisher:
- The Johns Hopkins University
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR8-images
- Title:
- Sloan Digital Sky Survey DR8 - Images
- Short Name:
- SDSSDR8
- Date:
- 05 Feb 2015 21:06:53
- Publisher:
- The Johns Hopkins University
- Description:
- 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
- ID:
- ivo://sdss.jhu/services/SIAPDR7-images
- Title:
- Sloan Digital Sky Survey DR7 - Images
- Short Name:
- SDSSDR7
- Date:
- 05 Feb 2015 21:06:16
- Publisher:
- The Johns Hopkins University
- Description:
- 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
- ID:
- ivo://nasa.heasarc/skyview/sdss
- Title:
- Sloan Digital Sky Survey g-band
- Short Name:
- SDSS
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Sloan Digital Sky Survey is the deepest large scale survey of the sky currently available. SkyView dynamically queries the SDSS archive (currently release DR9) to retrieve information and resample it into the user requested frame. Further information on the SDSS and many additional services are available at the <a href="https://www.sdss.org">SDSS website</a>. Provenance: Sloan Digital Sky Survey Team. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/sdssdr7
- Title:
- Sloan Digital Sky Survey g-band DR7
- Short Name:
- SDSSDR7
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Sloan Digital Sky Survey is the deepest large scale survey of the sky currently available. SkyView dynamically queries the SDSS archive to retrieve information and resample it into the user requested frame. Further information on the SDSS and many additional services are available at the <a href="https://www.sdss.org/">SDSS website</a>. Provenance: Sloan Digital Sky Survey Team. This is a service of NASA HEASARC.
- ID:
- ivo://sdss.jhu/services/SIAP-images
- Title:
- Sloan Digital Sky Survey Images (Latest Release)
- Short Name:
- SDSS SIAP
- Date:
- 05 Feb 2015 21:10:39
- Publisher:
- The Johns Hopkins University
- Description:
- 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
- ID:
- ivo://org.gavo.dc/smakced/q/im
- Title:
- SMAKCED H-band images of Early-Type Virgo Dwarf Galaxies
- Short Name:
- smakced H images
- Date:
- 23 Mar 2022 13:13:18
- Publisher:
- The GAVO DC team
- Description:
- The Stellar content, MAss and Kinematics of Cluster Early-type Dwarf galaxies (SMAKCED_) project is a survey of 121 Virgo cluster early type galaxies. This service publishes deep near-infrared (H band) images obtained by SMAKCED together with `resulting decompositions`_ and other properties of the galaxies in the sample. .. _SMAKCED: http://smakced.net .. _resulting decompositions: http://smakced.net/data.html
- ID:
- ivo://nasa.heasarc/skyview/goods-isaac-h
- Title:
- Southern GOODS Field: VLT ISAAC Observations, H band
- Short Name:
- GOODS ISAAC H
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- As part of the Great Observatories Origins Deep Survey (GOODS), near-infrared imaging observations of the Chandra Deep Field South (CDF-S) were carried out in J, H, Ks bands, using the ISAAC instrument mounted at the Antu Unit Telescope of the VLT at ESO's Cerro Paranal Observatory, Chile. <p> These data were obtained as part of the ESO Large Programme 168.A-0485 (PI: C. Cesarsky). Data covering four ISAAC fields in J and Ks bands were also drawn from the ESO programmes 64.O-0643, 66.A-0572 and 68.A-0544 (PI: E.Giallongo), which were part of the previous data releases. <p> This data release covers 172.4, 159.6, and 173.1 arcmin2 of the GOODS/CDF-S region in J, H and Ks respectively. More than 50% of the images reach a 5-sigma depth for point sources of at least 25.2 mag (J), 24.7 mag (H and Ks) in the AB system ("median depth"). <p> This final GOODS/ISAAC data release accumulates observational data which have been acquired in 12814 science integrations between October 1999 and January 2007 totaling 1.3 Msec integration time. [Above adapted from reference website.] <p> <i> SkyView</i> uses the mosaic files provided in this delivery. The Version 1.5 mosaic is used for the KS band. Provenance: Data downloaded from VLT archive. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/goods-vimos-r
- Title:
- Southern GOODS Field: VLT VIMOS Observations, R band
- Short Name:
- GOODS VIMOS R
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- As part of the Great Observatories Origins Deep Survey (GOODS), deep imaging in the Chandra Deep Field South (CDF-S) has been carried out, using the VIMOS instrument mounted at the Melipal Unit Telescope of the VLT at ESO's Cerro Paranal Observatory, Chile. <p> This data release contains the coadded images in U band from the ESO large programme 168.A-0485 (P.I. C. Cesarsky) which have been obtained in service mode observations between August 2004 and fall 2006. The 1-sigma depth for VIMOS U band in the area covered by the GOODS-ACS observations is ~30 AB (within an aperture of 1" radius, ranging from 29.5 and 30.2 AB). The PSF of the VIMOS U band mosaic is ~0.8" FWHM, but varies over the field. <p> Also included in this data release is a coadded image in R band obtained from data retrieved from the ESO archive. Due to the different observing strategies adopted in the programmes the resulting coverage of the GOODS-ACS area is more complex than for the U band. The depth of the VIMOS R band mosaic over the ACS area ranges from ~28 AB to 29 AB (1-sigma, 1" aperture radius). The PSF of the VIMOS R band mosaic is ~0".7 FWHM and varies over the field. [Adapted from reference website.] Provenance: Data downloaded from VLT archive. This is a service of NASA HEASARC.
- ID:
- ivo://mast.stsci/siap/stages
- Title:
- Space Telescope A901/902 Galaxy Evolution Survey (STAGES)
- Short Name:
- HST.STAGES
- Date:
- 23 Jul 2020 19:41:16
- Publisher:
- Space Telescope Science Institute Archive
- Description:
- 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.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SAFIRES
- Title:
- Spitzer Archival Far-Infrared Extragalactic Survey
- Short Name:
- SAFIRES
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer Archival FIR Extragalactic Survey (SAFIRES) is an offshoot of the Spitzer Space Telescope Enhanced Imaging Products (SEIP). SAFIRES applies the SEIP project's methods to the remaining two MIPS bands, located at far-infrared wavelengths of 70 and 160 microns. Due to the complexity of far-infrared observations, these bands require an expansion of SEIP's standard pipeline through the addition of reprocessing tools. These additional steps are required to remove obvious artifacts before extracting useful measurements. As a result, these bands were not included in the SEIP project, but were later funded through an additional NASA Astrophysics Data Analysis Program (ADAP) grant. To ensure high reliability, the SAFIRES sample includes no fields near the Galactic disk; these observations comprised more than half of the area observed by Spitzer, but the practical drawbacks of Galactic contamination would inhibit the ability to maintain the level of reliability desired in the SAFIRES products. As with SEIP, the SAFIRES source lists contains no extended sources. The remaining sample comprises nearly 1132 fields spanning almost 180 square degrees of sky.
- ID:
- ivo://irsa.ipac/Spitzer/Images/S-CANDELS
- Title:
- Spitzer-Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey
- Short Name:
- S-CANDELS
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer-Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey (S-CANDELS) is a Spitzer Cycle 8 Exploration Program (PI G. Fazio) that obtained deep IRAC channel 1 and 2 imaging in five widely separated extragalactic fields: the UKIDSS Ultra-Deep Survey (UDS), the Extended Chandra Deep Field South (ECDFS), COSMOS, the HST Deep Field North (HDFN), and the Extended Groth Strip (EGS). S-CANDELS builds upon the existing coverage of these fields obtained as part of the Spitzer Extended Deep Survey (SEDS), a Cycle 6 Exploration Program, by increasing the integration time from 12 hours to a total of 50 hours within a smaller area of 0.16 deg2.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SDWFS
- Title:
- Spitzer Deep Wide-Field Survey
- Short Name:
- SDWFS
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer Deep Wide-Field Survey is a four-epoch survey of roughly 10 square degrees of the NOAO Deep, Wide-Field Survey field in Boötes. The first visit to the field occurred very early in the Spitzer mission, in 2004 January, as part of the IRAC Shallow Survey (Eisenhardt et al. 2004). Subsequent visits to the field as part of the SDWFS program reimaged the same area to the same depth.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SEIP
- Title:
- Spitzer Enhanced Imaging Products
- Short Name:
- SEIP
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer Science Center and IRSA have released a set of Enhanced Imaging Products (SEIP) from the Spitzer Heritage Archive. These include Super Mosaics (combining data from multiple programs where appropriate) and a Source List of photometry for compact sources. The primary requirement on the Source List is very high reliability -- with areal coverage, completeness, and limiting depth being secondary considerations. The SEIP include data from the four channels of IRAC (3.6, 4.5, 5.8, 8 microns) and the 24 micron channel of MIPS. The full set of products for the Spitzer cryogenic mission includes around 42 million sources.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SERVS
- Title:
- Spitzer Extragalactic Representative Volume Survey
- Short Name:
- SERVS
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- SERVS is a warm Spitzer survey which images approximately 18 square degrees in the centers of the SWIRE XMM-LSS, ELAIS-S1, CDFS, Lockman and ELAIS-N1 fields to 20min (2mu Jy) depth at 3.6 and 4.5 microns. SERVS overlaps with the VISTA-VIDEO near infrared and Herschel-HERMES and SCUBA2-S2CLS far-infrared surveys.
- ID:
- ivo://irsa.ipac/Spitzer/Images/FLS
- Title:
- Spitzer First Look Survey
- Short Name:
- FLS
- Date:
- 16 Mar 2017 01:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer Extragalactic First Look Survey is composed of 4 square degrees of imaging with MIPS and IRAC centered at J1718+5930. Ancillary data are available from a wide variety of optical and radio observatories.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SHELA
- Title:
- Spitzer/HETDEX Exploratory Large-Area Survey
- Short Name:
- SHELA
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer/HETDEX Exploratory Large-Area (SHELA) survey covers ~24 sq. deg at 3.6 and 4.5 microns. The survey area falls within the footprints of the Sloan Digital Sky Survey "Stripe 82" region, the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX), and the Dark Energy Survey. The images and catalogs are 80% (50%) complete to limiting magnitudes of 22.0 (22.6) AB mag in the detection image, which is constructed from the weighted sum of the IRAC 3.6 and 4.5 micron images. The catalogs reach limiting sensitivities of 1.1 microJy at both 3.6 and 4.5 microns (1#, for R = 2" circular apertures).
- ID:
- ivo://irsa.ipac/Spitzer/Images/SINGS
- Title:
- Spitzer Infrared Nearby Galaxy Survey
- Short Name:
- SINGS
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer Infrared Nearby Galaxy Survey is a comprehensive infrared imaging and spectroscopic survey of 75 nearby galaxies. Its primary goal is to characterize the infrared emission of galaxies and their principal infrared-emitting components, across a broad range of galaxy properties and star formation environments. SINGS provides new insights into the physical processes connecting star formation to the interstellar medium properties of galaxies and provides a vital foundation for understanding infrared observations of the distant universe and ultraluminous and active galaxies.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SpIES
- Title:
- Spitzer IRAC Equatorial Survey
- Short Name:
- SpIES
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer IRAC Equatorial Survey (SpIES) is a large-area survey of 115 sq. degrees in the Equatorial SDSS Stripe 82 field. SpIES achieves 5 sigma depths of 6.13 microJy (21.93 AB magnitude) and 5.75 microJy (22.0 AB magnitude) at 3.6 and 4.5 microns, respectively.
- ID:
- ivo://nasa.heasarc/skyview/goodsirac-1
- Title:
- Spitzer IRAC GOODS 3\.6 micron data, channel 1
- Short Name:
- GOODSIRAC 1
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Spitzer IRAC medium infrared observations taken in all four IRAC channels in both the north and south GOODS fields. Provenance: IRAC Goods Team, IRSA data center. This is a service of NASA HEASARC.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SIMPLE
- Title:
- Spitzer IRAC/MUSYC Public Legacy Survey in the Extended Chandra Deep Field South
- Short Name:
- SIMPLE
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- SIMPLE consists of deep IRAC observations (several hours per pointing) covering the 0.5 x 0.5 deg area surrounding the GOODS CDF-South. This low-background region of the sky has by far the best supporting data of any cosmological survey field of comparable area, with deep observations from the X-rays to the thermal infrared.
- ID:
- ivo://irsa.ipac/Spitzer/Images/Level1
- Title:
- Spitzer Level 1 / Basic Calibrated Data
- Short Name:
- Spitzer Level 1
- Date:
- 16 Mar 2017 01:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- Level 1 / Basic Calibration Data (BCD) from Spitzer Space Telescope. BCDs are the individual data frames that emerge [calibrated] from the Spitzer pipeline.
- ID:
- ivo://irsa.ipac/Spitzer/Images/Level2
- Title:
- Spitzer Level 2 / post Basic Calibrated Data
- Short Name:
- Spitzer Level 2
- Date:
- 16 Mar 2017 01:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- Level 2 or post Basic Calibrated Data (PBCD) from Spitzer Space Telescope. This products come from combining the individual data frames or BCDs [such as mosaics of individual pointings].
- ID:
- ivo://irsa.ipac/Spitzer/Images/LVL
- Title:
- Spitzer Local Volume Legacy Survey
- Short Name:
- LVL
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- LVL consists of a sample of 258 galaxies, which have been mapped with both IRAC (4 bands) and MIPS (3 bands). In addition, ancillary data products consisting of images in the narrow-band H-alpha line emission and broad-band R (from the ground) and the UV continuum (2 bands) from GALEX are also available for many of the galaxies.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SMUVS
- Title:
- Spitzer Matching Survey of the Ultra-VISTA Deep Stripes
- Short Name:
- SMUVS
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer Matching Survey of the Ultra-VISTA Deep Stripes (SMUVS) consists of deep 3.6 and 4.5 imaging of three Ultra-VISTA near-infrared survey stripes in the COSMOS field. SMUVS reaches point-source sensitivities of about 25.0 AB mag at both 3.6 and 4.5 microns with a significance of 4 sigma, accounting for both survey sensitivity and source confusion. To this limit, the SMUVS catalogs contain a total of ~350,000 sources, each of which is detected significantly in at least one IRAC band. Because of its uniform and high sensitivity, relatively large area coverage, and the wide array of ancillary data available in COSMOS, the SMUVS survey will be useful for a large number of cosmological investigations.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SEP
- Title:
- Spitzer MIPS 24 and 70 micron Imaging of the South Ecliptic Pole
- Short Name:
- SEP
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer/MIPS 24 and 70 μm imaging of an 11.5 square degree region near the South Ecliptic Pole (SEP) has been carried out in order to complement sub-millimeter wavelength observations (250-500 μm) of the same region of sky taken with the Balloon-borne Large Aperture Sub-millimeter Telescope (BLAST), with the goal of better characterizing the nature of sub-millimeter selected galaxies and their role in galaxy evolution. This field has also been extensively mapped at other wavelengths, and will be imaged from 100-500 μm as part of the Herschel Multi-tiered Extragalactic Survey (HerMES).
- ID:
- ivo://nasa.heasarc/skyview/goodsmips
- Title:
- Spitzer MIPS GOODS 24 Micron Data
- Short Name:
- GOODSMIPS
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Spitzer MIPS observations of the GOODS North and South fields in the 24 micron channel. Provenance: IRSA, GOODS team. This is a service of NASA HEASARC.
- ID:
- ivo://irsa.ipac/Spitzer/Images/Abell1763
- Title:
- Spitzer Observations of Abell 1763
- Short Name:
- Abell 1763
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- This data set includes images of the galaxy cluster Abell 1763 at visible and infrared wavelengths: r', J, H, and Ks obtained using the Palomar 200in telescope, as well as the IRAC and MIPS images from Spitzer. The cluster is covered out to approximately 3 virial radii with deep 24 mum imaging (a 5sigma depth of 0.2 mJy). This same field of ~40' × 40' is covered in all four IRAC bands as well as the longer wavelength MIPS bands (70 and 160 mum). The r' imaging covers ~0.8 deg2 down to 25.5 mag, and overlaps with most of the MIPS field of view. The J, H, and Ks images cover the cluster core and roughly half of the filament galaxies, which extend toward the neighboring cluster, Abell 1770.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SpUDS
- Title:
- Spitzer Public Legacy Survey of the UKIDSS Ultra Deep Survey
- Short Name:
- SpUDS
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- SpUDS is a survey of the ~1 square degree UKIDSS Ultra Deep Survey (UDS). The survey consists of deep IRAC and 24 micron MIPS observations. The UDS is the largest deep near-infrared (JHK) survey in existence, and the first capable of sampling representative cosmological volumes (100x100 Mpc) out to the highest redshifts (z>6).
- ID:
- ivo://irsa.ipac/Spitzer/Images/SRELICS
- Title:
- Spitzer Reionization Lensing Cluster Survey
- Short Name:
- SRELICS
- Date:
- 01 May 2023 20:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer Reionization Lensing Cluster Survey (SRELICS, PI: Bradac) is the Spitzer counterpart to the RELICS HST Treasury program (PI: Coe) to survey 41 massive galaxy clusters.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SMC-Last
- Title:
- Spitzer's Last Look at the Small Magellanic Cloud
- Short Name:
- SMC-Last
- Date:
- 30 Aug 2023 22:46:07
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- SMC-Last (Program ID number 13096) built on the legacy of SAGE-SMC by adding two more epochs at 3.6 and 4.5 microns covering the entire 30 square degree footprint of the SAGE-SMC survey in late 2017 and early 2018. This program, when combined with the previous surveys, provides a minimum of four epochs at 3.6 and 4.5 microns creating a temporal baseline of over 9 yr covering the entire SMC and its surroundings. Up to nine epochs are available in the core of the SMC spanning a period of over 12 yr.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SSDF
- Title:
- Spitzer-South Pole Telescope Deep Field
- Short Name:
- SSDF
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer-South Pole Telescope Deep Field (SSDF) is a wide-area survey using IRAC to cover 94 square degrees of extragalactic sky, making it the largest IRAC survey completed to date outside the Milky Way midplane. The SSDF is centered at 23:30,-55:00, in a region that combines observations spanning a broad wavelength range from numerous facilities. These include millimeter imaging from the South Pole Telescope, far-infrared observations from Herschel/SPIRE, X-ray observations from the XMM XXL survey, near-infrared observations from the VISTA Hemisphere Survey, and radio-wavelength imaging from the Australia Telescope Compact Array, in a panchromatic project designed to address major outstanding questions surrounding galaxy clusters and the baryon budget.
- ID:
- ivo://irsa.ipac/Spitzer/Images/DeepDrill
- Title:
- Spitzer Survey of Deep Drilling Fields
- Short Name:
- DeepDrill
- Date:
- 23 May 2023 23:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) will observe several Deep Drilling Fields (DDFs) to a greater depth and with a more rapid cadence than the main survey. The "DeepDrill" survey (Program ID 11086, P.I. Lacy) used the Spitzer Space Telescope Infrared Array Camera (IRAC) to observe three of the four currently defined DDFs in two bands, centered on 3.6 um and 4.5 um. These observations expand the area which was covered by an earlier set of observations in these three fields by the Spitzer Extragalactic Representative Volume Survey (SERVS). The combined DeepDrill and SERVS data cover the footprints of the LSST DDFs in the Extended Chandra Deep Field-South field (ECDFS), the ELAIS-S1 field (ES1), and the XMM-Large-Scale Structure Survey field (XMM-LSS).
- ID:
- ivo://irsa.ipac/Spitzer/Images/S4G
- Title:
- Spitzer Survey of Stellar Structure in Galaxies
- Short Name:
- S4G
- Date:
- 23 May 2023 01:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Spitzer Survey of Stellar Structure in Galaxies (S4G) is a volume-, magnitude-, and size-limited survey of over 2300 nearby galaxies at 3.6 and 4.5μm. This is an extremely deep survey reaching an unprecedented 1σ surface brightness limit of μ3.6μm(AB) = 27 mag arcsec-2. This translates to a stellar surface density of << 1 M⊙ pc-2 ! S4G can thus probe the stellar structure in galaxies in a regime where the gas dominates the stars (typical HI surface density ~ a few M⊙ pc-2).
275. SRC-J Survey
- ID:
- ivo://vopdc.obspm/gepi/vopsat/srcj
- Title:
- SRC-J Survey
- Short Name:
- SRC-J
- Date:
- 10 Nov 2022
- Publisher:
- Paris Astronomical Data Centre - GEPI
- Description:
- VO-compliant publication of Schmidt survey SRC-J of the southern sky digitized with the MAMA microdensitometer at the Observatoire de Paris Image Analysis Centre (CAI).
- ID:
- ivo://padc.obspm.astro/srcj/q/i
- Title:
- SRC-J survey digitized by MAMA
- Short Name:
- POSSE
- Date:
- 07 Apr 2022 17:22:05
- Publisher:
- Paris Astronomical Data Centre
- Description:
- Pallomar Observatory plate scan service
- ID:
- ivo://jvo/subaru/moircs
- Title:
- Subaru MOIRCS data service
- Short Name:
- SUBARU_MOIRCS
- Date:
- 14 Nov 2019 03:50:26
- Publisher:
- JVO
- Description:
- MOIRCS (Multi-Object InfraRed Camera and Spectrograph) provides wide-field imaging and long-slit / multi-object (MOS) spectroscopic capabilities in the 0.9 ~ 2.5 µm spectral range under the natural seeing condition. The 4'?~7' field of view is covered by two Hawaii-2 2048?~2048 arrays with the spatial resolution of 0.117 arcsec/pixel.
- ID:
- ivo://jvo/subaru/spcam
- Title:
- Subaru Suprime-Cam data service
- Short Name:
- SUBARU_SUP
- Date:
- 04 Nov 2020 06:00:31
- Publisher:
- JVO
- Description:
- The Subaru Prime Focus Camera (Suprime-Cam) is a mosaic of ten 2048 x 4096 CCDs, located at the prime focus of Subaru Telescope, which covers a 34' x 27' field of view with a pixel scale of 0.20''. This service provides access to the JVO Subaru Suprime-Cam mosaic image archive. The purpose of this archive is to provide quick look images taken by Subaru/Suprime-Cam. Those images were processed by a pipeline developed by JVO.
- ID:
- ivo://jvo/subaru/sxds/v1.0
- Title:
- Subaru/XMM-Newton Deep Survey v1.0
- Short Name:
- SXDS_V1
- Date:
- 11 Sep 2021 01:04:42
- Publisher:
- JVO
- Description:
- The Subaru/XMM-Newton Deep Survey (SXDS) is a major new multi-wavelength survey of a ~1.3 square degree region of sky. The SXDS optical imagery represents an unprecedented combination of depth and area coverage, and will be combined with suitably deep images at other wavelengths to provide an accurate census of the contents of the Universe without suffering from the biasing effects of large-scale structure.
- ID:
- ivo://wfau.roe.ac.uk/sss-siap
- Title:
- SuperCOSMOS Sky Surveys SSS SIAP Cutout Service
- Short Name:
- SuperCOSMOS SIAP
- Date:
- 09 Jul 2019 14:41:02
- Publisher:
- WFAU, Institute for Astronomy, University of Edinburgh
- Description:
- Simple image access to SuperCOSMOS Sky Surveys (SSS) images (scans of photographic survey plates)
- ID:
- ivo://irsa.ipac/Spitzer/Images/SAGE
- Title:
- Surveying the Agents of a Galaxy's Evolution
- Short Name:
- SAGE
- Date:
- 16 Mar 2017 01:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Surveying the Agents of a Galaxy's Evolution (SAGE) survey covers the Large Magellanic Cloud (LMC; ~7deg×7deg) using the IRAC (3.6, 4.5, 5.8, and 8 mum) and MIPS (24, 70, and 160 mum) instruments on board the Spitzer Space Telescope. Three key science goals determined the coverage and depth of the survey. The detection of diffuse ISM with column densities >1.2×1021 H cm-2 permits detailed studies of dust processes in the ISM. SAGE's point-source sensitivity enables a complete census of newly formed stars with masses >3 Msolar that will determine the current star formation rate in the LMC. SAGE's detection of evolved stars with mass-loss rates >1×10-8 Msolar yr-1 will quantify the rate at which evolved stars inject mass into the ISM of the LMC. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability.
- ID:
- ivo://irsa.ipac/Spitzer/Images/SAGE-SMC
- Title:
- Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud
- Short Name:
- SAGE-SMC
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Small Magellanic Cloud (SMC) provides a unique laboratory for the study of the lifecycle of dust given its low metallicity (~1/5 solar) and relative proximity (~60 kpc). This motivated the SAGE-SMC (Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity Small Magellanic Cloud) Spitzer Legacy program with the specific goals of studying the amount and type of dust in the present interstellar medium, the sources of dust in the winds of evolved stars, and how much dust is consumed in star formation. This program mapped the full SMC (30 deg2) including the body, wing, and tail in seven bands from 3.6 to 160 mum using IRAC and MIPS on the Spitzer Space Telescope.
- ID:
- ivo://nasa.heasarc/suzamaster
- Title:
- Suzaku Master Catalog
- Short Name:
- SUZAMASTER
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table records high-level information for each Suzaku observation and provides access to the data archive. Each record is associated with a single observation. An observation contains data from all instruments on board Suzaku. This database table is generated at the Suzaku processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/swiftbalog
- Title:
- Swift BAT Instrument Log
- Short Name:
- SwiftBAT
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The BAT can operate several configuration modes simultaneously. Each of the simultaneous modes is listed in separate records within this table. For a given time interval, there are several records (partially overlapping in time), each describing a single configuration/mode. The BAT modes collect data for the entire FOV but also have the capability to record rates (tag mask rate) for up to a few specific sky positions (typically 3) that correspond to a pre-assigned target ID. It is possible that at least two or more of these positions do not coincide with the BAT or NFI pointing position and therefore the target ID does necessarily coincide with Target_ID of the BAT or NFI pointing position. This table records for the position (RA and Dec) and Target_ID parameters the correct values associated to each of the mask tag data. This database table is generated at the Swift processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/bat-flux-1
- Title:
- Swift BAT 70 Month All-Sky Survey: 14\-20 keV: flux
- Short Name:
- BAT-flux-1
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This BAT Hard X-ray Survey data is the 70-month survey product of the BAT instrument on the Swift observatory. Swift/BAT is a wide field-of-view (70x100 degrees) hard X-ray imager consisting of a coded mask and a large array of CdZnTe detectors (with an effective area of ~ 5000 cm<sup>2</sup>). <p> BAT is sensitive in the energy range 14-195 keV. The data are divided into 8 energy bands <table border> <tr><th>Band<th>Energy (keV)<th>Frequency (EHz) </tr> <tr><td>1<td> 14-20 <td> 3.38-4.84</tr> <tr><td>2<td> 20-24 <td> 4.84-5.80</tr> <tr><td>3<td> 24-35 <td> 5.80-8.46</tr> <tr><td>4<td> 35-50 <td> 8.46-12.1</tr> <tr><td>5<td> 50-75 <td> 12.1-18.1</tr> <tr><td>6<td> 75-100 <td> 18.1-24.2</tr> <tr><td>7<td> 100-150<td> 24.2-36.3</tr> <tr><td>8<td> 150-195<td> 36.3-47.2</tr> <tr><td>Sum (SNR only)<td>14-195<td> 3.38-47.2</tr> </table> Each band is represented as as two separate surveys, a signal-to-noise (SNR) map and a flux map. (e.g., BAT-snr-1 or BAT SNR 1 or BAT SNR 14-20, or BAT-Flux-1, ...). An additional summed survey, BAT-SNR-SUM or BAT SNR SUM or BAT SNR 14-195, is also available, but there is no summed flux survey. In our Web interface only the SNR surveys are shown in the Web form. Users can get flux maps corresponding to a given SNR image from the results pages. The batch interfaces may directly query any of the surveys since the user chooses the names explicitly rather than from a selection box. <p> The values displayed in the significance maps are the local signal to noise ratio in each pixel. The noise in these coded-mask images follows a Gaussian distribution with center at zero and a characteristic width (sigma) of 1.0. The noise is calculated locally for each pixel by measuring the RMS value of all pixel values in an annulus around each pixel and hence includs both statistical and systematic components. Known sources are excluded from the annuli. <p> The signal in each pixel is taken from the flux maps. <p> The flux values are in the native BAT survey units of counts/sec/detector. The detector is an individual piece of CZT in the BAT array with an area of 1.6 x 10<sup>-7</sup>m<sup>2</sub>. <p> While the Swift mission is primarily designed to follow gamma-ray bursts, the random distribution of bursts in the sky means that these survey's sky coverage is relatively uniform with the exposure at any point varying between about 6 to 16 megaseconds. The survey limits for source detection are about 10<sup>-11</sup> ergs/s/cm<sup>2</sup> over about half the sky and 1.3x10<sup>-11</sup> ergs/s/cm<sup>2</sup> over 90%. <p> These data replace the 9-month BAT datasets which we have retired. If you wish access to the older data please let us know. Note that for the 9-month data we provided access through the web page to the flux data and gave links to the signal-to-noise maps. Since the existence of sources is most easily seen in the SNR maps, we decided to invert that for this release. <p> For the 8 band data, the source data were provided by the BAT team as 6 FITS files. Each of these contained the 8 bands in separate image extensions for a region centered at l=0,b=+/-90 or l=0,90,180,270,b=0, the centers of 6 cubic facets. However these data are not the classical cube-faced projections, e.g., as used in COBE data. The data on the facets overlap, so that this is just a convenient way to tile the sky. <i>SkyView</i> separated each of the FITS image extensions into a separate file, but no other modifications were made to the data. The summed image was provided as six separate files. Provenance: NASA BAT Team. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/swiftuvot
- Title:
- Swift UVOT Combined V Intensity Images
- Short Name:
- SWIFTUVOT
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Swift UVOT instrument is a 30 cm modified Ritchey-Chretien reflecting telescope launched on board the Swift satellite on November 20, 2004. The range of optical and UV filters can accomodate wavebands between 1700 and 6500 Angstroms. A full field image covers 17x17 arcminutes and at maximum spatial sampling is imaged onto 2048x2048 0.5" pixels. A 1000 second observation can detect point sources to m=22.3 when no filter is used. The Swift Serendipitous Source Catalog (Page et al., 2015) detects sources down to m=23-26 for the six filters in very deep observations, but the typical limits are substantially brighter (~20-23 magnitude). <p> These surveys are mosaics of all Swift UVOT observations released between the start of the mission and July 2017. Data were extracted from the HEASARC archive from the UVOT products directory. Mosaics are provided in six filters and also with no filter, i.e., WHITE. The table below gives the number of observations and bandpasses for each of the filters. For each UVOT observation standard processing generates a counts and exposure file as a single multi-extension FITS file with a separate extension for each filter. To aid processing, these extensions were copied into separate files in directory trees for each filter. Four observations in which the exposure and counts maps did not agree on the filters used were omitted from the processing. <p> Some observations were recorded with 0.5" pixels while others were binned to 1". All 0.5" observations (typically fewer than 10%) were rebinned to the larger pixels for the counts maps since the counts data scales with the pixel size. Since the exposure values are intensive and do not vary significantly based upon the resolution, these data were not generally rebinned unless it was needed to ensure that Order 9 Hips data were produced. <p> The CDS Hipsgen software was used to generate Order 9 HiPS data (~0.8" pixels) for both the Counts and Exposure images. The HiPS (Hierarchical Progressive Survey VO standard) supports multi-resolution mosaics. Any quantitative use of these images should note that the rebinning increases the total counts by a factor of ~(1.0/0.8)^2 ~ 1.56. This software uses a bilinear interpolation to generate HEALPix tiles of an appropriate order (18 in this case). <i>SkyView</i> developed software was used to divide the level 9 counts maps tiles by the corresponding exposure maps to create intensity tiles. Pixels where the exposure was less than 5 seconds were left as NaNs. The lower order (8 to 3) order intensity tiles were then generated by averaging 2x2 sets of the higher order maps treating any missing maps or pixels as NaNs. A HiPS all-sky image was generated by averaged the Order 3 tiles. <p> Only the Intensity HIPS files are presented in the SkyView web page directly, but intensity, counts and exposure maps are available for all seven filters. Note that unlike the XRT HiPS data, the exposure and counts maps have not been clipped. I.e., the source FITS files have been aligned with the coordinate system and thus contain large numbers of unexposed pixels with 0 values. These 0's are simply propogated to HiPS tiles. NaNs are returned in regions which lie outside any of the original source images. For the Intensity map, any pixel for which the exposure was less than 5s is returned as a NaN. <table border> <tr><th align=center>Filter</th><th>Count</th><th>Central Wavelength (&#8491;;)</th><th>Bandpass (&#8491;;)</th><th>Central Frequency(THz)</th><th>Bandpass (THz)</th><th>Coverage</th></tr> <tr><th align=center>WHITE</th><td align='center'>3,000</td><td align='center'>3600</td><td align='center'>1600-6000</td><td align='center'>832</td><td align='center'>500-1874</td> <td>0.0017</td></tr> <tr><th align=center>V</th><td align='center'>30,557</td><td align='center'>5468</td><td align='center'>5083-5852</td>< <td align='center'>548</td><td align='center'>512-590</td> <td>0.0171</td></tr> <tr><th align=center>B</th><td align='center'>28,347</td><td align='center'>4392</td><td align='center'>3904-4880</td> <td align='center'>683</td><td align='center'>614-768</td> <td>0.0112<td></tr> <tr><th align=center>U</th><td align='center'>49,954</td><td align='center'>3465</td><td align='center'>3072-3875</td> <td align='center'>865</td><td align='center'>774-975</td> <td>0.0287</td></tr> <tr><th align=center>UVW1</th><td align='center'>60,690</td><td align='center'>2600</td><td align='center'>2253-2946</td> <td align='center'>1154</td><td align='center'>1017-1330</td><td>0.0277</td></tr> <tr><th align=center>UVM2</th><td align='center'>56,977</td><td align='center'>2246</td><td align='center'>1997-2495</td> <td align='center'>1334</td><td align='center'>1201-1501</td>>td>0.0314</td></tr> <tr><th align=center>UVW2</th><td align='center'>54,590</td><td align='center'>1928</td><td align='center'>1600-2256</td> <td align='center'>1554</td><td align='center'>1328-1874</td><td>0.0260</td></tr> </table> <strong>Observation counts and bandpasses for UVOT Filters</strong> <p> Provenance: Data generated from public images at HEASARC archive. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/swiftuvlog
- Title:
- Swift UVOT Instrument Log
- Short Name:
- SwiftUVOT
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The UVOT runs only one type of configuration filter/mode/window in a given time interval. This database table, therefore, contains for a given time interval a single record that describes one configuration. This database table is generated by the Swift Data Center. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/swiftxrt
- Title:
- Swift XRT Combined Intensity Images
- Short Name:
- SWIFTXRT
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Swift XRT (<a href="https://ads.harvard.edu/abs/2005SSRv..120..165B">Burrows et al 2005, SSRv, 120, 165</a>) is a sensitive, broad-band (0.2 - 10 keV) X-ray imager with an effective area of about 125 cm**2 at 1.5 keV. The 600 x 600 pixel CCD at the focus provides a 23.6' x 23.6' field of view with a pixel scale of 2.36". The point spread function is 18" (HPD) at 1.5 keV. <p> These XRT surveys represent the data from the first 12.5 years of Swift X-ray observations. They include all data taken in photon counting mode. A total of just over 8% of the sky has some non-zero exposure. The fraction of sky exposed as a function of the exposure is given in the following table: <table border> <tr><th>Exposure</th><td>>0</td> <td>10</td> <td>30</td> <td>100</td> <td>300</td> <td>1000</td> <td>3000</td> <td>1000</td> <td>30000</td> <td>100000</td><td>300000</td></tr> <tr><th>Coverage</th> <td> 8.42 </td><td> 8.37 </td><td> 8.29 </td><td> 7.67 </td><td> 7.29 </td><td> 5.68 </td> <td> 3.40 </td><td> 1.26 </td><td> 0.35 </td><td> 0.044 </td><td> 0.00118</td></th> </table> The individual exposure and counts maps have been combined into a Hierarchical Progressive Survey (HiPS) where the data are stored in tiles in the HEALPix projection at a number of different resulutions. The highest resolution pixels (HEALPix order 17) have a size of roughly 1.6". Data are also stored at lower resolutions at factors of 1/2, 1/4, 1/8, 1/16, and 1/32, and in an all sky image with a resolution 1/256 of the higest resolution. An intensity map has been created as the ratio of the counts and exposure maps. <p> These surveys combine the basic count and exposure maps provided as standard products in the Swift XRT archive in obsid/xrt/products/*xpc_(sk|ex).img.gz. The surveys were created as follows: <ul> <li>All of the exposure maps available in the archive in mid-May 2017 were combined using the CDS-developed Hipsgen tool. This includes 129,063 observations for which both count and exposure files were found in PC mode. Three exposures where there was a counts map but no exposure map were ignored. A few exposure files had more than one exposure extension. 1,082 files had two extensions and 1 file had 3 extensions. The 1084 HDUs in extensions were extracted as separate files and included in the total exposure. The value of 0 was given to the Hipsgen software as the null value for the FITS files. This caused the CDS software to treat such pixels as missing rather than 0 exposure. <li> The counts data was extracted from the counts maps for each observation using <i>SkyView</i> developed software. For any pixel in which a count was recorded, the corresponding exposure file was checked and if there was any exposure (in any of the associated extensions), then the count was retained. If there was no exposure in any of the extensions of the corresponding exposure file, the counts in the pixel were omitted. Once a count was accepted, the overlap between the counts map pixel and the pixels of the corresponding HiPS tile (or tiles) was computed. Each count was then assigned entirely to a single pixel in the HiPS tile randomly but with the destination pixel probabilities weighted by area of the overlap. Thus if several pixels were found in a given counts map pixel they might be assigned to different pixels in the output image. The HiPS pixels (~1.6") used were of substantially higher resolution than the XRT resolution of 18" and somewhat higher than the counts map resolution of 2.36". <p> A total of 183,750,428 photons were extracted from the counts maps while 15,226 were rejected as being from pixels with 0 exposure. There were 501 pixels which required special treatment as straddling the boundaries of the HEALPix projection. <li> The resulting counts tiles were then clipped using the exposure tiles that had been previously generated. Basically this transferred the coverage of the exposure tiles to the counts tiles. Any counts pixel where the corresponding exposure pixel was a NaN was changed to a NaN to indicate that there was no coverage in this region. <p> During the clipping process 137,730 HiPS level 8 were clipped (of 786,432 over the entire sky). There were 12,236 tiles for which there was some exposure but no counts found. During the clipping process 2 photons were found on pixels where there was no corresponding exposure in the exposure tiles. This can happen when the pixel assignment process noted above shifts a photon just outside the exposed region but should be -- as it was -- rare. These photons were deleted. <li> After creating the clipped level 8 counts maps, level 7 to 3 tiles and an all sky map where generated by averaging pixels 2x2 to decrease each level. When adding the four pixels in the level N map together only pixels whose value was not NaN were considered. <li> Finally an intensity map was created by dividing the counts tiles by the exposure tiles. To eliminate gross fluctuations due to rare counts in regions with very low exposure, only regions with exposure > 1 second were retained. A total of 30 photons were deleted due to this criterion. </ul> <p> Note that while any sampler may in principle be used with these data, the Spline sampler may give unexpected results. The spline computation propogates NaNs thought the image and means that even occasional NaNs can corrupt the output image completely. NaNs are very common in this dataset. Also, if the region straddles a boundary in the HEALPix projection, the size of the requested input region is likely to exceed memory limits since the HiPS data are considered a single very large image. Provenance: Data generated from public images at HEASARC archive. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/swiftxrlog
- Title:
- Swift XRT Instrument Log
- Short Name:
- SwiftXRT
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The XRT runs only one type of configuration mode/window in a given time interval. The table therefore contains for a given time interval a single record that describes one configuration. A new record is generated when the following is changing within an observation: new operating mode , new pointing mode, or new window configuration. This database table is generated by the Swift Data Center. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/sumss
- Title:
- Sydney University Molonglo Sky Survey
- Short Name:
- SUMSS
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Sydney University Molonglo Sky Survey (SUMSS) is a deep radio survey at 843 MHz of the entire sky south of declination -30&#176;;, made using the Molonglo Observatory Synthesis Telescope (<a href="https://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. Data were last updated on January 28, 2015. <p> Images can also be obtained from the <a href="https://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> Provenance: The SUMSS project team, University of Sydney. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/tartarus
- Title:
- Tartarus: Reduced ASCA AGN Data (Version 3.1)
- Short Name:
- ASCA/AGN
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Tartarus database contains the results of a detailed but systematic analysis of ASCA observations of active galactic nuclei (AGN). It contains source and background events files, spectra, ancillary response files and response matrices, images, and assorted light curves for a large number of ASCA AGN observations. Spectral fit results are done by automatic XSPEC fitting. This database table allows easy access to reduced AGN data for the whole community, allowing the maximum scientific return from the data. Availability of publishable light curves, images, and spectra (which can also be readily re-fitted) should be particularly valuable to astronomers with little direct experience in the reduction of X-ray data. Version 3.1 has been created by analyzing all ASCA observing sequences with targets designated as AGN, as indicated by a leading "7" in the ASCA observing sequence number. Version 3.1 contains products for all 611 observing sequences designated as AGN observations. This is a significant improvement over Versions 1 and 2. Moreover, the 611 sequences for which products are available are complete in the sense that either the target object was not detected (in which case an upper limit on GIS2 source counts is given) or the intended AGN target was detected and the data were fully analyzed. In order to obtain the most accurate background subtraction and minimize contamination from any nearby sources, version 3.1 makes more use of custom extraction regions than previous versions. It is expected that version 3.1 will be replaced when the final ASCA calibration is completed. This database table has been created by the Tartarus Team, and they, rather than Imperial College London or the HEASARC, are responsible for the contents. It was ingested by the HEASARC in August, 2005. This is a service provided by NASA HEASARC .
- ID:
- ivo://irsa.ipac/Spitzer/Images/Taurus
- Title:
- Taurus 2: Finishing the Spitzer Map of the Taurus Molecular Clouds
- Short Name:
- Taurus
- Date:
- 27 Oct 2022 19:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Taurus Spitzer Legacy project has mapped ≈44 square degrees of the Taurus star-formation region using the IRAC and MIPS cameras aboard the Spitzer Space Telescope.
- ID:
- ivo://irsa.ipac/AKARI/Images/AKARIFIS
- Title:
- The AKARI Far-Infrared All-Sky Survey Maps
- Short Name:
- AKARIFIS
- Date:
- 26 Apr 2023 17:15:24
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The AKARI Far-Infrared All-Sky Survey Maps cover >99% of the sky in four photometric bands centered at 65, 90, 140, and 160 microns, with spatial resolutions of 1'-1.5'.
- ID:
- ivo://svo.cab/caha
- Title:
- The CALAR ALTO PUBLIC ARCHIVE AT CAB
- Short Name:
- CAHA
- Date:
- 28 Jul 2020 15:48:31
- Publisher:
- Spanish Virtual Observatory
- Description:
- This data server provides access to astrometrically and photometrically corrected images of the Calar Alto Archive. It contains images of the instrument CAFOS, reduced using the pipeline Filabres (https://filabres.readthedocs.io/en/latest/index.html)
- ID:
- ivo://irsa.ipac/IRAS/Images/EIGA
- Title:
- The Extended IRAS Galaxy Atlas
- Short Name:
- EIGA
- Date:
- 31 Mar 2023 23:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- 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).
- ID:
- ivo://irsa.ipac/CHaMP/Images
- Title:
- The Galactic Census of High and Medium-mass Protostars
- Short Name:
- CHaMP
- Date:
- 01 May 2023 19:01:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- CHaMP is a multi-faceted survey of molecular clouds and star formation along the Carina Arm of the Milky Way (300d > l > 280d, -4d < b < +2d).
- ID:
- ivo://svo.cab/gtc
- Title:
- THE GTC ARCHIVE (USER REDUCED DATA) AT CAB
- Short Name:
- GTC
- Date:
- 28 May 2020 15:39:57
- Publisher:
- Spanish Virtual Observatory
- Description:
- SIAP service for GTC Public Data
- ID:
- ivo://nasa.heasarc/skyview/hawaii-hdf-b
- Title:
- The Hawaii Hubble Deep Field North: Band B
- Short Name:
- Hawaii HDF B
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Hawaii-HDF-N is an intensive multi-color imaging survey of 0.2 sq. degrees centered on the HDF-N. Data were collected on the NOAO 4m Mayall telescope, the National Astronomical Observatory of Japan 8.2m Subaru telescope and the University of Hawaii 2.2m telescope. Deep U, B, V, R, I, and z' data were obtained over the whole field and deep HK' data over the Chandra Deep Field North. Details are available in the references. [Adapted from reference website.] <P> Two different images are given in the V band (V0201 and V0401) from observations separated by about a month that had substantial differences in seeing. Provenance: Data downloaded from the reference website. A formatting error in the FITS files was corrected.. This is a service of NASA HEASARC.
299. The HI 4-PI Survey
- ID:
- ivo://nasa.heasarc/skyview/hi4pi
- Title:
- The HI 4-PI Survey
- Short Name:
- HI4PI
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The HI 4-PI Survey (HI4PI) is a 21-cm all-sky survey of neutral atomic hydrogen. It is constructed from the Effelsberg-Bonn HI Survey (EBHIS), made with the 100-m radio telescope at Effelsberg/Germany, and the Galactic All-Sky Survey (GASS), observed with the Parkes 64-m dish in Australia. HI4PI comprises HI line emission from the Milky Way. This dataset is the atomic neutral hydrogen (HI) column density map derived from HI4PI (|Vlsr| < 600 km/s). Provenance: Argelander-Institut für Astronomie (AIfA), Max-Planck-Institut für Radioastronomie (MPIfR), and CSIRO/Australia; data provided by B. Winkel. This is a service of NASA HEASARC.
- ID:
- ivo://iacvo/nebula
- Title:
- The IAC Morphological Catalog of Northern Galactic Planetary Nebulae
- Short Name:
- IAC-PNebula
- Date:
- 11 Aug 2023 13:03:05
- Publisher:
- Instituto de Astrofísica de Canarias
- Description:
- The IAC Morphological Catalog of Northern Galactic Planetary Nebulae (PNs)
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