- ID:
- ivo://nasa.heasarc/skyview/sdss
- Title:
- Sloan Digital Sky Survey g-band
- Short Name:
- SDSS
- Date:
- 07 Mar 2025
- 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.
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- ID:
- ivo://nasa.heasarc/skyview/sdssdr7
- Title:
- Sloan Digital Sky Survey g-band DR7
- Short Name:
- SDSSDR7
- Date:
- 07 Mar 2025
- 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://nasa.heasarc/skyview/goods-isaac-h
- Title:
- Southern GOODS Field: VLT ISAAC Observations, H band
- Short Name:
- GOODS ISAAC H
- Date:
- 07 Mar 2025
- 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:
- 07 Mar 2025
- 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://nasa.heasarc/skyview/goodsirac-1
- Title:
- Spitzer IRAC GOODS 3\.6 micron data, channel 1
- Short Name:
- GOODSIRAC 1
- Date:
- 07 Mar 2025
- 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://nasa.heasarc/skyview/goodsmips
- Title:
- Spitzer MIPS GOODS 24 Micron Data
- Short Name:
- GOODSMIPS
- Date:
- 07 Mar 2025
- 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://nasa.heasarc/suzamaster
- Title:
- Suzaku Master Catalog
- Short Name:
- SUZAMASTER
- Date:
- 07 Mar 2025
- 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. The Suzaku satellate operated from July 2005 till September 2015. This database table was generated at the Suzaku proceesing site with the final data reprocessing (September 2016) after the mission stopped operating. During operation, it was 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:
- 07 Mar 2025
- 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:
- 07 Mar 2025
- 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:
- 07 Mar 2025
- 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.
