- 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.
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- 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:
- 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.
- ID:
- ivo://nasa.heasarc/swiftuvlog
- Title:
- Swift UVOT Instrument Log
- Short Name:
- SwiftUVOT
- Date:
- 07 Mar 2025
- 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 .
