- ID:
- ivo://nasa.heasarc/skyview/iras
- Title:
- IRAS Sky Survey Atlas: 12 micron
- Short Name:
- IRAS
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The IRAS data include all data distributed as part of the IRAS Sky Survey Atlas. Data from the four IRAS bands are shown as individual surveys in SkyView. Users should be aware that IPAC does not encourage the use of data near the ecliptic plane as they feel that contribution from local cirrus emission is significant. <p> The data are distributed in sets of 430 maps. Each map covers approximately 12.5x12.5 degrees, and the map centers are offset by 5 degrees so that there is a 2.5 degree overlap. IPAC has processed to a uniform standard so that excellent mosaics of the maps can be made. Users should be cautious of data in saturated regions. Known problems in the analysis mean that data values are unlikely to be correct. Note that IPAC has optimized the processing of these data for features of 5' or more although the resolution of the data is closer to the 1.5' pixel size. <p> There are occasional pixels in the IRAS maps which are given as NULL values. Unless these are explicitly trapped by user software, these data will appear as large negative values. SkyView ignores these pixels when determining the color scale to display an image. <p> Essentially the entire sky is covered by the survey. However there are a few regions not surveyed and the data values in these regions are suspect. These are given to users as delivered from IPAC. Provenance: NASA IPAC/Jet Propulsion Laboratory. This is a service of NASA HEASARC.
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- ID:
- ivo://nasa.heasarc/isolog
- Title:
- ISO (Infrared Space Observatory) Observation Log
- Short Name:
- ISO
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database is the ISO (Infrared Space Observatory) Observation Log of Validated Data. ISO is an ESA (European Space Agency) project with instruments funded by ESA member states (especially the PI countries of France, Germany, the Netherlands and the United Kingdom), and with the participation of ISAS (Japan) and NASA (USA). ISO operated from November 1995 till May 1998, almost a year longer than expected. As an unprecedented observatory for infrared astronomy, able to examine the cool and hidden places in the Universe, ISO successfully made nearly 30,000 scientific observations. The ISO data can be retrieved from the ISO Data Archive (<a href="http://iso.esac.esa.int/ida/">http://iso.esac.esa.int/ida/</a>), which is available at the ISO Data Centre (<a href="http://iso.esac.esa.int/">http://iso.esac.esa.int/</a>), and comprises about 150,000 observations, including calibration, parallel mode and serendipitous observations. The present catalog contains all observations performed in standard observing modes exempt from technical problems; special flags indicate calibration observations. The catalog gives observation details and provides links to quick-look images depicting the data and to observation-specific documentation. The ISO helpdesk can be reached at <a href="http://iso.esac.esa.int/esupport/">http://iso.esac.esa.int/esupport/</a> This online catalog was last updated by the HEASARC in September 2004 based on the machine-readable table <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VI/111/isolog.dat.gz">https://cdsarc.cds.unistra.fr/ftp/cats/VI/111/isolog.dat.gz</a> obtained from the CDS data center. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/iuelog
- Title:
- IUE (International Ultraviolet Explorer) Final Merged Observation Log
- Short Name:
- IUE
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This IUE (International Ultraviolet Explorer) Observation Log contains a summary of all IUE Newly Extracted Spectra (INES), which resulted from a post-processing effort at VILSPA. It was constructed by using verified data from the IUE Final Archive Master Catalog. The observations cover the whole life of the IUE satellite, from March 1978 to September 1996. This online catalog was ingested by the HEASARC in August 2004 based on the machine-readable table VI/110/inescat.dat obtained from the CDS data center. In May 2020, the program_id values of "\" were changed by the HEASARC to nulls for improved database compatibility. This is a service provided by NASA HEASARC .
494. IXPE Master Catalog
- ID:
- ivo://nasa.heasarc/ixmaster
- Title:
- IXPE Master Catalog
- Short Name:
- IXMASTER
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Launched in late 2021, the Imaging X-ray Polarimetry Explorer (IXPE) is a NASA Small Explorer Mission in collaboration with the Italian Space Agency (ASI). The mission measures X-ray polarization from compact objects such as neutron stars and black holes, which serve as laboratories for exploring extreme gravitational and magnetic fields. With its imaging capabilities, IXPE will also map the magnetic-field structure of a few extended sources such as supernova remnants and pulsar wind nebulae. This table contains a list of (a) unobserved targets that are planned for observation by IXPE in the future and (b) IXPE observations which have been processed and successfully validated by the IXPE team. The data from these observations may or may not be public and the user should check the value of the public_date parameter to determine the status of a specified data set. Only those ObsIDs which have a public_date in the past will have data publicly available. Observations with a public_date parameter value which is either blank or a date in the future have been ingested into the HEASARC archive but will remain encrypted until their public date. This contents of this database table are generated by the IXPE Team and updated regularly with new observations. These updates are then delivered to the HEASARC and ingested into the HEASARC database in a timely fashion. Note that some parameters have been added and are populated by the HEASARC. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/kaporixmm
- Title:
- Kappa Orionis XMM-Newton X-Ray Point Source Catalog
- Short Name:
- KAPORIXMM
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- X-rays are a powerful probe of activity in the early stages of star formation. They allow us to identify young stars even after they have lost the IR signatures of circumstellar disks and provide constraints on their distance. Here, the authors report on XMM-Newton observations that detected 121 young stellar objects (YSOs) in two fields between the filamentary dark cloud complex Lynds 1641S and the star Kappa Ori. These observations extend the Survey of Orion A with XMM and Spitzer (SOXS). The YSOs are contained in a ring of gas and dust apparent at millimeter wavelengths, and in far-IR and near-IR surveys. The X-ray luminosity function of the YSOs detected in the two fields indicates a distance of 250-280 pc, much closer than the Orion A cloud and similar to the distance estimates for Kappa Ori. The authors propose that the ring is a 5-8 pc diameter shell that has been swept up by Kappa Ori. This ring contains several groups of stars detected by Spitzer and WISE including one surrounding the Herbig Ae/Be star V1818 Ori. In this interpretation, the Kappa Ori ring is one of several shells swept up by massive stars within the Orion Eridanus Superbubble and is unrelated to the southern portion of Orion A/L 1641S. The XMM-Newton observations consist of two fields, north (Field N = KN) and south (Field S = KS), and were obtained in 2015 March 10 and 15 using EPIC as the primary instrument. Table 1 in the reference paper shows the details of the exposures, each one with a duration of about 50 ks and taken with the Medium filter. The authors used SAS version 14.0 to reduce the observation data files (ODFs) and to obtain calibrated lists of events for the MOS and pn instruments. They filtered the events in the 0.3-0.8 keV energy band and used only events with FLAG = 0 and PATTERN < 12 as prescribed by the SAS manual. With SAS, the authors obtained exposure maps in the 0.3-8.0 keV band and performed source detection with a code based on wavelet convolution that operated simultaneously on MOS and pn data. They used a threshold of significance of 4.5 sigma of the local background to discriminate real sources from spurious background fluctuations. However, they added few sources to the final list with significance S in 4.0 < S < 4.5 for the cases of positional match with objects in SIMBAD or PPMX catalogs. The final list was also checked for spurious sources that could appear at the border of the CCDs. In sum, the authors detected 238 X-ray sources with significance > 4 sigma of the local background; 104 sources are in KN and 134 in KS. The authors cross-correlated the positions of the X-ray sources with the coordinates of the IR catalog of Megeath et al. (2012, AJ, 144, 192). This IR catalog is the result of a survey of Orion with Spitzer that produced a classification of protostars and stars with disks. Of the 238 X-ray sources, 191 are identified within 8 arcseconds of one of 206 IR objects, 99 sources in KS, 92 sources in KN. Some X-ray sources were multiple matches within 8 arcsec of IR objects. For these cases, the authors assigned the most likely counterparts based on IR photometry and visual inspection of X-rays and IR images. However, nine X-ray sources were left associated with two or three IR objects. Among the IR matches, the authors found 15 stars with disks in KN and 35 in KS with X-ray detection. One protostar in KN and three in KS were detected in X-rays. The authors used X-ray detection of sources without IR excess as criteria to identify disk-less stars (hereafter Class III stars). They classified as Class III stars those IR objects with X-ray detections, with [4.5um]-[8.0um] colors < 0.3 mag and brighter than [4.5um] magnitude < 14. At the distance of the ONC (400 pc), the [4.5um] magnitude ~ 14 threshold at an age of 4-5 Myrs roughly identifies M3-M4 spectral types and masses around 0.3 solar masses. With this selection scheme, the authors identified 48 objects in KN and 19 in KS as Class III candidates. This table was created by the HEASARC in August 2016 based on the electronic version of Table 2 from the reference paper which was obtained from the CDS (their catalog J/ApJ/820/L28 file table2.dat). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/kommersgrb
- Title:
- Kommers et al. (2001) BATSE Non-Triggered Gamma-Ray Burst Catalog
- Short Name:
- Kommers
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This is the Kommers et al. (2001) Non-Triggered Burst Supplement to the BATSE Gamma-Ray Burst (GRB) Catalog. It contains 873 "non-triggered" GRBs that were detected in a search of the BATSE Archival continuous data recorded between 1991 December 9 and 1997 December 17 for which the BATSE on-board burst trigger was not activated, for example because the burst was too faint to exceed the on-board detection threshold or it occurred while the on-board trigger was disabled for technical reasons. For each burst, the catalog gives an estimated source direction, duration, peak flux, and fluence. This catalog increases the number of GRBs detected using BATSE by 48% during the time period covered by the search. This database table was created at the HEASARC in September 2001 using the authors' file <a href="http://space.mit.edu/BATSE/ntgrb-ascii.html">http://space.mit.edu/BATSE/ntgrb-ascii.html</a> This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/kvttmcomis
- Title:
- Kvant TTM/COMIS X-Ray Source Catalog
- Short Name:
- KVTTMCOMIS
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- A catalog of X-ray sources in the 2-30 keV energy band as observed by the TTM/COMIS (Coded Mask Imaging Spectrometer) telescope onboard the Mir-Kvant observatory is presented. Brief information about the 67 sources detected at a confidence level higher than 4 sigma between 1988 and 1998 is provided. X-ray properties and characteristic spectra of different types of sources are briefly described in the reference paper. This table was created by the HEASARC in April 2011 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/PAZh/26/355">CDS catalog J/PAZh/26/355</a> file table1.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/cdfs-less
- Title:
- LABOCA Extended Chandra Deep Field South Submillimetre Survey
- Short Name:
- CDFS LESS
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The LABOCA Extended Chandra Deep Field South (ECDFS) Submillimetre Survey (LESS) is a public legacy survey of the ECDFS at 870 μm using the LABOCA camera (Siringo et al. 2009) on the APEX telescope. <p> The LABOCA data presented here were obtained between 2007 May and 2008 November in excellent conditions using time from both ESO and Max Planck allocations. The mapping pattern was designed to uniformly cover the 30'x30' extent of the ECDFS, centered on 03:32:29.0, -27:48:47.0 (J2000). The project used a total of 310 hrs of observations to achieve a beam-smoothed noise of 1.2 mJy/beam over 900 sq. arcmin (and <1.6mJy/beam over 1260 sq. arcmin). The flux calibration of the map came from observations of Mars, Uranus and Neptune (as well as secondary calibrators) and is accurate to within 8.5%. Provenance: Data downloaded from ESO archive. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/lalaboocxo
- Title:
- LALA Bootes Field Chandra X-Ray Point Source Catalog
- Short Name:
- LALABOOCXO
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the results of an analysis of a deep, 172 ks Chandra observation of the Large Area Lyman Alpha survey (LALA) Bootes field which was obtained with the Advanced CCD Imaging Spectrometer (ACIS-I) on board the Chandra X-Ray Observatory. This is one of the deepest Chandra images of the extragalactic sky, with only the 2 Ms Chandra Deep Field North (CDF-N) and the 1 Ms Chandra Deep Field South (CDF-S) observations being substantially deeper. In this table, the X-ray source catalog obtained from this image is presented, along with some results from an analysis of the X-ray source counts and optical identifications. The X-ray image is composed of two individual observations obtained in 2002 and reaches 0.5 - 2.0 and 2.0 - 10.0 keV flux limits of 1.5 x 10<sup>-16</sup> and 1.0 x 10<sup>-15</sup> ergs/cm<sup>2</sup>/s, respectively, for point sources near the aim point. A total of 168 X-ray sources were detected: 160 in the 0.5 - 7.0 keV band, 132 in the 0.5 - 2.0 keV band, and 111 in the 2.0 - 7.0 keV band. Since X-ray source number 122 has two possible optical counterparts, it is listed twice, once for each counterpart, and the total number of entries in this table is this 169. The primary optical data are R-band imaging from the NOAO Deep Wide-Field Survey (NDWFS), with a limiting magnitude of R = 25.7 magnitudes, (Vega, 3-sigma detection level, and a 4" diameter aperture). Optical counterparts within 1.5" or the 3-sigma X-ray positional uncertainties, whichever was larger, were detected above this level in the R band for 144 of the 168 X-ray sources. At least 90% of the optical counterparts should be the correct matches, and, at worst, there might be ~14 false matches. This table was created by the HEASARC in March 2007 based on the CDS table J/AJ/127/213 file table1.dat, This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/lalacetcxo
- Title:
- LALA Cetus Field Chandra X-Ray Point Source Catalog
- Short Name:
- LALACETCXO
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The 174 ks Chandra Advanced CCD Imaging Spectrometer (ACIS) exposure of the Large Area Lyman Alpha Survey (LALA) Cetus field is the second of the two deep Chandra images on LALA fields. In their paper, the authors present the Chandra X-ray sources detected in the Cetus field, along with an analysis of X-ray source counts, the stacked X-ray spectrum, and the optical identifications. A total of 188 X-ray sources were detected: 174 in the 0.5-7.0 keV band, 154 in the 0.5-2.0 keV band, and 113 in the 2.0-7.0 keV band. The X-ray source counts were derived and compared with the 172 ks exposure LALA Bootes field (available as the LALABOOCXO table in Browse). Interestingly, the authors find consistent hard-band X-ray source density, but a (36 +/- 12)% higher soft-band X-ray source density in the Cetus field. The weighted stacked spectrum of the detected X-ray sources can be fitted by a power law with photon index Gamma = 1.55. Based on the weighted stacked spectrum, the authors find that the resolved fraction of the X-ray background drops from (72 +/- 1)% at 0.5-1.0 keV to (63 +/- 4)% at 6.0-8.0 keV. The unresolved spectrum can be fitted by a power law over the range 0.5-7 keV, with a photon index Gamma = 1.22. Optical counterparts are also presented for 154 of the X-ray sources, down to a limiting magnitude of r' = 25.9 (Vega), using a deep r'-band image obtained with the MMT. This table was created by the HEASARC in October 2010 based on the CDS table J/ApJ/669/765 file table1.dat This is a service provided by NASA HEASARC .
