- ID:
- ivo://nasa.heasarc/heabib
- Title:
- High Energy Astrophysics Comprehensive Bibliography Catalog
- Short Name:
- HEABIB
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This bibliographic catalog is created by essentially matching scientific publications archived in the ADS with specific observations archived in the HEASARC. The papers can be refereed, unrefereed, or even arXiv preprints that have already been accepted or initially submitted for publication. Each observation in HEASARC's database tables has an ID parameter and each publication has a unique bibliographic reference code (bibcode), allowing a specific match to be made. The information in this table comes from correspondence from the author. This table is updated automatically shortly after the data is received. This is a service provided by NASA HEASARC .
Number of results to display per page
Search Results
- ID:
- ivo://nasa.heasarc/hic
- Title:
- Hipparcos Input Catalog
- Short Name:
- HIC
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table contains the Hipparcos Input Main Cataloge of 118209 stars. The Hipparcos Input Catalogue was constructed as the observing program for the European Space Agency's Hipparcos astrometry mission. The requirements of the project in terms of completeness, sky coverage, astrometric and photometric accuracy, as well as the necessary optimization of the scientific impact, resulted in an extended effort to compile and homogenize existing data, to clarify sources and identifications, and, where needed, to collect new data matching the required accuracy. This has resulted in an unprecedented catalog of stellar data including up-to-date information of positions, proper motions, magnitudes and colors, and (wherever available) spectral types, radial velocities, multiplicity and variability information. The catalog is complete to well-defined magnitude limits and includes a substantial sampling of the most important stellar categories present in the solar neighborhood beyond these limits. The magnitudes vary from 7.3 to 9 mag as a function of galactic latitude and spectral type, and there are no stars fainter than about V=13 mag. The 118209 stars of the Hipparcos Input Catalogue were selected from some 214000 distinct candidates contained in some 214 observations programs. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/hipparcos
- Title:
- Hipparcos Main Catalog
- Short Name:
- Hipparcos
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Hipparcos and Tycho Catalogues are the primary products of the European Space Agency's astrometric mission, Hipparcos. The satellite, which operated for four years, returned high quality scientific data from November 1989 to March 1993. Each of the catalogues contains a large quantity of very high quality astrometric and photometric data. In addition there are associated annexes featuring variability and double/multiple star data, and solar system astrometric and photometric measurements. In the case of the Hipparcos Catalogue, the principal parts are provided in both printed and machine-readable form (on CDROM). In the case of the Tycho Catalogue, results are provided in machine-readable form only (on CDROM). Although in general only the final reduced and calibrated astrometric and photometric data are provided, some auxiliary files containing results from intermediate stages of the data processing, of relevance for the more-specialised user, have also been retained for publication. (Some, but not all, data files are available from the Centre de Donnees astronomiques de Strasbourg.) The global data analysis tasks, proceeding from nearly 1000 Gbit of raw satellite data to the final catalogues, was a lengthy and complex process, and was undertaken by the NDAC and FAST Consortia, together responsible for the production of the Hipparcos Catalogue, and the Tycho Consortium, responsible for the production of the Tycho Catalogue. A fourth scientific consortium, the INCA Consortium, was responsible for the construction of the Hipparcos observing programme, compiling the best-available data for the selected stars before launch into the Hipparcos Input Catalogue. The production of the Hipparcos and Tycho Catalogues marks the formal end of the involvement in the mission by the European Space Agency and the four scientific consortia. For much more information about this catalog, such as fuller descriptions of the parameters, the user is urged to check the Hipparcos and Tycho Catalogs website at <a href="https://www.cosmos.esa.int/web/hipparcos/catalogues">https://www.cosmos.esa.int/web/hipparcos/catalogues</a>. This database table was created by the HEASARC in April 2000 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/239">CDS Catalog I/239</a> file hip_main.dat.gz, the Hipparcos Main Catalog. It was updated in October 2002 to fix some entries which were missing coordinates. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/hipnewcat
- Title:
- Hipparcos New Astrometric Catalog
- Short Name:
- HIPNEWCAT
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- A new reduction of the astrometric data as produced by the Hipparcos mission has been published, claiming accuracies for nearly all stars brighter than Hipparcos magnitude H_p = 8 to be better, by up to a factor 4, than in the original catalog. The new Hipparcos astrometric catalog has been checked for the quality of the data and the consistency of the formal errors as well as the possible presence of error correlations. The differences with the earlier publication of the Hipparcos Catalog are explained in the reference paper. The internal errors are followed through the reduction process, and the external errors are investigated on the basis of a comparison with radio observations of a small selection of stars, and the distribution of negative parallaxes. Error correlation levels are investigated and the reduction by more than a factor 10 as obtained in the new catalog is explained. The formal errors on the parallaxes for the new catalog are confirmed. The presence of a small amount of additional noise, though unlikely, cannot be ruled out. The new reduction of the Hipparcos astrometric data provides an improvement by a factor 2.2 in the total weight compared to the Hipparcos catalog published in 1997, and, according to the author, provides much improved data for a wide range of studies on stellar luminosities and local galactic kinematics. Note that this catalog version is slightly different from the one published in the book, as an error that sometimes affected the goodness of fit value for the solution was corrected. The first version of these data archived at the CDS (between June and 15 September 2008) also contained errors which were corrected after this date. This table was created by the HEASARC in August 2009 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/311">CDS Catalog I/311</a> file hip2.dat, "the Astrometric Catalogue". This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/hitomaster
- Title:
- Hitomi Master Catalog
- Short Name:
- HITOMASTER
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table records high-level information for the observations obtained with Hitomi and provides access to the data archive. The Hitomi mission was launched on a JAXA H-IIA into low Earth orbit on February 17, 2016, at 5:45 pm JPS from Tanegashima Space Center. Hitomi was equipped with four different instruments that together cover a wide energy range 0.3-600 keV. The Soft X-ray Spectrometer (SXS), which combined a lightweight Soft X-ray Telescope paired with a X-ray Calorimeter Spectrometer, provided non-dispersive 7-eV resolution in the 0.3-10 keV bandpass with a field of view of about 3 arcminutes. The Soft X-ray Imager (SXI) expanded the field of view with a new generation CCD camera in the energy range of 0.5-12 keV at the focus of the second lightweights Soft X-ray Telescope; the Hard X-ray Imager (HXI, two units) performed sensitive imaging spectroscopy in the 5-80 keV band; the non-imaging Soft Gamma-ray Detector (SGD, two units) extended Hitomi's energy band to 600 keV. On March 27, 2016, JAXA lost contact with the satellite and, on April 28, announced the cessation of the efforts to restore mission operations. At that time Hitomi was in check-out phase and had started the calibration observations. Data were collected from six celestial objects (Perseus, N132D, IGR_J16318-4848, RXJ1856.5-3754, G21.5-0.9, and Crab) as well as black sky for a total of about one month of data. The data from these observations were divided into intervals of one day if the observation of a specific pointing was longer that one day. A sequence number was assigned to each observing day and within data from all instruments are included. The day division was mainly to limit the data size within a sequence number. There are in total 42 sequences, and each record in this database table is dedicated to a single sequence. The early observations do not contain data from all instruments and in cases the object was not always placed at the aim point. This database contains parameters to indicate which instrument was on and if the celestial source was in the field of view. The SXS was the first instrument to turn on and therefore all observations contain SXS data, although the thermal equilibrium was reached after March 4 2016. The second instrument was the SXI followed by the HXIs and, finally, the two SGDs. This database table was generated at the Hitomi Science Data Center processing site (Angelini, L., Terada, Y, et al., 2016, SPIE 9905E, 14) with additions to indicate which instrument was on and if the source was in the FOV. It was ingested into the HEASARC database in June 2017. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/hperseicxo
- Title:
- H Persei Chandra X-Ray Point Source Catalog
- Short Name:
- HPERSEICXO
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains some of the results from a Chandra/ACIS-I observations of the massive ~ 13-14 Myr-old cluster, h Persei, part of the famous Double Cluster (h and Chi Persei) in Perseus. Combining the list of 330 Chandra-detected sources with new optical/IR photometry and optical spectroscopy reveals ~ 165 X-ray bright stars with V <~ 23. Roughly 142 have optical magnitudes and colors consistent with cluster membership. The observed distribution of X-ray luminosity L<sub>x</sub> peaks at L<sub>x</sub> ~ 10<sup>30.3</sup> erg s<sup>-1</sup> and likely traces the bright edge of a far larger population of ~ 0.4-2 M<sub>sun</sub> X-ray active stars. From a short list of X-ray active stars with IRAC 8-micron excess from warm, terrestrial zone dust, the authors derive a maximum X-ray flux incident on forming terrestrial planets. Although there is no correlation between X-ray activity and IRAC excess, the fractional X-ray luminosity correlates with optical colors and spectral type. By comparing the distribution of L<sub>x</sub>/L<sub>star</sub> versus spectral type and (V-I) in h Per with results for other 1-100 Myr-old clusters, the authors show that stars slightly more massive than the Sun (>~ 1.5 M<sub>sun</sub>) fall out of X-ray saturation by ~ 10-15 Myr. Changes in stellar structure for >~ 1.5 M<sub>sun</sub> stars likely play an important role in this decline of X-ray emission. Chandra observations of h Persei were taken with a 41.1 ks exposure on 2004 December 2, (Obs. ID 5407; Sequence Number 200341) with the ACIS detector (chips 0, 1, 2, 3, 6, and 7). The data were obtained in dithered, timed mode, with a frametime of 3.2 s. On-board event rejection and event telemetry was in the VFAINT mode. The field was centered on RA(2000) = 2h19m00s, Dec(2000) = 57d07'12", close to the center of h Persei from Bragg & Kenyon (2005, AJ, 130, 134) (RA(2000) = 2h18m56.4s, Dec(2000) = 57d08'25") and observed at a roll angle of 229 degrees. The data were not registered to an astrometric reference frame (e.g., Two Micron All Sky Survey, 2MASS). The ACIS-I field covers a 17' x 17' area. This table was created by the HEASARC in March 2009 based on the electronic versions of Tables 1 and 2 from the paper which were obtained from the Astronomical Journal web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/hstpaec
- Title:
- HST Planned and Archived Observations
- Short Name:
- HSTPAEC
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This is the HST Planned and Archived Exposures Catalog (PAEC) as obtained from the Space Telescope Science Institute (STScI) Archive which created the original compilation from their Archive and Proposal databases. This database table provides a summary of all approved HST observations, including already completed observations and those which are planned to be executed as part of the current cycle or are reserved for execution by Guaranteed Time Observer (GTO) programs for the upcoming cycles. This database table provides a summary of both planned and completed HST observations. Much more information can be obtained about each exposure, and the data themselves can be retrieved, using STScI's Multimission Archive (URL is <a href="http://archive.stsci.edu/hst/">http://archive.stsci.edu/hst/</a>) or STScI's Archive Web Interface (URL is <a href="http://archive.stsci.edu/hst/search.php">http://archive.stsci.edu/hst/search.php</a>). Note that a number of solar system and other objects have 0 values for their 2000 equinox RA and declination coordinates in the original HST table and hence also in this HEASARC database. This HEASARC version of the HSTPAEC will be updated on a regular basis, usually within one month of the data files on the STScI Web site (URL <a href="http://archive.stsci.edu/hst/paec.html">http://archive.stsci.edu/hst/paec.html</a>) being updated. This database table is recreated by the HEASARC on a routine basis, usually within one month of the PAEC data files at the STScI Hubble Data Archive (HDA) being modified. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/hubbleudf
- Title:
- Hubble Ultra Deep Field Catalog
- Short Name:
- UDF
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Hubble Ultra Deep Field (UDF, Principle Investigator: Steven V. W. Beckwith) is a 400-orbit Hubble Space Telescope (HST) Cycle 12 program to image a single field of the Wide Field Camera (WFC) of the Advanced Camera for Surveys (ACS) in four filters: F435W (B), F606W (V), F775W (i), and F850LP (z). The observations took place over 4 months from September 2003 to January 2004 under two program IDs: 9978 and 10086. The observations consist of half-orbit exposures, cycling through each of the filters in a 4-point dither pattern to provide sub-pixel sampling, as well as a larger-scale 3-point line pattern to cover the 2 second of arc gap between the two ACS/WFC chips. The total exposure times are summarized below, with typical exposure times of 1200s for individual images. The AB magnitude zero-points for ACS are current as of March 2004. <pre> Number of Number of Total Exp. AB mag. Orbits Exposures Time (s) zero-point B (F435W): 56 112 134880 25.673 V (F606W): 56 112 135320 26.486 i (F775W): 144 288 347110 25.654 z (F850LP): 144 288 346620 24.862 </pre> This HEASARC Browse table contains the list of sources found in the deepest UDF image, the i-band image. The formal i-band catalog contains a total of 10,040 sources. A visual inspection of all the sources revealed an additional 5 spurious sources (which do not form part of the catalog). Moreover, the deblending algorithms in SExtractor caused an additional 100 sources to be missed, owing to their proximity to brighter sources. These sources were identified manually, and formally added by doing another SExtractor run with considerably different deblending parameters, in order to detect them all. An initial list of 208 sources was produced, which was then reduced to a total of 100 sources after visual inspection and rejection of sources that were clearly part of previously identified sources. These additional sources are denoted by ID numbers 20001 - 20208. Although the i-band image is the deepest image, there remain additional sources that were not detected in i-band, even though they may be detected in one of the other bands. Therefore, the authors produced a second catalog based on detection in the z-band image (not part of the present table), and an additional 39 sources are included from this catalog that were detected at > 10 sigma in the z-band image, but were not in the catalog that was run using the i-band image for detection. These additional sources are denoted by ID numbers above 30000. More details are found in the file <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/258/intro.txt">https://cdsarc.cds.unistra.fr/ftp/cats/II/258/intro.txt</a> or from the UDF home page at <a href="http://www.stsci.edu/hst/udf/">http://www.stsci.edu/hst/udf/</a>. This table was created by the HEASARC in May 2005 based on CDS table II/258/udf-i.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ic1396acxo
- Title:
- IC1396A&Trumpler37ClusterChandraX-RayPointSourceCatalog
- Short Name:
- IC1396ACXO
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Rich, young stellar clusters produce H II regions whose expansion into the nearby molecular cloud is thought to trigger the formation of new stars. However, the importance of this mode of star formation is uncertain. This investigation seeks to quantify triggered star formation (TSF) in IC 1396A (aka the Elephant Trunk Nebula), a bright-rimmed cloud (BRC) on the periphery of the nearby giant HII region IC 1396 produced by the Trumpler 37 cluster. X-ray selection of young stars from Chandra X-ray Observatory data is combined with existing optical and infrared surveys to give a more complete census of the TSF population. Over 250 young stars in and around IC 1396A are identified; this doubles the previously known population. A spatio-temporal gradient of stars from the IC 1396A cloud towards the primary ionizing star HD 206267 is found. The current project consists of two Chandra-ACIS X-ray observations of IC 1396A, a Guaranteed Time observation (ObsID No. 11807 obtained on 2010 March 31; PI: Garmire) and a Guest Observer observation (ObsID No. 10990 obtained on 2010 June 9; PI: Getman). Both observations were pointed at the head of the globule but had different roll angles. For each observation, the authors considered only results arising from the imaging array (ACIS-I) of four abutted 1024 x 1024 pixel front-side illuminated charge-coupled devices (CCDs) covering about 17 x 17 arcmin<sup>2</sup> on the sky, Similar to the Chandra catalog of X-ray sources in the Carina Nebula (Broos et al. 2011, ApJS, 194, 2), this list of candidate sources in IC 1396A is trimmed to omit sources with fewer than 3 total source counts (the sum of the net counts and the background counts, NC + BC < 3) and the probability for being a background fluctuation greater than 1% (prob_no_src > 0.01). The final catalog comprises 415 X-ray sources, roughly half of which sources are extragalactic with extremely optically faint counterparts (Section 3.2 of the reference paper), and the rest are young stars associated with the Trumpler 37 and IC 1396A star-forming regions. UVR<sub>c</sub> I<sub>c</sub> observations were carried out with the 1.2-m telescope at the Fred Lawrence Whipple Observatory (FLWO), using the 4Shooter CCD array, between 2000 September and 2002 September. 4Shooter is an array of four CCDs, covering a square of 25 arcminutes on the side. Two 4Shooter fields were taken to cover an ~45 x 25 arcmin<sup>2</sup> area centered on the star HD 206267. The FLWO fields contain the whole ACIS field, except for a small gap in between the four CCDs of 4Shooter. All but a few Chandra stars were observed in 2000 September. UVR<sub>J</sub> I<sub>J</sub> observations of Trumpler 37/IC 1396A were obtained in service mode during three nights in 2007 June 9-11 using the wide-field camera, LAICA, mounted on the 3.5-m telescope in Calar Alto, Spain. LAICA is a 2 x 2 mosaic of four CCDs, each covering a 15.3 x 15.3 arcmin<sup>2</sup> field of view (FOV) with a large gap of 15.3 x 15.3 arcmin<sup>2</sup> in between. The project combines four LAICA pointings covering an ~45 x 45 arcmin<sup>2</sup> area around HD 206267, including nearly the entire ACIS field. The Spitzer observation was obtained on 2003 December 20 with the IRAC detector in all four IRAC channels (3.6, 4.5, 5.8 and 8.0 micron). Two adjacent fields subtending ~37 x 42 arcmin<sup>2</sup> in channel pairs 3.6/5.8 micron and 4.5/8.0 micron were centered on Trumpler 37. To reduce unnecessary data processing the authors analyzed only a portion of the original data that encompassed the Chandra-ACIS field with a coverage of ~19 x 19 arcmin<sup>2</sup> area in all four channels centered on Rim A of the IC 1396A globule. This covers 93% of the ACIS field omitting its north-western and south-western edges. An automated cross-correlation between the Chandra source positions and the optical-IR source positions was made using a search radius of 2 arcseconds within ~6 arcminutes of the ACIS field center, and a search radius of 3.5 arcseconds in the outer regions of the ACIS field where the X-ray source positions are more uncertain due to the deterioration of the Chandra telescope PSF. This was followed by a careful visual examination of each source in both bands to remove dubious sources and associations. This table was created by the HEASARC in April 2017 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/426/2917">CDS Catalog J/MNRAS/426/2917</a> files table1.dat, table2.dat, and table3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ic10cxo
- Title:
- IC 10 Chandra X-ray Point Source Catalog
- Short Name:
- IC10CXO
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The authors monitored the Cassiopeia dwarf galaxy (IC 10) in a series of 10 Chandra ACIS-S observations to capture its variable and transient X-ray source population, which is expected to be dominated by High Mass X-ray Binaries (HMXBs). They present a sample of 21 X-ray sources that are variable between observations at the 3-sigma level, from a catalog of 110 unique point sources (the HEASARC notes that there are actually 111 sources in the CDS version of the catalog from which this HEASARC table originates). The authors find four transients (flux variability ratio greater than 10) and a further eight objects with ratios >5. The observations span the years 2003-2010 and reach a limiting luminosity of >10<sup>35</sup> erg/s, providing sensitivity to X-ray binaries in IC 10 as well as flare stars in the foreground Milky Way. The nature of the variable sources is investigated from light curves, X-ray spectra, energy quantiles, and optical counterparts. The purpose of this study is to discover the composition of the X-ray binary population in a young starburst environment. IC 10 provides a sharp contrast in stellar population age (<10 million years) when compared to the Magellanic Clouds (40-200 Myr) where most of the known HMXBs reside. The authors find 10 strong HMXB candidates, 2 probable background active galactic nuclei, 4 foreground flare-stars or active binaries, and 5 not yet classifiable sources. Complete classification of the sample requires optical spectroscopy for radial velocity analysis and deeper X-ray observations to obtain higher S/N spectra and search for pulsations. A catalog (contained in this HEASARC table) has been created and supporting data sets (the data used to create the light curves shown in Figures 3, 4 and 5 in the reference paper) are available at <a href="http://cdsarc.u-strasbg.fr/ftp/cats/J/ApJ/836/50/">http://cdsarc.u-strasbg.fr/ftp/cats/J/ApJ/836/50/</a>. A monitoring series of 7x15 ks Chandra/ACIS observations, spaced at roughly six-week intervals was obtained during 2009-2010. A pair of very deep ACIS-S3 observations (2x45ks) made in 2006 November provided a reference data set for improved source positions and spectral information. The original Wang+ (2005, MNRAS, 362, 1065) Chandra (ACIS-S3) observation of 30 ks made in 2003 was also included in this analysis. The complete listing of 10 Chandra observation identifiers (ObsIDs) comprising the data set is summarized in Table 1 of the reference paper, also shown here: <pre> MJD |Date |ObsID|Flag|Exp.|RA(J2000)Dec(J2000)|Roll|Num. Sources ks hh mm ss dd mm ss deg. 52710.7|2003 Mar 12 |03953|a |28.9|00 20 25 +59 16 55|339.27|31 54041.8|2006 Nov 2 |07082| |40.1|00 20 04 +59 16 45|223.70|48 54044.2|2006 Nov 5 |08458| |40.5|00 20 04 +59 16 45|223.70|41 55140.7|2009 Nov 5 |11080| |14.6|00 20 17 +59 17 56|226.53|19 55190.2|2009 Dec 25 |11081| | 8.1|00 20 19 +59 18 02|286.15|24 55238.5|2010 Feb 11 |11082| |14.7|00 20 23 +59 17 10|320.56|24 55290.6|2010 Apr 4 |11083| |14.7|00 20 34 +59 19 01| 10.32|25 55337.8|2010 May 21 |11084| |14.2|00 20 25 +59 20 16| 67.89|27 55397.5|2010 Jul 20 |11085| |14.5|00 20 11 +59 19 13|121.25|22 55444.6|2010 Sep 5 |11086| |14.7|00 20 15 +59 18 11|157.71|27 |2006 Nov 2-5 |57082|b |80.6|00 20 04 +59 16 45|223.70|63 </pre> Flag values as follows: <pre> a = ObsID 03953 used about half of the CCD area in subarray mode. b = Merged 2006 data set referred to as ObsID 57082 consists of the nearly contiguous ObsIDs 07082 and 08458, which had identical pointings. </pre> Roll is the spacecraft roll angle, and Num. Sources is the number of unique point sources detected in each observation after combining wavdetect lists from the soft (S: 0.3-1.5 keV), broad (B: 0.3-8 keV) and hard (H: 2.5-8 keV) energy bands. This table was created by the HEASARC in November 2017 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/836/50">CDS Catalog J/ApJ/836/50</a> file table2.dat. This is a service provided by NASA HEASARC .
