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Henry Draper Extension Charts Catalog
The Henry Draper (HD) Catalog (Cannon and Pickering 1918 - 1924, Ann. Astron. Obs. Harvard College 91 - 99) and its first extension, the Henry Draper Extension (HDE) Catalog (Cannon 1934, Ann. Astron. Obs. Harvard College 100, 1 - 6), provided spectral classification and rough positions for 272,150 stars and has been widely made use of by the astronomical community for over half a century. A second extension of the HD Catalog, the so-called Henry Draper Extension Charts (HDEC), subsequently extended this spectral classification to fainter magnitudes (Cannon 1937, Ann. Astron. Obs. Harvard College 105, 1; Cannon and Mayall 1949, Ann. Astron. Obs. Harvard College 112), thus adding nearly another 87,000 stars with derived spectral types. The information in the HDEC was published in the form of charts rather than tables like the HD and HDE Catalogs, and consequently has been barely utiized by modern astronomers. In the 1990's, after a pilot project of Roeser et al. (1991, Astr. Ap. Suppl., 88, 277) had demonstrated that it seemed feasible to `revive' the HDEC data, they were converted into a catalog of accurate astrometric parameters along with magnitudes and spectral types by Nesterov et al. (1995, Astr. Ap. Suppl., 110, 367), who used measurements of Cartesian coordinates of stars in the charts and the positions in the Astrographic Catalog (AC) for subsequent cross-identification. The Nesterov et al. (1991) reference should be consulted for the full details on the procedures used to create this HDEC catalog. The HDEC catalog contains information on 86,933 stars, comprising accurate (0.5 arcseconds error) positions, (for more than 96 per cent of them) proper motions with a typical accuracy of 5.5 milliarcseconds (mas) per year, and the original spectral classifications. The current database contains the main portion of the catalog. An additional set of information, primarily comprising HD entries with cross-identifications with known or suspected variable stars, was included in the A.J. Cannon Memorial Volume (Cannon and Mayall 1949). This list was extended by Nesterov et al. (1991) to more than 500 identifications with variable stars. This latter expanded list, together with a list of entries which have uncertain identifications, is not included in the HEASARC version of this catalog, but it is available on the HEASARC website in the directory <a href="/FTP/heasarc/dbase/misc_files/hdec/">/FTP/heasarc/dbase/misc_files/hdec/</a> as the file <a href="/FTP/heasarc/dbase/misc_files/hdec/hdec.remarks">hdec.remarks</a>. If the parameter "remarks" is set to "R" for an entry in the HDEC catalog, this means that there is a remark about that particular star in the above file. This database was created by the HEASARC in April 1998 based on the machine-readable ADC/<a href="https://cdsarc.cds.unistra.fr/ftp/cats/III/182">CDS Catalog III/182</a>. This is a service provided by NASA HEASARC .
TIC (TESS Input Catalog ConeSearch)
The TESS Input Catalog is a comprehensive collection of 1.73 billion sources on the sky, providing stellar parameters for evaluation of potential planetary transit signals. It combines sources from many other catalogs, including 2MASS, LAMOST, SuperBlink, HSOY, RAVE, APOGEE, UCAC, KIC, EPIC, Tycho-2, APASS, AllWISE, SDSS, Gaia DR2, and Hipparcos. It was constructed for the TESS mission to serve as a source for selecting targets to observe with the TESS two-minute cadence, and to provide stellar parameter information for evaluating the properties of transit candidates.MAST catalog holdings are available via Cone Search endpoints. All available missions are listed at http://archive.stsci.edu/vo/mast_services.html.This service provides access to the TESS input catalog (TIC), currently version 8.2
Pan-STARRS DR1 "Best" Catalog ConeSearch
Pan-STARRS is a system for wide-field astronomical imaging developed and operated by the Institute for Astronomy at the University of Hawaii. Pan-STARRS1 (PS1) is the first part of Pan-STARRS to be completed and is the basis for Data Release 1 (DR1). The PS1 survey used a 1.8 meter telescope and its 1.4 Gigapixel camera (GPC1; see PS1 GPC1 camera) to image the sky in five broadband filters (g, r, i, z, y). The PS1 Science Consortium funded the operation of the Pan-STARRS1 telescope, situated at Haleakala Observatories near the summit of Haleakala in Hawaii, for the purposes of astronomical research. The PS1 consortium is made up of astronomers and engineers from 14 institutions from six countries.The Pan-STARRS Data Release 1 Object Catalog "Best" filtered exists in the MAST holdings and is thus available through a cone search. The filtered data is a ~2billion row subset based on an object having more than 2 detections.All available catalogs are listed at http://archive.stsci.edu/vo/mast_services.html.
M 108 Chandra X-Ray Compact Source Catalog
This table contains a list of discrete sources found in a 60-ks Chandra ACIS-S observation of the isolated edge-on spiral galaxy NGC 3556 (M108). In the reference paper in which the authors present this table, they also give a multiwavelength analysis of the various discrete X-ray sources and of the diffuse X-ray features. Among 33 discrete X-ray sources detected within the I<sub>B</sub> = 25 mag arcsec<sup>-2</sup> isophotal ellipse of the galaxy, the authors identify a candidate for the galactic nucleus, an ultraluminous X-ray source that might be an accreting intermediate-mass black hole, a possible X-ray binary with a radio counterpart, and two radio-bright giant H II regions. They also detect large amounts of extraplanar diffuse X-ray emission, which extend about 10 kpc radially in the disk and >~4 kpc away from the galactic plane. The diffuse X-ray emission exhibits significant substructures, possibly representing various blown-out superbubbles or chimneys of hot gas heated in massive star-forming regions. This Chandra observation of NGC 3556 (observation ID 2025) was taken between 2001 September 8 and 9 for an exposure of 60 ks. The ACIS-S instrument was at the focal plane of the telescope. This table was created by the HEASARC in August 2015 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/598/969">CDS Catalog J/ApJ/598/969</a> file table2.dat. This is a service provided by NASA HEASARC .
UVOT Bright Star Catalog
This catalog was compiled from 4 catalogs: Tycho-2, GVCS III, NGC, and the Yale Bright Star Catalog. All catalogs were preprocessed before compiling this catalog to achieve uniform columns and units. Next, they were merged into one catalogue before eliminating "red" objects and precessing all coordinates to epoch 2000.0. The catalog was then corrected for missing decimal points. Finally, the catalog was sorted by R.A. for ease of locating objects within the catalogue. The original catalog contained 239,853 objects brighter than 12.0 mags. This table was originally created by the HEASARC in July 2008 based on an input table supplied by the Swift Project which was compiled by Elizabeth Auden at MSSL. It was renamed to UVOTBSCAT in January 2009. This is a service provided by NASA HEASARC .
Giant Metrewave Radio Telescope Field I 150-MHz Radio Source Catalog
Foreground removal is a major challenge for detecting the redshifted 21-cm neutral hydrogen (HI) signal from the Epoch of Reionization. The authors have used 150-MHz Giant Metrewave Radio Telescope (GMRT) observations to characterize the statistical properties of the foregrounds in four different fields of view. The observational data were used to assess point source subtraction. Considering the brightest source (~1 Jy) in each field, the authors find that the residual artefacts are less than 1.5% in the most sensitive field (FIELD I). Considering all the sources in the fields, they find that the bulk of the image is free of artefacts, the artefacts being localized to the vicinity of the brightest sources. The authors have used FIELD I, which has an rms noise of 1.3 mJy beam<sup>-1</sup>, to study the properties of the radio source population to a limiting flux of 9 mJy. The differential source count is well fitted with a single power law of slope -1.6. They find there is no evidence for flattening of the source counts towards lower flux densities which suggests that source population is dominated by the classical radio-loud active galactic nuclei. The authors have observed FIELD I in GMRT Time Allocation Committee (GTAC) cycle 15 in 2008 January, whereas FIELD II and FIELD III were observed in cycle 17 during 2010 February. These target fields were selected at high Galactic latitudes (b > 10<sup>o</sup>) which were up at night time during the GTAC cycles 15 and 17, and which contain relatively few bright sources (>= 0.3 Jy) in the 1400 MHz NRAO VLA Sky Survey (NVSS). Finally, FIELD IV was observed in cycle 8 (2005 June). Full details of these 4 observations are given in Table 1 of the reference paper. This table contains the 150-MHz source catalog for the most sensitive observation, namely the 9.8-hour observation of Field I (centered on J2000.0 RA and Dec of 5<sup>h</sup> 30<sup>m</sup> 00<sup>s</sup>, +60<sup>o</sup> 00' 00"), which was made on 2008 January 8. This table was created by the HEASARC in September 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/426/3295">CDS Catalog J/MNRAS/426/3295</a> file tablea1.dat This is a service provided by NASA HEASARC .
Carina OB1 Association XMM-Newton X-Ray Point Source Catalog
This database table contains the Carina OB1 Association XMM-Newton X-Ray Point Source Catalog. The X-ray properties of the stellar population in the Carina OB1 Association have been examined with special emphasis on early-type stars. Their spectral characteristics provide some clues to understanding the nature of X-ray formation mechanisms in the winds of single and binary early-type stars. A timing and spectral analysis of five observations with XMM-Newton is performed using various statistical tests and thermal spectral models. 235 point sources have been detected within the field of view. Several of these sources are probably pre-main sequence stars with characteristic short-term variability. Seven sources are possible background AGNs. X-ray count rates in three energy bands and the X-ray variability status are given for 557 detections of the 235 point source. Cross-identifications of X-ray sources with optical and infrared catalogs are also presented. This table was created by the HEASARC in April 2008 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/477/593">CDS Catalog J/A+A/477/593</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
Spitzer Deep Wide-Field Survey 8 micron Epoch 2 Catalog
The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of 10 square degrees in the Boötes field of the NOAO Deep Wide-Field Survey using the IRAC instrument on the Spitzer Space Telescope. SDWFS, a Spitzer Cycle 4 Legacy project, occupies a unique position in the area-depth survey space defined by other Spitzer surveys. The four epochs that make up SDWFS permit - for the first time - the selection of infrared-variable and high proper motion objects over a wide field on timescales of years. Because of its large survey volume, SDWFS is sensitive to galaxies out to z ~ 3 with relatively little impact from cosmic variance for all but the richest systems. The SDWFS data sets will thus be especially useful for characterizing galaxy evolution beyond z ~ 1.5.The delivery consists of four band-matched catalogs for each of the four epochs and for the total SDWFS coadd data, a total of 20 catalogs. Vega magnitudes are reported for each IRAC band: 3.6, 4.5, 5.8, and 8 microns. Each source was measured three ways: 4 arcsec diameter aperture, 6 arcsec diameter aperture, and Kron radius aperture (MAG_AUTO in SExtractor). Source coordinates correspond to 2MASS catalog positions to within 0.2 arcsec. The tabulated uncertainties are twice the SExtractor (statistical only) uncertainties as an attempt to account for systematic uncertainties.
HEAO 1 A3 MC LASS Catalog
This database table contains information from the HEAO 1 A3 MC LASS Catalog of X-ray Sources. The MC experiment contained two four-grid modulation collimators with an egg-crate collimator with an overall FOV of 4 x 4 degrees (FWHM). The objects in the catalog are possible HEAO 1 A1 sources. The HEAO 1 experiment began on day 224, 19 August 1977 and ended on day 739, 9 January 1979. This is a service provided by NASA HEASARC .
9C 15-GHz Ryle Telescope Survey of VSA Fields Source Catalog
The fields chosen for the first observations of the cosmic microwave background (CMB) with the Very Small Array (VSA) have been surveyed with the Ryle Telescope at 15 GHz. The authors have covered three regions around RA = 00<sup>h</sup>20<sup>m</sup> and Dec = +30<sup>o</sup>, RA = 09<sup>h</sup>40m and Dec = +32<sup>o</sup> and RA = 15<sup>h</sup>40<sup>m</sup> and Dec = +43<sup>o</sup> (J2000.0), comprising an area of 520 deg<sup>2</sup>. There are 465 sources in this entire area which are above the estimated completeness limit of ~ 25 mJy, although a total of ~ 760 sources were detected, some as faint as 10 mJy. The prime motivation of this study was to define a catalog of the foreground sources that must be monitored by the VSA during its observations at 34 GHz. In particular, it provides a means of identifying GigaHertz peaked spectrum (GPS) sources, which are important for the study of radio source evolution, as well as being a significant foreground for CMB observations over a range of wavelengths. Since this will be a new and quite extensive survey, it was desgignated as '9C' or the Ninth Cambridge survey. For the purpose of this particular component of the 9C survey, the authors designated as a subset, 3 circular areas, VSA1, VSA2 and VSA3, defined by the properties listed in Table 2 of the reference paper and reproduced below: <pre> Field Centre J2000.0 Center B1950.0 Radius Area RA Dec RA Dec (degrees) (sq. degrees) VSA1 00 17 36.5 +30 16 39 00 15 00.0 +30 00 00 5.5 95.0 VSA2 09 40 57.7 +31 46 21 09 38 00.0 +32 00 00 6.0 113.0 VSA3 15 36 42.7 +43 20 11 15 35 00.0 +43 30 00 5.0 78.5 </pre> There are 242 sources which were both above the 25 mJy completeness limit and were in the 286.5 deg<sup>2</sup> contained within these 3 circular fields. These source were listed in 3 tables in the reference paper, Table 4 (VSA1), Table 5 (VSA2) and Table 6 (VSA3). These have been combined into this one HEASARC table, in which the HEASARC added a new parameter vsa_field, which is set to 1 for the VSA1 sources, 2 for the VSA2 sources, and 3 for the VSA3 sources. This table was created in November 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/342/915">CDS catalog J/MNRAS/342/915</a> files table4.dat, table5.dat and table6.dat. This is a service provided by NASA HEASARC .
M 31 Revised Bologna Clusters and Candidates Catalog (Version 5)
The Revised Bologna Catalogue of M 31 globular clusters and candidates (RBC, V.5, August 2012) lists all the confirmed globular clusters (GCs), all the known candidates GCs, and also all the objects that were identified as candidate GCs in the past and were subsequently recognized not to be genuine clusters, each entry being properly classified (GC, candidate GC, foreground star, background galaxy, HII region, etc.). The latter entries are maintained in the catalog to avoid re-discoveries of objects that may look like M 31 GCs and have been already classified as non-GCs. Please take into account the classification flag(s) when you use the RBC. Please acknowledge the use of this catalog. The proper reference is: Galleti S., Federici L., Bellazzini M., Fusi Pecci F., Macrina S. "2MASS NIR photometry for 693 candidate globular clusters in M 31 and the Revised Bologna Catalogue (V.1.0)", Astron.&Astrophys., 2004, 416, 917 (2004A&A...416..917G) This table was created by the HEASARC in November 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/V/143">CDS Catalog V/143</a> file rbc5.dat, Version 5 of the Revised Bologna Catalogue of M 31 globular clusters and candidates. This is a service provided by NASA HEASARC .
SACY (Search for Associations Containing Young Stars) Catalog
The SACY (Search for Associations Containing Young Stars) Catalog contains the results from a high-resolution optical spectroscopic survey aimed to search for nearby young associations and young stars among optical counterparts of ROSAT All-Sky Survey X-ray sources in the Southern Hemisphere. 1953 late-type (B-V>=0.6), potentially young, optical counterparts were selected out of a total of 9574 1RXS sources for follow-up observations. At least one high-resolution spectrum was obtained for each of 1511 targets. This paper is the first in a series presenting the results of the SACY survey in which the sample of X-ray selected stars and the supporting optical observations are described. The SACY sample is defined by Hipparcos (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/239">CDS Cat. <I/239></a>) and Tycho-2 (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/259">CDS Cat. <I/259></a>) stars within an error radius of 2.6 times the positional error of the ROSAT All-Sky Bright Source Catalogue (1RXS, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/IX/10">CDS Cat. <IX/10></a>). The used cut-off (B-V=0.6), corresponding approximately to a G0 dwarf, is near the hottest stars where the strength of the LiI line can be used as an youth indicator. All Hipparcos stars having M_v < 2.0 have been excluded. The northern boundary limits of the survey are given in Table 1 of the reference paper. In addition to the 1511 stars observed at least once, 115 stars with data taken from the literature have been added in order to complement the sample. In addition to these 1626 stars in the SACY sample (sources with source number prefixes of 'S'), entries for 165 other observed stars (sources with source number prefixes of 'O') are also included in this table. Most of the spectroscopic observations (~70%) were performed with the FEROS spectrograph at the 1.5m/ESO telescope at La Silla between January 1999 and September 2002 (ON-ESO agreement and ESO program identification 67.C-0123). Two more runs (ESO program identifications 072.C-0393 and 077.C-0138) were carried out at the 2.2m/ESO telescope. Another set of data (~30%) was collected at the coude spectrograph attached to 1.60m telescope at the Observatorio rio do Pico dos Dias (OPD), LNA, Brazil. Some spectra are a re-analysis of the ones taken for the PDS program. A few observations were collected using the CORALIE attached to the Swiss Euler Telescope at La Silla. UBV(RI)c photometry for part of the sample was obtained using FOTRAP at the 0.60m Zeiss telescope of the OPD. When a star was not observed photometrically by the authors, they tried to obtain some useful photometric data from the Hipparcos and Tycho Catalogues or in the available literature in the SIMBAD. For multiple stars, magnitudes and colors were corrected in order to take into account the presence of the companion(s). This table was created by the HEASARC in March 2007 based on the CDS table J/A+A/460/695, files table3.dat and table4.dat This is a service provided by NASA HEASARC .
Lynga Open Clusters Catalog
This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances. This is a service provided by NASA HEASARC .
DeepDrill SHARK Simulated Lightcone Catalog
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).The SHARK simulated lightcone was built from the SHARK semi-analytic model of galaxy formation and evolution (Lagos et al. 2018, 2019) to compare with the DeepDrill survey. This lightcone has an area of 107.9 deg^2, and a flux selection at the [3.6] band > 0.575 uJy (equivalent to an AB magnitude of 24.5), with the same redshift range of 0 < z < 6.Note: as a catalog of simulated data, spatial queries are not expected to be very useful, and thus ra and dec have not been indexed. Consequently, positional searches will be very slow.
eHOPS Aquila SED Fits Catalog
The Extension of HOPS Out to 500 ParSecs (eHOPS) project used archival data to survey all the major star forming molecular clouds within 500 pc of the Sun, except Orion (which was surveyed by HOPS). The first eHOPS data release covers the Aquila molecular clouds (d ~ 436 pc). For every source detected in the Herschel/PACS bands, the eHOPS-Aquila catalog contains 1-850 micron SEDs assembled from 2MASS, Spitzer, Herschel, WISE, and JCMT/SCUBA-2 data. A total of 172 protostars are found in Aquila, tightly concentrated in the molecular filaments that thread the clouds. Of these, 72 (42%) are Class 0 protostars, 53 (31%) Class I protostars, 43 (25%) are flat-spectrum protostars, and 4 (2%) are Class II sources. Ten of the Class 0 protostars are young PACS Bright Red Sources similar to those discovered in Orion. eHOPS compares the SEDs to a grid of radiative transfer models to constrain the luminosities, envelope densities, and envelope masses of the protostars.
NGC 6357/Pismis 24 Chandra Point Source Optical/IR Identifications Catalog
Circumstellar disks are expected to evolve quickly in massive young clusters harboring many OB-type stars. Two processes have been proposed to drive the disk evolution in such cruel environments: (1) gravitational interaction between circumstellar disks and nearby passing stars (stellar encounters), and (2) photoevaporation by UV photons from massive stars. The relative importance of both mechanisms is not well understood. Studies of massive young star clusters can provide observational constraints on the processes of driving disk evolution. The authors investigate the properties of young stars and their disks in the NGC 6357 complex, concentrating on the most massive star cluster within the complex: Pismis 24. They use infrared data from the 2MASS and Spitzer GLIMPSE surveys, complemented with their own deep Spitzer imaging of the central regions of Pismis 24, in combination with X-ray data to search for young stellar objects (YSOs) in the NGC 6357 complex. The infrared data constrain the disk presence and are complemented by optical photometric and spectroscopic observations, obtained with VLT/VIMOS, that constrain the properties of the central stars. For those stars with reliable spectral types, they combine spectra and photometry to estimate the masses and ages. For cluster members without reliable spectral types, they obtain the mass and age probability distributions from R and I-band photometry, assuming these stars have the same extinction distribution as those in the "spectroscopic" sample. The authors compare the disk properties in the Pismis 24 cluster with those in other clusters/star-forming regions employing infrared color-color diagrams. The authors discover two new young clusters in the NGC 6357 complex. They give a revised distance estimate for Pismis 24 of 1.7 +/- 0.2 kpc. They also find that the massive star Pis 24-18 is a binary system, with the secondary being the main X-ray source of the pair. The authors provide photometry in 9 bands between 0.55 and 8 micron (µm) for the members of the Pismis 24 cluster. They derive the cluster mass function and find that up to the completeness limit at low masses it agrees well with the initial mass function of the Trapezium cluster. They derive a median age of 1 Myr for the Pismis 24 cluster members. The R-band observations were performed on 2008 April 1 and 6, and the I-band observations were done on 2008 May 1, both using the VIMOS instrument on the VLT. The near-IR photometry in the J, H and K<sub>s</sub> bands were taken from the 2MASS. The mid-IR photometry at 3.6, 4.5, 5.8 and 8.0 um were obtained withe the Spitzer IRAC camera, both from the GLIMPSE I survey and from deep observations of the central Pismis 24 region carried out by the authors on 2006 September 29. The X-ray observations were made by the Chandra ACIS-I instrument and previously published by Wang et al. (2007, ApJS, 168, 100: the HEASARC NGC6357CXO table). The X-ray sources were matched to sources detected in the VIMOS R and I bands based on positional coincidence, using a 1.5 arcseconds tolerance. The accuracy of the optical and X-ray positions was 0.6 and 1.0 arcseconds, respectively. Given the high space density of sources in the central regions of Pismis 24, there may be a substantial number (up to 1/6 of the sources) of "false positives", according to the authors. This table contains the list of 643 optical/IR counterparts to the Chandra X-ray sources found by Wang et al. (2007) which were identified by the present authors: for 136 of the 779 X-ray sources, no counterparts were found. This table was created by the HEASARC in March 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/539/A119">CDS Catalog J/A+A/539/A119</a> files table1.dat and table3.dat. This is a service provided by NASA HEASARC .
Fornax A (NGC 1316) Chandra X-Ray Source Catalog
This table contains some of the results from a Chandra ACIS sub-arcsecond resolution X-ray observation of the archetypal merger radio galaxy NGC 1316 (Fornax A). The authors detect 81 point sources within the 25th magnitude isophotal ellipse D<sub>25</sub> of NGC 1316 (L<sub>X</sub> in the range of 2 x 10<sup>37</sup> to 8 x 10<sup>39</sup> ergs s<sup>-1</sup>), with hard (kT ~ 5 keV) X-ray spectra, typical of X-ray binaries, and a spatial radial distribution consistent with that of the optical (i.e., stellar) surface brightness. In the reference paper, they derive the X-ray luminosity function (XLF) of these sources, correcting for the incompleteness at the faint end caused by the presence of the diffuse emission from the hot ISM in the central regions of NGC 1316 and by the widening of the Chandra point-spread functions at increasing distance from the aim point. With these corrections, the XLF is well reproduced by a single unbroken power law with a slope of -1.3 down to their threshold luminosity of ~ 3 x 10<sup>37</sup> ergs s<sup>-1</sup>. NGC 1316 was observed for 30 ks on 2001 April 17 (ObsID 2022), with the Chandra Advanced CCD Imaging Spectrometer (ACIS). The authors used the back-illuminated (BI) CCD S3 (CCD ID 7) because of its sensitivity at low energies. To include NGC 1317 (6.3 arcminutes away from NGC 1316) in the same S3 chip, a small offset was applied to the SIM (Science Instrument Module) position. NGC 1316 was kept close to on-axis to achieve the best spatial resolution. To detect X-ray sources, the authors used WAVDETECT, a wavelet detection algorithm available in CIAO. They set the WAVDETECT significance threshold parameter to be 10<sup>-6</sup>, which corresponds to 1 possibly spurious source, and the scale parameter to cover seven steps between 1 and 64 pixels. This made them sensitive to sources ranging from point-like to 32 arcseconds in size, and in particular accommodates the variation of the point-spread function (PSF) as a function of the off-axis angle of the sources. To extract source properties (such as count rates, spectra, etc.), the authors used the 95% encircled energy (at 1.5 keV) radius centered at the WAVDETECT centroid, with a minimum of 3 arcseconds to accommodate the radial variation of he PSF. Background counts were determined locally for each source from an annulus from 2 to 5 times the source radius, after excluding nearby sources. Extended sources were found at the locations of NGC 1316 and NGC 1317. In addition, the Chandra observations reveal 94 sources (the HEASARC notes that 95 are contained in this table), 83 of them in CCD S3. Of these, 81 sources (77 in S3 and 4 in S2) are within the D<sub>25</sub> ellipse. The source density increases toward the center of NGC 1316, indicating that most of them are related to NGC 1316. Three sources are found within the D<sub>25</sub> ellipse of NGC 1317, with the brightest, extended one at the center of NGC 1317. The list of detected sources also includes sources found on CCDs other than S3 (CCD number 7). After correcting for effective exposure and vignetting, the X-ray flux in the 0.3 - 8.0 keV band is calculated with an energy conversion factor (ECF) assuming a power-law source spectrum with a slope of 1.7 and N<sub>H</sub> = 3 x 10<sup>20</sup> cm<sup>-2</sup>; ECF = 6.037 x 10<sup>-12</sup> erg cm<sup>-2</sup> s<sup>-1</sup> ergs per 1 count s<sup>-1</sup> for the back-illuminated (BI) chips and 9.767 x 10<sup>-12</sup> ergs per 1 count s<sup>-1</sup> for the front-illuminated (FI) CCD chips. With the adopted distance of 18.6 Mpc, the X-ray luminosities of the point sources range from ~ 2 x 10<sup>37</sup> to ~ 8 x 10<sup>39</sup> erg s<sup>-1</sup>. This table was created by the HEASARC in July 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/586/826">CDS Catalog J/ApJ/586/826</a> file table1.dat. This is a service provided by NASA HEASARC .
BeppoSAX/GRBM Gamma-Ray Burst Catalog
This is the catalog of gamma-ray bursts (GRBs) detected with the Gamma Ray Burst Monitor (GRBM) aboard the BeppoSAX satellite. It includes 1082 GRBs with 40 - 700 keV fluences in the range from 1.3 x 10<sup>-7</sup> to 4.5 x 10<sup>-4</sup> erg/cm<sup>2</sup>, and 40 - 700 keV peak fluxes from 3.7x10<sup>-8</sup> to 7.0 x 10<sup>-5</sup> erg/cm<sup>2</sup>/s. Some relevant parameters of each GRB are reported in the catalog. This table was created by the HEASARC in January 2010 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/180/192">CDS catalog J/ApJS/180/192</a>, file table2.dat. This is a service provided by NASA HEASARC .
Spitzer Extragalactic First Look Survey SDSS Spectroscopic Catalog
The Extragalactic First Look Survey is composed of 4 square degrees of imaging with MIPS and IRAC centered at J1718+5930, with extensive ancillary data from ground-based optical and radio telescopes. As one of the first observations made with Spitzer after the completion of Science Verification at the end of 2003 November, the aim of this 67 hr survey was to characterize the extragalactic source populations observed with Spitzer down to sub-millijansky levels in the mid-infrared. This catalog presents the SDSS spectroscopic information from Papovich et al. (2006).
VLA-COSMOS 3-GHz Large Project Source Catalog
This table contains some of the results from the VLA-COSMOS 3-GHz Large Project based on 384 hours of observations with the Karl G. Jansky Very Large Array (VLA) at 3 GHz (10 cm) toward the 2 square degree Cosmic Evolution Survey (COSMOS) field. The final mosaic reaches a median rms of 2.3 µJy (µJy) beam<sup>-1</sup> over the 2 square degrees at an angular resolution of 0.75 arcseconds. To fully account for the spectral shape and resolution variations across the broad (2-GHz) band, the authors imaged all the data with a multiscale, multifrequency synthesis algorithm. In this table, the catalog of 10,830 radio sources down to 5 sigma is presented, out of which 67 are combined from multiple components. Comparing the positions of these 3-GHz sources with those from the Very Long Baseline Array (VLBA)-COSMOS survey, the authors estimate that the astrometry is accurate to 0.01 arcseconds at the bright end (signal-to-noise ratio, S/N<sub>3GHz</sub> > 20). Survival analysis on these data combined with the VLA-COSMOS 1.4-GHz Joint Project catalog yields an expected median radio spectral index alpha = -0.7. The authors compute completeness corrections via Monte Carlo simulations to derive the corrected 3-GHz source counts. Their counts are in agreement with previously derived 3-GHz counts based on single-pointing (0.087 square degrees) VLA data. In summary, the VLA-COSMOS 3-GHz Large Project simultaneously provides the largest and deepest radio continuum survey at high (0.75") angular resolution to date, bridging the gap between last-generation and next-generation surveys. The catalog contains sources selected down to a 5-sigma (where sigma ~2.3 µJy/beam) threshold. This catalog can be used for statistical analyses, accompanied with the corrections given in the data & catalog release paper. All completeness and bias corrections and source counts presented in the paper were calculated using this sample. The total fraction of spurious sources in the COSMOS 2 sq.deg. field is below 2.7% within this catalog. However, an increase of spurious sources up to 24% at 5.0 < S/N < 5.5 is present (for details see Sec. 5.2., Fig. 17 and Table 3 of the reference paper). A subsample with a minimal spurious source fraction can be selected by requiring an additional cutoff S/N >= 5.5 for single component sources (MULTI=0). The total fraction of spurious sources in the COSMOS 2 sq.deg. field within such a selected sample is below 0.4%, and the fraction of spurious sources is below 3% even at the lowest S/N of 5.5. This table was created by the HEASARC in June 2017 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/602/A1">CDS Catalog J/A+A/602/A1</a> file table1.dat, the VLA-COSMOS 3-GHz radio source catalog. This is a service provided by NASA HEASARC .
ScienceDex guides
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.