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2,001 results for “x-rays”
Swift BAT 100-Month Supergiant Fast X-Ray Transient Catalog
Supergiant Fast X-ray Transients (SFXTs) are High Mass X-ray Binaries (HMXBs) that are defined by their hard X-ray flaring behavior. During such flares they reach peak luminosities of 10<sup>36</sup> - 10<sup>37</sup> erg/s for a few hours (in the hard X-ray), i.e., much shorter timescales than those characterizing Be/X-ray binaries. The authors have investigated the characteristics of bright flares (detections in excess of 5 sigma) for a sample of SFXTs and their relation to the orbital phase. They have retrieved all Swift/BAT Transient Monitor light curves, and collected all detections in excess of 5 sigma from both daily- and orbital-averaged light curves in the time range from 2005 February 12 to 2013 May 31 (MJD 53413 - 56443). The authors also considered all on-board detections as recorded in the same time span and selected those within 4 arcminutes of each source in their sample and in excess of 5 sigma. This table contains the catalog of over a thousand Burst Alert Telescope (BAT) flares from 11 SFXTs, down to 15-150 keV fluxes of ~6 x 10<sup>-10</sup>erg/cm<sup>2</sup>/s (daily timescale) and ~1.5 x 10<sup>-9</sup>erg/cm<sup>2</sup>/s (orbital timescale, averaging ~800s) and spanning 100 months. The great majority of these flares are unpublished. This population is characterized by short (a few hundred seconds) and relatively bright (in excess of 100 milliCrab, 15-50 keV) events. In the hard X-ray, these flares last in general much less than a day. Clustering of hard X-ray flares can be used to indirectly measure the length of an outburst, even when the low-level emission is not detected. In their paper, the authors construct the distributions of flares, of their significance (in terms of sigma) and their flux as a function of orbital phase, to infer the properties of these binary systems. In particular, they observe a trend of clustering of flares at some phases as P_orb increases, as consistent with a progression from tight, circular or mildly eccentric orbits at short periods, to wider and more eccentric orbits at longer orbital periods. Finally, the authors estimate the expected number of flares for a given source for their limiting flux and provide the recipe for calculating them for the limiting flux of future hard X-ray observatories. The BAT observes 88% of the sky daily, on average, so it is ideally suited to detect flaring in hard X-ray sources. Since 2005-02-12, the BAT Transient Monitor (Krimm et al. 2013, ApJS, 209, 14) has been providing near real-time light curves in the 15-50 keV energy range of more than 900 sources with a mean variance for one-day mosaics of 5.3 milliCrab. Several flares from SFXTs are regularly caught every year by the BAT Transient Monitor (BATTM). The catalog contains a total of 1117 flares from 11 SFXT sources (the only other confirmed SFXT, IGR J11215-5952, never triggered the BAT: see Section 2.2 of the reference paper for more information about this source). They are divided into 46 BAT triggers (bat_subsample_flag = 'T', 43 in outbursts), 126 daily-averaged BATTM light curves (bat_subsample_flag = 'D'), 267 orbital-averaged BATTM light curves (bat_subsample_flag = 'O'), and 678 on-board detections (bat_subsample_flag = 'B'). For each flare, the time of the occurrence, duration, flux, and significance are reported. Given the cut in sigma applied to the available BATTM and on-board detections, this catalog is a flux-limited sample of flares. Assuming a Crab-like spectrum (power-law of photon index 2.15), 5 sigma detections for one day and an average orbit typically correspond to fluxes of 5.98 x 10<sup>-10</sup> and 1.46 x 10<sup>-9</sup> erg cm<sup>-2</sup> s<sup>-1</sup>, respectively, in the 15-150 keV band (or 3.38 x 10<sup>-10</sup> and 8.24 x 10<sup>-10</sup> erg cm<sup>-2</sup> s<sup>-1</sup> in the 15-50 keV band). This table was created by the HEASARC in August 2015 based on the union of <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/562/A2">CDS Catalog J/A+A/562/A2</a> files sample.dat (the properties of the confirmed SFXTs) and table4.dat (the catalog of the 1117 flares detected by the Swift BAT from 11 of the 12 confirmed SFXTs). This is a service provided by NASA HEASARC .
X-Ray Selected High-z AGN Catalog
This table contains the results from an analysis of the largest high-redshift (z > 3) X-ray-selected active galactic nucleus (AGN) sample to date, combining the Chandra Cosmological Evolution Survey and Chandra Multi-wavelength Project surveys and doubling the previous samples. The sample comprises 209 X-ray-detected AGNs, over a wide range of rest-frame 2-10 keV luminosities log L<sub>X</sub> = 43.3 - 46.0 erg/s. X-ray hardness ratios show that ~39 per cent of the sources are highly obscured, N<sub>H</sub> > 10<sup>22</sup> cm<sup>-2</sup>, in agreement with the ~37 per cent of type-2 AGNs found in this sample based on their optical classification. For ~26 per cent of objects, there are mismatched optical and X-ray classifications. Utilizing the 1/V<sub>max</sub> method, the authors confirm that the comoving space density of all luminosity ranges of AGNs decreases with redshift above z > 3 and up to z ~ 7. With a significant sample of AGNs (N = 27) at z > 4, it is found that both source number counts in the 0.5-2 keV band and comoving space density are consistent with the expectation of a luminosity-dependent density evolution (LDDE) model at all redshifts, while they exclude the luminosity and density evolution (LADE) model. The measured comoving space density of type-1 and type-2 AGNs shows a constant ratio between the two types at z > 3. These results for both AGN types at these redshifts are consistent with the expectations of LDDE model. The high-redshift AGN sample used in this work has been selected from the C-COSMOS X-ray catalog, combining the spectroscopic and photometric information available from the identification catalogue of X-ray C-COSMOS sources (Civano et al. 2011, ApJ, 741, 91; 2012, ApJS, 201, 30) and the ChaMP (Chandra Multi-wavelength Project) X-ray catalog using only the 323 ChaMP ObsIDs overlapping with Sloan Digital Sky Survey (SDSS; Richards et al. 2006, AJ, 131, 2766) DR5 imaging. This table was created by the HEASARC in March 2016 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/445/1430">CDS catalog J/MNRAS/445/1430</a> file tablea1.dat. This is a service provided by NASA HEASARC .
ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al.)
This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl & Pietsch (1999, A&AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10<sup>36</sup> erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy. This database was created at the HEASARC in June 2000 based on the ADC/<a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+AS/142/41">CDS Catalog J/A+AS/142/41</a>, and is derived from Table 2 of the reference. This is a service provided by NASA HEASARC .
NGC 6231 XMM-Newton X-Ray Source Catalog
This table contains the results of an X-ray campaign towards the young open cluster NGC 6231. The XMM-Newton observations, of a total duration of ~ 180 ks, reveal that NGC 6231 is very rich in the X-ray domain too. Indeed, 610 X-ray sources were detected in the present field of view, centered on the colliding wind binary HD 152248 in the cluster core (RA, Dec J2000.0 of 16 54 10.06, -41 49 30.1). The limiting sensitivity of this survey is approximately 6 x 10^-15<sup>erg/s/cm</sup>2 but clearly depends on the location in the field of view and on the source spectrum. Using different existing catalogs, over 85% of the X-ray sources could be associated with at least one optical and/or infrared counterpart within a limited cross-correlation radius of 2.5 or 3-arcsec according to the optical/IR catalog used. The surface density distribution of the X-ray sources presents a slight N-S elongation. Once corrected for the spatial sensitivity variation of the EPIC instruments, the radial profile of the source surface density is well described by a King profile with a central density of about 8 sources per arcmin<sup>2</sup> and a core radius close to 3.1 arcminutes. The distribution of the X-ray sources seems closely related to the optical source distribution. The expected number of foreground and background sources should represent about 9% of the detected sources, thus strongly suggesting that most of the observed X-ray emitters are physically belonging to NGC 6231. Finally, beside a few bright but soft objects -- corresponding to the early-type stars of the cluster -- most of the sources are relatively faint (~5 x 10<sup>-15</sup> erg/s/cm<sup>2</sup>) with an energy distribution peaked around 1.0 - 2.0 keV. The catalog of the 610 X-ray sources detected in the 30'-diameter field of view of XMM-Newton is presented here, including the equatorial coordinates, logarithmic likelihoods and count rates for the three EPIC instruments and for various energy ranges, as well as the cross-identification of the X-ray sources with various optical/infrared catalogs (2MASS, GSC2.2, USNO B1.0, SSB06) and their most commonly used names (HD/HDE, CD, CPD, Segg., SBL98, Braes), with only the closest identifications being reported here. This table was created by the HEASARC in March 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/454/1047">CDS catalog J/A+A/454/1047</a> files table3.dat and table6.dat. This is a service provided by NASA HEASARC .
LMC X-Ray Discrete Sources
This database table contains 105 "discrete" (i.e., more compact than 1.25 arcminutes) and 9 "large-diameter" (detected using a detection circle radius of 2 arcminutes) Einstein IPC X-ray sources in the direction of the Large Magellanic Cloud (LMC) that are tabulated in Tables 2 and 4, respectively, of Wang et al. (1991, ApJ, 374, 475). For full details of the data processing and selection used to create this source catalog, the above reference should be consulted. This is a service provided by NASA HEASARC .
Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)
This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/455/1165/refs.dat">https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/455/1165/refs.dat</a> Individual notes on each HMXB are available at the URL <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/455/1165/notes.dat">https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/455/1165/notes.dat</a> This database was first created by the HEASARC in January 2001, based on the 2000 version of this catalog. It was updated to the 4th edition in September 2006, based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/455/1165">CDS catalog J/A+A/455/1165</a>. This is a service provided by NASA HEASARC .
M 101 XMM-Newton X-Ray Point Source Catalog
The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D<sub>25</sub> ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D<sub>25</sub> ellipse of M101. This table was created by the HEASARC in October 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/357/401">CDS Catalog J/MNRAS/357/401</a> files table1.dat and table2.dat. This is a service provided by NASA HEASARC .
Extremely Luminous X-Ray Source Candidates Catalog
Using Chandra archive data, the authors conducted a thorough survey of luminous X-ray sources. They directly analyzed about 9400 Chandra ACIS observations and cross-correlated the detected X-ray sources with 77,000 galaxies within a distance of 250 Mpc. The final catalog includes 119 unique luminous X-ray source candidates with L<sub>X</sub> > 3 x 10<sup>40</sup> erg/s from 93 galaxies or 41 HLX candidates with L<sub>X</sub> > 1 x 10<sup>41</sup> erg/s from 35 galaxies. The authors derive a moderate contamination rate due to foreground or background sources. In the reference paper, they also cross-correlate the catalog with FIRST, perform variability and periodicity tests, and analyze one HLX candidate in particular. This catalog could be a starting point to perform follow-up observations. In order to know whether an X-ray source falls within a particular galaxy, for each galaxy, the authors collected its center's RA, Dec, distance, and D<sub>25</sub> isophotal info, which includes major axis length, minor axis length, and the position angle of the major axis from the PGC2003 Catalog (Paturel et al. 2003, A&A, 412, 45), which includes the full RC3 catalog and has all of the necessary parameters except for distance. The authors restricted the minimum major axis length to be 10 arcseconds, and collected their distances from NED as much as possible. Their final sample includes 77,000 galaxies within 250 Mpc. The authors used all of the Chandra ACIS data in TE mode that were released before 2014, which includes 9400 ObsIDs. A roughly linear relation between the flux and count rate derived by PIMMS 4.6b was established assuming a power-law spectral shape and galactic foreground extinction (Kalberla et al. 2005, A&A, 440, 775). Any source with a PIMMS luminosity larger than 5 x 10<sup>39</sup> erg s<sup>-1</sup> would be recalculated by the CIAO script model flux assuming a power-law index of 1.7 in the 0.3 - 8.0 keV energy band. After the recalculation, 1,809 X-ray sources with L<sub>x</sub> > 3 x 10<sup>40</sup> erg s<sup>-1</sup> falling within 640 D<sub>25</sub> contours covered by 905 ObsIDs were picked out. A large fraction of the 1,809 sources are galactic nuclei and some of them are repeated. Only off-nuclear sources are considered in this paper. In addition, the centers of the galaxies given by PGC2003 are not necessarily precise and the specific environments of the 1,809 sources are different. Therefore, the authors visually checked the Chandra and DSS images simultaneously, since two-band inspection can help to exclude the nuclear sources, bright knots, and extended sources. X-ray sources with clear DSS features would be dropped because, for a source with a visual magnitude <20 and a distance >30 Mpc, its absolute magnitude would be brighter than -12.4, which is beyond the limit of the brightest star clusters. This table was created by the HEASARC in February 2017 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/222/12">CDS Catalog J/ApJS/222/12</a> file table1.dat, the list of very luminous X-ray source candidates found within the D<sub>25</sub> ellipses of Chandra ACIS-observed PGC2003 galaxies lying within 250 Mpc. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
MSL MARS ALPHA PARTICLE X-RAY SPECTROMETER 2 EDR V1.0
Unprocessed experiment data copied from the memory buffer of the APXS instrument aboard the Mars Science Laboratory rover.
RASS X-Ray Variable Sources Catalog
The RASS X-Ray Variable Sources Catalog contains the results of a systematic search for variability among the ROSAT All-Sky Survey (RASS) X-ray sources. Lightcurves were generated for about 30,000 X-ray point sources which were detected sufficiently high above the background. For the variability study different search algorithms were developed in order to recognize flares, periods and trends, respectively. The variable X-ray sources were optically identified with counterparts in the SIMBAD, the USNO-A2.0 and NED data bases, but a significant part of the X-ray sources remain without cataloged optical counterparts. A complete list of the 1207 X-ray variable sources that were found is presented in this table. This table was created by the HEASARC in July 2003 based on CDS table J/A+A/403/247/table7.dat. This is a service provided by NASA HEASARC .
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 .
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 .
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 .
IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog
This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s<sup>-1</sup> and shows a large variation by a factor of up to ~6 on timescales of ~10<sup>4</sup> s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/246">CDS Catalog II/246</a>) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K<sub>S</sub>, respectively. This table was created by the HEASARC in October 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/362/1065">CDS Catalog J/MNRAS/362/1065</a> files table1.dat, table2.dat and table3.dat. This is a service provided by NASA HEASARC .
NGC 4214 Chandra X-Ray Point Source Catalog
This table contains a comprehensive X-ray point source catalog of the IAB(s)m galaxy NGC 4214 similar to the LMC, one of the nearest examples of a starburst galaxy with a substantial population of Wolf-Rayet stars, as part of the Chandra Local Volume Survey. The combined archival observations of this galaxy have an effective exposure time of 79 ks. When combined with the catalogs of sources in NGC 55 and NGC 2403 given in this same reference paper, and the authors' previously published catalogs for NGC 300 (Binder et al. 2012, ApJ, 758, 15) and NGC 404 (Binder et al. 2013, ApJ, 763, 128), the CLVS contains 629 high-significance X-ray sources total down to a limiting unabsorbed luminosity of ~ 5 x 10<sup>35</sup> erg s<sup>-1</sup> in the 0.35-8.0 keV band in each of the five galaxies. In the reference paper, the authors present X-ray hardness ratios, spectral analysis, radial source distributions, and an analysis of the temporal variability for the X-ray sources detected at high significance. To constrain the nature of each X-ray source, they carried out cross-correlations with multi-wavelength data sets. They searched overlapping Hubble Space Telescope observations for optical counterparts to their X-ray detections to provide preliminary classifications for each X-ray source as a likely X-ray binary, background active galactic nucleus, supernova remnant, or foreground star. The authors utilized archival X-ray observations: NGC 4214 was observed by the Chandra X-Ray Observatory using the ACIS-S array on three occasions for a total of 79 ks: <pre> Obs. ID Date Eff. Exposure time (ks) 2030 2001 Oct 16 25 4743 2004 Apr 03 26 5197 2004 Jul 30 28 </pre> The iterative source detection strategy that was used is described in Section 2.3 of Binder et al. (2012, ApJ, 758, 15). ACIS-Extract (AE) was run a final time on the source list that was produces after an initial run of wavdetect followed by several iterations of AE, and the Poisson probability of not being a source (pns) value was computed in each of the following nine energy bands: 0.5 - 8.0, 0.5 - 2.0, 2.0 - 8.0, 0.5 - 1.0, 1.0 - 2.0, 2.0 - 4.0, 4.0 - 8.0, 0.35 - 1.0 or 0.35 - 8.0 keV. To be included in the final NGC 4214 catalog, a source was required to have a pns value less than 4 x 10<sup>-6</sup> in any of the nine energy bands. The final CLVS source catalog for NGC 2403 contains 116 sources. This table was created by the HEASARC in September 2015 based on machine-readable versions of those parts of Table 5 and 8 from the reference paper which pertained to the 116 high-significance (pns < 4 x 10<sup>-6</sup>) X-ray sources which were detected in NGC 4214. It does not include the 95 lower-significance sources in NGC 4214 which had 4 x 10<sup>-6</sup> < pns < 1.0 x 10<sup>-3</sup>, some of which are likely to be genuine X-ray sources. This is a service provided by NASA HEASARC .
IC 1805 XMM-Newton X-Ray Source Catalog
Very young open clusters are ideal places to study the X-ray properties of a homogeneous population of early-type stars. In this respect, the IC 1805 open cluster is very interesting as it hosts the O4 If+ star HD 15570 that is thought to be in an evolutionary stage intermediate between a normal O-star and a Wolf-Rayet star. Such a star could provide a test for theoretical models aiming at explaining the empirical scaling relation between the X-ray and bolometric luminosities of O-type stars. The authors have observed IC 1805 with XMM-Newton and further collected optical spectroscopy of some of the O-star members of the cluster. The optical spectra allowed them to revisit the orbital solutions of BD +60 497 and HD 15558, and provided the first evidence of binarity for BD +60 498. X-ray emission from colliding winds does not appear to play an important role among the O-stars of IC 1805. Notably, the X-ray fluxes do not vary significantly between archival X-ray observations and the present XMM-Newton pointing. The very fast rotator BD +60 513, and to a lesser extent the O4 If+ star HD 15570, appear somewhat underluminous. While the underluminosity of HD 15570 is only marginally significant, its amplitude is found to be compatible with theoretical expectations based on its stellar and wind properties. A number of other X-ray sources are detected in the field, and the brightest objects, many of which are likely low-mass pre-main sequence stars, are analyzed in detail. This table provides the full catalog of the 191 X-ray sources detected with the EPIC detectors onboard XMM-Newton in the direction of the IC 1805 cluster. The coordinates of the sources were cross-correlated with the optical and IR catalogs of Straizys et al. (2013, A&A, 554, A3), Wolff et al. (2011, ApJ, 726, 19), and the SIMBAD database. The authors adopted in each case a correlation radius of 4 arcseconds. This table was created by the HEASARC in October 2016 based on the electronic version of Table A1 from the reference paper which was obtained from the CDS (their catalog J/A+A/594/A82 file tablea1.dat). This is a service provided by NASA HEASARC .
RCW 38 Chandra X-Ray Point Source Catalog 2
This table contains some of the results from a study of the structure of the high-mass star-forming region RCW 38 and the spatial distribution of its young stellar population. Spitzer Infrared Array Camera (IRAC) photometry (3-8 micron) is combined with Two Micron All Sky Survey (2MASS) near-IR data to identify young stellar objects (YSOs) by IR-excess emission from their circumstellar material. Chandra X-ray data are used to identify class III pre-main-sequence stars lacking circumstellar material. The authors identify 624 YSOs: 23 class 0/I and 90 flat spectrum (FS) protostars, 437 class II stars, and 74 class III stars. They also identify 29 (27 new) O star candidates over the IRAC field. Seventy-two stars exhibit IR-variability, including 7 class 0/I and 12 flat spectrum YSOs. A further 177 tentative candidates are identified by their location in the IRAC [3.6] versus [3.6]-[5.8] color-magnitude diagram. The authors find strong evidence of subclustering in the region. Three subclusters were identified surrounding the central cluster, with massive and variable stars in each subcluster. The central region shows evidence of distinct spatial distributions of the protostars and pre-main-sequence stars. A previously detected IR cluster, DB2001_Obj36, has been established as a subcluster of RCW 38. This suggests that star formation in RCW 38 occurs over a more extended area than previously thought. The gas-to-dust ratio is examined using the X-ray derived hydrogen column density, NH and the K-band extinction, and found to be consistent with the diffuse interstellar medium, in contrast with Serpens and NGC 1333. The authors posit that the high photoionizing flux of massive stars in RCW 38 affects the agglomeration of the dust grains. This table contains the list of 536 X-ray sources found in the Chandra data using a three-pass method with the CIAO 3.4 Wavdetect tool. This table was created by the HEASARC in January 2012 based on an electronic version of Table 2 from the reference paper which was obtained from the ApJ website. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
XMM-Newton Large-Scale Structure Uniform 10-ksec Exposure X-Ray Source Catalog
This table contains some of the X-ray results from the final release of the multiwavelength XMM-Large Scale Structure (LSS) data set, covering the full survey area of 11.1 deg<sup>2</sup>. The 124 XMM-Newton observations used in the complete XMM-LSS are described in Section 2 and Table 1 of the primary reference paper (Chiappetti et al. 2013, hereafter Paper II). The X-ray data were processed with the latest XMM-LSS XAMIN pipeline version. The catalogs in Paper II supersede the catalog from the first paper in this series (Paper I: Pierre et al. 2007, MNRAS, 382, 279, available at the HEASARC as the XMMLSS table) pertaining to the initial 5 deg<sup>2</sup>. The authors provide X-ray source lists in the customary soft and hard energy bands (0.5-2 keV and 2-10 keV, respectively) for a total of 5572 objects in the catalog limited to 10 ks exposures presented in this table, and a total of 6721 objects in the deep full-exposure 2XLSSd catalog (available at the HEASARC as the XMMLSSDEEP table), above a detection likelihood of 15 in at least one band. At the XMMLSS web site which they maintain (<a href="http://cosmosdb.iasf-milano.inaf.it/XMM-LSS/">http://cosmosdb.iasf-milano.inaf.it/XMM-LSS/</a>), the authors also provide a multiwavelength catalog, cross-correlating their list of X-ray sources with infrared, near-infrared, optical and ultraviolet catalogs. Customary data products, such as X-ray FITS images and thumbnail images from the Canada-France-Hawaii Telescope Legacy Survey and the Spitzer Wide-Area Infrared Extragalactic Survey, are made available there, together with their data base in Milan, which can be queried interactively. In this table, the authors provide the source list for the full area (11.1 square degrees) of the XMM-LSS, with a total of 5572 point-like or extended sources above a detection likelihood of 15 in either the 0.5-2 or 2-10 keV bands. This table, the "standard" 2XLSS catalog containing the results of the analysis of the survey area using uniform 10-ksec exposures for all pointings longer than 10 ksec, lists the main X-ray parameters, while further multiwavelength parameters and data products (X-ray images and optical/IR thumbnails) are available at the Milan XMM-LSS database site referenced above. It supersedes the first XMM-LSS version (Pierre et al. 2007, available at the HEASARC as the XMMLSS table). Analogously to Paper I, only sources with an off-axis angle < 13 arcmin were processed by the authors' X-ray data processing pipeline software, XAMIN. The catalog includes all the extended sources classified in the customary C1 and C2 classes (see Section 3.6 of Paper II) plus all point-like sources with a point source detection likelihood (DET_LH) greater than 15 (so-called non-spurious sources). This table was created by the HEASARC in February 2013 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/429/1652">CDS catalog J/MNRAS/429/1652</a> file 2xlss.dat. This is a service provided by NASA HEASARC .
NGC 3293 Chandra X-Ray Point Source Catalog
NGC 3293 is a young stellar cluster at the northwestern periphery of the Carina Nebula Complex that has remained poorly explored until now. The authors wanted to characterize the stellar population of NGC 3293 in order to evaluate key parameters of the cluster population like the age and the mass function, and to test claims of an abnormal initial mass function (IMF) and a deficit of <= 2.5*M<sub>sun</sub> stars. Thus, they performed a deep (71 ksec) X-ray observation of NGC 3293 with Chandra in which they detected 1026 individual X-ray point sources. These X-ray data directly probe the low-mass (M <= 2*M<sub>sun</sub>) stellar population by means of the strong X-ray emission of young low-mass stars. The authors have identified counterparts for 74% of the X-ray sources in their deep near-infrared images. These data clearly show that NGC 3293 hosts a large population of ~ 1*M<sub>sun</sub> stars, refuting claims of a lack of M <= 2.5*M<sub>sun</sub> stars. The analysis of the color-magnitude diagram suggests an age of ~8-10 Myr for the low-mass population of the cluster. There are at least 511 X-ray detected stars with color-magnitude positions that are consistent with young stellar members within 7 arcminutes from the cluster center. The number ratio of X-ray detected stars in the 1-2 solar mass range versus the M >= 5*M<sub>sun</sub> stars (known from optical spectroscopy) is well consistent with the expectation from a normal field initial mass function. Most of the early B-type stars and ~20% of the later B-type stars are detected as X-ray sources. These data shows that NGC 3293 is one of the most populous stellar clusters in the entire Carina Nebula Complex (only excelled by Tr 14, and very similar to Tr 16 and Tr 15). The cluster has probably harbored several O-type stars, the supernova explosions of which may have had an important impact on the early evolution of the Carina Nebula Complex. The authors used the Chandra X-ray Observatory to perform a deep pointing of the cluster NGC 3293 with the Imaging Array of the Chandra Advanced CCD Imaging Spectrometer (ACIS-I). The 71-ksec observation was performed as an open time project with ObsID 16648 (PI: T. Preibisch) during Chandra Observing Cycle 15 in October 2015 (start date: 2015-10-07 T10:14:23, end date: 2015-10-08 T06:43:28). The imaging array ACIS-I provides a field of view of 17' x 17' on the sky (which corresponds to a scale of 11.3 x 11.3pc at the cluster distance of 2.3 kpc), and has a pixel size of 0.492". The aimpoint of the observation was RA(J2000) = 10<sup>h</sup> 35<sup>m</sup> 50.07<sup>s</sup>, Dec(J2000) = -58<sup>o</sup> 14' 00", which is close to the optical center of the cluster (see Fig. 1 in the reference paper). The pointing roll angle (i.e., the orientation of the detector with respect to the celestial North direction) was 140.19<sup>o</sup>. In addition to ACIS-I, one CCD detector (CCD 7 = S3) of the spectroscopic array ACIS-S was also operational during this pointing. It covers an 8.3' x 8.3' area on the sky southwest of the cluster center. While the ACIS-I chips are front-illuminated (FI), the S3 chip is back-illuminated (BI), and thus its response extends to energies below that accessible by the FI chips. This causes a substantially higher level of background in the S3 chip. Furthermore, the PSF is seriously degraded at the rather large off-axis angles of the S3 chip. These two effects led to a considerably higher detection limit for point sources in the area covered by the S3 chip compared to the region covered by the ACIS-I array. Nevertheless, the S3 data were included in the data analysis and source detection, and contributed four point sources to the total source list. At the distance of 2.3 kpc, the expected ACIS point source sensitivity limit for a three-count detection on-axis in a 71-ks observation corresponds to a minimum X-ray luminosity of L<sub>x</sub> ~ 10<sup>29.7</sup> erg s<sup>-1</sup> in the 0.5-8.0 keV energy band, assuming an extinction of A<sub>V</sub> ~ 1 mag (N<sub>H</sub> ~ 2 x 10<sup>21</sup> cm<sup>-2</sup>) typical for the stars in the central region of NGC 3293, and a thermal plasma with kT = 1 keV (which is a typical value for young stars). Using the empirical relation between X-ray luminosity and stellar mass and the temporal evolution of X-ray luminosity from the sample of young stars in the Orion Nebula Cluster, which was very well studied in the Chandra Orion Ultradeep Project (Preibisch et al. 2005, ApJS, 160, 401; Preibisch & Feigelson 2005, ApJS, 160, 390), the authors expected to detect ~90% of the ~ 1*M<sub>sun</sub> stars in the central region of the young cluster NGC 3293. The X-ray properties of the 97 B-type stars in the ACIS-
Magellanic Clouds High-Mass X-Ray Binaries Catalog
This database table contains a catalog of high-mass X-ray binaries (HMXBs) in the Small and Large Magellanic Clouds (SMC and LMC). The catalog lists source name(s), coordinates, apparent magnitudes, orbital parameters, and X-ray luminosities for 128 HMXBs, together with the stellar parameters of the components, other characteristic properties and a comprehensive selection of the relevant literature. The aim of this catalog is to provide easy access to the basic information on the X-ray sources and their counterparts in other wavelength ranges (UV, optical, IR, radio). Most of the sources have been identified as Be/X-ray binaries. Some sources, however, are only tentatively identified as HMXBs on the basis of a transient character and/or a hard X-ray spectrum. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 May 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/442/1135/refs.dat">CDS</a>. Individual notes on each HMXB are also available for <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/442/1135/notes1.dat">SMC systems</a> and for <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/442/1135/notes2.dat">LMC systems</a> at the same site. This Browse table contains the combination of 92 HMXBs in the SMC and 36 HMXBs in the LMC which were listed in Tables 1 and 2, respectively, of the published version of this catalog. The HEASARC has added a parameter called cloud_id which can be used to identify which Magellanic Cloud any specified HMXB belongs to (the SMC or the LMC). This database was created by the HEASARC in December 2005 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/442/1135">CDS Catalog J/A+A/442/1135</a>, table1.dat and table2.dat. This is a service provided by NASA HEASARC .
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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.