Five hundred sixty-five measurements of 99 binary star systems are presented, obtained during 1984-1986 by means of speckle interferometry at the 1.8 m Perkins telescope on Anderson Mesa, Arizona. These observations were collected as part of a systematic program in which frequent speckle observations of nearby binary systems were to be used to attempt the detection of unseen companions through the analysis of residual motions in wide, visual binaries. This is the first of several papers in which these observations are presented and discussed.

This catalog contains the results of a complete X-ray survey of the Hyades cluster region using X-ray data from the ROSAT All-Sky Survey (RASS) that was published by Stern, Schmitt and Kahabka in 1995. The Hyades survey covered over 900 square degrees of the sky. Over 185 optically identified Hyades were detected down to a limiting X-ray luminosity of about 1-2x10²⁸ ergs/s in the 0.1-1.8keV energy band. Among solar-like stars, i.e., main-sequence stars of spectral type G, the RASS detection rate was about 90%. Stern et al. argue that the presence of many binary systems in the cluster is a key factor influencing the Hyades X-ray luminosity function. Short-period (a few days or less) binaries are anomalously X-ray bright, as might have been expected; however, the X-ray luminosity functions of K and possibly M binary stars of all types are significantly different from their single counterparts, confirming the results of Pye et al. (1994, MNRAS, 266, 798) based on a smaller K star sample drawn from deep ROSAT pointings. Comparison with Einstein Observatory studies of a subset of Hyades stars demonstrates a general lack of significant (> a factor of 2) long-term X-ray variability. Stern et al. suggest that this may be the result of the dominance of a small-scale, turbulent dynamo in the younger Hyades stars compared to the large-scale, cyclic dynamo observed in the Sun. The HYADESXRAY database consists of X-ray data for 440 probable and possible Hyades members that were included in the Stern et al. survey and were listed in Table 1 of their published paper. The database contains both stars which were detected as X-ray sources and those which were not: for the latter, upper limits to their X-ray emission are provided. For all listed stars, their X-ray luminosities based on a Hyades distance of 45 pc are provided; for some stars, for which individually determined distances from either the Schwan (1991, A&A, 243, 386) or the Hanson (1975, AJ, 80, 379) proper motion surveys are available, their X-ray luminosities based on these alternate distances are also provided. There were 4 stars detected as RASS sources out of over 180 new Hyades candidates listed in the Reid (1992, MNRAS, 257, 257) proper motion survey which were included in Table 2 (but not Table 1) of the Stern et al. paper. These stars are not included in the current database, but are listed in the help section entitled Reid_Stars (q.v.). Similarly, there were 20 stars detected as RASS sources but which were considered by Stern et al. to be non-members of the Hyades which were included in their Table 3 (but not Table 1). These stars are not included in the current database, but are listed in the help section entitled Rejected_Hyades (q.v.). This HEASARC catalog was created in July 1997, derived from CDS Catalog J/ApJ/448/683 obtained from https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/448/683/. Additional information provided in the HEASARC documentation was taken from the original published version of the paper containing this catalog. This is a service provided by NASA HEASARC .

VizieR Online Data Catalog: Massive binary stars from an HST/FGS survey(Aldoretta E.J.+, 2015)

The authors have combined their catalog of eclipsing binaries from the All-Sky Automated Survey (ASAS) with the ROSAT All-Sky Survey (RASS) Bright and Faint Source Catalogs (RASSBSC and RASSFSC). The combination using a matching radius of 50 arcseconds results in 836 eclipsing binaries that display coronal activity and is the largest sample of active binary stars assembled to the date of publication. By using the (V-I) colors of the ASAS eclipsing binary catalog, the authors are able to determine the distances and thus bolometric luminosities for the majority of eclipsing binaries that display significant stellar activity. A typical value for the ratio of soft X-ray to bolometric luminosity is L_X/L_bol ~ a few x 10^-4, similar to the ratio of soft X-ray to bolometric flux F_X/F_bol in the most active regions of the Sun. Unlike rapidly rotating isolated late-type dwarfs - stars with significant outer convection zones - a tight correlation between Rossby number and activity of eclipsing binaries is absent. The authors find evidence for the saturation effect and marginal evidence for the so-called "super-saturation" phenomena. Their work shows that wide-field stellar variability searches can produce a high yield of binary stars with strong coronal activity. The authors expect that only 1.4% (i.e., 12 out of 836) of the matches between the ASAS eclipsing binary and RASS sources will be false given their maximum angular separation criterion of 50 arcseconds. This Browse table excludes 29 contact binaries for which the separate distance estimates made by the authors using the source V-band and I-band magnitudes differed by more than 20%, and hence contains 807 (836 - 29) eclipsing and X-ray emitting binary systems. Complete information on ASAS and its freely accessible data are available at the ASAS web site: http://www.astrouw.edu.pl/asas/. This table was created by the HEASARC in July 2010 based on CDS catalog J/AcA/58/405 file catalog.dat. This is a service provided by NASA HEASARC .

VizieR Online Data Catalog: The Galactic Bulge Survey: X-ray observations(Jonker P.G.+, 2011)

Photometric data from the All-Sky Automatic Survey (ASAS) - South (Declination less than 29 degrees) Survey have been used for the identification of bright stars located near the sources from the ROSAT All Sky Survey Bright Source Catalog (RASSBSC). In total, 6,028 stars brighter than 12.5 magnitude in the I- or the V-bands have been selected and analyzed for periodicity. Altogether, 2,302 variable stars have been found with periods ranging from 0.137 days to 193 days. Most of these stars have X-ray emission of coronal origin, but there are a few cataclysmic binaries and early type stars with colliding winds. Whenever it was possible, the authors collected data available in the literature so as to verify the periods and to classify variable objects. The catalog includes 1,936 stars (1,233 new) considered to be variable due to presence of spots (rotationally variable), 127 detached eclipsing binary stars (33 new), 124 contact binaries (11 new), 96 eclipsing stars with deformed components (19 new), 13 ellipsoidal variables (4 new), 5 miscellaneous variables and one pulsating RR Lyr type star (blended with an eclipsing binary). More than 70% of the new variable stars have amplitudes smaller than 0.1 magnitudes, but for the star ASAS 063656-0521.0 the authors have found the largest known amplitude of brightness variations due to the presence of spots (up to Delta V = 0.8 magnitudes). This table was created by the HEASARC in May 2018, based on CDS Catalog J/AcA/62/67 files catalog.dat and remarks.dat. This is a service provided by NASA HEASARC .

ALMA 12CO data cubes from VANDAM Perseus Survey. Visit https://dataone.org/datasets/sha256%3A7a762b9669a6e5f6e5c192d6acafc78beefd079f96dd1845172bac69b9e90fc7 for complete metadata about this dataset.

VizieR Online Data Catalog: A first catalog of variable stars measured by ATLAS(Heinze A.N.+, 2018)

A stellar common envelope occurs in a binary system when the atmosphere of an evolving star expands to encompass an orbiting companion object. Such systems are predicted to evolve rapidly, ejecting the stellar envelope and leaving the companion in a tighter orbit around a stripped star. We use radio timing to identify a pulsar, PSR J1928+1815, with a spin period of 10.55 ms in a compact binary system with an orbital period of 3.60 hours. The companion star has 1.0 to 1.6 solar masses and eclipses the pulsar for about 17% of the orbit, so is most likely a stripped helium star but is undetected at other wavelengths. We interpret this system as having recently undergone a common envelope phase, producing a compact binary., , # Data from: A pulsar-helium star compact binary system formed by common envelope evolution

Dataset DOI: 10.5061/dryad.f1vhhmh6z

Description of the data and file structure

Processed FAST data of PSR J1928+1815, a binary pulsar discovered in FAST GPPS survey.

Files and variables

File: yhz25dat.tar.gz

Description:Â Processed FAST data of PSR J1928+1815, a binary pulsar discovered in FAST GPPS survey.

1) Folded pulsar profiles of PSR J1928+1815. These profiles have a bin number of 128 a sub-bint integration time is 300 s and 4 frequency channels. The radio frequency range is 1.0 to 1.5 GHz.

2) We link three observations during which the pulsar was eclipsed to the 'nodect' folder .

3) The sum polarization profile is in 'sum_profile' folder.

4) The ephemeris and TOAs of PSR J1928+1815 is in 'timing' folder.

Code/software

The code used for view the data is PSRCHIVE package ([https://psrchive.sourceforge.net/](https://psrchive.source...,

The Third Catalogue of Nearby Stars (Gliese & Jahreiss Preliminary Version of the third Catalogue of Nearby Stars, 1991) includes over 1850 stars which lie north of Dec. = -30 deg and are either identified as spectral type M, or are unclassified but with an absolute visual magnitude estimate M_V > +8.0. Although there is no uniformity in selection criteria, and many of the stars lack basic data (radial velocities, spectral types, accurate photometry), the observational properties of these stars underlie most estimates of the fundamental characteristics of the Galactic Disk. We have obtained optical spectroscopy of 1746 of the 1876 stars -- the remaining 130 are binary companions of brighter stars and inaccessible to our observations. These spectra allow us, first, to exclude 61 stars as either degenerates or as misclassified earlier-type (B-K) stars lying beyond the 25 pc limit; to establish radial velocities accurate to +/- 10 km/s for all stars confirmed as late-type dwarfs; to determine spectral types and absolute magnitudes from the TiO bandstrength, allowing more accurate distance estimates for stars with inaccurate (or no) trigonometric parallax measurements; and to identify stars with Halpha emission (chromospherically active stars) and with strong CaH absorption (perhaps including some metal-poor disk subdwarfs). We have determined the nearby-star luminosity function from complete samples derived by applying both the distance limits defined by Wielen (1974) and by using limits derived from our own analysis. In both cases, we find good agreement with Wielen's results to M_V ~ +11, but lower densities at the maximum (M_V ~ +12). The latter analysis results in a luminosity function, Phi(CNS), which closely matches photometric parallax analyses for M_V < +11 and M_V > +14 -- we do not recover the apparent excess of low-luminosity stars inferred from analysis of the 5 pc sample. However, Phi(CNS) does lie below Phi(phot) at the peak (M_V ~ 12), and we suggest that this offset is caused by the inclusion of unrecognized binaries in the photometric surveys. We have also reanalyzed the local stellar kinematics using the complete sample and find that the velocity distributions show significant departures from single Gaussian velocity dispersions., The Third Catalogue of Nearby Stars (Gliese & Jahreiss Preliminary Version of the third Catalogue of Nearby Stars, 1991) includes over 1850 stars which lie north of Dec. = -30 deg and are either identified as spectral type M, or are unclassified but with an absolute visual magnitude estimate M_V > +8.0. Although there is no uniformity in selection criteria, and many of the stars lack basic data (radial velocities, spectral types, accurate photometry), the observational properties of these stars underlie most estimates of the fundamental characteristics of the Galactic Disk. We have obtained optical spectroscopy of 1746 of the 1876 stars -- the remaining 130 are binary companions of brighter stars and inaccessible to our observations. These spectra allow us, first, to exclude 61 stars as either degenerates or as misclassified earlier-type (B-K) stars lying beyond the 25 pc limit; to establish radial velocities accurate to +/- 10 km/s for all stars confirmed as late-type dwarfs; to determine spectral types and absolute magnitudes from the TiO bandstrength, allowing more accurate distance estimates for stars with inaccurate (or no) trigonometric parallax measurements; and to identify stars with Halpha emission (chromospherically active stars) and with strong CaH absorption (perhaps including some metal-poor disk subdwarfs). We have determined the nearby-star luminosity function from complete samples derived by applying both the distance limits defined by Wielen (1974) and by using limits derived from our own analysis. In both cases, we find good agreement with Wielen's results to M_V ~ +11, but lower densities at the maximum (M_V ~ +12). The latter analysis results in a luminosity function, Phi(CNS), which closely matches photometric parallax analyses for M_V < +11 and M_V > +14 -- we do not recover the apparent excess of low-luminosity stars inferred from analysis of the 5 pc sample. However, Phi(CNS) does lie below Phi(phot) at the peak (M_V ~ 12), and we suggest that this offset is caused by the inclusion of unrecognized binaries in the photometric surveys. We have also reanalyzed the local stellar kinematics using the complete sample and find that the velocity distributions show significant departures from single Gaussian velocity dispersions.

This catalog includes the hard X-ray sources detected in the first 157 months of observations with the Burst Alert Telescope (BAT) coded-mask imager on board the Swift observatory. The results of the 157 months survey catalog has been obtained using data from February 2007 to December 2017 and provide a uniform hard X-ray all-sky survey with a sensitivity of 8.40 x 10^-12 erg/s/cm² over 90% of the sky and 7.24 x 10^-12 erg/s/cm² over 50% of the sky in the 14-195 keV band. The exposure time in all sky ranges from ~ 15 Ms to ~ 35 Ms, where ~ 50% of the sky achieves an exposure time of ~ 22.8 Ms. The 157 months survey provides 1891 hard X-ray sources in the 14-195 keV band above the 4.8 sigma significance level, where 259 are new detections from the 105-month catalog of which 54 are previously known source in X-ray. The sources identification is mostly from NED and SIMBAD and the 157-month catalog reports for positive identification the counterpart R.A. and Dec and the alternative name. The sources are classified in 17 different classes as follows:

 Class Source Type Number of Sources 0 Unknown 221 1 Galactic 4 2 Galaxy 16 3 Galaxy Cluster 26 4 Seyfert I 446 5 Seyfert II 464 6 Other AGN 130 7 Beamed AGN (Blazar/FSRQ) 192 8 LINER 7 9 Cataclysmic Variable Star (CV) 81 10 Pulsar 27 11 Supernova Remnant (SNR) 7 12 Star 26 13 High Mass X-ray Binary (HMXB) 108 14 Low Mass X-ray Binary (LMXB) 118 15 Other X-ray Binary (XRB) 17 16 Tidal Disruption Event 1 Total 1891 

The data reduction, analysis, and catalog generation of the Swift-BAT are conducted following the same procedures of the previous catalog survey (Tueller+ 2010, J/ApJS/1167/186, Baumgartner+ 2013, J/ApJS/207/19). The BAT survey data are collected into arrays (Detector Plane Histograms, DPHs) where the data are binned in ~ 300 s time interval and in 8 energy band channels (14-20, 20-24, 24-35, 35-50, 50-75, 75-100, 100- 197 150, and 150-195 keV) and 1 energy total band (14-195 keV). Three different mosaic images are created from the DPH dividing the sky in 6 regions. The first set has images created in 8 energy bands to span a contiguous time interval (snapshot). The second set has images co-adding data on a time period of a month. The third set is created in 8 energy bands by Crab-weighting the monthly images in each of the energy band with the following weights (Baumgartner+ 2013, J/ApJS/207/19): 27.000, 35.260, 22.700, 29.444, 21.272, 16.062, 8.449, 2.630. The benchmark Crab spectrum adopted is F(E) = 10.17E−2.15 photon cm2 s keV. The source detection algorithm uses the Crab-weighted mosaic images. For each source detected lightcurves and spectra are derived. The lightcurves are obtained from the snapshot images, the mosaic monthly images and the Crab-weighted mosaic images. The spectra are obtained from an additional set of mosaic images by adding all the snapshots for the 157 months period in 8-bands. All the analyses use HEASoft tools version 6.23, and the most recent BAT calibration database (updated on Oct. 3, 2017). Data products are generated for each source detected and these are: three different lightcurves in FITS format obtained from the snapshot, monthly and Crab-weighted monthly mosaic images and the equivalent plots as GIF images; an 8-channel average spectrum in FITS obtained using all 157 months; and a GIF file showing the spectrum with the fit to the best parameter of the power-law model. The snapshot lightcurves report rates for the 8-energy band, the monthly and Crab-weighted monthly mosaic lightcurves reports rated for the 8-energy band and the total band 14-195 keV. This table was ingested by the HEASARC in February 2025 based upon the published 157-month catalog. The catalog is also available at https://swift.gsfc.nasa.gov/results/bs157mon/. This is a service provided by NASA HEASARC .

We propose to undertake a snapshot survey of AGB stars and protoplanetary nebulae keyOpen PPNekeyClose in order to discern the evolutionary sequence that produces axially symmetric planetary nebulae keyOpen PNekeyClose . It is now well established that most PNe are axially symmetric. However comma the origin of this axial symmetry remains a topic of current research. Our snapshot survey addresses two aspects of this issuedoblePoint at which point in the intermediate mass star.s evolution does the axial symmetry arise and do binary companions play an important role in creating this axial symmetry. The survey comma using a list of approximately 40 candidate targets comma will show AGB and PPNe circumstellar envelopes keyOpen CSEskeyClose in various stages of development resulting in a database of images from which meaningful statistics can be derived on the evolutionary stage at which the axial symmetry originates. In addition comma some binary companions may be detected. The objects in this survey overlap with those imaged in a high resolution keyOpen <0.9d_commakeyClose midinfrared imaging study by Meixner et al. Our proposed HST snapshot survey will complement the midIR survey in wavelength and spatial resolution. In particular comma the high angular resolution of HST will permit us to investigate the structure of CSEs from an earlier stage of development than has been possible in the midIR.

The X-ray source populations within galaxies are typically difficult to identify and classify with X-ray data alone. The authors break through this barrier by combining deep new Chandra ACIS-I observations with extensive Hubble Space Telescope (HST) imaging from the Panchromatic Hubble Andromeda Treasury (PHAT) of the M 31 disk. They detect 373 X-ray sources down to 0.35-8.0keV flux of 10^-15erg/cm^-2/s over 0.4deg², 170 of which are reported for the first time. The authors identify optical counterpart candidates for 188 of the 373 sources, after using the HST data to correct the absolute astrometry of our Chandra imaging to 0.1". While 58 of these 188 are associated with point sources potentially in M 31, over half (107) of the counterpart candidates are extended background galaxies, 5 are star clusters, 12 are foreground stars, and 6 are supernova remnants. Sources with no clear counterpart candidate are most likely to be undetected background galaxies and low-mass X-ray binaries in M 31. The hardest sources in the 1-8keV band tend to be matched to background galaxies. The 58 point sources that are not consistent with foreground stars are bright enough that they could be high-mass stars in M 31; however, all but 8 have optical colors inconsistent with single stars, suggesting that many could be background galaxies or binary counterparts. For point-like counterparts, the authors examine the star formation history of the surrounding stellar populations to look for a young component that could be associated with a high-mass X-ray binary. The associated star formation histories for sources in the catalog are available in the linked table M31PHATSFH. In 2015 October, the authors observed the Panchromatic Hubble Andromeda Treasury (PHAT) footprint with Chandra with 7 pointings. The footprints are overlaid on a GALEX NUV image of M 31, along with the corresponding HST coverage, in Figure 1 of the reference paper. At each pointing they observed for about 50ks in VF mode (Chandra ObsID 17008 to 17014 spanning 2015 Oct 06 to 2015 Oct 26). This table was created by the HEASARC in April 2020 based upon the CDS Catalog J/ApJS/239/13 file table4.dat and table6.dat. This is a service provided by NASA HEASARC .

This Zenodo has an assortment of data files related to Schochet, Tayar & Andrews (2024) "A Lack of Mass-Gap Compact Object Binaries in APOGEE" which sought to identify binary systems with a single stellar component that may be host to a "mass-gap" black hole/neutron star companion. These files utilize data from the Sloan Digital Sky Survey IV's (Blanton et al. 2017) Apache Point Galactic Evolution Experiment (Majewski et al. 2017) Data Release 17 (Abdurro'uf et al. 2022), including stellar abundances from the ASPCAP pipeline (Garcia Perez et al. 2016) and with spectra reduced using the Doppler (Nidever et al. 2015). Radius values used in the catalog come from Gaia + SED fitting (Yu et al. 2023).

In this repository you will find:

Files

• APOGEE_likely_binaries.csv: datafile contains basic information and IDs for the 4751 likely binary objects from our data reductions (2MASS ID, SNR, nvisits, vsini, vscatter, teff, log(g), M/H and errors for the final 3 stellar parameters).
• For systems with a radius value from Yu et al. 2023 (4288/4751), we also provide:
  • apogee_objects_with_kiauhoku_masses.csv: this file contains masses and ages from the four grids of kiauhoku (Claytor et al. 2020) which include models from MIST (MESA Isochrones and Stellar Tracks, Choi et al. 2016 & Paxton et al. 2010), YREC (Yale Rotating stellar Evolution Code, Tayar et al. 2022 & Pinsonneault et al. 1989) Dart/DSEP (Dartmouth Stellar Evolution Program, Dotter et al. 2008), and GARSTEC/Gars (Garching Stellar Evolution Code, Serenelli et al. 2013 & Weiss & Schlattl 2008). These are in the final columns of the csv file, and other columns include Gaia IDs, APOGEE starflag and ASPCAP flags, and RA/Dec along with APOGEE Telescope and Field information for each target.
  • estimated_companions.csv: this file contains estimated minimum companion masses from the tidal synchronization method (CO_mass_rsync) and Joker method (CO_mass_joker) used in Schochet et al., and velocity semi-amplitude, eccentricity, and period values from the Joker (K_joker, e_joker, P_joker; Price-Whelan et al. 2017).

Programs

• spectra_replotter.ipynb: This program replots spectra from the APOGEE servers when given a 2MASS ID, Field, and the telescope (APO/LCO) used for a specific observed object. It will then print out an image of that object's spectra with the apVisit/asVisit files (pre-RV-shift reduction) plotted above the apStar/asStar files (post-RV-shift reduction) so that radial velocity shifts can be quickly identified by eye

Notes

estimated_companions.csv and apogee_objects_with_kiauhoku_masses.csv contain Fiber Dispersion in their data frames, as a reference to the observed trend that vscatter tends to be much lower for objects with 0 fiber dispersion, while objects with fiber dispersion > 0 show larger vscatters, in case there is future focus on investigating this phenomena

Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss4.org.

SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, Center for Astrophysics | Harvard & Smithsonian (CfA), the Chilean Participation Group, the French Participation Group, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatório Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.

The authors identify 233 X-ray sources, of which 95 are new, in a 222-ks exposure of omega Centauri with the Chandra X-ray Observatory's Advanced CCD Imaging Spectrometer detector. The limiting unabsorbed flux in the core is f_X(0.5-6.0keV) ~= 3 x 10^-16 erg/s/cm² (L_x ~= 1 x 10³⁰ erg/s at 5.2kpc). The authors estimate that ~60 +/- 20 of these are cluster members, of which ~30 lie within the core (r_c = 155 arcsec), and another ~30 between 1-2 core radii. They identify four new optical counterparts, for a total of 45 likely identifications. Probable cluster members include 18 cataclysmic variables (CVs) and CV candidates, one quiescent low-mass X-ray binary, four variable stars, and five stars that are either associated with omega Cen's anomalous red giant branch or are sub-subgiants. The authors estimate that the cluster contains 40 +/- 10 CVs with L_x_> 10³¹ erg/s, confirming that CVs are underabundant in omega Cen relative to the field. Intrinsic absorption is required to fit X-ray spectra of six of the nine brightest CVs, suggesting magnetic CVs, or high-inclination systems. Though no radio millisecond pulsars (MSPs) are currently known in omega Cen, more than 30 unidentified sources have luminosities and X-ray colors like those of MSPs found in other globular clusters; these could be responsible for the Fermi-detected gamma-ray emission from the cluster. The authors identify a CH star as the counterpart to the second brightest X-ray source in the cluster and argue that it is a symbiotic star. This is the first such giant/white dwarf binary to be identified in a globular cluster. The data were obtained over two long exposures of omega Cen using the imaging array of the Chandra X-ray Observatory's ACIS-I on 2012 April 16 and 17. The data sets have a combined exposure time of ~222ks (173.7 and 48.5ks for ObsIDs 13726 and 13727, respectively). This table was created by the HEASARC in June 2018 based upon the CDS Catalog J/MNRAS/479/2834 file table1.dat. This is a service provided by NASA HEASARC .

This catalog presents the results of a systematic search for point-like and moderately extended soft (0.1-2.4 keV) X-ray sources in a raster of nine pointings covering a field of 8.95 square degrees which was performed with the ROSAT PSPC between October 1991 and October 1993 in the direction of the Small Magellanic Cloud (SMC). 248 objects were detected and are included in this first version of the SMC catalog of soft X-ray sources. The authors set up seven source classes defined by selections in the count rate, hardness ratio and source extent parameters. They found five high luminosity super-soft sources (1E 0035.4-7230, 1E 0056.8-7146, RX J0048.4-7332, RX J0058.6-7146 and RX J0103-7254), one low-luminosity super-soft source RX J0059.6-7138 correlating with the planetary nebula L357, 51 candidate hard X-ray binaries including eight bright hard X-ray binary candidates, 19 supernova remnants (SNRs), 19 candidate foreground stars and 53 candidate background active galactic nuclei (and quasars). Likely classifications are given for about 60% of the catalogued sources. The total count rate of the detected point-like and moderately extended sources in the catalog is 6.9 +/- 0.3 counts s^-1, comparable to the background subtracted total rate from the integrated field of about 6.1 +/- 0.1 counts s^-1. This online catalog was created by the HEASARC in July 1999 based on tables obtained from the ADC/CDS data centers. This is a service provided by NASA HEASARC .

We propose EPIC observations of 3 fields in the Magellanic Bridge the extendedregion joining the Large and Small Magellanic Clouds with the aim ofcharacterising recent star formation through the Xray binary population.Together with already available optical photometry, these observations arecentral to our understanding of how the environment (e.g. local metallicity, gascontent) affects star formation and evolution in turbulent intergalacticenvironments. For Xray sources detected in outburst, these observations willpermit rigorous study of individual sources through spectral and temporalanalysis, while fainter and quiescent sources will be detected and identifiedthrough hardness ratios, variability and optical followup, allowing us a first look at the faint end of this unique population. truncated!, Please see actual data for full text [truncated!, Please see actual data for full text]

VizieR Online Data Catalog: GALAH survey. FGK binary stars(Traven G.+, 2020)

The authors have detected 523 X-ray sources in a survey of the Small Magellanic Cloud (SMC) Wing with the Chandra X-ray Observatory. By cross-correlating the X-ray data with optical and near-infrared catalogs, they have found 300 matches. Using a technique that combines X-ray colors and X-ray to optical flux ratios, they have been able to assign preliminary classifications to 265 of the objects. The identifications include 4 pulsars, 1 high-mass X-ray binary (HMXB) candidate, 34 stars and 185 active galactic nuclei (AGN). In addition, the authors have classified 32 sources as hard AGN which are likely absorbed by local gas and dust, and 9 soft AGN whose nature is still unclear. Considering the abundance of HMXBs discovered so far in the Bar of the SMC the number that have been detected in the Wing is low. Observations in the Wing of the SMC were made from 2005 July to 2006 March with Chandra. The survey consisted of 20 fields, with exposure times ranging from 8.6 - 10.3 ks. X-ray parameters for 523 sources detected in the Wing of the SMC with Chandra are presented. For each source equatorial coordinates, positional error, net counts (total counts minus background counts) in the 0.5 - 8.0 keV band, signal-to-noise of the detection and source flux in the 0.5 - 8.0 keV band are given. The median, compressed median and normalized quartile ratio of the photon energy distribution, determined using quantile analysis, are given for sources with three or more counts. For the sources that have optical counterparts the V- and R-band magnitudes, B-V color, X-ray to optical flux ratios based on the V- and R-band magnitudes, and a preliminary classification for the sources are given. This table was created by the HEASARC in June 2008 based on the CDS Catalog J/MNRAS/383/330 file table2.dat. This is a service provided by NASA HEASARC .

The prevalence of millisecond pulsars (MSPs) in and around the Galactic center and the bulge has been one of the key questions in pulsar astronomy. In addition to finding more exotic and interesting binary systems at and around the Galactic center and bulge due to the enhanced density of stars/stellar remnants, MSPs are also proposed to be one of the candidates to explain the observed Fermi gamma-ray excess. However, most of the MSPs discovered so far are field (disk) MSPs or those in globular clusters. Initial steps towards addressing the question of Galactic center/bulge MSPs were made with the discovery of the first MSPs in a Galactic filament, but more progress comes from the discovery of a sample of MSPs around the Galactic center. Blind surveys targeting MSPs can suffer from many observational biases that smear the pulses due to binary acceleration, scattering from the enhanced density, and so on, which increases the parameter space for discovery and can sometimes make the problem intractable. However, if pulsar candidates can be identified reliably from imaging surveys, then targeted observations can make the problem tractable in identifying the pulsations. We followed up a sample of polarized sources identified in the MeerKAT bulge imaging survey and discovered a sample of 16 new MSPs. Here we request the timing observations of 8 interesting MSPs (a subset of our discovery sample), to study the binary nature of these sources and their potential inclusion in pulsar timing array efforts.