HCGXRBS ivo://nasa.heasarc/hcgxrbs NASA/GSFC HEASARC Tzanavaris et al. 2026-10-02 NASA/GSFC HEASARC help desk heasarc-vo at athena.gsfc.nasa.gov Survey Source This catalog presents the study of a sample of 15 compact groups (CGs) observed with Chandra/ACIS, Swift/UVOT and Spitzer/IRAC-MIPS for which archival data exist, allowing the authors to obtain SFRs, stellar masses, sSFRs and X-ray fluxes and luminosities for individual, off-nuclear point sources, which they summed to obtain total X-ray luminosities originating in off-nuclear point sources in a galaxy. Details on the Swift and Spitzer observations and data for systems in this sample can be found in Tzanavaris et al. (2010ApJ...716..556T) and Lenkic et al. (2016MNRAS.459.2948L). For Chandra/ACIS observations, see Tzanavaris et al. (2014ApJS..212....9T) and Desjardins et al. (2013ApJ...763..121D; 2014ApJ...790..132D). The authors obtained total galaxy X-ray luminosities, L<sub>X</sub>, originating from individually detected point sources in a sample of 47 galaxies in 15 compact groups of galaxies (CGs). For the great majority of the galaxies, they found that the detected point sources most likely are local to their associated galaxy, and are thus extragalactic X-ray binaries (XRBs) or nuclear active galactic nuclei (AGNs). For spiral and irregular galaxies, they found that, after accounting for AGNs and nuclear sources, most CG galaxies are either within the +/- 1 sigma scatter of the Mineo et al. L<sub>X</sub>-star formation rate (SFR) correlation or have higher L<sub>X</sub> than predicted by this correlation for their SFR. These "excesses" may be due to low metallicities and high interaction levels. For elliptical and S0 galaxies, after accounting for AGNs and nuclear sources, most CG galaxies were found to be consistent with the Boroson et al. L<sub>X</sub>-stellar mass correlation for low-mass XRBs, with larger scatter, likely due to residual effects such as AGN activity or hot gas. Assuming non-nuclear sources are low- or high-mass XRBs, the authors used appropriate XRB luminosity functions to estimate the probability that stochastic effects can lead to such extreme L<sub>X</sub> values. They found that, although stochastic effects do not in general appear to be important, for some galaxies there is a significant probability that high L<sub>X</sub> values can be observed due to strong XRB variability. This table was created by the HEASARC in May 2019 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/817/95">CDS Catalog J/ApJ/817/95</a> file table3.dat This is a service provided by NASA HEASARC . 2016ApJ...817...95T https://heasarc.gsfc.nasa.gov/W3Browse/all/hcgxrbs.html Catalog Research served-by HEASARC TAP https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=hcgxrbs& GET text/xml 180 99999 true 330.51958333 -31.97905556 0.0166666666666667 https://heasarc.gsfc.nasa.gov/xamin/vo/tap https://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hcgxrbs GET text/xml https://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hcgxrbs&Action=More+Options&Action=Parameter+Search&ConeAdd=1 CHANDRA 0.0166666666666667 X-ray public hcgxrbs X-Ray Observations of Compact Group Galaxies name Source Designation meta.id;meta.main char nullable ra Right Ascension degree pos.eq.ra;meta.main double nullable dec Declination degree pos.eq.dec;meta.main double nullable sfr Star Formation Rate Solar_Mass/yr phys.SFR double nullable mass Stellar Mass Solar_Mass phys.mass double nullable lx Total X-Ray Point Source Luminosity in the 0.5-8.0keV Chandra Band erg/s phys.luminosity;em.X-ray double nullable lx_pos_err Upper Uncertainty for Total X-Ray Point Source Luminosity erg/s stat.error;phys.luminosity;em.X-ray double nullable lx_neg_err Lower Uncertainty for Total X-Ray Point Source Luminosity erg/s stat.error;phys.luminosity;em.X-ray double nullable num_detections Number of Detected Point Sources meta.number short nullable fx_max Upper Limit for Flux erg/s/cm^2 phot.flux;em.X-ray;stat.max double nullable h1_prob Probability of Measuring a Total Galaxy Luminosity >= Observed Value stat.fit.goodness double nullable bii Galactic Latitude degree pos.galactic.lat double nullable mass_error Uncertainty in Stellar Mass Solar_Mass stat.error;phys.mass double nullable cg_prob Probability That Source within the Galaxy Boundaries Belongs to the CG Galaxy stat.fit.goodness double nullable h2_prob Probability of Measuring a Total Galaxy Luminosity >= Observed Value stat.fit.goodness double nullable lx_fraction Fraction of the Total Luminosity Contributed by a Central Source phys.luminosity;arith.ratio double nullable sfr_error Uncertainty in Star Formation Rate Solar_Mass/yr stat.error;phys.SFR double nullable morph_type Morphological Hubble Type Based on Best-Fitting SED Template src.morph.type char nullable lx_max Upper Limit for 0.5-8.0keV Luminosity erg/s phys.luminosity;em.X-ray;stat.max double nullable lii Galactic Longitude degree pos.galactic.lon double nullable "__x_ra_dec" System unit vector column double nullable "__y_ra_dec" System unit vector column double nullable "__z_ra_dec" System unit vector column double nullable "__row" System index column char nullable