J/AJ/146/135ivo://CDS.VizieR/J/AJ/146/135doi:10.26093/cds/vizier.51460135CDSAgar J.R.R.Barmby P.2017-09-19T14:24:13Z2014-07-21T13:27:35ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxiesglobular-star-clustersx-ray-binary-starsThe Andromeda galaxy, M31, has several times the number of globular clusters found in the Milky Way. It contains a correspondingly larger number of low-mass X-ray binaries (LMXBs) associated with globular clusters, and as such can be used to investigate the cluster properties that lead to X-ray binary formation. The best tracer of the spatial structure of M31 globulars is the high-resolution imaging available from the Hubble Space Telescope (HST), and we have used HST data to derive structural parameters for 29 LMXB-hosting M31 globular clusters. These measurements are combined with structural parameters from the literature for a total of 41 (of 50 known) LMXB clusters and a comparison sample of 65 non-LMXB clusters. Structural parameters measured in blue bandpasses are found to be slightly different (smaller core radii and higher concentrations) than those measured in red bandpasses; this difference is enhanced in LMXB clusters and could be related to stellar population differences. Clusters with LMXBs show higher collision rates for their mass compared to clusters without LMXBs, and collision rates estimated at the core radius show larger offsets than rates estimated at the half-light radius. These results are consistent with the dynamical formation scenario for LMXBs. A logistic regression analysis finds that, as expected, the probability of a cluster hosting an LMXB increases with increasing collision rate and proximity to the galaxy center. The same analysis finds that probability of a cluster hosting an LMXB decreases with increasing cluster mass at a fixed collision rate, although we caution that this could be due to sample selection effects. Metallicity is found to be a less important predictor of LMXB probability than collision rate, mass, or distance, even though LMXB clusters have a higher metallicity on average. This may be due to the interaction of location and metallicity: a sample of M31 LMXBs with a greater range in galactocentric distance would likely contain more metal-poor clusters and make it possible to disentangle the two effects.2013AJ....146..135Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/146/135CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/146/20 : Structural parameters for 79 GCs in M31 (Wang+, 2013)J/A+A/531/A155 : HST photometry in six M31 globular clusters (Perina+, 2011)J/AJ/141/61 : Star clusters in M31. II. (Caldwell+, 2011)J/ApJ/725/200 : An updated catalog of M31 globular-like clusters (Fan+, 2010)J/AJ/137/94 : Star clusters in M31 (Caldwell+, 2009)J/MNRAS/392/L55 : GCs in M31 from K-band photometry (Peacock+, 2009)J/A+A/471/127 : New globular clusters in M 31 (Galleti+, 2007)J/AJ/133/2764 : M31 globular clusters structural parameters (Barmby+, 2007)J/ApJS/161/304 : Star clusters in the MW and satellites (McLaughlin+, 2005)J/A+A/373/63 : M31 second ROSAT PSPC survey (Supper+, 2001)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/146/135https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/146/135http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/146/135https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/146/135https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/146/135http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/146/135GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/146/135/table1 (New HST data for 29 globular clusters with Low-Mass X-ray Binaries (LMXB))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/146/135/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/146/135/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/146/135/table1?GETtext/xml+votable180.050000true10.577720841.2339250.0055555555555555566/2623 2666 2705 2709 6031https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/146/135?format=asciiOpticaldefaultJ/AJ/146/135/table1New HST data for 29 globular clusters with Low-Mass X-ray Binaries (LMXB)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGlobular cluster name (G1)meta.id;meta.maincharprimaryFDisplay fitting results from Table3 (in all observed filters)meta.ref.urlcharCamCamera (ACS or WFPC2)meta.id;instrcharFltFilter (F336W, F435W, F475W, F555W, F606W, F814W)meta.id;instr.filtercharNfNumber of filters in which this cluster was observedmeta.numberintnullableExpExposure timestime.duration;obs.exposureintE(B-V)Reddening (1)magphot.color.excessfloat(V-m)0Extinction-corrected color (2)magphot.colorfloat[Fe/H]Metallicity (3)log(Sun)phys.abund.ZfloatM/LvRatio of total mass to visual luminosity (4)solMass/solLumphys.composition.massLightRatiofloatRBCCross-match with the Revised Bologna Catalog of M31 Globular Clusters (RBC; Galleti et al., 2007, cat. J/A+A/471/127)meta.ref.urlintnullableSimbadNameSimbad column added by the CDSmeta.idchar_RAPositions from the SIMBAD database (right ascension part)degpos.eq.ra;meta.main_DEPositions from the SIMBAD database (declination part)degpos.eq.dec;meta.mainJ/AJ/146/135/table3Model-fitting resultsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGlobular cluster name (G1)meta.id;meta.maincharCamCamera (WFC or WFPC)meta.id;instrcharFltFilter (F336, F435, F475, F555, F606, F814)meta.id;instr.filtercharNpNumber of pointsmeta.numberintModModel code (1)meta.id;stat.fitcharchi2Unreduced {Chi}^2^ of best-fitting modelstat.fit.chi2floatIbkgModel-fit background intensitysolLum.pc**-2instr.backgroundfloate_IbkgUncertainty in IbkgsolLum.pc**-2stat.errorfloatW0? Model-fit central potentialarith.factor;phys.gravityfloatnullableE_W0? Upper 68% confidence interval in W0stat.error;stat.maxfloatnullablee_W0? Lower 68% confidence interval in W0stat.errorfloatnullablecModel-fit concentration (2)stat.fit.paramfloatE_cUpper 68% confidence interval in cstat.error;stat.maxfloate_cLower 68% confidence interval in cstat.errorfloatmu0Model-fit central surface brightness (3)mag.arcsec**-2phot.mag.sbfloatE_mu0Upper 68% confidence interval in mu0mag.arcsec**-2stat.error;stat.maxfloate_mu0Lower 68% confidence interval in mu0mag.arcsec**-2stat.errorfloatlogr0Log of fitted angular scale radiuslog(arcsec)phys.angSize;srcfloatE_logr0Upper 68% confidence interval in logr0log(arcsec)stat.error;stat.maxfloate_logr0Lower 68% confidence interval in logr0log(arcsec)stat.errorfloatlogR0Log of physical scale radiuspcphys.size.radius;instr.scalefloatE_logR0Upper 68% confidence interval in logR0pcstat.error;stat.maxfloate_logR0Lower 68% confidence interval in logR0pcstat.errorfloat