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J/MNRAS/392/L55 Globular clusters in M31 from K-band photometry (Peacock+, 2009)

Wide field CAMera survey of M31 globular clusters: low-mass X-ray binaries. Peacock M.B., Maccarone T.J., Waters C.Z., Kundu A., Zepf S.E., Knigge C., Zurek D.R. <Mon. Not. R. Astron. Soc., 392, L55-L59 (2009)> =2009MNRAS.392L..55P
ADC_Keywords: Galaxies, nearby ; Clusters, globular ; Morphology ; Magnitudes Keywords: binaries: general - globular clusters: general - X-rays: binaries Abstract: We investigate the relationship between low-mass X-ray binaries (LMXBs) and globular clusters (GCs) using United Kingdom Infrared Telescope (UKIRT) observations of M31 and existing Chandra, XMM-Newton and ROSAT catalogues. By fitting King models to these data, we have estimated the structural parameters and stellar collision rates of 239 of its GCs. We show a highly significant trend between the presence of a LMXB and the stellar collision rate of a cluster. The stellar collision rate is found to be a stronger predictor of which clusters will host LMXBs than the host cluster mass. We argue that our results show that the stellar collision rate of the clusters is the fundamental parameter related to the production LMXBs. This is consistent with the formation of LMXBs through dynamical interactions with little direct dependence on the neutron star retention fraction or cluster mass. Description: To investigate the properties of the GCs in M31, we obtained K-band photometry using the Wide Field CAMera (WFCAM) on the United Kingdom Infrared Telescope (UKIRT) under the service program USERV1652. Our observations were taken on the nights of 2005 November 30 and 2007 August 06 with seeing of 0.85-1.00 and 0.6-0.8arcsec, respectively. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 70 239 K-band magnitude and structural parameters for 239 globular clusters (GCs) in M31
See also: J/A+A/471/127 : New globular clusters in M 31 (Galleti+, 2007) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Name Globular cluster name (1) 9- 15 F7.2 --- chi2/nu χ2 per degree of freedom for best fitting model (2) 17- 20 F4.1 --- W0 Central potential depth 22- 25 F4.2 --- c Core concentration index (log(rt/rc)) 27- 30 F4.1 mag Kmag K magnitude 32- 35 F4.2 pc rc Core radius (5) 37- 41 F5.2 pc rh Half-mass radius (5) 43- 47 F5.1 pc rt Total radius (5) 49- 53 F5.2 [solLum/pc3] logrhoc Central mass density 55- 59 F5.2 [-] logGamma Stellar collision rate 61- 67 A7 --- X X-ray source associated with GC flag (6) 69- 70 A2 --- Fl Flag based on residual (7)
Note (1): Names from Galleti et al., 2007, Cat. J/A+A/471/127 Note (2): usually dominated by stars in GC frame. Note (5): Assuming the distance of M31 to be 780kpc (McConnachie et al., 2005MNRAS.356..979M). Note (6): X-ray source associated with GC flag: 0 = no source S01 = Supper (2001, Cat. J/A+A/373/63), ROSAT T04 = Trudolyubov (2004ApJ...616..821T), Chandra & XMM Note (7): Flag as follows: 1 = good 2 = elliptical 3 = bad residual 4 = bright star in field 5 = asterism/no clear cluster 6 = unphysical parameters
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 05-May-2009
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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