The Megasecond Chandra X-Ray Visionary Project Observation of NGC 3115. III. Luminosity Functions of LMXBS and Dependence on Stellar Environments

Dacheng Lin, University of New Hampshire, Durham
Jimmy A. Irwin, University of Alabama - Tuscaloosa
Ka-Wah Wong, Minnesota State University Mankato
Zachary G. Jennings, University of California Observatories
Jeroen Homan, MIT Kavli Institute for Astrophysics and Space Research
Aaron J. Romanowsky, San Jose State University
Jay Strader, Michigan State University
Jean P. Brodie, University of California Observatories
Gregory R. Sivakoff, University of Alberta
Ronald A. Remillard, MIT Kavli Institute for Astrophysics and Space Research


We studied the X-ray luminosity function (XLF) of low-mass X-ray binaries (LMXBs) in the nearby lenticular galaxy NGC 3115, using the Megasecond Chandra X-ray Visionary Project Observation. With a total exposure time of ~1.1 Ms, we constructed the XLF down to a limiting luminosity of ~1036 erg s−1, which is much deeper than that typically reached for other early-type galaxies. We found significant flattening of the overall LMXB XLF from dN/dLL−2.2±0.4 above 5.5 × 1037 erg s−1 to dN/dLL−1.0±0.1 below it, although we could not rule out a fit with a higher break at ~1.6 × 1038 erg s−1. We also found evidence that the XLF of LMXBs in globular clusters (GCs) is overall flatter than that of field LMXBs. Thus, our results for this galaxy do not support the idea that all LMXBs are formed in GCs. The XLF of field LMXBs seems to show spatial variation, with the XLF in the inner region of the galaxy being flatter than that in the outer region, probably due to contamination of LMXBs from undetected and/or disrupted GCs in the inner region. The XLF in the outer region is probably the XLF of primordial field LMXBs, exhibiting dN/dLL−1.2±0.1 up to a break close to the Eddington limit of neutron star LMXBs (~1.7 × 1038 erg s−1). The break of the GC LMXB XLF is lower, at ~1.1 × 1037 erg s−1. We also confirm previous findings that the metal-rich/red GCs are more likely to host LMXBs than the metal-poor/blue GCs, which is more significant for more luminous LMXBs, and that more massive GCs are more likely to host LMXBs.