THE MEGASECOND CHANDRA X-RAY VISIONARY PROJECT OBSERVATION OF NGC 3115. III. LUMINOSITY FUNCTIONS OF LMXBS AND DEPENDENCE ON STELLAR ENVIRONMENTS
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Dacheng-2015-The megasecond chand.pdf
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604.58 KB
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Checksum (MD5)
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Author(s)
Lin, Dacheng
Irwin, Jimmy A.
Wong, Ka-Wah
Jennings, Zachary G.
Homan, Jeroen
Romanowsky, Aaron J.
Strader, Jay
Brodie, Jean P.
Sivakoff, Gregory R.
Remillard, Ronald A
Date Issued
July 2015
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Lin, Dacheng, Jimmy A. Irwin, Ka-Wah Wong, Zachary G. Jennings, Jeroen Homan, Aaron J. Romanowsky, Jay Strader, Jean P. Brodie, Gregory R. Sivakoff, and Ronald A. Remillard. “THE MEGASECOND CHANDRA X-RAY VISIONARY PROJECT OBSERVATION OF NGC 3115. III. LUMINOSITY FUNCTIONS OF LMXBS AND DEPENDENCE ON STELLAR ENVIRONMENTS.” The Astrophysical Journal 808, no. 1 (July 15, 2015): 20. © 2015 The American Astronomical Society
Version
Final published version
Abstract
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 ~10[superscript 36] erg s[superscript −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/dL ∝ L[superscript −2.2±0.4] above 5.5 × 10[superscript 37] erg s[superscript −1] to dN/dL ∝ L[superscript −1.0±0.1] below it, although we could not rule out a fit with a higher break at ~1.6 × 10[superscript 38] erg s[superscript −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/dL ∝ L[superscript −1.2±0.1] up to a break close to the Eddington limit of neutron star LMXBs (~1.7 × 10[superscript 38] erg s[superscript −1]). The break of the GC LMXB XLF is lower, at ~1.1 × 10[superscript 37] erg s[superscript −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.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-637X/808/1/20
