X-Ray Binary Luminosity Function Scaling Relations for Local Galaxies Based on Subgalactic Modeling

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dc.contributor.authorLehmer, Bret D.
dc.contributor.authorEufrasio, Rafael T.
dc.contributor.authorTzanavaris, Panayiotis
dc.contributor.authorBasu-Zych, Antara
dc.contributor.authorFragos, Tassos
dc.contributor.authorPrestwich, Andrea
dc.contributor.authorYukita, Mihoko
dc.contributor.authorZezas, Andreas
dc.contributor.authorHornschemeier, Ann E.
dc.contributor.authorPtak, Andrew
dc.date.accessioned2019-10-03T15:41:26Z
dc.date.available2019-10-03T15:41:26Z
dc.date.issued2019-06-26
dc.description.abstractWe present new Chandra constraints on the X-ray luminosity functions (XLFs) of X-ray binary (XRB) populations, as well as their scaling relations, for a sample of 38 nearby galaxies (D = 3.4–29 Mpc). Our galaxy sample is drawn primarily from the Spitzer Infrared Nearby Galaxies Survey (SINGS) and contains a wealth of Chandra (5.8 Ms total) and multiwavelength data, allowing for star formation rates (SFRs) and stellar masses (Må) to be measured on subgalactic scales. We divided the 2478 X-ray-detected sources into 21 subsamples in bins of specific SFR (sSFR ≡ SFR/Må) and constructed XLFs. To model the XLF dependence on sSFR, we fit a global XLF model, containing contributions from high-mass XRBs (HMXBs), low-mass XRBs (LMXBs), and background sources from the cosmic X-ray background that respectively scale with SFR, Må, and sky area. We find an HMXB XLF that is more complex in shape than previously reported and an LMXB XLF that likely varies with sSFR, potentially due to an age dependence. When applying our global model to XLF data for each individual galaxy, we discover a few galaxy XLFs that significantly deviate from our model beyond statistical scatter. Most notably, relatively low-metallicity galaxies have an excess of HMXBs above ≈10³⁸ erg s⁻¹ , and elliptical galaxies that have relatively rich populations of globular clusters (GCs) show excesses of LMXBs compared to the global model. Additional modeling of how the XRB XLF depends on stellar age, metallicity, and GC specific frequency is required to sufficiently characterize the XLFs of galaxies.en_US
dc.description.sponsorshipggestions, which have improved the quality of this paper. We gratefully acknowledge support from the National Aeronautics and Space Administration (NASA) Astrophysics Data Analysis Program (ADAP) grant NNX13AI48G (B.D.L., R.T.E., A.Z.) and Chandra X-ray Center grant GO8-19039X (B.D.L. and A. P.). A.Z. acknowledges funding from the European Union’s Seventh Framework Programme (FP/2007–2013)/ERC grant agreement No. 617001.en_US
dc.description.urihttps://iopscience.iop.org/article/10.3847/1538-4365/ab22a8en_US
dc.format.extent29 pagesen_US
dc.genrejournal articlesen_US
dc.identifierdoi:10.13016/m2kpyw-65gk
dc.identifier.citationBret D. Lehmer, et.al, X-Ray Binary Luminosity Function Scaling Relations for Local Galaxies Based on Subgalactic Modeling, The Astrophysical Journal Supplement Series, Volume 243, Number 1, https://doi.org/10.5281/zenodo.2875827en_US
dc.identifier.urihttps://doi.org/10.5281/zenodo.2875827
dc.identifier.urihttp://hdl.handle.net/11603/14970
dc.language.isoen_USen_US
dc.publisherThe American Astronomical Societyen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Center for Space Sciences and Technology
dc.relation.ispartofUMBC Faculty Collection
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.rights©2019 IOP Science
dc.subjectgalaxies: evolutionen_US
dc.subjectstars: formationen_US
dc.subjectX-rays: binariesen_US
dc.subjectX-rays: galaxiesen_US
dc.titleX-Ray Binary Luminosity Function Scaling Relations for Local Galaxies Based on Subgalactic Modelingen_US
dc.typeTexten_US

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