Discovery of a Large Population of Ultraluminous X-ray Sources in the Bulge-less Galaxies NGC 337 and ESO 501-23

Abstract

We have used Chandra observations of eight bulge-less disk galaxies to identify new ultraluminous X-ray source (ULX) candidates, study their high mass X-ray binary (HMXB) population, and search for low-luminosity active galactic nuclei (AGN). We report the discovery of 16 new ULX candidates in our sample of galaxies. Eight of these are found in the star forming galaxy NGC 337, none of which are expected to be background contaminants. The HMXB luminosity function of NGC 337 implies a star formation rate (SFR) of 6.8${}_{-3.5}^{+4.4}$ \msun\ yr${}^{-1}$, consistent at 1.5$\sigma$ with a recent state of the art SFR determination. We also report the discovery of a bright ULX candidate (X-1) in ESO 501-23. X-1's spectrum is well fit by an absorbed power law with $\Gamma =1.18_{-0.11}^{+0.19}$ and N${}_{\mathrm{H}}$ = 1.13${}_{-1.13}^{+7.07}\times 10^{20}$ cm${}^{-2}$, implying a 0.3-8 keV flux of $1.08_{-0.07}^{+0.05}\times 10^{-12}$ \esc. Its X-ray luminosity (L${}_X$) is poorly constrained due to uncertainties in the host galaxy's distance, but we argue that its spectrum implies L${}_X>10^{40}$ \es. An optical counterpart to this object may be present in HST imaging. We also identify ULX candidates in IC 1291, PGC 3853, NGC 5964 and NGC 2805. We find no evidence of nuclear activity in the galaxies in our sample, placing a flux upper limit of $4\times 10^{-15}$ \esc\ on putative AGN. Additionally, the type II-P supernova SN 2011DQ in NGC 337, which exploded 2 months before our X-ray observation, is undetected.

20 pages, 5 figures, 7 tables. A short Youtube video describing the main results of this paper can be found at: http://www.youtube.com/watch?v=5JnJC5ZqMpI&list=PL151C58BBFB53B1EA&index=1

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Cited by in corpus (2)

• On the radio properties of the intermediate-mass black hole candidate ESO 243-49 HLX-1
• An Optically Obscured AGN in a Low Mass, Irregular Dwarf Galaxy: A Multi-Wavelength Analysis of J1329+3234