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Young Accreting Compact Objects in M31: The Combined Power of NuSTAR, Chandra, and Hubble

Lazzarini, M. and Hornschemeier, A. E. and Williams, B. F. and Wik, D. and Vulic, N. and Yukita, M. and Zezas, A. and Lewis, A. R. and Durbin, M. and Ptak, A. and Bodaghee, A. and Lehmer, B. D. and Antoniou, V. and Maccarone, T. (2018) Young Accreting Compact Objects in M31: The Combined Power of NuSTAR, Chandra, and Hubble. Astrophysical Journal, 862 (1). Art. No. 28. ISSN 1538-4357. doi:10.3847/1538-4357/aacb2a.

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We present 15 high-mass X-ray binary (HMXB) candidates in the disk of M31 for which we are able to infer compact object type, spectral type of the donor star, and age using multiwavelength observations from NuSTAR, Chandra, and the Hubble Space Telescope. The hard X-ray colors and luminosities from NuSTAR permit the tentative classification of accreting X-ray binary systems by compact object type, distinguishing black hole from neutron star systems. We find hard-state black holes, pulsars, and non-magnetized neutron stars associated with optical point-source counterparts with similar frequency. We also find nine non-magnetized neutron stars coincident with globular clusters and an equal number of pulsars with and without point-source optical counterparts. We perform spectral energy distribution (SED) fitting for the most likely optical counterparts to the HMXB candidates, finding seven likely high-mass stars and one possible red helium-burning star. The remaining seven HMXB optical counterparts have poor SED fits, so their companion stars remain unclassified. Using published star formation histories, we find that the majority of HMXB candidates—X-ray sources with UV-bright point-source optical counterpart candidates—are found in regions with star formation bursts less than 50 Myr ago, and three are associated with young stellar ages (<10 Myr). This is consistent with similar studies of HMXB populations in the Magellanic Clouds, M33, NGC 300, and NGC 2403.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Lazzarini, M.0000-0003-3252-352X
Hornschemeier, A. E.0000-0001-8667-2681
Williams, B. F.0000-0002-7502-0597
Wik, D.0000-0001-8952-676X
Vulic, N.0000-0001-7855-8336
Yukita, M.0000-0001-6366-3459
Zezas, A.0000-0001-8952-676X
Lewis, A. R.0000-0002-5238-0282
Ptak, A.0000-0001-5655-1440
Bodaghee, A.0000-0002-7315-3732
Lehmer, B. D.0000-0003-2192-3296
Antoniou, V.0000-0001-7539-1593
Maccarone, T.0000-0003-0976-4755
Additional Information:© 2018 The American Astronomical Society. Received 2018 March 19; revised 2018 May 31; accepted 2018 June 5; published 2018 July 19. We thank Antara Basu-Zych for useful discussions that led to an improvement of the paper. We acknowledge funding through Chandra program award GO5-17077Z (PI Hornschemeier). Support for this work was provided in part by Chandra Award Number GO5-16085X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060.
Subject Keywords:galaxies: individual (M31) – pulsars: general – stars: black holes – stars: neutron – X-rays: binaries – X-rays: galaxies
Issue or Number:1
Record Number:CaltechAUTHORS:20180613-100106697
Persistent URL:
Official Citation:M. Lazzarini et al 2018 ApJ 862 28
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:87055
Deposited By: Joy Painter
Deposited On:13 Jun 2018 17:58
Last Modified:15 Nov 2021 20:44

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