A Caltech Library Service

Identification of an X-Ray Pulsar in the BeXRB System IGR J18219−1347

O'Connor, B. and Göğüş, E. and Huppenkothen, D. and Kouveliotou, C. and Gorgone, N. and Townsend, L. J. and Calamida, A. and Fruchter, A. and Buckley, D. A. H. and Baring, M. G. and Kennea, J. A. and Younes, G. and Arzoumanian, Z. and Bellm, E. and Cenko, S. B. and Gendreau, K. and Granot, J. and Hailey, C. and Harrison, F. and Hartmann, D. and Kaper, L. and Kutyrev, A. and Slane, P. O. and Stern, D. and Troja, E. and van der Horst, A. J. and Wijers, R. A. M. J. and Woudt, P. (2022) Identification of an X-Ray Pulsar in the BeXRB System IGR J18219−1347. Astrophysical Journal, 927 (2). Art. No. 139. ISSN 0004-637X. doi:10.3847/1538-4357/ac5032.

[img] PDF - Published Version
Creative Commons Attribution.

[img] PDF - Submitted Version
See Usage Policy.


Use this Persistent URL to link to this item:


We report on observations of the candidate Be/X-ray binary (BeXRB) IGR J18219−1347 with the Swift/X-ray Telescope, the Nuclear Spectroscopic Telescope ARray, and the Neutron Star Interior Composition Explorer during Type-I outbursts in 2020 March and June. Our timing analysis revealed the spin period of a neutron star with P_(spin) = 52.46 s. This periodicity, combined with the known orbital period of 72.4 days, indicates that the system is a BeXRB. Furthermore, by comparing the spectral energy distribution of the infrared counterpart to that of known BeXRBs, we confirm this classification and set a distance of approximately 10–15 kpc for the source. The broadband X-ray spectrum (1.5–50 keV) of the source is described by an absorbed power law with a photon index Γ ∼ 0.5 and a cutoff energy at ∼13 keV.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
O'Connor, B.0000-0002-9700-0036
Göğüş, E.0000-0002-5274-6790
Huppenkothen, D.0000-0002-1169-7486
Kouveliotou, C.0000-0003-1443-593X
Gorgone, N.0000-0002-1653-6411
Townsend, L. J.0000-0001-9788-3345
Calamida, A.0000-0002-0882-7702
Fruchter, A.0000-0002-6652-9279
Buckley, D. A. H.0000-0002-7004-9956
Baring, M. G.0000-0003-4433-1365
Kennea, J. A.0000-0002-6745-4790
Younes, G.0000-0002-7991-028X
Bellm, E.0000-0001-8018-5348
Cenko, S. B.0000-0003-1673-970X
Gendreau, K.0000-0001-7115-2819
Granot, J.0000-0001-8530-8941
Hailey, C.0000-0002-3681-145X
Harrison, F.0000-0003-2992-8024
Hartmann, D.0000-0002-8028-0991
Kaper, L.0000-0001-8025-8981
Kutyrev, A.0000-0002-2715-8460
Slane, P. O.0000-0002-6986-6756
Stern, D.0000-0003-2686-9241
Troja, E.0000-0002-1869-7817
van der Horst, A. J.0000-0001-9149-6707
Wijers, R. A. M. J.0000-0002-3101-1808
Woudt, P.0000-0002-6896-1655
Additional Information:© 2022 The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 November 24; revised 2022 January 21; accepted 2022 January 24; published 2022 March 10. The authors acknowledge useful discussions with Matteo Bachetti, Tomaso Belloni, and Oleg Kargaltsev. B.O., C.K., and N.G. acknowledge supported under NASA Grants 80NSSC20K0389 and 80NSSC19K091. L.J.T. is supported by the South African National Research Foundation. J.G. acknowledges support by the ISF-NSFC joint research program (grant No. 3296/19). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Space Science Data Center (SSDC, Italy) and the California Institute of Technology (Caltech, USA). This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO. These results also made use of Lowell Observatory's Lowell Discovery Telescope (LDT), formerly the Discovery Channel Telescope. Lowell operates the LDT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the LDT was provided by Discovery Communications. LMI was built by Lowell Observatory using funds from the National Science Foundation (AST-1005313). Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT) under program 2018-2-LSP-001. We additionally made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). Facilities: Swift - Swift Gamma-Ray Burst Mission, NuSTAR - , NICER - , SALT - , LDT - , UKIRT - , ZTF - , PS1. - Software: HEASoft v6.27.2, XRTDAS, NuSTARDAS v1.9.2, NICERDAS v7a, XSPEC v12.11.0 (Arnaud 1996), IRAF (Tody 1986), DAOPHOT (Stetson 1987), SExtractor (Bertin & Arnouts 1996), Swarp (Bertin 2010), SCAMP (Bertin 2006), (Lang et al. 2010), Stingray (Huppenkothen et al. 2019), Astropy (Astropy Collaboration et al. 2013).
Group:Astronomy Department, Space Radiation Laboratory, NuSTAR
Funding AgencyGrant Number
National Research Foundation (South Africa)UNSPECIFIED
Israel Science FoundationUNSPECIFIED
National Natural Science Foundation of China3296/19
Southern African Large Telescope (SALT)2018-2-LSP-001
Subject Keywords:X-ray astronomy; High mass x-ray binary stars; Pulsars; Neutron stars
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: X-ray astronomy (1810); High mass x-ray binary stars (733); Pulsars (1306); Neutron stars (1108)
Record Number:CaltechAUTHORS:20220119-233939590
Persistent URL:
Official Citation:B. O'Connor et al 2022 ApJ 927 139
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:113003
Deposited By: George Porter
Deposited On:20 Jan 2022 20:23
Last Modified:22 Mar 2022 17:34

Repository Staff Only: item control page