Swift/XRT Deep Galactic Plane Survey Discovery of a New Intermediate Polar Cataclysmic Variable, Swift J183920.1-045350

Creators: Gorgone, Nicholas M.; Woudt, Patrick A.; Buckley, David; Mukai, Koji; Kouveliotou, Chryssa; Huppenkothen, Daniela; Göğüş, Ersin; Bellm, Eric; Linford, Justin D.; van der Horst, Alexander J.; Baring, Matthew G.; Hartmann, Dieter; Barrett, Paul; Cenko, Bradley; Graham, Melissa; Granot, Johnathan; Harrison, Fiona; Kennea, Jamie; O'Connor, Brendan M.; Potter, Stephen; Stern, Daniel; Slane, Patrick; Wijers, Ralph

Abstract

We report on the Swift/XRT Deep Galactic Plane Survey discovery and multiwavelength follow-up observations of a new intermediate polar (IP) cataclysmic variable, Swift J183920.1-045350. A 449.7 s spin period is found in XMM-Newton and NuSTAR data, accompanied by a 459.9 s optical period that is most likely the synodic, or beat period, produced from a 5.6 hr orbital period. The orbital period is seen with moderate significance in independent long-baseline optical photometry observations taken with the ZTF and SAAO telescopes. We find that the X-ray pulse fraction of the source decreases with increasing energy. The X-ray spectra are consistent with the presence of an Fe emission line complex with both local and interstellar absorption. In the optical spectra, strong Hα, H i, He i, and He ii emission lines are observed, all common features in magnetic CVs. The source properties are thus typical of known IPs, with the exception of its estimated distance of 2.26_(−0.83)^(+1.93) kpc, which is larger than typical, extending the reach of the CV population in our Galaxy.

Additional Information

© 2021. The American Astronomical Society. Received 2021 April 10; revised 2021 September 10; accepted 2021 September 14; published 2021 December 24. The authors wish to thank Sylvia Rose Kowalski and Deena Mickelson for their roles in VLA data acquisition. They also thank Hannes Breytenbach for taking some of the SAAO data. P.A.W. acknowledges financial support from the University of Cape Town and the National Research Foundation. The SALT observations reported here were obtained through the SALT Large Science program 2018-2-LSP-001, with D.B. as PI, who also acknowledges support of the National Research Foundation. C.K. and N.G. acknowledge support under NASA grant 80NSSC19K0916 and Smithsonian Astrophysical Observatory grant GO9-20057X. B.O. is supported in part by the National Aeronautics and Space Administration through grants NNX16AB66G, NNX17AB18G, and 80NSSC20K0389. We thank the NRAO for the generous allocation of VLA time for our observations. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work has made use of data from the European Space Agency mission Gaia, processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions participating in the Gaia Multilateral Agreement. Facilities: Swift - Swift Gamma-Ray Burst Mission, NuSTAR - , XMM-Newton - , Chandra - , SALT - , SAAO - , Gaia - , Pan-STARRS - , ZTF - , APO - , VLA - . Software: casa (McMullin et al. 2007), heasoft (v6.23; Nasa High Energy Astrophysics Science Archive Research Center (Heasarc), 2014), ds9 (Joye & Mandel 2003; Smithsonian Astrophysical Observatory 2000), sas (v1.2; Gabriel et al. 2004), pyspeckit (Ginsburg & Mirocha 2011), stingray (Huppenkothen et al. 2019, v0.1;), ciao (Fruscione et al. 2006, v4.9;), pydis (Davenport 2019), pysalt package (Crawford et al. 2010), python 3 (Van Rossum & Drake 2009), iraf (Tody 1986, 1993), vartools (Hartman & Bakos 2016)

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