2018
DOI: 10.3847/1538-4357/aadcab
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A Multiwavelength View of the Neutron Star Binary 1FGL J1417.7–4402: A Progenitor to Canonical Millisecond Pulsars

Abstract: The Fermi γ-ray source 1FGL J1417.7-4407 (J1417) is a compact X-ray binary with a neutron star primary and a red giant companion in a ∼5.4 day orbit. This initial conclusion, based on optical and X-ray data, was confirmed when a 2.66 ms radio pulsar was found at the same location (and with the same orbital properties) as the optical/X-ray source. However, these initial studies found conflicting evidence about the accretion state and other properties of the binary. We present new optical, radio, and X-ray obser… Show more

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Cited by 42 publications
(38 citation statements)
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References 82 publications
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“…Using our best hot spot model, the inferred mass of the primary is M 1 = 1.77 +0.07 −0.03 , fairly massive for a typical neutron star, but fully consistent with the neutron star masses found in many redback MSPs (e.g., Kaplan et al 2013;Romani et al 2015b;Bellm et al 2016;Strader et al 2016;Sanchez & Romani 2017;Shahbaz et al 2017;Linares et al 2018;Swihart et al 2018). The secondary has a mass of M 2 = 0.51 +0.02 −0.01 , placing it in the highmass tail of the redback companion mass distribution (Strader et al 2019).…”
Section: Light Curve Fittingsupporting
confidence: 74%
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“…Using our best hot spot model, the inferred mass of the primary is M 1 = 1.77 +0.07 −0.03 , fairly massive for a typical neutron star, but fully consistent with the neutron star masses found in many redback MSPs (e.g., Kaplan et al 2013;Romani et al 2015b;Bellm et al 2016;Strader et al 2016;Sanchez & Romani 2017;Shahbaz et al 2017;Linares et al 2018;Swihart et al 2018). The secondary has a mass of M 2 = 0.51 +0.02 −0.01 , placing it in the highmass tail of the redback companion mass distribution (Strader et al 2019).…”
Section: Light Curve Fittingsupporting
confidence: 74%
“…For the remainder of this paper, we adopt this value for the distance. We note that this method has proven successful in the past at estimating reliable distances to similar systems (e.g., Swihart et al 2018). However, due to systematic effects such as the unknown metallicity and precise evolutionary state of the star, our estimate is likely uncertain by at least 20%.…”
Section: Distancementioning
confidence: 84%
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“…Nearly all of the spectra cover both Hα and Hβ, and while there is Balmer absorption present in most of the warmer spectra, there is no clear evidence for emission in any of the spectra. This is unlike some other redbacks, where the Balmer emission is attributed to a wind or shock (Swihart et al 2018).…”
Section: Soar Spectroscopymentioning
confidence: 58%
“…This system would have been in the disc state all the time, since our optical spectrum was taken recently and J0935 has been in its low-flux period since 2013 August based on the long-term γ-ray light curve. However it has been noted that several redbacks (and a black widow; PSR J1740−5340A, Sabbi et al 2003;3FGL J0838.8−2829, Halpern et al 2017; 2FGL J0846.0+2820, Swihart et al 2018;PSR J1048+2339, Strader et al 2019PSR J1311−3430, Romani et al 2015 can have strong variable emission lines and the lines (notable the Hα line) can appear to be double-peaked. This feature is interpreted as the indication of material driven from the heated side of a companion by the pulsar wind and possibly plus an intrabinary shock between the companion and the pulsar wind (Strader et al 2019 and references therein).…”
Section: Discussionmentioning
confidence: 99%