2019
DOI: 10.3847/1538-4357/ab125e
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PSR J1306-40: An X-Ray Luminous Redback with an Evolved Companion

Abstract: PSR J1306-40 is a millisecond pulsar binary with a non-degenerate companion in an unusually long ∼1.097 day orbit. We present new optical photometry and spectroscopy of this system, and model these data to constrain fundamental properties of the binary such as the component masses and distance. The optical data imply a minimum neutron star mass of 1.75 ± 0.09 M (1-sigma) and a high, nearly edge-on inclination. The light curves suggest a large hot spot on the companion, suggestive of a portion of the pulsar win… Show more

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Cited by 20 publications
(16 citation statements)
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“…As we can see from the Table, most of the RBs do exhibit high filling factor values. In the cases where F F has an estimation with F F < 1, the minimum value is of 0.70(6) for PSR J1431-4715 whereas the maximum value is of 0.92(6) for PSR J1306-40 (Swihart, et al 2019). 4 The minimum mass is computed considering a pulsar mass of 1.4 M ⊙ and an inclination of 90 o .…”
Section: Rbs Bwsmentioning
confidence: 99%
“…As we can see from the Table, most of the RBs do exhibit high filling factor values. In the cases where F F has an estimation with F F < 1, the minimum value is of 0.70(6) for PSR J1431-4715 whereas the maximum value is of 0.92(6) for PSR J1306-40 (Swihart, et al 2019). 4 The minimum mass is computed considering a pulsar mass of 1.4 M ⊙ and an inclination of 90 o .…”
Section: Rbs Bwsmentioning
confidence: 99%
“…Overall, the spectra of the optical source are consistent with that of a moderately cool, late-G to early-K type dwarf star (we reach similar conclusions from our light curve fitting in § 3.2). This spectral type is typical of redback secondaries (e.g., Bellm et al 2016;Linares et al 2018;Swihart et al 2019Swihart et al , 2020. There is no evidence for a second set of absorption lines in any of the optical spectra, as would be expected if this star was in a binary with a main sequence or evolved star, suggesting the companion is a compact object.…”
Section: Optical Spectroscopy and Orbital Parametersmentioning
confidence: 60%
“…When setting the companion mass equal to the approximate median redback companion mass (0.4 M ; Strader et al 2019), the best fit inclination is 81.9 +7.9 −12.1 , corresponding to a primary mass of 1.26 +0.15 −0.03 M . If the companion is on the more massive end of the redback distribution, approaching 0.6 M , such as the confirmed redback PSR J1306-40 (Keane et al 2018;Linares 2018;Swihart et al 2019) or the candidate redback 3FGL J0212.1+5320 (Li et al 2016;Shahbaz et al 2017), then the best fit inclination is i = 87.7 +2.3 −13.9 corresponding to M 1 = 1.43 +0.11 −0.01 M . These models are very good fits to the data and are nearly identical statistically, with χ 2 /d.o.f.…”
Section: Light Curve Modelingmentioning
confidence: 99%
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“…One approach that has been used successfully to identify MSP counterparts in the unassociated Fermi sources is to search for X-ray/optical matches inside the LAT error ellipses. X-rays in these binary systems are often produced by an intrabinary shock at the interface between the pulsar and companion winds (e.g., Gentile et al 2014;Romani & Sanchez 2016;Wadiasingh et al 2017), while the non-degenerate stellar companions typically display optical periodic variability due to tidal distortion of the secondary and/or irradiative heating of the tidally-locked companion surface (e.g., McConnell et al 2015;Sanchez & Romani 2017;Cho et al 2018;Swihart et al 2018;Draghis et al 2019;Swihart et al 2019;Yap et al 2019;Swihart et al 2021).…”
Section: Introductionmentioning
confidence: 99%