Investigating cannibalistic millisecond pulsar binaries using MESA: New constraints from pulsar spin and mass evolution

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Volume 693 (January 2025)

A&A, 693 (2025) A314

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Table 1.

Observed and estimated properties of the two observed huntsmen spiders.

Huntsman name	M_c, min	P_orb	P_spin	M_NS	M_c	e
1FGL J1417.7–440	0.2 M_⊙⁽¹⁾	5.37 d ⁽³⁾	2.66 ms ⁽¹⁾	$1 . 62_{- 0.17}^{+ 0.43} M_{⊙}$ $1.62^{+0.43}_{-0.17}\,\mathrm{M}_\odot$ ⁽²⁾	$0 . 28_{- 0.03}^{+ 0.07} M_{⊙}$ $0.28^{+0.07}_{-0.03}\,\mathrm{M}_\odot$ ⁽²⁾	0.0
2FGL J0846.0+2820	–	8.13 d ⁽⁴⁾	–	$1 . 96_{- 0.41}^{+ 0.41} M_{⊙}$ $1.96^{+0.41}_{-0.41}\,\mathrm{M}_\odot$ ⁽⁴⁾	$0 . 77_{- 0.20}^{+ 0.20} M_{⊙}$ $0.77^{+0.20}_{-0.20}\,\mathrm{M}_\odot$ ⁽⁴⁾	0.06 ⁽⁴⁾

Notes. The term M_c, min is the minimum mass, calculated assuming a pulsar mass of 1.4 M_⊙ and inclination of 90°; P_orb is the orbital period; P_spin is the observed pulsar spin; M_NS is the estimated pulsar mass; M_c is the companion mass observed from Fermi-LAT; and e is the observed eccentricity.

⁽¹⁾

Camilo et al. (2016),

⁽²⁾

Swihart et al. (2018),

⁽³⁾

Strader et al. (2015),

⁽⁴⁾

Swihart et al. (2017).

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