PSR J1227−6208 and its massive white dwarf companion: Pulsar emission analysis, timing update, and mass measurements

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Volume 690 (October 2024)

A&A, 690 (2024) A253

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This article has an erratum: [https://doi.org/10.1051/0004-6361/202453093e]

Table 5.

Orbital Keplerian and PK parameters from the DDH TEMPO2/TempoNEST fits, and mass constraints from the DDGR χ² mapping fits.

Data set	Global	Multibeam	MeerKAT+UWL

Keplerian orbital parameters
Orbital period, P_b (days)	6.7210192(3)	6.72102(2)	6.7210189(4)
Orbital eccentricity, e	0.00114918(4)	0.0011492(4)	0.00114918(5)
Longitude of periastron, ω (deg)	27.090(9)	27.07(3)	27.211(12)
Projected semi-major axis of the pulsar orbit, x (ls)	23.200666(3)	23.20066(3)	23.200665(3)
Epoch of periastron, T₀ (MJD)	55 991.6995(2)	55 991.6991(6)	58 525.52384(9)

Post-Keplerian (PK) orbital parameters

Rate of periastron advance $\dot{ω}$ $\dot\omega$ (deg yr⁻¹)	0.01710(83)	0.0252(48)	0.0163(11)
Orthometric amplitude of Shapiro delay, h₃ (μs)	3.45(23)	3.5 ± 1.8	3.44(23)
Orthometric ratio of Shapiro delay, ς	0.858(27)	0.76(27)	0.853(30)
Derivative of orbital period, Ṗ_b (10⁻¹³ s s⁻¹)	3.7 ± 2.5	−10 ± 30	8 ± 40
Estimated Shklovskii contribution to Ṗ_b (10⁻¹³s s⁻¹)	∼4.5	...	...
Estimated Galactic potential contribution to Ṗ_b (10⁻¹³ s s⁻¹)	∼(−4.5)	...	...
Derivative of projected semi-major axis, ẋ (10⁻¹⁵ ls s⁻¹)	−9.1 ± 7.2	−88 ± 42	−17 ± 11
Estimated maximum proper motion contribution to ẋ, $\| {\dot{x}}_{\max} \|$ $\|\dot x_{\mathrm{max}}\|$ (10⁻¹⁵ ls s⁻¹)	∼4.2	...	...

Mass and orbital geometry constraints

Mass function, f_M (M_⊙)	0.297	0.297	0.297
Total mass, M_t (M_⊙)	$3 . 1_{- 0.8}^{+ 0.6}$ $3.1^{+0.6}_{-0.8}$	5.5 ± 1.7	$3 . 0_{- 1.0}^{+ 0.7}$ $3.0^{+0.7}_{-1.0}$
Companion mass, M_c (M_⊙)	1.39(5)	...	1.31(7)
Pulsar mass, M_p (M_⊙)	1.53(10)	...	1.37(14)
Inclination angle, i (deg)	78.4(7)	...	78.9(8)
Longitude of ascending note, Ω_a (deg)	86/266 $_{- 78}^{+ 76}$ $^{+76}_{-78}$	...	...

Notes. The non-GR contributions to Ṗ_b and ẋ are derived only from the global fit constraints, where the proper motion measurement is the most significant (Table 4). Mass and orbital geometry constraints are derived from the χ² mapping of DDGR solutions, as exposed in Sections 4.3, 4.4, and 4.5.

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