Kavli Affiliate: Kiyoshi W. Masui
| First 5 Authors: Alexander Saffer, Emmanuel Fonseca, Scott Ransom, Ingrid Stairs, Ryan Lynch
| Summary:
The binary pulsar J0348+0432 was previously shown to have a mass of
approximately 2,${rm M_odot}$, based on the combination of radial-velocity
and model-dependent mass parameters derived from high-resolution optical
spectroscopy of its white-dwarf companion. We present follow-up timing
observations that combine archival observations with data acquired by the
Canadian Hydrogen Intensity Mapping Experiment (CHIME) pulsar instrument. We
find that the inclusion of CHIME/Pulsar data yields an improved measurement of
general-relativistic orbital decay in the system that falls within 1.2 $sigma$
of the original values published by Antoniadis et al. (2013) while being
roughly 6 times more precise due to the extended baseline. When we combine this
new orbital evolution rate with the mass ratio determined from optical
spectroscopy, we determine a pulsar mass of 1.806(37),${rm M_odot}$. For the
first time for this pulsar, timing alone significantly constrains the pulsar
mass. We explain why the new mass for the pulsar is $10%$ lower and discuss
how the mis-modeling of the initial observations of the white dwarf companion
likely led to an inaccurate determination of the pulsar mass.
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