A Lower Mass Estimate for PSR J0348+0432 Based on CHIME/Pulsar Precision Timing
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| Autores principales: | , , , , , , , , , , |
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| Formato: | Preprint |
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2024
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| _version_ | 1866929614845116416 |
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| author | Saffer, Alexander Fonseca, Emmanuel Ransom, Scott Stairs, Ingrid Lynch, Ryan Good, Deborah Masui, Kiyoshi W. McKee, James W. Meyers, Bradley W. Patil, Swarali Shivraj Tan, Chia Min |
| author_facet | Saffer, Alexander Fonseca, Emmanuel Ransom, Scott Stairs, Ingrid Lynch, Ryan Good, Deborah Masui, Kiyoshi W. McKee, James W. Meyers, Bradley W. Patil, Swarali Shivraj Tan, Chia Min |
| contents | 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 $σ$ 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2412_02850 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | A Lower Mass Estimate for PSR J0348+0432 Based on CHIME/Pulsar Precision Timing Saffer, Alexander Fonseca, Emmanuel Ransom, Scott Stairs, Ingrid Lynch, Ryan Good, Deborah Masui, Kiyoshi W. McKee, James W. Meyers, Bradley W. Patil, Swarali Shivraj Tan, Chia Min High Energy Astrophysical Phenomena 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 $σ$ 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. |
| title | A Lower Mass Estimate for PSR J0348+0432 Based on CHIME/Pulsar Precision Timing |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2412.02850 |