High-cadence Timing of Binary Pulsars with CHIME
We performed near-daily observations of the binary pulsars PSR J0218+4232, PSR J1518+4904, and PSR J2023+2853 with the Canadian Hydrogen Intensity Mapping Experiment (CHIME). For the first time, we detected the Shapiro time delay in all three pulsar binary systems, using only 2–4 yr of CHIME/Pulsar...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad28b2 |
| _version_ | 1797193767419117568 |
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| author | Chia Min Tan Emmanuel Fonseca Kathryn Crowter Fengqiu Adam Dong Victoria M. Kaspi Kiyoshi W. Masui James W. McKee Bradley W. Meyers Scott M. Ransom Ingrid H. Stairs |
| author_facet | Chia Min Tan Emmanuel Fonseca Kathryn Crowter Fengqiu Adam Dong Victoria M. Kaspi Kiyoshi W. Masui James W. McKee Bradley W. Meyers Scott M. Ransom Ingrid H. Stairs |
| author_sort | Chia Min Tan |
| collection | DOAJ |
| description | We performed near-daily observations of the binary pulsars PSR J0218+4232, PSR J1518+4904, and PSR J2023+2853 with the Canadian Hydrogen Intensity Mapping Experiment (CHIME). For the first time, we detected the Shapiro time delay in all three pulsar binary systems, using only 2–4 yr of CHIME/Pulsar timing data. We measured the pulsar masses to be ${1.49}_{-0.20}^{+0.23}$ M _⊙ , ${1.470}_{-0.034}^{+0.030}$ M _⊙ , and ${1.50}_{-0.38}^{+0.49}$ M _⊙ , respectively. The companion mass to PSR J0218+4232 was found to be ${0.179}_{-0.016}^{+0.018}$ M _⊙ . We constrained the mass of the neutron star companion of PSR J1518+4904 to be ${1.248}_{-0.029}^{+0.035}$ M _⊙ , using the observed apsidal motion as a constraint on the mass estimation. The binary companion to PSR J2023+2853 was found to have a mass of ${0.93}_{-0.14}^{+0.17}$ M _⊙ ; in the context of the near-circular orbit, this mass estimate suggests that the companion to PSR J2023+2853 is likely a high-mass white dwarf. By comparing the timing model obtained for PSR J0218+4232 with previous observations, we found a significant change in the observed orbital period of the system of $\dot{{P}_{{\rm{b}}}}=0.14(2)\times {10}^{-12}$ ; we determined that this variation arises from “Shklovskii acceleration” due to the relative motion of the binary system, and used this measurement to estimate a distance of d = (6.7 ± 1.0) kpc to PSR J0218+4232. This work demonstrates the capability of high-cadence observations, enabled by the CHIME/Pulsar system, to detect and refine general-relativistic effects of binary pulsars over short observing timescales. |
| first_indexed | 2024-04-24T05:45:37Z |
| format | Article |
| id | doaj.art-35a103da4daa40bd89c8460b990d6085 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-04-24T05:45:37Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-35a103da4daa40bd89c8460b990d60852024-04-23T14:48:08ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0196612610.3847/1538-4357/ad28b2High-cadence Timing of Binary Pulsars with CHIMEChia Min Tan0https://orcid.org/0000-0001-7509-0117Emmanuel Fonseca1https://orcid.org/0000-0001-8384-5049Kathryn Crowter2https://orcid.org/0000-0002-1529-5169Fengqiu Adam Dong3https://orcid.org/0000-0003-4098-5222Victoria M. Kaspi4https://orcid.org/0000-0001-9345-0307Kiyoshi W. Masui5https://orcid.org/0000-0002-4279-6946James W. McKee6https://orcid.org/0000-0002-2885-8485Bradley W. Meyers7https://orcid.org/0000-0001-8845-1225Scott M. Ransom8https://orcid.org/0000-0001-5799-9714Ingrid H. Stairs9https://orcid.org/0000-0001-9784-8670Department of Physics, McGill University , 3600 rue University, Montréal, QC H3A 2T8, Canada; The Trottier Space Institute at McGill , 3550 rue University, Montréal, QC H3A 2A7, Canada; International Centre for Radio Astronomy Research, Curtin University , Bentley, WA 6102, AustraliaDepartment of Physics and Astronomy, West Virginia University , Morgantown, WV 26506-6315, USA; Center for Gravitational Waves and Cosmology , Chestnut Ridge Research Building, Morgantown, WV 26505, USADepartment of Physics and Astronomy, University of British Columbia , 6224 Agricultural Road, Vancouver, BC V6T 1Z1, CanadaDepartment of Physics and Astronomy, University of British Columbia , 6224 Agricultural Road, Vancouver, BC V6T 1Z1, CanadaDepartment of Physics, McGill University , 3600 rue University, Montréal, QC H3A 2T8, Canada; The Trottier Space Institute at McGill , 3550 rue University, Montréal, QC H3A 2A7, CanadaMIT Kavli Institute for Astrophysics and Space Research , Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA; Department of Physics, Massachusetts Institute of Technology , 77 Massachusetts Avenue, Cambridge, MA 02139, USAE.A. Milne Centre for Astrophysics, University of Hull , Cottingham Road, Kingston-upon-Hull, HU6 7RX, UK; Centre of Excellence for Data Science, Artificial Intelligence and Modelling (DAIM), University of Hull , Cottingham Road, Kingston-upon-Hull, HU6 7RX, UKInternational Centre for Radio Astronomy Research, Curtin University , Bentley, WA 6102, AustraliaNational Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USADepartment of Physics and Astronomy, University of British Columbia , 6224 Agricultural Road, Vancouver, BC V6T 1Z1, CanadaWe performed near-daily observations of the binary pulsars PSR J0218+4232, PSR J1518+4904, and PSR J2023+2853 with the Canadian Hydrogen Intensity Mapping Experiment (CHIME). For the first time, we detected the Shapiro time delay in all three pulsar binary systems, using only 2–4 yr of CHIME/Pulsar timing data. We measured the pulsar masses to be ${1.49}_{-0.20}^{+0.23}$ M _⊙ , ${1.470}_{-0.034}^{+0.030}$ M _⊙ , and ${1.50}_{-0.38}^{+0.49}$ M _⊙ , respectively. The companion mass to PSR J0218+4232 was found to be ${0.179}_{-0.016}^{+0.018}$ M _⊙ . We constrained the mass of the neutron star companion of PSR J1518+4904 to be ${1.248}_{-0.029}^{+0.035}$ M _⊙ , using the observed apsidal motion as a constraint on the mass estimation. The binary companion to PSR J2023+2853 was found to have a mass of ${0.93}_{-0.14}^{+0.17}$ M _⊙ ; in the context of the near-circular orbit, this mass estimate suggests that the companion to PSR J2023+2853 is likely a high-mass white dwarf. By comparing the timing model obtained for PSR J0218+4232 with previous observations, we found a significant change in the observed orbital period of the system of $\dot{{P}_{{\rm{b}}}}=0.14(2)\times {10}^{-12}$ ; we determined that this variation arises from “Shklovskii acceleration” due to the relative motion of the binary system, and used this measurement to estimate a distance of d = (6.7 ± 1.0) kpc to PSR J0218+4232. This work demonstrates the capability of high-cadence observations, enabled by the CHIME/Pulsar system, to detect and refine general-relativistic effects of binary pulsars over short observing timescales.https://doi.org/10.3847/1538-4357/ad28b2PulsarsObservational astronomyInterferometers |
| spellingShingle | Chia Min Tan Emmanuel Fonseca Kathryn Crowter Fengqiu Adam Dong Victoria M. Kaspi Kiyoshi W. Masui James W. McKee Bradley W. Meyers Scott M. Ransom Ingrid H. Stairs High-cadence Timing of Binary Pulsars with CHIME The Astrophysical Journal Pulsars Observational astronomy Interferometers |
| title | High-cadence Timing of Binary Pulsars with CHIME |
| title_full | High-cadence Timing of Binary Pulsars with CHIME |
| title_fullStr | High-cadence Timing of Binary Pulsars with CHIME |
| title_full_unstemmed | High-cadence Timing of Binary Pulsars with CHIME |
| title_short | High-cadence Timing of Binary Pulsars with CHIME |
| title_sort | high cadence timing of binary pulsars with chime |
| topic | Pulsars Observational astronomy Interferometers |
| url | https://doi.org/10.3847/1538-4357/ad28b2 |
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