An Unusual Pulse Shape Change Event in PSR J1713+0747 Observed with the Green Bank Telescope and CHIME

Ross J. Jennings; James M. Cordes; Shami Chatterjee; Maura A. McLaughlin; Paul B. Demorest; Zaven Arzoumanian; Paul T. Baker; Harsha Blumer; Paul R. Brook; Tyler Cohen; Fronefield Crawford; H. Thankful Cromartie; Megan E. DeCesar; Timothy Dolch; Elizabeth C. Ferrara; Emmanuel Fonseca; Deborah C. Good; Jeffrey S. Hazboun; Megan L. Jones; David L. Kaplan; Michael T. Lam; T. Joseph W. Lazio; Duncan R. Lorimer; Jing Luo; Ryan S. Lynch; James W. McKee; Dustin R. Madison; Bradley W. Meyers; Chiara M. F. Mingarelli; David J. Nice; Timothy T. Pennucci; Benetge B. P. Perera; Nihan S. Pol; Scott M. Ransom; Paul S. Ray; Brent J. Shapiro-Albert; Xavier Siemens; Ingrid H. Stairs; Daniel R. Stinebring; Joseph K. Swiggum; Chia Min Tan; Stephen R. Taylor; Sarah J. Vigeland; Caitlin A. Witt

doi:10.3847/1538-4357/ad2930

An Unusual Pulse Shape Change Event in PSR J1713+0747 Observed with the Green Bank Telescope and CHIME

Ross J. Jennings^*, James M. Cordes, Shami Chatterjee, Maura A. McLaughlin, Paul B. Demorest, Zaven Arzoumanian, Paul T. Baker, Harsha Blumer, Paul R. Brook, Tyler Cohen, Fronefield Crawford, H. Thankful Cromartie, Megan E. DeCesar, Timothy Dolch, Elizabeth C. Ferrara, Emmanuel Fonseca, Deborah C. Good, Jeffrey S. Hazboun, Megan L. Jones, David L. KaplanMichael T. Lam, T. Joseph W. Lazio, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, James W. McKee, Dustin R. Madison, Bradley W. Meyers, Chiara M. F. Mingarelli, David J. Nice, Timothy T. Pennucci, Benetge B. P. Perera, Nihan S. Pol, Scott M. Ransom, Paul S. Ray, Brent J. Shapiro-Albert, Xavier Siemens, Ingrid H. Stairs, Daniel R. Stinebring, Joseph K. Swiggum, Chia Min Tan, Stephen R. Taylor, Sarah J. Vigeland, Caitlin A. Witt

^*Corresponding author for this work

Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

The millisecond pulsar J1713+0747 underwent a sudden and significant pulse shape change between 2021 April 16 and 17 (MJDs 59320 and 59321). Subsequently, the pulse shape gradually recovered over the course of several months. We report the results of continued multifrequency radio observations of the pulsar made using the Canadian Hydrogen Intensity Mapping Experiment and the 100 m Green Bank Telescope in a 3 yr period encompassing the shape change event, between 2020 February and 2023 February. As of 2023 February, the pulse shape had returned to a state similar to that seen before the event, but with measurable changes remaining. The amplitude of the shape change and the accompanying time-of-arrival residuals display a strong nonmonotonic dependence on radio frequency, demonstrating that the event is neither a glitch (the effects of which should be independent of radio frequency, ν) nor a change in dispersion measure alone (which would produce a delay proportional to ν ⁻²). However, it does bear some resemblance to the two previous “chromatic timing events” observed in J1713+0747, as well as to a similar event observed in PSR J1643−1224 in 2015.

Original language	English
Article number	179
Number of pages	15
Journal	The Astrophysical Journal
Volume	964
Issue number	2
Early online date	29 Mar 2024
DOIs	https://doi.org/10.3847/1538-4357/ad2930
Publication status	Published - 1 Apr 2024

Bibliographical note

Acknowledgments:
The NANOGrav Physics Frontiers Center receives support from the National Science Foundation (NSF) under award number 1430284. The Green Bank Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. We acknowledge that CHIME is located on the traditional, ancestral, and unceded territory of the Syilx/Okanagan people. We are grateful to the staff of the Dominion Radio Astrophysical Observatory, which is operated by the National Research Council of Canada. CHIME is funded by a grant from the Canada Foundation for Innovation (CFI) 2012 Leading Edge Fund (Project 31170) and by contributions from the provinces of British Columbia, Québec, and Ontario. The CHIME/FRB Project, which enabled development in common with the CHIME/Pulsar instrument, is funded by a grant from the CFI 2015 Innovation Fund (Project 33213) and by contributions from the provinces of British Columbia and Québec, and by the Dunlap Institute for Astronomy and Astrophysics at the University of Toronto. Additional support was provided by the Canadian Institute for Advanced Research (CIFAR), McGill University and the McGill Space Institute thanks to the Trottier Family Foundation, and the University of British Columbia. The CHIME/Pulsar instrument hardware was funded by NSERC RTI-1 grant No. EQPEQ 458893-2014. This research was enabled in part by support provided by WestGrid (www.westgrid.ca) and Compute Canada (www.computecanada.ca.).

Support for H.T.C. is provided by NASA through the NASA Hubble Fellowship Program grant No. HST-HF2-51453.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. T.D. is supported by an NSF Astronomy and Astrophysics grant (AAG) award number 2009468. E.C.F. is supported by NASA under award number 80GSFC21M0002. M.T.L. is supported by an NSF Astronomy and Astrophysics grant (AAG) award number 2009468. The Flatiron Institute is supported by the Simons Foundation. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J.W.M. is a CITA Postdoctoral Fellow: this work was supported by Ontario Research Fundresearch Excellence Program (ORF-RE) and the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference CRD 523638-18. T.T.P. acknowledges support from the MTA-ELTE Extragalactic Astrophysics Research Group, funded by the Hungarian Academy of Sciences (Magyar Tudományos Akadémia), which was used during the development of this research. S.M.R. is a CIFAR Fellow. Pulsar research at UBC is supported by an NSERC Discovery Grant and by CIFAR. Portions of this work performed at NRL were supported by ONR 6.1 basic research funding.

Keywords

Millisecond pulsars
Radio astrometry
Pulsars

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Jennings, R. J., Cordes, J. M., Chatterjee, S., McLaughlin, M. A., Demorest, P. B., Arzoumanian, Z., Baker, P. T., Blumer, H., Brook, P. R., Cohen, T., Crawford, F., Cromartie, H. T., DeCesar, M. E., Dolch, T., Ferrara, E. C., Fonseca, E., Good, D. C., Hazboun, J. S., Jones, M. L., ... Witt, C. A. (2024). An Unusual Pulse Shape Change Event in PSR J1713+0747 Observed with the Green Bank Telescope and CHIME. The Astrophysical Journal, 964(2), Article 179. https://doi.org/10.3847/1538-4357/ad2930

@article{77bc94f404d74bc988b5ee0ecb39f860,

title = "An Unusual Pulse Shape Change Event in PSR J1713+0747 Observed with the Green Bank Telescope and CHIME",

abstract = "The millisecond pulsar J1713+0747 underwent a sudden and significant pulse shape change between 2021 April 16 and 17 (MJDs 59320 and 59321). Subsequently, the pulse shape gradually recovered over the course of several months. We report the results of continued multifrequency radio observations of the pulsar made using the Canadian Hydrogen Intensity Mapping Experiment and the 100 m Green Bank Telescope in a 3 yr period encompassing the shape change event, between 2020 February and 2023 February. As of 2023 February, the pulse shape had returned to a state similar to that seen before the event, but with measurable changes remaining. The amplitude of the shape change and the accompanying time-of-arrival residuals display a strong nonmonotonic dependence on radio frequency, demonstrating that the event is neither a glitch (the effects of which should be independent of radio frequency, ν) nor a change in dispersion measure alone (which would produce a delay proportional to ν −2). However, it does bear some resemblance to the two previous “chromatic timing events” observed in J1713+0747, as well as to a similar event observed in PSR J1643−1224 in 2015.",

keywords = "Millisecond pulsars, Radio astrometry, Pulsars",

author = "Jennings, {Ross J.} and Cordes, {James M.} and Shami Chatterjee and McLaughlin, {Maura A.} and Demorest, {Paul B.} and Zaven Arzoumanian and Baker, {Paul T.} and Harsha Blumer and Brook, {Paul R.} and Tyler Cohen and Fronefield Crawford and Cromartie, {H. Thankful} and DeCesar, {Megan E.} and Timothy Dolch and Ferrara, {Elizabeth C.} and Emmanuel Fonseca and Good, {Deborah C.} and Hazboun, {Jeffrey S.} and Jones, {Megan L.} and Kaplan, {David L.} and Lam, {Michael T.} and {W. Lazio}, {T. Joseph} and Lorimer, {Duncan R.} and Jing Luo and Lynch, {Ryan S.} and McKee, {James W.} and Madison, {Dustin R.} and Meyers, {Bradley W.} and Mingarelli, {Chiara M. F.} and Nice, {David J.} and Pennucci, {Timothy T.} and Perera, {Benetge B. P.} and Pol, {Nihan S.} and Ransom, {Scott M.} and Ray, {Paul S.} and Shapiro-Albert, {Brent J.} and Xavier Siemens and Stairs, {Ingrid H.} and Stinebring, {Daniel R.} and Swiggum, {Joseph K.} and Tan, {Chia Min} and Taylor, {Stephen R.} and Vigeland, {Sarah J.} and Witt, {Caitlin A.}",

note = "Acknowledgments: The NANOGrav Physics Frontiers Center receives support from the National Science Foundation (NSF) under award number 1430284. The Green Bank Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. We acknowledge that CHIME is located on the traditional, ancestral, and unceded territory of the Syilx/Okanagan people. We are grateful to the staff of the Dominion Radio Astrophysical Observatory, which is operated by the National Research Council of Canada. CHIME is funded by a grant from the Canada Foundation for Innovation (CFI) 2012 Leading Edge Fund (Project 31170) and by contributions from the provinces of British Columbia, Qu{\'e}bec, and Ontario. The CHIME/FRB Project, which enabled development in common with the CHIME/Pulsar instrument, is funded by a grant from the CFI 2015 Innovation Fund (Project 33213) and by contributions from the provinces of British Columbia and Qu{\'e}bec, and by the Dunlap Institute for Astronomy and Astrophysics at the University of Toronto. Additional support was provided by the Canadian Institute for Advanced Research (CIFAR), McGill University and the McGill Space Institute thanks to the Trottier Family Foundation, and the University of British Columbia. The CHIME/Pulsar instrument hardware was funded by NSERC RTI-1 grant No. EQPEQ 458893-2014. This research was enabled in part by support provided by WestGrid (www.westgrid.ca) and Compute Canada (www.computecanada.ca.). Support for H.T.C. is provided by NASA through the NASA Hubble Fellowship Program grant No. HST-HF2-51453.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. T.D. is supported by an NSF Astronomy and Astrophysics grant (AAG) award number 2009468. E.C.F. is supported by NASA under award number 80GSFC21M0002. M.T.L. is supported by an NSF Astronomy and Astrophysics grant (AAG) award number 2009468. The Flatiron Institute is supported by the Simons Foundation. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J.W.M. is a CITA Postdoctoral Fellow: this work was supported by Ontario Research Fundresearch Excellence Program (ORF-RE) and the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference CRD 523638-18. T.T.P. acknowledges support from the MTA-ELTE Extragalactic Astrophysics Research Group, funded by the Hungarian Academy of Sciences (Magyar Tudom{\'a}nyos Akad{\'e}mia), which was used during the development of this research. S.M.R. is a CIFAR Fellow. Pulsar research at UBC is supported by an NSERC Discovery Grant and by CIFAR. Portions of this work performed at NRL were supported by ONR 6.1 basic research funding.",

year = "2024",

month = apr,

day = "1",

doi = "10.3847/1538-4357/ad2930",

language = "English",

volume = "964",

journal = "The Astrophysical Journal",

issn = "0004-637X",

publisher = "Institute of Physics Publishing Ltd",

number = "2",

}

Jennings, RJ, Cordes, JM, Chatterjee, S, McLaughlin, MA, Demorest, PB, Arzoumanian, Z, Baker, PT, Blumer, H, Brook, PR, Cohen, T, Crawford, F, Cromartie, HT, DeCesar, ME, Dolch, T, Ferrara, EC, Fonseca, E, Good, DC, Hazboun, JS, Jones, ML, Kaplan, DL, Lam, MT, W. Lazio, TJ, Lorimer, DR, Luo, J, Lynch, RS, McKee, JW, Madison, DR, Meyers, BW, Mingarelli, CMF, Nice, DJ, Pennucci, TT, Perera, BBP, Pol, NS, Ransom, SM, Ray, PS, Shapiro-Albert, BJ, Siemens, X, Stairs, IH, Stinebring, DR, Swiggum, JK, Tan, CM, Taylor, SR, Vigeland, SJ & Witt, CA 2024, 'An Unusual Pulse Shape Change Event in PSR J1713+0747 Observed with the Green Bank Telescope and CHIME', The Astrophysical Journal, vol. 964, no. 2, 179. https://doi.org/10.3847/1538-4357/ad2930

TY - JOUR

T1 - An Unusual Pulse Shape Change Event in PSR J1713+0747 Observed with the Green Bank Telescope and CHIME

AU - Jennings, Ross J.

AU - Cordes, James M.

AU - Chatterjee, Shami

AU - McLaughlin, Maura A.

AU - Demorest, Paul B.

AU - Arzoumanian, Zaven

AU - Baker, Paul T.

AU - Blumer, Harsha

AU - Brook, Paul R.

AU - Cohen, Tyler

AU - Crawford, Fronefield

AU - Cromartie, H. Thankful

AU - DeCesar, Megan E.

AU - Dolch, Timothy

AU - Ferrara, Elizabeth C.

AU - Fonseca, Emmanuel

AU - Good, Deborah C.

AU - Hazboun, Jeffrey S.

AU - Jones, Megan L.

AU - Kaplan, David L.

AU - Lam, Michael T.

AU - W. Lazio, T. Joseph

AU - Lorimer, Duncan R.

AU - Luo, Jing

AU - Lynch, Ryan S.

AU - McKee, James W.

AU - Madison, Dustin R.

AU - Meyers, Bradley W.

AU - Mingarelli, Chiara M. F.

AU - Nice, David J.

AU - Pennucci, Timothy T.

AU - Perera, Benetge B. P.

AU - Pol, Nihan S.

AU - Ransom, Scott M.

AU - Ray, Paul S.

AU - Shapiro-Albert, Brent J.

AU - Siemens, Xavier

AU - Stairs, Ingrid H.

AU - Stinebring, Daniel R.

AU - Swiggum, Joseph K.

AU - Tan, Chia Min

AU - Taylor, Stephen R.

AU - Vigeland, Sarah J.

AU - Witt, Caitlin A.

N1 - Acknowledgments: The NANOGrav Physics Frontiers Center receives support from the National Science Foundation (NSF) under award number 1430284. The Green Bank Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. We acknowledge that CHIME is located on the traditional, ancestral, and unceded territory of the Syilx/Okanagan people. We are grateful to the staff of the Dominion Radio Astrophysical Observatory, which is operated by the National Research Council of Canada. CHIME is funded by a grant from the Canada Foundation for Innovation (CFI) 2012 Leading Edge Fund (Project 31170) and by contributions from the provinces of British Columbia, Québec, and Ontario. The CHIME/FRB Project, which enabled development in common with the CHIME/Pulsar instrument, is funded by a grant from the CFI 2015 Innovation Fund (Project 33213) and by contributions from the provinces of British Columbia and Québec, and by the Dunlap Institute for Astronomy and Astrophysics at the University of Toronto. Additional support was provided by the Canadian Institute for Advanced Research (CIFAR), McGill University and the McGill Space Institute thanks to the Trottier Family Foundation, and the University of British Columbia. The CHIME/Pulsar instrument hardware was funded by NSERC RTI-1 grant No. EQPEQ 458893-2014. This research was enabled in part by support provided by WestGrid (www.westgrid.ca) and Compute Canada (www.computecanada.ca.). Support for H.T.C. is provided by NASA through the NASA Hubble Fellowship Program grant No. HST-HF2-51453.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. T.D. is supported by an NSF Astronomy and Astrophysics grant (AAG) award number 2009468. E.C.F. is supported by NASA under award number 80GSFC21M0002. M.T.L. is supported by an NSF Astronomy and Astrophysics grant (AAG) award number 2009468. The Flatiron Institute is supported by the Simons Foundation. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J.W.M. is a CITA Postdoctoral Fellow: this work was supported by Ontario Research Fundresearch Excellence Program (ORF-RE) and the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference CRD 523638-18. T.T.P. acknowledges support from the MTA-ELTE Extragalactic Astrophysics Research Group, funded by the Hungarian Academy of Sciences (Magyar Tudományos Akadémia), which was used during the development of this research. S.M.R. is a CIFAR Fellow. Pulsar research at UBC is supported by an NSERC Discovery Grant and by CIFAR. Portions of this work performed at NRL were supported by ONR 6.1 basic research funding.

PY - 2024/4/1

Y1 - 2024/4/1

N2 - The millisecond pulsar J1713+0747 underwent a sudden and significant pulse shape change between 2021 April 16 and 17 (MJDs 59320 and 59321). Subsequently, the pulse shape gradually recovered over the course of several months. We report the results of continued multifrequency radio observations of the pulsar made using the Canadian Hydrogen Intensity Mapping Experiment and the 100 m Green Bank Telescope in a 3 yr period encompassing the shape change event, between 2020 February and 2023 February. As of 2023 February, the pulse shape had returned to a state similar to that seen before the event, but with measurable changes remaining. The amplitude of the shape change and the accompanying time-of-arrival residuals display a strong nonmonotonic dependence on radio frequency, demonstrating that the event is neither a glitch (the effects of which should be independent of radio frequency, ν) nor a change in dispersion measure alone (which would produce a delay proportional to ν −2). However, it does bear some resemblance to the two previous “chromatic timing events” observed in J1713+0747, as well as to a similar event observed in PSR J1643−1224 in 2015.

AB - The millisecond pulsar J1713+0747 underwent a sudden and significant pulse shape change between 2021 April 16 and 17 (MJDs 59320 and 59321). Subsequently, the pulse shape gradually recovered over the course of several months. We report the results of continued multifrequency radio observations of the pulsar made using the Canadian Hydrogen Intensity Mapping Experiment and the 100 m Green Bank Telescope in a 3 yr period encompassing the shape change event, between 2020 February and 2023 February. As of 2023 February, the pulse shape had returned to a state similar to that seen before the event, but with measurable changes remaining. The amplitude of the shape change and the accompanying time-of-arrival residuals display a strong nonmonotonic dependence on radio frequency, demonstrating that the event is neither a glitch (the effects of which should be independent of radio frequency, ν) nor a change in dispersion measure alone (which would produce a delay proportional to ν −2). However, it does bear some resemblance to the two previous “chromatic timing events” observed in J1713+0747, as well as to a similar event observed in PSR J1643−1224 in 2015.

KW - Millisecond pulsars

KW - Radio astrometry

KW - Pulsars

U2 - 10.3847/1538-4357/ad2930

DO - 10.3847/1538-4357/ad2930

M3 - Article

SN - 0004-637X

VL - 964

JO - The Astrophysical Journal

JF - The Astrophysical Journal

IS - 2

M1 - 179

ER -

An Unusual Pulse Shape Change Event in PSR J1713+0747 Observed with the Green Bank Telescope and CHIME

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Bibliographical note

Keywords

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