PALFA Discovery of a Highly Relativistic Double Neutron Star Binary

Publikation: Beitrag in Fachzeitschrift › Artikel › Forschung › Peer-Review

Autoren

  • K. Stovall
  • P. C.C. Freire
  • S. Chatterjee
  • P. B. Demorest
  • D. R. Lorimer
  • M. A. McLaughlin
  • N. Pol
  • J. Van Leeuwen
  • R. S. Wharton
  • Bruce Allen
  • M. Boyce
  • A. Brazier
  • K. Caballero
  • F. Camilo
  • R. Camuccio
  • J. M. Cordes
  • F. Crawford
  • J. S. Deneva
  • R. D. Ferdman
  • J. W.T. Hessels
  • F. A. Jenet
  • V. M. Kaspi
  • B. Knispel
  • P. Lazarus
  • R. Lynch
  • E. Parent
  • C. Patel
  • Z. Pleunis
  • S. M. Ransom
  • P. Scholz
  • A. Seymour
  • X. Siemens
  • I. H. Stairs
  • J. Swiggum
  • W. W. Zhu

Organisationseinheiten

Externe Organisationen

  • National Radio Astronomy Observatory Socorro
  • Max-Planck-Institut für Radioastronomie (MPIfR)
  • Cornell Center for Astrophysics and Planetary Science
  • West Virginia University
  • Center for Gravitational Waves and Cosmology
  • Netherlands Institute for Radio Astronomy (ASTRON)
  • Universiteit van Amsterdam (UvA)
  • Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut)
  • University of Wisconsin Milwaukee
  • McGill University
  • Cornell University
  • University of Texas Rio Grande Valley
  • Square Kilometer Array (SKA)
  • Franklin and Marshall College, Lancaster
  • George Mason University
  • University of East Anglia
  • National Research Council of Canada
  • Arecibo Observatory
  • University of British Columbia
  • CAS - National Astronomical Observatories
Forschungs-netzwerk anzeigen

Details

OriginalspracheEnglisch
AufsatznummerL22
FachzeitschriftAstrophysical Journal Letters
Jahrgang854
Ausgabenummer2
PublikationsstatusVeröffentlicht - 16 Feb. 2018

Abstract

We report the discovery and initial follow-up of a double neutron star (DNS) system, PSR J1946+2052, with the Arecibo L-Band Feed Array pulsar (PALFA) survey. PSR J1946+2052 is a 17 ms pulsar in a 1.88 hr, eccentric (e = 0.06) orbit with a 1.2 M o companion. We have used the Jansky Very Large Array to localize PSR J1946+2052 to a precision of 0.″09 using a new phase binning mode. We have searched multiwavelength catalogs for coincident sources but did not find any counterparts. The improved position enabled a measurement of the spin period derivative of the pulsar (P = 9 ± 2 × 10-19); the small inferred magnetic field strength at the surface (B S = 4 × 109 G) indicates that this pulsar has been recycled. This and the orbital eccentricity lead to the conclusion that PSR J1946+2052 is in a DNS system. Among all known radio pulsars in DNS systems, PSR J1946+2052 has the shortest orbital period and the shortest estimated merger timescale, 46 Myr; at that time it will display the largest spin effects on gravitational-wave waveforms of any such system discovered to date. We have measured the advance of periastron passage for this system, , implying a total system mass of only 2.50 ± 0.04 M o, so it is among the lowest-mass DNS systems. This total mass measurement combined with the minimum companion mass constrains the pulsar mass to ≲1.3 M o.

ASJC Scopus Sachgebiete

Zitieren

PALFA Discovery of a Highly Relativistic Double Neutron Star Binary. / Stovall, K.; Freire, P. C.C.; Chatterjee, S. et al.
in: Astrophysical Journal Letters, Jahrgang 854, Nr. 2, L22, 16.02.2018.

Publikation: Beitrag in Fachzeitschrift › Artikel › Forschung › Peer-Review

Stovall, K, Freire, PCC, Chatterjee, S, Demorest, PB, Lorimer, DR, McLaughlin, MA, Pol, N, Van Leeuwen, J, Wharton, RS, Allen, B, Boyce, M, Brazier, A, Caballero, K, Camilo, F, Camuccio, R, Cordes, JM, Crawford, F, Deneva, JS, Ferdman, RD, Hessels, JWT, Jenet, FA, Kaspi, VM, Knispel, B, Lazarus, P, Lynch, R, Parent, E, Patel, C, Pleunis, Z, Ransom, SM, Scholz, P, Seymour, A, Siemens, X, Stairs, IH, Swiggum, J & Zhu, WW 2018, 'PALFA Discovery of a Highly Relativistic Double Neutron Star Binary', Astrophysical Journal Letters, Jg. 854, Nr. 2, L22. https://doi.org/10.3847/2041-8213/aaad06
Stovall, K., Freire, P. C. C., Chatterjee, S., Demorest, P. B., Lorimer, D. R., McLaughlin, M. A., Pol, N., Van Leeuwen, J., Wharton, R. S., Allen, B., Boyce, M., Brazier, A., Caballero, K., Camilo, F., Camuccio, R., Cordes, J. M., Crawford, F., Deneva, J. S., Ferdman, R. D., ... Zhu, W. W. (2018). PALFA Discovery of a Highly Relativistic Double Neutron Star Binary. Astrophysical Journal Letters, 854(2), Artikel L22. https://doi.org/10.3847/2041-8213/aaad06
Stovall K, Freire PCC, Chatterjee S, Demorest PB, Lorimer DR, McLaughlin MA et al. PALFA Discovery of a Highly Relativistic Double Neutron Star Binary. Astrophysical Journal Letters. 2018 Feb 16;854(2):L22. doi: 10.3847/2041-8213/aaad06
Stovall, K. ; Freire, P. C.C. ; Chatterjee, S. et al. / PALFA Discovery of a Highly Relativistic Double Neutron Star Binary. in: Astrophysical Journal Letters. 2018 ; Jahrgang 854, Nr. 2.
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@article{bc3c1e53536c4cb681cd98513ebe5e73,
title = "PALFA Discovery of a Highly Relativistic Double Neutron Star Binary",
abstract = "We report the discovery and initial follow-up of a double neutron star (DNS) system, PSR J1946+2052, with the Arecibo L-Band Feed Array pulsar (PALFA) survey. PSR J1946+2052 is a 17 ms pulsar in a 1.88 hr, eccentric (e = 0.06) orbit with a 1.2 M o companion. We have used the Jansky Very Large Array to localize PSR J1946+2052 to a precision of 0.″09 using a new phase binning mode. We have searched multiwavelength catalogs for coincident sources but did not find any counterparts. The improved position enabled a measurement of the spin period derivative of the pulsar (P = 9 ± 2 × 10-19); the small inferred magnetic field strength at the surface (B S = 4 × 109 G) indicates that this pulsar has been recycled. This and the orbital eccentricity lead to the conclusion that PSR J1946+2052 is in a DNS system. Among all known radio pulsars in DNS systems, PSR J1946+2052 has the shortest orbital period and the shortest estimated merger timescale, 46 Myr; at that time it will display the largest spin effects on gravitational-wave waveforms of any such system discovered to date. We have measured the advance of periastron passage for this system, , implying a total system mass of only 2.50 ± 0.04 M o, so it is among the lowest-mass DNS systems. This total mass measurement combined with the minimum companion mass constrains the pulsar mass to ≲1.3 M o.",
keywords = "pulsars: individual (PSR J1946+2052)",
author = "K. Stovall and Freire, {P. C.C.} and S. Chatterjee and Demorest, {P. B.} and Lorimer, {D. R.} and McLaughlin, {M. A.} and N. Pol and {Van Leeuwen}, J. and Wharton, {R. S.} and Bruce Allen and M. Boyce and A. Brazier and K. Caballero and F. Camilo and R. Camuccio and Cordes, {J. M.} and F. Crawford and Deneva, {J. S.} and Ferdman, {R. D.} and Hessels, {J. W.T.} and Jenet, {F. A.} and Kaspi, {V. M.} and B. Knispel and P. Lazarus and R. Lynch and E. Parent and C. Patel and Z. Pleunis and Ransom, {S. M.} and P. Scholz and A. Seymour and X. Siemens and Stairs, {I. H.} and J. Swiggum and Zhu, {W. W.}",
note = "Funding information: The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (NSF; AST-1100968), and in alliance with Ana G. M{\'e}ndez-Universidad Metropolitana, and the Universities Space Research Association. The National Radio Astronomy Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. K.S., A.B., S.C., J.M.C., P.D., M.A.M., S.M.R., and F.C. are (partially) supported by the NANOGrav Physics Frontiers Center (NSF award 1430284). N.P. and M.A.M. are supported by NSF award number 1517003. I.H.S. and V.M.K. both acknowledge NSERC Discovery Grants and the Canadian Institute for Advanced Research (CIFAR). V.M.K. received further support from an NSERC Discovery Accelerator Supplement, NSERC{\textquoteright}s Harzberg Award, the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. S.M.R. is a CIFAR Senior Fellow. P.C.C.F., J.v.L., R.S.W., and J.W.T.H. gratefully acknowledge financial support by the European Research Council, under the European Union{\textquoteright}s Seventh Frame-work Programme (FP/2007-2013) grant agreements 279702 (BEACON), 617199 (ALERT), 610058 (BLACKHOLECAM), and 337062 (DRAGNET), respectively. P.C.C.F. further acknowledges support from the Max Planck Society; J.W.T.H. from a NWO Vidi fellowship; J.S.D. was supported by the NASA Fermi program; and W.W.Z. by the Chinese Academy of Science Pioneer Hundred Talents Program and the National Key R&D Program of China No. 2017YFA0402600. We thank Lijing Shao and Nobert Wex for stimulating discussions and useful suggestions. Facilities: Arecibo, EVLA, GBT.",
year = "2018",
month = feb,
day = "16",
doi = "10.3847/2041-8213/aaad06",
language = "English",
volume = "854",
journal = "Astrophysical Journal Letters",
issn = "2041-8205",
publisher = "IOP Publishing Ltd.",
number = "2",

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Download

TY - JOUR

T1 - PALFA Discovery of a Highly Relativistic Double Neutron Star Binary

AU - Stovall, K.

AU - Freire, P. C.C.

AU - Chatterjee, S.

AU - Demorest, P. B.

AU - Lorimer, D. R.

AU - McLaughlin, M. A.

AU - Pol, N.

AU - Van Leeuwen, J.

AU - Wharton, R. S.

AU - Allen, Bruce

AU - Boyce, M.

AU - Brazier, A.

AU - Caballero, K.

AU - Camilo, F.

AU - Camuccio, R.

AU - Cordes, J. M.

AU - Crawford, F.

AU - Deneva, J. S.

AU - Ferdman, R. D.

AU - Hessels, J. W.T.

AU - Jenet, F. A.

AU - Kaspi, V. M.

AU - Knispel, B.

AU - Lazarus, P.

AU - Lynch, R.

AU - Parent, E.

AU - Patel, C.

AU - Pleunis, Z.

AU - Ransom, S. M.

AU - Scholz, P.

AU - Seymour, A.

AU - Siemens, X.

AU - Stairs, I. H.

AU - Swiggum, J.

AU - Zhu, W. W.

N1 - Funding information: The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (NSF; AST-1100968), and in alliance with Ana G. Méndez-Universidad Metropolitana, and the Universities Space Research Association. The National Radio Astronomy Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. K.S., A.B., S.C., J.M.C., P.D., M.A.M., S.M.R., and F.C. are (partially) supported by the NANOGrav Physics Frontiers Center (NSF award 1430284). N.P. and M.A.M. are supported by NSF award number 1517003. I.H.S. and V.M.K. both acknowledge NSERC Discovery Grants and the Canadian Institute for Advanced Research (CIFAR). V.M.K. received further support from an NSERC Discovery Accelerator Supplement, NSERC’s Harzberg Award, the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. S.M.R. is a CIFAR Senior Fellow. P.C.C.F., J.v.L., R.S.W., and J.W.T.H. gratefully acknowledge financial support by the European Research Council, under the European Union’s Seventh Frame-work Programme (FP/2007-2013) grant agreements 279702 (BEACON), 617199 (ALERT), 610058 (BLACKHOLECAM), and 337062 (DRAGNET), respectively. P.C.C.F. further acknowledges support from the Max Planck Society; J.W.T.H. from a NWO Vidi fellowship; J.S.D. was supported by the NASA Fermi program; and W.W.Z. by the Chinese Academy of Science Pioneer Hundred Talents Program and the National Key R&D Program of China No. 2017YFA0402600. We thank Lijing Shao and Nobert Wex for stimulating discussions and useful suggestions. Facilities: Arecibo, EVLA, GBT.

PY - 2018/2/16

Y1 - 2018/2/16

N2 - We report the discovery and initial follow-up of a double neutron star (DNS) system, PSR J1946+2052, with the Arecibo L-Band Feed Array pulsar (PALFA) survey. PSR J1946+2052 is a 17 ms pulsar in a 1.88 hr, eccentric (e = 0.06) orbit with a 1.2 M o companion. We have used the Jansky Very Large Array to localize PSR J1946+2052 to a precision of 0.″09 using a new phase binning mode. We have searched multiwavelength catalogs for coincident sources but did not find any counterparts. The improved position enabled a measurement of the spin period derivative of the pulsar (P = 9 ± 2 × 10-19); the small inferred magnetic field strength at the surface (B S = 4 × 109 G) indicates that this pulsar has been recycled. This and the orbital eccentricity lead to the conclusion that PSR J1946+2052 is in a DNS system. Among all known radio pulsars in DNS systems, PSR J1946+2052 has the shortest orbital period and the shortest estimated merger timescale, 46 Myr; at that time it will display the largest spin effects on gravitational-wave waveforms of any such system discovered to date. We have measured the advance of periastron passage for this system, , implying a total system mass of only 2.50 ± 0.04 M o, so it is among the lowest-mass DNS systems. This total mass measurement combined with the minimum companion mass constrains the pulsar mass to ≲1.3 M o.

AB - We report the discovery and initial follow-up of a double neutron star (DNS) system, PSR J1946+2052, with the Arecibo L-Band Feed Array pulsar (PALFA) survey. PSR J1946+2052 is a 17 ms pulsar in a 1.88 hr, eccentric (e = 0.06) orbit with a 1.2 M o companion. We have used the Jansky Very Large Array to localize PSR J1946+2052 to a precision of 0.″09 using a new phase binning mode. We have searched multiwavelength catalogs for coincident sources but did not find any counterparts. The improved position enabled a measurement of the spin period derivative of the pulsar (P = 9 ± 2 × 10-19); the small inferred magnetic field strength at the surface (B S = 4 × 109 G) indicates that this pulsar has been recycled. This and the orbital eccentricity lead to the conclusion that PSR J1946+2052 is in a DNS system. Among all known radio pulsars in DNS systems, PSR J1946+2052 has the shortest orbital period and the shortest estimated merger timescale, 46 Myr; at that time it will display the largest spin effects on gravitational-wave waveforms of any such system discovered to date. We have measured the advance of periastron passage for this system, , implying a total system mass of only 2.50 ± 0.04 M o, so it is among the lowest-mass DNS systems. This total mass measurement combined with the minimum companion mass constrains the pulsar mass to ≲1.3 M o.

KW - pulsars: individual (PSR J1946+2052)

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JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

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