PSR J2021+3651: A new γ-ray pulsar candidate

M. S.E. Roberts; J. W.T. Hessels; S. M. Ransom; V. M. Kaspi; P. C.C. Freire; F. Crawford; D. R. Lorimer

doi:10.1016/j.asr.2003.04.021

PSR J2021+3651: A new γ-ray pulsar candidate

M. S.E. Roberts, J. W.T. Hessels, S. M. Ransom, V. M. Kaspi, P. C.C. Freire, F. Crawford, D. R. Lorimer

Physics

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

Abstract

The COS B high energy γ-ray source 2CG 075+00, also known as GeV J2020+3658 or 3EG J2021+3716, has avoided identification with a low energy counterpart for over 20 years. We present a likely identification with the discovery and subsequent timing of a young and energetic pulsar, PSR J2021+3651, with the Wideband Arecibo Pulsar Processor at the Arecibo Observatory. PSR J2021+3651 has a rotation period P ∼ 104 ms and Ṗ ∼ 9.6 × 10 ^-14 , implying a characteristic age τ _c ∼ 17 kyr and a spin-down luminosity Ė ∼ 3.4 × 10 ³⁶ erg s ^-1 . The pulsar is also coincident with the ASCA source AX J2021.1+3651. The implied luminosity of the associated X-ray source suggests the X-ray emission is dominated by a pulsar wind nebula unresolved by ASCA. The pulsar's unexpectedly high dispersion measure (DM ∼ 371 pc cm ^-3 ) and the d ≥ 10 kpc DM distance pose a new question: is PSR J2021+3651 an extremely efficient γ-ray pulsar at the edge of the Galaxy? This is a question for AGILE and GLAST to answer.

Original language	English (US)
Pages (from-to)	577-580
Number of pages	4
Journal	Advances in Space Research
Volume	33
Issue number	4
DOIs	https://doi.org/10.1016/j.asr.2003.04.021
State	Published - 2004

Keywords

GeV 2020+3658
High energy γ-rays
PSR J2021+3651
Pulsars
Young pulsar
γ-ray pulsar

ASJC Scopus subject areas

Aerospace Engineering
Astronomy and Astrophysics
Geophysics
Atmospheric Science
Space and Planetary Science
General Earth and Planetary Sciences

Access to Document

10.1016/j.asr.2003.04.021

Cite this

@article{510a70d3177e47469024cc9c00623d7c,

title = "PSR J2021+3651: A new γ-ray pulsar candidate",

abstract = " The COS B high energy γ-ray source 2CG 075+00, also known as GeV J2020+3658 or 3EG J2021+3716, has avoided identification with a low energy counterpart for over 20 years. We present a likely identification with the discovery and subsequent timing of a young and energetic pulsar, PSR J2021+3651, with the Wideband Arecibo Pulsar Processor at the Arecibo Observatory. PSR J2021+3651 has a rotation period P ∼ 104 ms and Ṗ ∼ 9.6 × 10 -14 , implying a characteristic age τ c ∼ 17 kyr and a spin-down luminosity Ė ∼ 3.4 × 10 36 erg s -1 . The pulsar is also coincident with the ASCA source AX J2021.1+3651. The implied luminosity of the associated X-ray source suggests the X-ray emission is dominated by a pulsar wind nebula unresolved by ASCA. The pulsar's unexpectedly high dispersion measure (DM ∼ 371 pc cm -3 ) and the d ≥ 10 kpc DM distance pose a new question: is PSR J2021+3651 an extremely efficient γ-ray pulsar at the edge of the Galaxy? This is a question for AGILE and GLAST to answer.",

keywords = "GeV 2020+3658, High energy γ-rays, PSR J2021+3651, Pulsars, Young pulsar, γ-ray pulsar",

author = "Roberts, {M. S.E.} and Hessels, {J. W.T.} and Ransom, {S. M.} and Kaspi, {V. M.} and Freire, {P. C.C.} and F. Crawford and Lorimer, {D. R.}",

note = "Funding Information: We thank Jim Cordes for useful discussions. We acknowledge support from NSERC, CFI, an NSF CAREER Award and a Sloan Fellowship. M.S.E.R. is a Quebec Merit fellow. S.M.R. is a Tomlinson fellow. J.W.T.H. is an NSERC PGS A fellow. V.M.K. is a Canada Research Chair. The Arecibo Observatory is part of the National Astronomy and Ionosphere Center, which is operated by Cornell University under a cooperative agreement with the National Science Foundation. ",

year = "2004",

doi = "10.1016/j.asr.2003.04.021",

language = "English (US)",

volume = "33",

pages = "577--580",

journal = "Advances in Space Research",

issn = "0273-1177",

publisher = "Elsevier Ltd",

number = "4",

}

TY - JOUR

T1 - PSR J2021+3651

T2 - A new γ-ray pulsar candidate

AU - Roberts, M. S.E.

AU - Hessels, J. W.T.

AU - Ransom, S. M.

AU - Kaspi, V. M.

AU - Freire, P. C.C.

AU - Crawford, F.

AU - Lorimer, D. R.

N1 - Funding Information: We thank Jim Cordes for useful discussions. We acknowledge support from NSERC, CFI, an NSF CAREER Award and a Sloan Fellowship. M.S.E.R. is a Quebec Merit fellow. S.M.R. is a Tomlinson fellow. J.W.T.H. is an NSERC PGS A fellow. V.M.K. is a Canada Research Chair. The Arecibo Observatory is part of the National Astronomy and Ionosphere Center, which is operated by Cornell University under a cooperative agreement with the National Science Foundation.

PY - 2004

Y1 - 2004

N2 - The COS B high energy γ-ray source 2CG 075+00, also known as GeV J2020+3658 or 3EG J2021+3716, has avoided identification with a low energy counterpart for over 20 years. We present a likely identification with the discovery and subsequent timing of a young and energetic pulsar, PSR J2021+3651, with the Wideband Arecibo Pulsar Processor at the Arecibo Observatory. PSR J2021+3651 has a rotation period P ∼ 104 ms and Ṗ ∼ 9.6 × 10 -14 , implying a characteristic age τ c ∼ 17 kyr and a spin-down luminosity Ė ∼ 3.4 × 10 36 erg s -1 . The pulsar is also coincident with the ASCA source AX J2021.1+3651. The implied luminosity of the associated X-ray source suggests the X-ray emission is dominated by a pulsar wind nebula unresolved by ASCA. The pulsar's unexpectedly high dispersion measure (DM ∼ 371 pc cm -3 ) and the d ≥ 10 kpc DM distance pose a new question: is PSR J2021+3651 an extremely efficient γ-ray pulsar at the edge of the Galaxy? This is a question for AGILE and GLAST to answer.

AB - The COS B high energy γ-ray source 2CG 075+00, also known as GeV J2020+3658 or 3EG J2021+3716, has avoided identification with a low energy counterpart for over 20 years. We present a likely identification with the discovery and subsequent timing of a young and energetic pulsar, PSR J2021+3651, with the Wideband Arecibo Pulsar Processor at the Arecibo Observatory. PSR J2021+3651 has a rotation period P ∼ 104 ms and Ṗ ∼ 9.6 × 10 -14 , implying a characteristic age τ c ∼ 17 kyr and a spin-down luminosity Ė ∼ 3.4 × 10 36 erg s -1 . The pulsar is also coincident with the ASCA source AX J2021.1+3651. The implied luminosity of the associated X-ray source suggests the X-ray emission is dominated by a pulsar wind nebula unresolved by ASCA. The pulsar's unexpectedly high dispersion measure (DM ∼ 371 pc cm -3 ) and the d ≥ 10 kpc DM distance pose a new question: is PSR J2021+3651 an extremely efficient γ-ray pulsar at the edge of the Galaxy? This is a question for AGILE and GLAST to answer.

KW - GeV 2020+3658

KW - High energy γ-rays

KW - PSR J2021+3651

KW - Pulsars

KW - Young pulsar

KW - γ-ray pulsar

UR - http://www.scopus.com/inward/record.url?scp=1842640365&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=1842640365&partnerID=8YFLogxK

U2 - 10.1016/j.asr.2003.04.021

DO - 10.1016/j.asr.2003.04.021

M3 - Article

AN - SCOPUS:1842640365

SN - 0273-1177

VL - 33

SP - 577

EP - 580

JO - Advances in Space Research

JF - Advances in Space Research

IS - 4

ER -

PSR J2021+3651: A new γ-ray pulsar candidate

Abstract

Keywords

ASJC Scopus subject areas

Access to Document

Other files and links

Fingerprint

Cite this