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) |
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Pages (from-to) | 577-580 |
Number of pages | 4 |
Journal | Advances in Space Research |
Volume | 33 |
Issue number | 4 |
DOIs | |
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
- Earth and Planetary Sciences(all)