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Title: PSR J1907+0602: A radio-faint gamma-ray pulsar powering a bright TeV pulsar wind nebula

Abstract

Here, we present multiwavelength studies of the 106.6 ms γ-ray pulsar PSR J1907+06 near the TeV source MGRO J1908+06. Timing observations with Fermi result in a precise position determination for the pulsar of R.A. = 19 h07 m54$$s\atop{.}$$7(2), decl. = +06°02'16(2)'' placing the pulsar firmly within the TeV source extent, suggesting the TeV source is the pulsar wind nebula of PSR J1907+0602. Pulsed γ-ray emission is clearly visible at energies from 100 MeV to above 10 GeV. The phase-averaged power-law index in the energy range E > 0.1 GeV is Γ = 1.76 ± 0.05 with an exponential cutoff energy E c = 3.6 ± 0.5 GeV. We present the energy-dependent γ-ray pulsed light curve as well as limits on off-pulse emission associated with the TeV source. We also report the detection of very faint (flux density of sime 3.4 μJy) radio pulsations with the Arecibo telescope at 1.5 GHz having a dispersion measure DM = 82.1 ± 1.1 cm –3 pc. This indicates a distance of 3.2 ± 0.6 kpc and a pseudo-luminosity of L 1400 sime 0.035 mJy kpc 2. Furthermore, a Chandra ACIS observation revealed an absorbed, possibly extended, compact (lesssim4'') X-ray source with significant nonthermal emission at R.A. = 19 h07 m54$$s\atop{.}$$76, decl. = +06°02'14farcs6 with a flux of 2.3 +0.6 –1.4 × 10 –14 erg cm –2 s –1. From archival ASCA observations, we place upper limits on any arcminute scale 2-10 keV X-ray emission of ~1 × 10 –13 erg cm –2 s –1. The implied distance to the pulsar is compatible with that of the supernova remnant G40.5 – 0.5, located on the far side of the TeV nebula from PSR J1907+0602, and the S74 molecular cloud on the nearer side which we discuss as potential birth sites.

Authors:
 [1]
  1. Naval Research Lab. (NRL), Washington, DC (United States); National Academy of Sciences, Washington, DC (United States); et al.
Publication Date:
Research Org.:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Org.:
USDOE
Contributing Org.:
Fermi LAT Collaboration
OSTI Identifier:
1357576
Grant/Contract Number:  
AC02-76SF00515
Resource Type:
Accepted Manuscript
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 711; Journal Issue: 1; Journal ID: ISSN 0004-637X
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; gamma rays: general; pulsars: general; pulsars: individual (PSR J1907+0602); supernovae: individual (SNL G40.5-0.5)

Citation Formats

Abdo, A. A. PSR J1907+0602: A radio-faint gamma-ray pulsar powering a bright TeV pulsar wind nebula. United States: N. p., 2010. Web. doi:10.1088/0004-637X/711/1/64.
Abdo, A. A. PSR J1907+0602: A radio-faint gamma-ray pulsar powering a bright TeV pulsar wind nebula. United States. doi:10.1088/0004-637X/711/1/64.
Abdo, A. A. Sat . "PSR J1907+0602: A radio-faint gamma-ray pulsar powering a bright TeV pulsar wind nebula". United States. doi:10.1088/0004-637X/711/1/64. https://www.osti.gov/servlets/purl/1357576.
@article{osti_1357576,
title = {PSR J1907+0602: A radio-faint gamma-ray pulsar powering a bright TeV pulsar wind nebula},
author = {Abdo, A. A.},
abstractNote = {Here, we present multiwavelength studies of the 106.6 ms γ-ray pulsar PSR J1907+06 near the TeV source MGRO J1908+06. Timing observations with Fermi result in a precise position determination for the pulsar of R.A. = 19h07m54$s\atop{.}$7(2), decl. = +06°02'16(2)'' placing the pulsar firmly within the TeV source extent, suggesting the TeV source is the pulsar wind nebula of PSR J1907+0602. Pulsed γ-ray emission is clearly visible at energies from 100 MeV to above 10 GeV. The phase-averaged power-law index in the energy range E > 0.1 GeV is Γ = 1.76 ± 0.05 with an exponential cutoff energy Ec = 3.6 ± 0.5 GeV. We present the energy-dependent γ-ray pulsed light curve as well as limits on off-pulse emission associated with the TeV source. We also report the detection of very faint (flux density of sime 3.4 μJy) radio pulsations with the Arecibo telescope at 1.5 GHz having a dispersion measure DM = 82.1 ± 1.1 cm–3 pc. This indicates a distance of 3.2 ± 0.6 kpc and a pseudo-luminosity of L 1400 sime 0.035 mJy kpc2. Furthermore, a Chandra ACIS observation revealed an absorbed, possibly extended, compact (lesssim4'') X-ray source with significant nonthermal emission at R.A. = 19h07m54$s\atop{.}$76, decl. = +06°02'14farcs6 with a flux of 2.3+0.6 –1.4 × 10–14 erg cm–2 s–1. From archival ASCA observations, we place upper limits on any arcminute scale 2-10 keV X-ray emission of ~1 × 10–13 erg cm–2 s–1. The implied distance to the pulsar is compatible with that of the supernova remnant G40.5 – 0.5, located on the far side of the TeV nebula from PSR J1907+0602, and the S74 molecular cloud on the nearer side which we discuss as potential birth sites.},
doi = {10.1088/0004-637X/711/1/64},
journal = {Astrophysical Journal},
number = 1,
volume = 711,
place = {United States},
year = {2010},
month = {2}
}

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