DISCOVERY OF THE ENERGETIC PULSAR J1747-2809 IN THE SUPERNOVA REMNANT G0.9+0.1

Journal Article · Mon Jul 20 04:00:00 EDT 2009 · Astrophysical Journal (Online)

DOI:https://doi.org/10.1088/0004-637X/700/1/L34; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21313918

Camilo, F ^[1]; Ransom, S M ^[2]; Gaensler, B M ^[3]; Lorimer, D R ^[4]

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1. Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 (United States)
2. National Radio Astronomy Observatory, Charlottesville, VA 22903 (United States)
3. Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006 (Australia)
4. Department of Physics, West Virginia University, Morgantown, WV 26506 (United States)

The supernova remnant G0.9+0.1 has long been inferred to contain a central energetic pulsar. In observations with the NRAO Green Bank Telescope at 2 GHz, we have detected radio pulsations from PSR J1747-2809. The pulsar has a rotation period of 52 ms, and a spin-down luminosity of E-dot=4.3x10{sup 37} erg s{sup -1}, the second largest among known Galactic pulsars. With a dispersion measure of DM = 1133 pc cm{sup -3}, PSR J1747-2809 is distant, at {approx}13 kpc according to the NE2001 electron density model, although it could be located as close as the Galactic center. The pulse profile is greatly scatter-broadened at a frequency of 2 GHz, so that it is effectively undetectable at 1.4 GHz, and is very faint, with period-averaged flux density of 40 {mu}Jy at 2 GHz.

• OSTI ID: 21313918
• Journal Information: Astrophysical Journal (Online), Journal Name: Astrophysical Journal (Online) Journal Issue: 1 Vol. 700; ISSN 1538-4357
• Country of Publication: United States
• Language: English

Related Subjects

99 GENERAL AND MISCELLANEOUS
ELECTRON DENSITY
FLUX DENSITY
GHZ RANGE 01-100
LUMINOSITY
NEUTRON STARS
PULSARS
PULSATIONS
ROTATION
SUPERNOVA REMNANTS
TELESCOPES