Chandra observations of the old pulsar PSR B1451-68

B. Posselt, G. G. Pavlov, R. N. Manchester, O. Kargaltsev, G. P. Garmire

Research output: Contribution to journalArticle

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Abstract

We present 35ks Chandra ACIS observations of the 42Myr old radio pulsar PSR B1451-68. A point source is detected 0″.32 ± 0″.73 from the expected radio pulsar position. It has ∼200 counts in the 0.3-8keV energy range. We identify this point source as the X-ray counterpart of the radio pulsar. PSR B1451-68 is located close to a Two Micron All Sky Survey point source for which we derive 7% as the upper limit on the flux contribution to the measured pulsar X-ray flux. The pulsar spectrum can be described by either a power-law model with photon index Γ = 2.4+0.4 -0.3 and a unrealistically high absorbing column density N H = (2.5 +1.2 - 1.3) × 1021cm-2, or by a combination of a kT = 0.35+0.12 - 0.07 keV blackbody and a Γ = 1.4 ± 0.5 power-law component for N DM H = 2.6 × 1020cm-2, estimated from the pulsar dispersion measure. At the parallactic, a Lutz-Kelker bias corrected distance of 480pc, the non-thermal X-ray luminosities in the 0.3-8keV energy band are either L nonth 0.3-8 keV = (11.3 ± 1.7) × 1029ergs-1 or L nonth 0.3-8 keV = (5.9+4.9 - 5.0) × 10 29ergs-1, respectively. This corresponds to non-thermal X-ray efficiencies of either or νnonth0.38 keV= L nonth0.38keV/Ė ∼ 5 × 10?3 or 10-3, respectively.

Original languageEnglish (US)
Article number146
JournalAstrophysical Journal
Volume749
Issue number2
DOIs
StatePublished - Apr 20 2012

Fingerprint

pulsars
point source
radio
point sources
power law
x rays
energy
energy bands
luminosity
photons

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Posselt, B., Pavlov, G. G., Manchester, R. N., Kargaltsev, O., & Garmire, G. P. (2012). Chandra observations of the old pulsar PSR B1451-68. Astrophysical Journal, 749(2), [146]. https://doi.org/10.1088/0004-637X/749/2/146
Posselt, B. ; Pavlov, G. G. ; Manchester, R. N. ; Kargaltsev, O. ; Garmire, G. P. / Chandra observations of the old pulsar PSR B1451-68. In: Astrophysical Journal. 2012 ; Vol. 749, No. 2.
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abstract = "We present 35ks Chandra ACIS observations of the 42Myr old radio pulsar PSR B1451-68. A point source is detected 0″.32 ± 0″.73 from the expected radio pulsar position. It has ∼200 counts in the 0.3-8keV energy range. We identify this point source as the X-ray counterpart of the radio pulsar. PSR B1451-68 is located close to a Two Micron All Sky Survey point source for which we derive 7{\%} as the upper limit on the flux contribution to the measured pulsar X-ray flux. The pulsar spectrum can be described by either a power-law model with photon index Γ = 2.4+0.4 -0.3 and a unrealistically high absorbing column density N H = (2.5 +1.2 - 1.3) × 1021cm-2, or by a combination of a kT = 0.35+0.12 - 0.07 keV blackbody and a Γ = 1.4 ± 0.5 power-law component for N DM H = 2.6 × 1020cm-2, estimated from the pulsar dispersion measure. At the parallactic, a Lutz-Kelker bias corrected distance of 480pc, the non-thermal X-ray luminosities in the 0.3-8keV energy band are either L nonth 0.3-8 keV = (11.3 ± 1.7) × 1029ergs-1 or L nonth 0.3-8 keV = (5.9+4.9 - 5.0) × 10 29ergs-1, respectively. This corresponds to non-thermal X-ray efficiencies of either or νnonth0.38 keV= L nonth0.38keV/Ė ∼ 5 × 10?3 or 10-3, respectively.",
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Posselt, B, Pavlov, GG, Manchester, RN, Kargaltsev, O & Garmire, GP 2012, 'Chandra observations of the old pulsar PSR B1451-68', Astrophysical Journal, vol. 749, no. 2, 146. https://doi.org/10.1088/0004-637X/749/2/146

Chandra observations of the old pulsar PSR B1451-68. / Posselt, B.; Pavlov, G. G.; Manchester, R. N.; Kargaltsev, O.; Garmire, G. P.

In: Astrophysical Journal, Vol. 749, No. 2, 146, 20.04.2012.

Research output: Contribution to journalArticle

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T1 - Chandra observations of the old pulsar PSR B1451-68

AU - Posselt, B.

AU - Pavlov, G. G.

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AU - Garmire, G. P.

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N2 - We present 35ks Chandra ACIS observations of the 42Myr old radio pulsar PSR B1451-68. A point source is detected 0″.32 ± 0″.73 from the expected radio pulsar position. It has ∼200 counts in the 0.3-8keV energy range. We identify this point source as the X-ray counterpart of the radio pulsar. PSR B1451-68 is located close to a Two Micron All Sky Survey point source for which we derive 7% as the upper limit on the flux contribution to the measured pulsar X-ray flux. The pulsar spectrum can be described by either a power-law model with photon index Γ = 2.4+0.4 -0.3 and a unrealistically high absorbing column density N H = (2.5 +1.2 - 1.3) × 1021cm-2, or by a combination of a kT = 0.35+0.12 - 0.07 keV blackbody and a Γ = 1.4 ± 0.5 power-law component for N DM H = 2.6 × 1020cm-2, estimated from the pulsar dispersion measure. At the parallactic, a Lutz-Kelker bias corrected distance of 480pc, the non-thermal X-ray luminosities in the 0.3-8keV energy band are either L nonth 0.3-8 keV = (11.3 ± 1.7) × 1029ergs-1 or L nonth 0.3-8 keV = (5.9+4.9 - 5.0) × 10 29ergs-1, respectively. This corresponds to non-thermal X-ray efficiencies of either or νnonth0.38 keV= L nonth0.38keV/Ė ∼ 5 × 10?3 or 10-3, respectively.

AB - We present 35ks Chandra ACIS observations of the 42Myr old radio pulsar PSR B1451-68. A point source is detected 0″.32 ± 0″.73 from the expected radio pulsar position. It has ∼200 counts in the 0.3-8keV energy range. We identify this point source as the X-ray counterpart of the radio pulsar. PSR B1451-68 is located close to a Two Micron All Sky Survey point source for which we derive 7% as the upper limit on the flux contribution to the measured pulsar X-ray flux. The pulsar spectrum can be described by either a power-law model with photon index Γ = 2.4+0.4 -0.3 and a unrealistically high absorbing column density N H = (2.5 +1.2 - 1.3) × 1021cm-2, or by a combination of a kT = 0.35+0.12 - 0.07 keV blackbody and a Γ = 1.4 ± 0.5 power-law component for N DM H = 2.6 × 1020cm-2, estimated from the pulsar dispersion measure. At the parallactic, a Lutz-Kelker bias corrected distance of 480pc, the non-thermal X-ray luminosities in the 0.3-8keV energy band are either L nonth 0.3-8 keV = (11.3 ± 1.7) × 1029ergs-1 or L nonth 0.3-8 keV = (5.9+4.9 - 5.0) × 10 29ergs-1, respectively. This corresponds to non-thermal X-ray efficiencies of either or νnonth0.38 keV= L nonth0.38keV/Ė ∼ 5 × 10?3 or 10-3, respectively.

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