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Title:
Chandra Observation of the Relativistic Binary J1906+0746
Authors:
Kargaltsev, O.; Pavlov, G. G.
Affiliation:
AA(Department of Astronomy, University of Florida, Bryant Space Science Center, Gainesville, FL 32611, USA ), AB(The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA )
Publication:
The Astrophysical Journal, Volume 702, Issue 1, pp. 433-440 (2009). (ApJ Homepage)
Publication Date:
09/2009
Origin:
IOP
ApJ Keywords:
pulsars: individual: PSR J1906+0746, stars: neutron, X-rays: ISM
DOI:
10.1088/0004-637X/702/1/433
Bibliographic Code:
2009ApJ...702..433K

Abstract

PSR J1906+0746 is a young radio pulsar (τ = 112 kyr, P = 144 ms) in a tight binary (P orb = 3.98 hr) with a compact high-mass companion (M comp sime 1.36 M sun), at the distance of about 5 kpc. We observed this unique relativistic binary with the Chandra Advanced CCD Imaging Spectrometer detector for 31.6 ks. Surprisingly, not a single photon was detected within the 3'' radius from the J1906+0746 radio position. For a plausible range of hydrogen column densities, n H = (0.5-1) × 1022 cm-2, the nondetection corresponds to the 90% upper limit of (3-5) × 1030 erg s-1 on the unabsorbed 0.5-8 keV luminosity for the power-law model with Γ = 1.0-2.0, and ~1032 erg s-1 on the bolometric luminosity of the thermal emission from the neutrons star surface. The inferred limits are the lowest known for pulsars with spin-down properties similar to those of PSR J1906+0746. We have also tentatively detected a puzzling extended structure which looks like a tilted ring with a radius of 1farcm6 centered on the pulsar. The measured 0.5-8 keV flux of the feature, ≈3.1 × 10-14 erg cm-2 s-1, implies an unabsorbed luminosity of 1.2 × 1032 erg s-1 (4.5 × 10-4 of the pulsar's \dot{E}) for n H = 0.7 × 1022 cm-2. If the ring is not a peculiar noise artifact, the pulsar wind nebula around an unusually underluminous pulsar would be the most plausible interpretation.
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