C.D.S. - SIMBAD4 rel 1.7 - 2021.04.15CEST07:40:44

2011ApJ...729L..16G - Astrophys. J., 729, L16 (2011/March-2)

Discovery of an energetic 38.5 ms pulsar powering the gamma-ray source IGR J18490-0000/HESS J1849-000.


Abstract (from CDS):

We report the discovery of a 38.5 ms X-ray pulsar in observations of the soft γ-ray source IGR J18490-0000 with the Rossi X-ray Timing Explorer (RXTE). PSR J1849-0001 is spinning down rapidly with period derivative 1.42 x10–14 s/s, yielding a spin-down luminosity {dot}E = 9.8x1036 erg/s, characteristic age τ_c ≡P/2{dot}P = 42.9 kyr, and surface dipole magnetic field strength Bs= 7.5x1011 G. Within the INTEGRAL/IBIS error circle lies a point-like XMM-Newton and Chandra X-ray source that shows evidence of faint extended emission consistent with a pulsar wind nebula (PWN). The XMM-Newton spectrum of the point source is well fitted by an absorbed power-law model with photon index ΓPSR= 1.1±0.2, NH= (4.3±0.6)x1022/cm2, and FPSR(2-10 keV) = (3.8±0.3)x10–12 erg/cm2/s, while the spectral parameters of the extended emission are roughly ΓPWN~ 2.1 and FPWN(2-10 keV) ~ 9x10–13 erg/cm2/s. IGR J18490-0000 is also coincident with the compact TeV source HESS J1849-000. For an assumed distance of 7 kpc in the Scutum arm tangent region, the 0.35-10 TeV luminosity of HESS J1849-000 is 0.13% of the pulsar's spin-down energy, while the ratio F(0.35-10 TeV)/FPWN(2-10 keV) ~ 2. These properties are consistent with leptonic models of TeV emission from PWNe, with PSR J1849-0001 in a stage of transition from a synchrotron X-ray source to an inverse Compton γ-ray source.

Abstract Copyright:

Journal keyword(s): ISM: supernova remnants - pulsars: individual (PSR J1849-0001, IGR J18490-0000, HESS J1849-000) - stars: neutron

Simbad objects: 3

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Number of rows : 3

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
1 PSR J1849-0001 Psr 18 49 01.83 -00 01 19.1           ~ 39 0
2 NAME Sgr Arm PoG 19 00 -30.0           ~ 544 1
3 NAME Scutum Spiral Arm PoG ~ ~           ~ 291 0

    Equat.    Gal    SGal    Ecl

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