2008A&A...489..263D


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.16CEST13:31:43

2008A&A...489..263D - Astronomy and Astrophysics, volume 489, 263-279 (2008/10-1)

Detailed high-energy characteristics of AXP 1RXS J170849-400910. Probing the magnetosphere using INTEGRAL, RXTE, and XMM-Newton.

DEN HARTOG P.R., KUIPER L. and HERMSEN W.

Abstract (from CDS):

1RXS J170849-400910 is one of four anomalous X-ray pulsars which emit persistent luminous radiation in soft X-rays (<10keV) as well as in hard X-rays (>10keV). In this paper we present detailed spectral and temporal characteristics over the whole X-ray band. For this purpose data have been used from INTEGRAL, RXTE and XMM-Newton. The hard X-ray (>10keV) time-averaged total spectrum, accumulated over four years with the imager IBIS-ISGRI onboard INTEGRAL adding up to 5.2 Ms net exposure, can be described by a power law with a photon index Γ= 1.13±0.06 and extends to ∼175keV. The 20-175keV flux is (7.76±0.34)x10–11erg/cm2/s which exceeds the 2-10keV (unabsorbed) flux by a factor of ∼2.3. No evidence for a spectral break is found below 300keV. Also, no significant long-term time variability has been detected above 20keV on time scales of 1 and 0.5 year. Pulsed emission is measured with INTEGRAL up to 270keV, i.e. to much higher energies than the total emission, with a detection significance of 12.3σ (20-270keV). The pulse profiles from 0.5keV up to 270keV show drastic morphology changes below ∼20keV. Three different pulse components can be recognized in these pulse profiles: 1) a hard pulse peaking around phase 0.8 which contributes to the pulse profiles above ∼4keV; 2) a softer pulse which peaks around phase 0.4 not contributing in the hard X-ray domain and 3) a very soft pulse component below 2keV. A combined time-averaged pulsed spectrum (2.8-270keV) from INTEGRAL, RXTE-PCA and HEXTE (collected over nine years) can be described with a soft and a hard power-law component: Γs=2.79 ±0.07 and Γh=0.86±0.16. In the pulsed spectrum extracted from a 25.5ks net exposure XMM-Newton observation we find a discontinuity between 2keV and 3keV. Above these energies the spectrum is consistent with the spectrum taken with RXTE-PCA. The pulse profiles and the total-pulsed spectrum prove to be stable over the whole nine-years time span over which the data have been taken. Also detailed phase-resolved spectroscopy of the pulsed emission confirms the long-term stability as the spectra taken at different epochs connect smoothly. The phase-resolved spectra reveal complex spectral shapes which do not follow the shape of the total-pulsed spectrum. The spectral shape gradually changes with phase from a soft single power law to a complex multi-component shape and then to a hard single power law. The spectrum switches from a very hard (Γ=0.99±0.05) to a very soft (Γ=3.58±0.34) single power-law shape within a 0.1-wide phase interval. The discontinuity measured between 2keV and 3keV with XMM-Newton is a result of a curved component. This component which is most apparent within phase interval 0.7-0.9 significantly contributes in the energy range between 4keV and 20keV. It has a very steep spectrum below 5keV with a photon index Γ~-1.5. From the phase-resolved spectra we identify three independent components with different spectral shapes which together can accurately describe all phase-resolved spectra (2.8-270keV). The three shapes are a soft power law (Γ=3.54), a hard power law (Γ=0.99) and a curved shape (described with two logparabolic functions). The phase distributions of the normalizations of these spectral components form three decoupled pulse profiles. The soft component peaks around phase 0.4 while the other two components peak around phase 0.8. The width of the curved component (∼0.25 in phase) is about half the width of the hard component. After 142, 1RXS J1708-40 is the second anomalous X-ray pulsar for which such detailed phase-resolved spectroscopy has been performed. These results give important constraints showing that three dimensional modeling covering both the geometry and different production processes is required to explain our findings.

Abstract Copyright:

Journal keyword(s): stars: neutron - X-rays: individual: 1RXS J170849-400910 - gamma rays: observations - X-rays: individual: 4U 0142+61

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 PSR J0146+6145 Psr 01 46 22.21 +61 45 03.8   28.100 25.620     ~ 520 0
2 PSR J0218+42 Psr 02 18 06.3604 +42 32 17.365           ~ 304 2
3 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4881 1
4 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5724 4
5 PSR B1509-58 Psr 15 13 55.52 -59 08 08.8     13.06     ~ 805 1
6 PSR J1550-5418 Psr 15 50 54.18 -54 18 23.9           ~ 353 1
7 PSR J1617-5055 Psr 16 17 29.35 -50 55 12.8           ~ 102 1
8 PSR J1708-4008 Psr 17 08 49.0 -40 09 10           ~ 269 0
9 NAME Galactic Center gam 17 45 39.60213 -29 00 22.0000           ~ 12108 0
10 AX J1809.8-1943 Psr 18 09 51.07 -19 43 51.8           ~ 385 0
11 PSR J1811-1926 Psr 18 11 29.15 -19 25 25.4           ~ 113 1
12 PSR J1824-2452A Psr 18 24 32.009 -24 52 11.10           ~ 444 2
13 AX J1838.0-0655 SNR 18 38 03.13 -06 55 33.4           ~ 71 2
14 PSR J1846-0258 Psr 18 46 24.94 -02 58 30.1           ~ 310 2
15 PSR J1930+1852 Psr 19 30 30.13 +18 52 14.1           ~ 83 1
16 PSR B1937+21 Psr 19 39 39.6 +21 37 22           ~ 981 2
17 NAME Galactic Ridge ? ~ ~           ~ 444 1

    Equat.    Gal    SGal    Ecl

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2021.04.16-13:31:44

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