C.D.S. - SIMBAD4 rel 1.7 - 2021.05.15CEST01:08:27

2008A&A...489..245D - Astronomy and Astrophysics, volume 489, 245-261 (2008/10-1)

Detailed high-energy characteristics of AXP 4U 0142+61. Multi-year observations with INTEGRAL, RXTE, XMM-Newton, and ASCA.


Abstract (from CDS):

142 is one of the Anomalous X-ray Pulsars exhibiting hard X-ray emission above 10keV discovered with INTEGRAL. In this paper we present detailed spectral and temporal characteristics both in the hard X-ray (>10keV) and soft X-ray (<10keV) domains obtained using data from INTEGRAL, XMM-Newton, ASCA and RXTE. Accumulating data collected over four years with the imager IBIS-ISGRI aboard INTEGRAL, the time-averaged total spectrum shows a power-law like shape with photon index Γ=0.93±0.06. 142 is detected up to 229keV and the flux between 20keV and 229keV is (15.01±0.82)x10–11erg/cm2/s, which exceeds the energy flux in the 2-10keV band by a factor of ∼2.3. Using simultaneously collected data with the spectrometer SPI of INTEGRAL the combined total spectrum yields the first evidence for a spectral break above 100keV. Assuming a logparabolic function for the spectral shape above 20keV the peak energy of 142 is 228+65–41keV. There is no evidence for significant long-term time variability of the total emission from 142. Both the total flux and the spectral index are stable within the 17% level (1σ). Pulsed emission is measured with ISGRI up to 160keV. The 20-160keV profile shows a broad double-peaked pulse with a 6.2σ detection significance. The total pulsed spectrum can be described with a very hard power-law shape with a photon index Γ=0.40±0.15 and a 20-150keV flux of (2.68±1.34)x10–11erg/cm2/s. To perform accurate phase-resolved spectroscopy over the total X-ray window, we produced pulse profiles in absolute phase for INTEGRAL-ISGRI, RXTE-PCA, XMM-Newton-PN and ASCA-GIS. The two known pulses in all soft X-ray profiles below 10keV are located in the same phases. Three XMM-Newton observations in 2003-2004 show statistically identical profiles. However, we find a significant profile morphology change between an ASCA-GIS observation in 1999 following a possible glitch of 142. This change can be accounted for by differences in relative strengths and spectral shapes (0.8-10keV) of the two pulses. The principle peak in the INTEGRAL pulse profile above 20keV is located at the same phase as one of the pulses detected below 10keV. The second pulse detected with INTEGRAL is slightly shifted with respect to the second peak observed in the soft X-ray band. We performed consistent phase-resolved spectroscopy over the total high-energy band and identify at least three genuinely different pulse components with different spectra. The high level of consistency between the detailed results from the four missions is indicative of a remarkably stable geometry underlying the emission scenario. Finally, we discuss the derived detailed characteristics of the high-energy emission of 142 in relation to three models for the non-thermal hard X-ray emission.

Abstract Copyright:

Journal keyword(s): stars: neutron - stars: pulsars: individual: 4U 0142+61 - gamma rays: observations

Simbad objects: 8

goto Full paper

goto View the reference in ADS

Number of rows : 8

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
1 PSR J0146+6145 Psr 01 46 22.21 +61 45 03.8   28.100 25.620     ~ 521 0
2 EM* GGA 104 HXB 01 47 00.2121223849 +61 21 23.661992704 11.76 12.09 11.366 11.00 10.52 B1IIIe 173 0
3 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4889 1
4 PSR J1708-4008 Psr 17 08 49.0 -40 09 10           ~ 269 0
5 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 239 1
6 4C -04.71 Rad 18 41 19.8 -04 56 06           ~ 306 3
7 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 801 0
8 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 597 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2008A&A...489..245D and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact