2009A&A...501.1031K


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET01:35:07

2009A&A...501.1031K - Astronomy and Astrophysics, volume 501, 1031-1046 (2009/7-3)

High-energy characteristics of the schizophrenic pulsar PSRJ1846-0258 in Kes 75. Multi-year RXTE and INTEGRAL observations crossing the magnetar-like outburst.

KUIPER L. and HERMSEN W.

Abstract (from CDS):

PSRJ1846-0258 is a young rotation-powered pulsar with one of the highest surface magnetic field strengths, located in the centre of SN-remnant Kes-75. In June 2006 a magnetar-like outburst took place. Using multi-year RXTE and INTEGRAL observations covering the epoch of the outburst, we aim to study the temporal and spectral characteristics of PSRJ1846-0258 over a broad ∼3-300keV energy range to derive constraints on theoretical scenarios aiming to explain this schizophrenic behaviour. We explored all publically available RXTE observations of PSRJ1846-0258 to generate accurate ephemerides over the period January 30, 2000-November 7, 2007. Phase-folding procedures yielded pulse profiles for RXTE PCA (∼3-30keV), RXTE HEXTE (∼15-250keV) and INTEGRAL ISGRI (∼20-300keV). The pulsed spectrum over the full ∼3-300keV energy range was derived, as well as the total spectrum (including the pulsar wind nebula) over the 20-300keV band with the ISGRI. The timing, spatial, and spectral analyses were applied for epochs before, during, and after the magnetar-like outburst to study the evolution of the high-energy characteristics. ISGRI detected PSRJ1846-0258/Kes-75 before outburst during 2003-2006 with a power-law-shape spectrum over the 20-300keV energy range with photon index Γ=1.80±0.06 and energy flux (20-300keV) of (6.62±0.35)x10–11erg/cm2/s. More than 90 days after the onset of the outburst, still during the decay phase, the same spectral shape was measured (Γ=1.75–0.31+0.27) with an indication for a 52% (2.3σ) enhanced total emission, while one year after the outburst the hard X-ray non-thermal emission of PSRJ1846-0258/Kes-75 was found to be back to its pre-outburst values. PCA monitoring of PSRJ1846-0258 before the outburst yielded phase-coherent ephemerides confirming the earlier derived breaking index of the spindown. During the outburst, incoherent solutions have been derived. We show that the radiative outburst was triggered by a major spin-up glitch near MJD 53883±3 with a glitch size Δν/ν in the range (2.0-4.4)x10–6. Using all pre-outburst observations of ISGRI and HEXTE for the first time pulse profiles have been obtained up to 150keV with a broad single asymmetric pulse. The pulse shape did not vary with energy over the 2.9-150keV energy range, nor did it change during the magnetar-like outburst. The time-averaged pre-outburst ∼3-300keV pulsed spectrum measured with the PCA, HEXTE, and ISGRI was fitted with a power-law model with Γ=1.20±0.01. A fit with a curved power-law model gives an improved fit. Around 150keV the pulsed fraction approaches 100%. For the first 32 days of the magnetar-like outburst, the 3-30keV pulsed spectrum can be represented with two power laws, a soft component with index Γs=2.96±0.06 and a hard component with the pre-outburst value Γh ∼1.2. Above ∼9 keV, all spectra during outburst are consistent with the latter single power-law shape with index ∼1.2. The 2-10 keV flux increased by a factor ∼5 and the 10-30 keV flux increased with only 35%. After ∼120 days the soft outburst and the enhancement of the hard non-thermal component both vanish. The varying temporal and spectral characteristics of PSRJ1846-0258 can be explained in a scenario of a young high-B-field pulsar in which a major glitch triggered a sudden release of energy. Resonant cyclotron upscattering could subsequently generate the decaying/cooling soft pulsed component measured during outburst between 3 and 10keV. The (variation in the) non-thermal hard X-ray component can be explained with synchrotron emission in a slot-gap or outer-gap pulsar model.

Abstract Copyright:

Journal keyword(s): pulsars: individual: PSRJ1846-0258 - pulsars: individual: PSR B1509-58 - pulsars: individual: 4U 0142+61 - pulsars: individual: 1RXS J170849-400910 - X-rays: general - gamma rays: observations

Simbad objects: 24

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Number of rows : 24

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     ~ 512 0
2 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4838 1
3 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5671 4
4 PSR B0540-69 Psr 05 40 10.84 -69 19 54.2           ~ 804 3
5 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1127 2
6 PSR J1119-6127 Psr 11 19 14.30 -61 27 49.5           ~ 333 1
7 PSR B1509-58 Psr 15 13 55.52 -59 08 08.8           ~ 799 1
8 PSR J1708-4008 Psr 17 08 49.0 -40 09 10           ~ 264 0
9 PSR J1808-2024 Psr 18 08 39.32 -20 24 40.1           ~ 1118 2
10 [GH2008] 14 SNR 18 38 03.13 -06 55 33.4           ~ 70 2
11 [KRL2007b] 332 HXB 18 41 00.43 -05 35 46.5           B1Ib 117 1
12 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 235 1
13 4C -04.71 Rad 18 41 19.8 -04 56 06           ~ 301 3
14 [KRL2007b] 335 HXB 18 45 01.5 -04 33 58   16.24 14.06 12.71 11.42 O9Ia 78 0
15 2MASS J18453684+0051474 HXB 18 45 36.8356137141 +00 51 47.438374606     20.6     B0-2IV-Ve 104 0
16 2MASS J18461279-0222261 HX? 18 46 12.792 -02 22 26.18   20.5   16.6   ~ 16 0
17 PSR J1846-0258 Psr 18 46 24.94 -02 58 30.1           ~ 300 2
18 SNR G029.7-00.3 SNR 18 46 25.5 -02 59 14           ~ 296 2
19 IGR J18483-0311 HXB 18 48 17.2064881183 -03 10 16.876608322 23.702 25.162 21.884 17.888 15.88 B0.5Ia 110 0
20 4U 1850-03 HXB 18 48 17.7 -02 25 13           Be? 97 1
21 IGR J18485-0047 gam 18 48 25.44648 -00 46 34.8816           ~ 15 0
22 PSR J1849-0001 Psr 18 49 01.83 -00 01 19.1           ~ 39 0
23 2MASS J18553040-0236167 HXB 18 55 30.4059836401 -02 36 16.737233178           B0Iaep 82 0
24 NAME Scutum Region reg ~ ~           ~ 28 0

    Equat.    Gal    SGal    Ecl

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2020.11.28-01:35:07

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