Esposito 2010 SGR0418+5729的早期X射线和光学观测

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注意现在的软伽马重复暴远不是几年前的四个了。

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Title:		Early X-ray and optical observations of the soft gamma-ray repeater SGR0418+5729
Authors:		Esposito, P.; Israel, G. L.; Turolla, R.; Tiengo, A.; Götz, D.; de Luca, A.; Mignani, R. P.; Zane, S.; Rea, N.; Testa, V.; Caraveo, P. A.; Chaty, S.; Mattana, F.; Mereghetti, S.; Pellizzoni, A.; Romano, P.
Affiliation:		AA(INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano, via E. Bassini 15, I-20133 Milano, Italy; INFN - Istituto Nazionale di Fisica Nucleare, sezione di Pavia, via A. Bassi 6, I-27100 Pavia, Italy),)
Publication:		Monthly Notices of the Royal Astronomical Society, Volume 405, Issue 3, pp. 1787-1795. (MNRAS Homepage)
Publication Date:		07/2010
Origin:		WILEY
MNRAS Keywords:		stars: neutron, pulsars: general, X-rays: individual: SGR0418+5729
Abstract Copyright:		(c) Journal compilation © 2010 RAS
DOI:		10.1111/j.1365-2966.2010.16551.x
Bibliographic Code:		2010MNRAS.405.1787E

Abstract

Emission of two short hard X-ray bursts on 2009 June 5 disclosed the existence of a new soft gamma-ray repeater, now catalogued as SGR0418+5729. After a few days, X-ray pulsations at a period of 9.1s were discovered in its persistent emission. SGR0418+5729 was monitored almost since its discovery with the Rossi X-ray Timing Explorer (2-10keV energy range) and observed many times with Swift (0.2-10keV). The source persistent X-ray emission faded by a factor of ~10 in about 160 d, with a steepening in the decay about 19 d after the activation. The X-ray spectrum is well described by a simple absorbed blackbody, with a temperature decreasing in time. A phase-coherent timing solution over the ~160 d time-span yielded no evidence for any significant evolution of the spin period, implying a 3σ upper limit of 1.1 × 10^-13s s^-1 on the period derivative and of ~3 × 10¹³G on the surface dipole magnetic field. Phase-resolved spectroscopy provided evidence for a significant variation of the spectrum as a function of the stellar rotation, pointing to the presence of two emitting caps, one of which became hotter during the outburst. Finally, a deep observation of the field of SGR0418+5729 with the new Gran Telescopio Canarias 10.4-m telescope allowed us to set an upper limit on the source optical flux of i' > 25.1mag, corresponding to an X-ray-to-optical flux ratio exceeding 10⁴, consistent with the characteristics of other magnetars.

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