Volume 425, Number 1, October I 2004
|Page(s)||L5 - L8|
|Published online||10 September 2004|
Letter to the Editor
Correlated Infrared and X-ray variability of the transient Anomalous X-ray Pulsar XTE J1810-197*
Universitá di Roma 2, via della Ricerca Scientifica 1, 00133 Roma, Italy e-mail: firstname.lastname@example.org
2 INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone, Italy
3 Affiliated with International Center for Relativistic Astrophysics
4 CNR - IASF, Sezione di Milano “G. Occhialini”, via Bassini 15, 20133 Milano, Italy
5 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
6 Università degli Studi di Milano, Dipartimento di Fisica, v. Celoria 16, 20133 Milano, Italy
7 CNR - IASF, Sezione di Palermo, via Ugo La Malfa 153, 90146 Palermo, Italy
8 Astrophysics Missions Division, Research and Scientific Support Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands
9 European Southern Observatory, Karl-Schwarzschild str. 2, 85748 Garching, Germany
10 European Southern Observatory, Av. Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile
11 INAF - Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate (Lc), Italy
Accepted: 7 August 2004
We report on observations aimed at searching for flux variations from the proposed IR counterpart of the Anomalous X-ray Pulsar (AXP) XTE J1810-197. These data, obtained in March 2004 with the adaptive optics camera NAOS-CONICA at the ESO VLT, show that the candidate proposed by Israel et al. ([CITE], ApJ, 603, L97) was fainter by and with respect to October 2003, confirming it as the IR counterpart of XTE J1810-197. We also report on an XMM-Newton observation carried out the day before the VLT observations. The 0.5-10 keV absorbed flux of the source was erg cm-2 s-1, which is less by a factor of about two compared to the previous XMM-Newton observation on September 2003. Therefore, we conclude that a similar flux decrease took place in the X-ray and IR bands. We briefly discuss these results in the framework of the proposed mechanism(s) responsible for the IR variable emission of AXPs.
Key words: stars: pulsars: individual: XTE J1810–197 / stars: neutron / X-rays: stars
© ESO, 2004
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