Astron. Astrophys. 333, L55-L58 (1998)

Letter to the Editor

Detection of an X-ray pulsed signal from the supernova remnant N157B in the Large Magellanic Cloud

G. Cusumano ¹, M.C. Maccarone ¹, T. Mineo ¹, B. Sacco ¹, E. Massaro ², R. Bandiera ³ and M. Salvati <sup>3

1</sup> Istituto di Fisica Cosmica ed Applicazioni all' Informatica, CNR, Via U. La Malfa 153, I-90146 Palermo, Italy
² Istituto Astronomico, Unità GIFCO Roma-1, Università "La Sapienza", Via G.M. Lancisi 29, I-00161, Roma, Italy
³ Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy

Received 18 March 1998 / Accepted 24 March 1998

Abstract

The supernova remnant N157B was in the field of view during an observation of the LMC with the BeppoSAX satellite. A signal with a 16 ms periodicity was detected in the MECS data. The pulse profile is characterized by a single narrow peak with a flux of (5.1 1.1) 10^-13 erg cm^-2 s^-1. In this paper the dynamical state of the plerion-shell system is discussed, and inferences are drawn on the optical luminosity of the pulsar and the plerion.

Key words: stars stars: neutron pulsars: individual X-rays: stars

SIMBAD Objects

Contents

• 1. Introduction
• 2. Observation and data reduction
• 3. Timing and spectral analysis
• 4. Discussion
• References

© European Southern Observatory (ESO) 1998

Online publication: April 20, 1998
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