Discovery of X-ray emission from the protostellar jet L1551 IRS5 (HH 154)

¹ Astrophysics Division – Space Science Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands
² Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
³ Nordic Optical Telescope, Apartado 474, 38700 Santa Cruz de la Palma, Canarias, Spain

Corresponding author: F. Favata, Fabio.Favata@rssd.esa.int

Received: 20 July 2001
Accepted: 27 September 2001

Abstract

We have for the first time detected X-ray emission associated with a protostellar jet, on the jet emanating from the L1551 IRS5 protostar. The IRS5 protostar is hidden behind a very large absorbing column density, making the direct observation of the jet's emission possible. The observed X-ray emission is likely associated with the shock “working surface”, i.e. the interface between the jet and the circumstellar medium. The X-ray luminosity emanating from the jet is, at erg s^-1, a significant fraction of the luminosity normally associated with the coronal emission from young stars. The spectrum of the X-ray emission is compatible with thermal emission from a hot plasma, with a temperature of 4 MK, higher than the temperature expected (on the basis of the jet's velocity) for the shock front produced by the jet hitting the circumstellar medium.