Evidence of non-thermal X-ray emission from HH 80

Abstract

Protostellar jets appear at all stages of star formation when the accretion process is still at work. Jets travel at velocities of hundreds of km/s, creating strong shocks when interacting with interstellar medium. Several cases of jets have been detected in X-rays, typically showing soft emission. For the first time, we report evidence of hard X-ray emission possibly related to non-thermal processes not explained by previous models of the post-shock emission predicted in the jet/ambient interaction scenario. HH 80 is located at the south head of the jet associated to the massive protostar IRAS 18162-2048. It shows soft and hard X-ray emission in regions that are spatially separated, with the soft X-ray emission region situated behind the region of hard X-ray emission. We propose a scenario for HH 80 where soft X-ray emission is associated to thermal processes from the interaction of the jet with denser ambient matter and the hard X-ray emission is produced by synchrotron radiation at the front shock.

Accepted for publication in ApJL

References in corpus (9)

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Cited by in corpus (9)

• Toward gas exhaustion in the W51 high-mass protoclusters
• Detection of non-thermal emission from the massive protostellar jet HH80-81 at low radio frequencies using GMRT
• Particle acceleration in the Herbig-Haro objects HH 80 and HH 81
• Formation of X-ray emitting stationary shocks in magnetized protostellar jets
• Chandra observations of the HII complex G5.89-0.39 and TeV gamma-ray source HESSJ1800-240B
• Structure of X-ray emitting jets close to the launching site: from embedded to disk-bearing sources
• Studying the non-thermal lobes of IRAS 16547-4247 through a multi-wavelength approach
• Radio Observations of the Star Formation Activities in the NGC 2024 FIR 4 Region
• GMRT observations of the protostellar jet associated with \iras