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Radio monitoring of the hard state jets in the 2011 outburst of MAXI J1836?194

Radio monitoring of the hard state jets in the 2011 outburst of MAXI J1836?194
Radio monitoring of the hard state jets in the 2011 outburst of MAXI J1836?194
MAXI J1836?194 is a Galactic black hole candidate X-ray binary that was discovered in 2011 when it went into outburst. In this paper, we present the full radio monitoring of this system during its ‘failed’ outburst, in which the source did not complete a full set of state changes, only transitioning as far as the hard intermediate state. Observations with the Karl G. Jansky Very Large Array (VLA) and Australia Telescope Compact Array (ATCA) show that the jet properties changed significantly during the outburst. The VLA observations detected linearly polarized emission at a level of ?1 per cent early in the outburst, increasing to ?3 per cent as the outburst peaked. High-resolution images with the Very Long Baseline Array (VLBA) show an ?15 mas jet along the position angle ?21 ± 2°, in agreement with the electric vector position angle found from our polarization results (?21 ± 4°), implying that the magnetic field is perpendicular to the jet. Astrometric observations suggest that the system required an asymmetric natal kick to explain its observed space velocity. Comparing quasi-simultaneous X-ray monitoring with the 5 GHz VLA observations from the 2011 outburst shows an unusually steep hard-state radio/X-ray correlation of LR?L1.8±0.2X, where LR and LX denote the radio and X-ray luminosities, respectively. With ATCA and Swift monitoring of the source during a period of re-brightening in 2012, we show that the system lay on the same steep correlation. Due to the low inclination of this system, we then investigate the possibility that the observed correlation may have been steepened by variable Doppler boosting.
0035-8711
1745-1759
Russell, T.D.
a3056d2c-1f5d-4dac-8903-aa77e4af2e9e
Miller-Jones, J.C.A.
de372f09-251a-4a6c-93d9-a30ec089473f
Curran, P.A.
ea641045-4e92-47a9-b852-80ca5c39a232
Soria, R.
56ae49f7-b9b8-4eed-bae0-3947ea14ec19
Altamirano, D.
d5ccdb09-0b71-4303-9538-05b467be075b
Russell, T.D.
a3056d2c-1f5d-4dac-8903-aa77e4af2e9e
Miller-Jones, J.C.A.
de372f09-251a-4a6c-93d9-a30ec089473f
Curran, P.A.
ea641045-4e92-47a9-b852-80ca5c39a232
Soria, R.
56ae49f7-b9b8-4eed-bae0-3947ea14ec19
Altamirano, D.
d5ccdb09-0b71-4303-9538-05b467be075b

Russell, T.D., Miller-Jones, J.C.A. and Curran, P.A. et al. (2015) Radio monitoring of the hard state jets in the 2011 outburst of MAXI J1836?194. Monthly Notices of the Royal Astronomical Society, 450 (2), 1745-1759. (doi:10.1093/mnras/stv723).

Record type: Article

Abstract

MAXI J1836?194 is a Galactic black hole candidate X-ray binary that was discovered in 2011 when it went into outburst. In this paper, we present the full radio monitoring of this system during its ‘failed’ outburst, in which the source did not complete a full set of state changes, only transitioning as far as the hard intermediate state. Observations with the Karl G. Jansky Very Large Array (VLA) and Australia Telescope Compact Array (ATCA) show that the jet properties changed significantly during the outburst. The VLA observations detected linearly polarized emission at a level of ?1 per cent early in the outburst, increasing to ?3 per cent as the outburst peaked. High-resolution images with the Very Long Baseline Array (VLBA) show an ?15 mas jet along the position angle ?21 ± 2°, in agreement with the electric vector position angle found from our polarization results (?21 ± 4°), implying that the magnetic field is perpendicular to the jet. Astrometric observations suggest that the system required an asymmetric natal kick to explain its observed space velocity. Comparing quasi-simultaneous X-ray monitoring with the 5 GHz VLA observations from the 2011 outburst shows an unusually steep hard-state radio/X-ray correlation of LR?L1.8±0.2X, where LR and LX denote the radio and X-ray luminosities, respectively. With ATCA and Swift monitoring of the source during a period of re-brightening in 2012, we show that the system lay on the same steep correlation. Due to the low inclination of this system, we then investigate the possibility that the observed correlation may have been steepened by variable Doppler boosting.

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Accepted/In Press date: 28 March 2015
e-pub ahead of print date: 28 April 2015
Published date: 21 June 2015
Organisations: Astronomy Group

Identifiers

Local EPrints ID: 396178
URI: http://eprints.soton.ac.uk/id/eprint/396178
ISSN: 0035-8711
PURE UUID: 38a92d30-6f84-49f4-90e7-8c56049dd4a6
ORCID for D. Altamirano: ORCID iD orcid.org/0000-0002-3422-0074

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Date deposited: 07 Jun 2016 11:16
Last modified: 26 Nov 2021 03:02

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Contributors

Author: T.D. Russell
Author: J.C.A. Miller-Jones
Author: P.A. Curran
Author: R. Soria
Author: D. Altamirano ORCID iD

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