2018A&A...619A..40M


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.20CET09:51:56

2018A&A...619A..40M - Astronomy and Astrophysics, volume 619A, 40-40 (2018/11-1)

The radio jets of SS 433 at millimetre wavelengths.

MARTI J., BUJALANCE-FERNANDEZ I., LUQUE-ESCAMILLA P.L., SANCHEZ-AYASO E., PAREDES J.M. and RIBO M.

Abstract (from CDS):


Context. SS 433 is historically a well-known microquasar in the Galaxy that has been deeply studied during the four decades elapsed since its discovery. However, observations at very high radio frequencies with good angular resolution are still very scarce in the literature. The present paper tries to partially fill this gap using archival data of the source obtained with the Atacama Large Millimeter Array (ALMA).
Aims. We aim to study the SS 433 jet properties at radio frequencies corresponding to millimetre wavelengths where the synchrotron emitting particles are expected to lose their energy much faster than at lower frequencies of centimetre wavelengths.
Methods. We applied the methods of connected radio interferometry adapted to the ALMA spectral domain for data calibration and reduction. Afterwards, the resulting map was corrected for relativistic and geometric effects. While a detailed theoretical modelling was beyond our scope, we assessed the broad evolutive properties of the jet brightness profile in the context of a semi-analytic model.
Results. A resolved view of the SS 433 radio core and jets is presented. In addition to spectral index and magnetic field measurements, we are able to estimate the age of the oldest visible ejecta still radiating significantly at millimetre wavelengths. By combining our findings with those of previous authors at lower frequencies, we confirm that the energy loss of the radiating electrons is dominated by adiabatic expansion instead of synchrotron radiative losses. In addition, we find suggestive evidence for the previously proposed period of slowed expansion within the first months of the ejecta flow, needed to simultaneously match the radiative lifetime observed in the centimetre domain. Our results argue for the need for future coordinated millimetre and centimetre interferometric observations with good time sampling throughout the SS 433 precessional cycle to better understand energetic processes in stellar relativistic jets.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: jets - ISM: jets and outflows - X-rays: binaries - stars: individual: SS 433

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 4C 09.57 BLL 17 51 32.81857318 +09 39 00.7284829   17.46 16.78 15.57   ~ 795 1
2 ICRF J183005.9+061915 QSO 18 30 05.9399600344 +06 19 15.947596681       19.5   ~ 70 1
3 ICRF J183241.9+073155 QSO 18 32 41.9891776188 +07 31 55.117454335   19.5 19.5     ~ 11 1
4 SS 433 HXB 19 11 49.5645897701 +04 58 57.824087535   16.3 13.0     A7Ib: 1905 3

    Equat.    Gal    SGal    Ecl

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2020.01.20-09:51:56

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