2013MNRAS.428.2500C


Query : 2013MNRAS.428.2500C

2013MNRAS.428.2500C - Mon. Not. R. Astron. Soc., 428, 2500-2515 (2013/January-3)

The 'universal' radio/X-ray flux correlation: the case study of the black hole GX 339-4.

CORBEL S., CORIAT M., BROCKSOPP C., TZIOUMIS A.K., FENDER R.P., TOMSICK J.A., BUXTON M.M. and BAILYN C.D.

Abstract (from CDS):

The existing radio and X-ray flux correlation for Galactic black holes in the hard and quiescent states relies on a sample which is mostly dominated by two sources (GX 339-4 and V404 Cyg) observed in a single outburst. In this paper, we report on a series of radio and X-ray observations of the recurrent black hole GX 339-4 with the Australia Telescope Compact Array, the Rossi X-ray Timing Explorer and the Swift satellites. With our new long-term campaign, we now have a total of 88 quasi-simultaneous radio and X-ray observations of GX 339-4 during its hard state, covering a total of seven outbursts over a 15-yr period. Our new measurements represent the largest sample for a stellar mass black hole, without any bias from distance uncertainties, over the largest flux variations and down to a level that could be close to quiescence, making GX 339-4 the reference source for comparison with other accreting sources (black holes, neutrons stars, white dwarfs and active galactic nuclei). Our results demonstrate a very strong and stable coupling between radio and X-ray emission, despite several outbursts of different nature and separated by a period of quiescence. The radio and X-ray luminosity correlation of the form LX∝L0.62±0.01Rad confirms the non-linear coupling between the jet and the inner accretion flow powers and better defines the standard correlation track in the radio-X-ray diagram for stellar mass black holes. We further note epochs of deviations from the fit that significantly exceed the measurement uncertainties, especially during the time of formation and destruction of the self-absorbed compact jets. The jet luminosity could appear brighter (up to a factor of 2) during the decay compared to the rise for a given X-ray luminosity, possibly related to the compact jets. We furthermore connect the radio/X-ray measurements to the near-infrared/X-ray empirical correlation in GX 339-4, further demonstrating a coupled correlation between these three frequency ranges. The level of radio emission would then be tied to the near-infrared emission, possibly by the evolution of the broad-band properties of the jets. We further incorporated our new data of GX 339-4 in a more global study of black hole candidates strongly supporting a scale invariance in the jet-accretion coupling of accreting black holes, and confirms the existence of two populations of sources in the radio/X-ray diagram.

Abstract Copyright: © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2012)

Journal keyword(s): accretion, accretion discs - black holes physics - binaries: general - stars: individual: GX 339-4 - ISM: jets and outflows - radio continuum: stars - X-rays: binaries

VizieR on-line data: <Available at CDS (J/MNRAS/428/2500): table1.dat>

Simbad objects: 32

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Number of rows : 32
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* V518 Per HXB 04 21 42.7227473352 +32 54 26.939156184 13.00 13.50 13.2     M4.5V 638 1
2 1A 0620-00 HXB 06 22 44.5423857312 -00 20 44.290460544 10.60 11.40 11.2     K3V-K7V 1073 0
3 V* KV UMa HXB 11 18 10.7930420496 +48 02 12.314730120     12.25     K5V-M1V 768 0
4 V* BW Cir HXB 13 58 09.700 -64 44 05.80 17.90 18.00 16.9     ~ 217 1
5 V* IL Lup HXB 15 47 08.2768672752 -47 40 10.284587760     11.96     ~ 453 1
6 V* V381 Nor HXB 15 50 58.6637920704 -56 28 35.258385000   17.95 16.6     K3III 1103 0
7 EQ 1646-50 ? 16 50 -50.1           ~ 5 0
8 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60     11.89     K4V 370 0
9 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1799 1
10 MAXI J1659-152 LXB 16 59 01.680 -15 15 28.73           ~ 221 0
11 V* V821 Ara HXB 17 02 49.3876391280 -48 47 23.087954544 16.20 16.30 15.5     ~ 1950 0
12 [KRL2007b] 222 LXB 17 09 07.61 -36 24 25.7           ~ 245 1
13 IGR J17177-3656 LXB 17 17 39.0 -36 56 17           ~ 23 0
14 V* V1228 Sco LXB 17 19 58.990 -31 45 01.11           ~ 110 1
15 NAME Slow Burster LXB 17 31 57.73 -33 50 02.5     15.50     ~ 799 1
16 NAME Great Annihilator LXB 17 43 54.83 -29 44 42.6           ~ 659 1
17 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 675 0
18 [CHM2006] Candidate 1b LXB 17 49 38.039 -28 21 17.50           ~ 72 0
19 XTE J1752-223 LXB 17 52 15.090 -22 20 32.36           ~ 186 0
20 2MAXI J1753-013 LXB 17 53 28.2898766424 -01 27 06.256555272 15.30 16.73 16.46 16.15 15.64 ~ 330 0
21 2XMM J180112.4-254436 LXB 18 01 12.40 -25 44 36.1           ~ 376 1
22 V* V4641 Sgr HXB 18 19 21.6343259256 -25 24 25.849595952     13.654   13.092 B9III 436 1
23 V* V406 Vul HXB 18 58 41.580 +22 39 29.40 15.00 15.65 15.31     G5V-K0V 347 0
24 [KRL2007b] 353 HXB 19 08 53.080 +09 23 04.84     15.80     ~ 101 0
25 X Aql X-1 LXB 19 11 16.0571313336 +00 35 05.868232692           ~ 1087 1
26 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2463 0
27 ICRF J193925.0-634245 Sy2 19 39 25.0245304992 -63 42 45.640373400   18.87 18.37 17.64   ~ 1116 1
28 HD 226868 HXB 19 58 21.6757355952 +35 12 05.784512688 9.38 9.72 8.91 8.42   O9.7Iabpvar 4138 0
29 V* QZ Vul HXB 20 02 49.58 +25 14 11.3   19.64 18.2     K3V-K6V 408 0
30 V* V404 Cyg HXB 20 24 03.8254458776 +33 52 01.962185735           G9/K0III/V 1189 0
31 NAME Galactic Bulge reg ~ ~           ~ 3930 0
32 NAME Galactic Ridge ? ~ ~           ~ 472 1

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2022.10.02-20:35:29

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