J/MNRAS/428/2500 GX 339-4 radio/X-ray flux correlation (Corbel+, 2013)
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., Bailyn C.D.
<Mon. Not. R. Astron. Soc., 428, 2500-2515 (2013)>
=2013MNRAS.428.2500C 2013MNRAS.428.2500C
ADC_Keywords: Binaries, X-ray ; Radio sources
Keywords: accretion, accretion discs - black holes physics - binaries: general -
stars: individual: GX 339-4 - ISM: jets and outflows -
radio continuum: stars - X-rays: binaries
Abstract:
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).
Description:
All radio observations discussed in this paper were conducted with the
Australia Telescope Compact Array (ATCA) located in Narrabri, New
South Wales, Australia. The ATCA synthesis telescope is an east-west
array consisting of six 22-m antennas. It uses orthogonal linearly
polarized feeds and records full Stokes parameters. We carried out all
observations simultaneously at 4.8GHz (6.3cm)/8.64GHz (3.5cm) and
in a limited cases also at 1.384GHz (21.7cm)/2.496GHz (12.0cm).
Objects:
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RA (2000) DE Designation(s)
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17 02 49.36 -48 47 22.8 GX 339-4 = V* V821 Ara
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 123 88 Summary of data used for the radio/X-ray flux
correlation in GX 339-4
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See also:
J/A+A/542/A56 : Spectral analysis of 2010-11 outburst of GX339-4 (Nandi+, 2012)
J/AJ/143/130 : VIJH light curves of the X-Ray binary GX339-4 (Buxton+, 2012)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 "Y/M/D" Date Calendar date, mid-point of the radio
observations
12 A1 --- m_Date [ab] Multiplicity index on Date
13 A1 --- l_MJD [~] Limit flag on MJD
14- 21 F8.2 d MJD Modified Julian date
23 A1 --- l_S4.8 Limit flag on S4.8 (3σ level)
24- 28 F5.2 mJy S4.8 ?=- Flux density at 4.8 or 5.5GHz
30- 33 F4.2 mJy e_S4.8 ? rms uncertainty on S4.8
35 A1 --- l_S8.6 Limit flag on S8.6 (3σ level)
36- 40 F5.2 mJy S8.6 ?=- Flux density at 8.6 or 9.0GHz
42- 45 F4.2 mJy e_S8.6 ? rms uncertainty on S8.6
47- 51 F5.2 --- SpI ?=- Radio spectral index
53- 56 F4.2 --- e_SpI ? rms in SpIndex
58- 65 F8.5 10-13W/m2 FX ?=- X-ray flux (3-9keV) (1)
67- 73 F7.5 10-13W/m2 e_FX ? rms uncertainty on FX
74 A1 --- u_FX [)] Uncertainty flag on FX
76- 79 F4.2 --- HR ?=- X-ray hardness ratio (2)
81- 92 A12 --- Com Comment on the data origin (3)
94-123 A30 --- UL Comments on combined upper limits
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Note (1): In 10-10erg/cm2/s. The Galactic ridge emission has been
subtracted from the quoted unabsorbed 3-9keV X-ray flux.
Note (2): We defined the hardness ratio (HR) as the ratio of count rate in the
bands 9.4-18.5keV and 2.5-6.1keV and the intensity as the count rate in the
energy band 2.5-18.5keV. See the concluding part of Section 2.2.
Note (3): Note as follows:
C03 = see also Corbel et al. (2003A&A...400.1007C 2003A&A...400.1007C)
N05 = see also Nowak et al. (2005ApJ...626.1006N 2005ApJ...626.1006N)
RXTE GBM = X-ray flux from RXTE/PCA Galactic Bulge Monitoring of Craig
Markwardt
Swift/XRT = X-ray flux from Swift/XRT. Chandra/ACIS: X-ray flux from
Chandra/ACIS
S.2.4 = See complementary information in Section 2.4.
S.3.4.2 = See complementary information in Section 3.4.2.
Na = Data points from original C03 sample, but these two points
with optically thin radio spectra are representative of the
re-ignition of the compact jets during the soft to hard state
transition (e.g. see Section 3.4).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 31-Jan-2014