J/MNRAS/447/2059 Black hole binaries quasi-periodic oscillations (Motta+, 2015)
Geometrical constraints on the origin of timing signals from black holes.
Motta S.E., Casella P., Henze M., Munoz-Darias T., Sanna A., Fender R.,
Belloni T.
<Mon. Not. R. Astron. Soc., 447, 2059-2072 (2015)>
=2015MNRAS.447.2059M 2015MNRAS.447.2059M (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, X-ray ; Black holes
Keywords: binaries: close - stars: black holes - stars: jets - stars: low-mass -
stars: oscillations - X-rays: binaries
Abstract:
We present a systematic study of the orbital inclination effects on black
hole transients fast time-variability properties. We have considered all
the black hole binaries that have been densely monitored by the Rossi X-ray
Timing Explorer satellite. We find that the amplitude of low-frequency
quasi-periodic oscillations (QPOs) depends on the orbital inclination.
Type-C QPOs are stronger for nearly edge-on systems (high inclination),
while type-B QPOs are stronger when the accretion disc is closer to face-on
(low inclination). Our results also suggest that the noise associated with
type-C QPOs is consistent with being stronger for low-inclination sources,
while the noise associated with type-B QPOs seems inclination independent.
These results are consistent with a geometric origin of the type-C QPOs -
for instance arising from relativistic precession of the inner flow within
a truncated disc - while the noise would correspond to intrinsic brightness
variability from mass accretion rate fluctuations in the accretion flow.
The opposite behaviour of type-B QPOs - stronger in low-inclinations
sources - supports the hypothesis that type-B QPOs are related to the jet,
the power of which is the most obvious measurable parameter expected
to be stronger in nearly face-on sources.
Description:
In this work, we use data collected by the Rossi X-ray Timing Explorer
(RXTE)/Proportional Counter Array (PCA) satellite to analyse the effects
of inclination on the fast time-variability properties of black hole
binaries (BHBs). For our analysis, we considered only the sources that
have shown low-frequency QPOs (LFQPOs). We only investigate those that
have been densely monitored by RXTE, in order to maximize the chances
of observing high-inclination features (i.e. X-ray absorption dips or
eclipses), if present. We examined all the RXTE archival observations
of the sources in our sample. For each observation, we computed power
spectra from RXTE/PCA data using custom software under IDL in the energy
band 2-26 keV (absolute PCA channel 0 to 62). We used 128 s-long intervals
and a Nyquist frequency of 1024 Hz. We averaged the power density spectrum
(PDS) and subtracted the contribution due to Poissonian noise (see
Zhang et al. 1995ApJ...449..930Z 1995ApJ...449..930Z). The PDS were normalized according to
Leahy, Elsner & Weisskopf (1983ApJ...272..256L 1983ApJ...272..256L) and converted to square
fractional rms (Belloni & Hasinger 1990A&A...230..103B 1990A&A...230..103B). We selected for
our analysis only observations where a somewhat narrow (quality factor Q>2)
low-frequency (<50 Hz) feature was identifiable on top of flat-top or
power-law shaped noise components in the PDS.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 139 16 List of BH transients and outbursts included
in this work
table2.dat 99 564 QPO, noise and total rms from all the
observations on the sources of our sample
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See also:
J/ApJ/698/1398 : H1743-322 2003 outburst (McClintock+, 2009)
J/MNRAS/415/292 : MAXI J1659-152 2010 outburst analysis (Munoz-Darias+, 2011)
J/MNRAS/422/679 : Spectral parameters for MAXI J1543-564 (Stiele+, 2012)
J/MNRAS/426/1701 : High-frequency QPO in black hole binaries (Belloni+, 2012)
J/MNRAS/428/1704 : XTE J1550-564 quasi-periodic oscillations (Li+, 2013)
J/MNRAS/428/2500 : GX 339-4 radio/X-ray flux correlation (Corbel+, 2013)
J/MNRAS/431/L107 : Outbursts of GX339-4 at 5.5 and 9.0GHz fluxes
(Corbel+, 2013)
J/MNRAS/431/3510 : GX 339-4 X-ray binary (Salvesen+, 2013)
J/ApJ/808/144 : Swift/XRT 0.5-10keV obs. of MAXI J1659-152 (Kalamkar+, 2015)
J/ApJS/222/15 : WATCHDOG: an all-sky database of Galactic BHXBs
(Tetarenko+, 2016)
J/ApJ/853/150 : Spectral analysis of low-mass X-ray binaries (Sonbas+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Name Name of system
17 A1 --- n_Name [*] System from Table 2, added in this Table
by the CDS
19- 52 A34 --- Outb-Y Year(s) of outburst
54- 69 A16 --- Outb-M Months of outburst
71- 72 A2 --- lbi [<≥∼ ] Limit flag on b_i
73- 76 F4.1 deg b_i [20.7/75]? Inclination, lower value (1)
78- 80 F3.1 deg ebi [1/3.8]? Uncertainty in b_i (1)
81 A1 --- nbi [abc] Note on b_i (2)
83- 84 I2 deg B_i [55]? Inclination, upper value (1)
86-117 A32 --- Com Comments (3)
119 A1 --- n_Com [d] Note on Com (4)
121-130 A10 --- Ref Reference(s) (5)
132 I1 --- TypeA [1/5]? Number of Type-A QPO
134-135 I2 --- TypeB [1/42]? Number of Type-B QPO
137-139 I3 --- TypeC [2/108]? Number of Type-C QPO
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Note (1): Inclination measurements come either form the X-rays or from
multiwavelength observations (moslty optical and radio).
Note (2): Note as follows:
a = Assuming that the radio jet is perpendicular to the accretion disc;
b = Inclination ∼60° if accretion disc does not contribute to the optical
luminosity in quiescence;
c = The constrain is placed assuming that the mass of the BH should not be
larger than 20 M☉.
Note (3): In the column comments we report some information about the behaviour
of the sources relevant to distinguish between high- and low-inclination
systems. With high-inclination evolution (High-IE), intermediate-inclination
evolution (Int.-IE) and low-inclination evolution (Low-IE) we refer to high,
intermediate and low disc temperatures, respectively, as reported in
Munoz-Darias et al. (2013MNRAS.432.1330M 2013MNRAS.432.1330M). As discussed by these authors,
the differences in the disc temperatures can be largely ascribed to the
inclination of the disc to the line of sight. With the term spikes, we refer
to flux spikes visible in both the light curve and hardness-intensity diagrams
(HIDs) of most high-inclination systems (see Munoz-Darias et al.
2013MNRAS.432.1330M 2013MNRAS.432.1330M). The term winds or dipping indicate that equatorial winds
or absorption dips, respectively, have been reported for that source.
Note (4): Note as follows:
d = See Soleri et al. (2013MNRAS.429.1244S 2013MNRAS.429.1244S).
Note (5): Reference as follows:
0 = Neustroev et al. (2014MNRAS.445.2424N 2014MNRAS.445.2424N);
1 = Orosz et al. (2002ApJ...568..845O 2002ApJ...568..845O);
2 = Orosz et al. (2004ApJ...616..376O 2004ApJ...616..376O);
3 = Munoz-Darias, Casares & Martinez-Pais (2008MNRAS.385.2205M 2008MNRAS.385.2205M);
4 = Miller-Jones et al. (2011MNRAS.415..306M 2011MNRAS.415..306M);
5 = Corral-Santana et al. (2011MNRAS.413L..15C 2011MNRAS.413L..15C);
6 = Orosz et al. (2011ApJ...730...75O 2011ApJ...730...75O);
7 = Homan et al. (2001ApJS..132..377H 2001ApJS..132..377H);
8 = Kuulkers et al. (1998ApJ...494..753K 1998ApJ...494..753K);
9 = Tomsick, Lapshov & Kaaret (1998ApJ...494..747T 1998ApJ...494..747T);
10 = Greene, Bailyn & Orosz (2001ApJ...554.1290G 2001ApJ...554.1290G);
11 = Corbel et al. (2005ApJ...632..504C 2005ApJ...632..504C);
12 = Steiner et al. (2012MNRAS.427.2552S 2012MNRAS.427.2552S);
13 = Homan et al. (2005ApJ...623..383H 2005ApJ...623..383H);
14 = Kuulkers et al. (2013A&A...552A..32K 2013A&A...552A..32K).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- Type Type of QPO (1)
4- 19 A16 --- Name Name of system
21- 23 I3 --- No [1/564] Observation number
25- 39 A15 --- ID Observation identifier
41- 46 F6.3 Hz Freq [0.106/31.555] Frequency
48- 53 F6.4 Hz E_Freq [0.001/0.694] Upper limit uncertainty in Freq
55- 60 F6.4 Hz e_Freq [0.001/0.694] Lower limit uncertainty in Freq
62- 65 F4.1 % rmsQPO [0.3/22.2] rms of the QPO
67- 69 F3.1 % E_rmsQPO [0/3.3] Upper limit uncertainty in rmsQPO
71- 73 F3.1 % e_rmsQPO [0/1.7] Lower limit uncertainty in rmsQPO
75- 78 F4.1 % rmsNoise [0/44.5] rms of the noise
80- 82 F3.1 % E_rmsNoise [0/7.4]? Upper limit uncertainty in rmsNoise
84- 86 F3.1 % e_rmsNoise [0/4.6]? Lower limit uncertainty in rmsNoise
88- 91 F4.1 % rmsTot [3.4/64.1] Total rms for observation
93- 95 F3.1 % E_rmsTot [0/7] Upper limit uncertainty in rmsTot
97- 99 F3.1 % e_rmsTot [0/4.4] Lower limit uncertainty in rmsTot
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Note (1): Type as follows:
C1 = Type-C - Low inclination;
C2 = Type-C - Intermediate inclination;
C3 = Type-C - High inclination;
B1 = Type-B - Low inclination (< 70°);
B2 = Type-B - Intermediate inclination;
B3 = Type-B - High inclination (> 70°).
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 28-Oct-2019