J/MNRAS/428/1704 XTE J1550-564 quasi-periodic oscillations (Li+, 2013)
The energy dependence of the centroid frequency of the low-frequency
quasi-periodic oscillations in XTE J1550-564.
Li Z.B., Qu J.L., Song L.M., Ding G.Q., Zhang C.M.
<Mon. Not. R. Astron. Soc., 428, 1704-1714 (2013)>
=2013MNRAS.428.1704L 2013MNRAS.428.1704L
ADC_Keywords: Binaries, X-ray
Keywords: accretion, accretion discs - black hole physics -
stars: individual: XTE J1550-564 -
stars: low-mass - stars: oscillations - X-rays: binaries
Abstract:
In this paper, we investigate the energy dependence of the centroid
frequency of the low-frequency quasi-periodic oscillations (QPOs;
0.08-20Hz) in XTE J1550-564. We have used the observational data from
the Rossi X-ray Timing Explorer during the first half part of the
1998-1999 outburst. We have found that the centroid frequency of the
fundamental QPO did not vary with photon energy when its QPO frequency
was less than ∼0.4-0.8Hz and it did not increase much when its
frequency was between ∼0.8 and ∼3.3Hz. However, it clearly increased
with photon energy when it was larger than ∼3.3Hz. The most
interesting point is that it increased much more quickly with photon
energy when its centroid frequency was between ∼6 and ∼8.5Hz.
Subsequently, its rising rate dropped sharply when its frequency was
larger than ∼8.5Hz.
Description:
Sobczak et al. (2000ApJ...531..537S 2000ApJ...531..537S) and Remillard et al.
(2002ApJ...564..962R 2002ApJ...564..962R) have analysed the X-ray power density spectra
(PDS) for all 209 RXTE observations of XTE J1550-564 during its major
outburst of 1998-1999, and they have detected all three types of
LFQPOs. Most of these are type C and occurred in the first half of the
outburst (Sobczak et al. 2000ApJ...544..993S 2000ApJ...544..993S). We have reanalysed the
data and we have focused on those observations with LFQPOs during the
first half part of the 1998-1999 outburst that include all three types
of QPOs.
The observation IDs (ObsIDs) and QPO frequency are listed in Table 1.
The properties of the first-harmonic and subharmonic QPOs are listed
in Tables 2 and 3, respectively.
Objects:
--------------------------------------------------------
RA (2000) DE Designation(s)
--------------------------------------------------------
15 50 58.78 -56 28 35.0 XTE J1550-564 = V* V381 Nor
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 93 52 Fundamental QPO observations
table2.dat 93 39 First harmonic QPO observations
table3.dat 93 23 Subharmonic QPO observations
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See also:
J/A+A/496/765 : R light-curve of TT Ari (Kim+, 2009)
J/A+A/265/77 : VBLUW Observations of TT Ari (Hollander+ 1992)
J/ApJ/728/9 : QPO from XTE J1701-462 (Barret+, 2011)
J/MNRAS/426/1701 : High-frequency QPO in black hole binaries (Belloni+, 2012)
Byte-by-byte Description of file: table[123].dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- ObsID Observation ID of those observations
exhibiting low frequency QPOs
18- 25 F8.2 d MJD Modified Julian date
27- 32 F6.3 Hz b_Freq Lower value of frequency range
33 A1 --- --- [-]
34- 38 F5.2 Hz B_Freq Upper value of frequency range
40- 43 F4.2 --- chi2 χ2 value
45- 46 I2 --- dof [12/79] Degrees of freedom
48- 53 F6.3 Hz Freq QPO frequency (1)
55- 59 F5.3 Hz e_Freq rms uncertainty on QPO frequency
61- 65 F5.2 % Amp Amplitude of oscillation
67- 70 F4.2 % e_Amp rms uncertainty on Amplitude (95% confidence)
72- 79 F8.5 --- Slope Slope of frequency versus energy relation
81- 87 F7.5 --- e_Slope rms uncertainty on Slope
89- 93 F5.2 --- Corr [-1/1] Correlation coefficient frequency/energy
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Note (1): Fundamental frequency for table1, first harmonic for table2,
subharmonic for table3.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 31-Jan-2014