A study of the low-frequency quasi-periodic oscillations in the X-ray light curves of the black hole candidate XTE J1859+226

By P. Casella, T. Belloni, J. Homan, L. Stella. 2004

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We present the results of an extensive timing analysis of the 1999 outburst of the soft X-ray transient and black hole candidate XTE J1859+226 as observed with the Rossi X-Ray Timing Explorer . Three main different types of low frequency (1-9 Hz) quasi-periodic oscillations (QPOs) were observed and classified, strengthening the general picture that is emerging for the variability properties of black hole X-ray binaires. Rapid transitions between different power spectral shapes were observed and their link with the count rate was studied. Furthermore, we show that a frequency of ~6 Hz seems to hold a particular place: one of the three QPO types we found was very stable when at this frequency, as it happens in Z sources as well. The coherence of its subharmonic peak was higher when the fundamental was close to 6 Hz, thus suggesting the presence of some resonance at this frequency.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/588363a157a3b16e0d13b5e067943153bfea4971

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The evolution of the timing properties of the black-hole transient GX 339-4 during its 2002/2003 outburst (2005, unknown): “…stable states, which can be observed for months or years, while the remaining states are often associated to state transitions and show strong and fast variations in their properties (see e.g. Miyamoto et al. 1994; Takizawa et al. 1997; Homan et al. 2001; Nespoli et al. 2003; Casella et al. 2004).”
WATCHDOG: A COMPREHENSIVE ALL-SKY DATABASE OF GALACTIC BLACK HOLE X-RAY BINARIES (2015, background): “— [251] Casella et al. (2004), [252] Sriram et al. (2013b), [253] Stephen et al. (2005), [254] Remillard & Smith (200 ), [255] Karasev et al. (2007), [256] Karasev et al. (2008), [257] Krimm et al. (2010), [258] Woods et al. (2002), [259] in’t Zand et al. (2002b), [260] Gogus et al. (2004), [261]…”
Precise mass and spin measurements for a stellar-mass black hole through X-ray timing: the case of GRO J1655-40 (2013, methodology): “Besides type-C QPOs, BH binaries commonly show two other types of LFQPOs, dubbed as type-A and B QPOs (Wijnands, Homan & van der Klis 1999; Casella et al. 2004), which are thought to be intrinsically different from type-C QPOs (Motta et al. 2011) and hence unsuited to be used in the framework of…”
Jets from black hole X-ray binaries: testing, refining and extending empirical models for the coupling to X-rays (2009, background): “Note that Casella et al. (2004) find that this region of the HIDis very rich in strong quasi-periodic oscillations (QPOs), and provide more details of the QPO phenomenology.”
The Evolution of Black Hole States (2004, background): “…more the 2002/2003 outburst of GX 339–4 as a template, we see that when the hardness goes below a well defined threshold, the timing properties change sharply: a clear type B QPO appears in the power density spectrum (Figure 3, see also Casella et al., 2004 for similar behavior in XTE J1859+226).”
Low-frequency oscillations in black holes: a spectral-timing approach to the case of GX 339-4 (2011, methodology): “Similar fast transitions between different types of QPOs have already been observed in GX 339-4 (Miyamoto & Kitamoto 1991) and in other sources, such as XTE J1859+226 (Casella et al. 2004) and GS 1124-68 (Takizawa et al. 1997).”
X-Ray Properties of Black-Hole Binaries (2006, background): “Unexpectedly, the phase lag measurements showed groups distinguished by positive, negative, and ∼zero lags defining, respectively, LFQPO types A, B, and C (Wijnands et al. 1999; Cui et al. 2000b; Remillard et al. 2002b; Casella et al. 2004).”
The ABC of Low-Frequency Quasi-periodic Oscillations in Black Hole Candidates: Analogies with Z Sources (2005, background): “…trend towards soft lags (i.e. soft X-ray variations lag those at hard X-ray energies) for increasing QPO frequency (see Reig et al. 2000), but they are usually consistently soft at the subharmonic and hard at the second harmonic (see e.g. Remillard et al. 2002; Casella et al. 2004, C04 hereafter).”