Binary corrected X-ray light curve of Cygnus X-3: Implications 
for the timing properties of the compact binary system

Choudhury, Manojendu; Rao, A. R.; Vadawale, S.; Jain, Abhay; Singh, Nilkamal

doi:10.1051/0004-6361:20040110

Cited by 7 publications

(15 citation statements)

References 32 publications

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“…No signal is detected above 0.1 Hz. The slope and rms noise levels of the PDS are similar to previous studies (Choudhury et al 2004; Axelsson, Larsson & Hjalmarsdotter 2009). One noticeable difference can be seen in the power spectrum #2 with a lower noise level.…”

Section: Discussionsupporting

confidence: 88%

A giant radio flare from Cygnus X-3 with associated γ-ray emission

Corbel

Dubus

Tomsick

et al. 2012

Monthly Notices of the Royal Astronomical Society

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With frequent flaring activity of its relativistic jets, Cygnus X‐3 (Cyg X‐3) is one of the most active microquasars and is the only Galactic black hole candidate with confirmed high‐energy γ‐ray emission, thanks to detections by Fermi Large Area Telescope (Fermi/LAT) and AGILE. In 2011, Cyg X‐3 was observed to transit to a soft X‐ray state, which is known to be associated with high‐energy γ‐ray emission. We present the results of a multiwavelength campaign covering a quenched state, when radio emission from Cyg X‐3 is at its weakest and the X‐ray spectrum is very soft. A giant (∼20 Jy) optically thin radio flare marks the end of the quenched state, accompanied by rising non‐thermal hard X‐rays. Fermi/LAT observations (E≥ 100 MeV) reveal renewed γ‐ray activity associated with this giant radio flare, suggesting a common origin for all non‐thermal components. In addition, current observations unambiguously show that the γ‐ray emission is not exclusively related to the rare giant radio flares. A three‐week period of γ‐ray emission is also detected when Cyg X‐3 was weakly flaring in radio, right before transition to the radio quenched state. No γ‐rays are observed during the ∼1‐month long quenched state, when the radio flux is weakest. Our results suggest transitions into and out of the ultrasoft X‐ray (radio‐quenched) state trigger γ‐ray emission, implying a connection to the accretion process, and also that the γ‐ray activity is related to the level of radio flux (and possibly shock formation), strengthening the connection to the relativistic jets.

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Section: Discussionsupporting

confidence: 88%

A giant radio flare from Cygnus X-3 with associated γ-ray emission

Corbel

Dubus

Tomsick

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…Reig, Papadakis & Kylafis (2002) find that the power spectrum of the microquasar GRS 1915+105 is well fitted by a power law (equation 11) with index β ≃ 1 in the frequency range 10 −7 to 10 −5 Hz. A power spectrum with this slope, over the same frequency range, has been also found for the X-ray light curve of Cygnus X-3 by Choudhury et al (2004).…”

Section: Calibration From Microquasarssupporting

confidence: 67%

“…The X‐ray light curve of GRS 1915+105 has a power spectrum with amplitude P 0 ω 0 ∼ 0.02 at frequencies 10 −7 –10 −5 Hz (Reig et al 2002). An amplitude smaller by a factor of ∼10 has been measured for the X‐ray power spectrum of Cygnus X‐3 in the same frequency range (Choudhury et al 2004). However, there is evidence that the amplitude of the variability of the radio emission of these powerful microquasars is larger than that of their X‐ray emission (Nipoti et al, 2005).…”

Section: Conceptual Frameworkmentioning

confidence: 86%

Time variability of active galactic nuclei and heating of cooling flows

Nipoti

Binney

2005

Monthly Notices of the Royal Astronomical Society

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There is increasing evidence that active galactic nucleus (AGN) feedback is important in the energetics of cooling flows in galaxies and galaxy clusters. It is possible that, in most cooling‐flow clusters, radiative losses from the thermal plasma are balanced, over the cluster lifetime, by mechanical heating from the central radio source. We investigate the implications of the variability of AGN mechanical luminosity Lm on observations of cooling flows and radio galaxies in general. It is natural to assume that ℓ= ln (Lm/LX) is a Gaussian process. Then Lm will be lognormally distributed at fixed cooling luminosity LX, and the variance in a measure of Lm will increase with the time resolution of the measure. We test the consistency of these predictions with existing data for cooling flows and radio galaxies. These tests hinge on the power spectrum P(ω) of the Gaussian process ℓ(t). General considerations suggest that P is a power law P∼ω−β. Long‐term monitoring of Seyfert galaxies combined with estimates of the duty cycle of quasars imply that β≃ 1, which corresponds to flicker noise. The power spectra of microquasars have similar values of β. We combine a sample of sources in cooling flows that have cavities with the assumption that the average mechanical luminosity of the AGN equals the cooling flow's X‐ray luminosity. Given that the mechanical luminosities are characterized by flicker noise, we find that their spectral amplitudes ωP(ω) lie between the estimated amplitudes of quasars and the measured values for the radio luminosities of microquasars. The model, together with the observation that powerful radio galaxies lie within a narrow range in optical luminosity, predicts the luminosity function of radio galaxies. Both the shape and the normalization of the predicted function are in agreement with observations. Forthcoming radio surveys will test the prediction that the luminosity function turns over at about the smallest luminosities so far probed.

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“…ingale et al (1985) and was found to be well described by a power law of index β = −1.8 in the frequency range 10 −5 -0.1 Hz. This result has been more or less verified in further studies by Choudhury et al (2004;β ∼ −1.5) and Axelsson et al (2009; β ∼ −2 in the canonical, disk-dominated soft X-ray state and −1.8 in the canonical, Comptonizationdominated hard X-ray state). The PDS has no power above 0.1 Hz, a result which was discussed in Berger & van der Klis (1994; they placed an upper limit of 12% rms above 1 Hz) and subsequently in Axelsson et al (2009).…”

supporting

confidence: 60%

The re-occurrence of mHz quasi-periodic oscillations in Cygnus X−3

Koljonen

Hannikainen

McCollough

2011

Monthly Notices of the Royal Astronomical Society: Letters

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We have re-analysed archival RXTE data of the X-ray binary Cygnus X−3 with a view to investigate the timing properties of the source. As compared to previous studies, we use an extensive sample of observations that include all the radio/X-ray spectral states that have been categorized in the source recently. In this study we identify two additional instances of quasi-periodic oscillations that have centroid frequencies in the mHz regime. These events are all associated to a certain extent with major radio flaring, which in turn is associated with relativistic jet ejection events. We review briefly scenarios whereby the quasi-periodic oscillations may arise.

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Binary corrected X-ray light curve of Cygnus X-3: Implications for the timing properties of the compact binary system

Cited by 7 publications

References 32 publications

A giant radio flare from Cygnus X-3 with associated γ-ray emission

A giant radio flare from Cygnus X-3 with associated γ-ray emission

Time variability of active galactic nuclei and heating of cooling flows

The re-occurrence of mHz quasi-periodic oscillations in Cygnus X−3

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