Discovery of 10 mHz quasi-periodic oscillations likely from IGR J17091-3624
ATel #3225; D. Altamirano (Amsterdam), M. Linares (MIT), M. van der Klis, R. Wijnands, M. Kalamkar (Amsterdam), P. Casella (Southampton), A. Watts, A. Patruno, M. Armas-Padilla, Y. Cavecchi, N. Degenaar, R. Kaur, Y. Yang (Amsterdam), N. Rea (CSIC-IEEC)
on 17 Mar 2011; 19:56 UT
Credential Certification: Manuel Linares (firstname.lastname@example.org)
Subjects: X-ray, Black Hole, Neutron Star, Transient
We report the discovery of ~10 mHz quasi-periodic oscillations (QPOs)
in a 3.5 ks RXTE observation of the black hole candidate IGR
J17091-3624 (ATELs #3144, #3159, #3167, #3203) on March 14th
2011 (MJD 55634.66). Only PCU2 was active, with an average 2-60 keV
background-corrected count rate of 110 counts/s.
The QPO is visible by eye in the light curve during the first ~1000
seconds and the last ~1500 seconds, with an average 2-60 keV fractional
rms amplitude of 5.3+-0.4% and a mean frequency of ~10 mHz. The
fractional rms amplitude increases from ~3.5% below 5 keV to a maximum
of ~10% in the 15-30 keV range. No oscillation is detected in the
central ~1000 seconds of the observation, with a 3 sigma upper limit
on the fractional rms amplitude of 2.4%. In the same observation we
find two QPOs at 2.3+-0.3 Hz and 8.0+-0.3Hz, with fractional rms
amplitudes of 10.9+-0.8% and 6.7+-1.2%, respectively.
IGR J17091-3624 is located in a crowded field, with the bright
neutron-star system GX 349+2 and the black-hole candidate IGR
J17098-3628 at a distance of ~41 and ~9 arcmin, respectively. An
offset of 25' was applied during the observation described here,
avoiding the contribution from GX 349+2 but including
both the nominal target and IGR J17098-3628 in the 1 degree PCA field
of view. IGR J17098-3628 is thought to be in quiescence (ATEL #3148),
but we cannot exclude that it is active.
Both IGR J17091-3624 and IGR J17098-3628 have been
tentatively identified as black-hole candidates (Lutovinov &
Revnivtsev 2003, AstL, 29, 719; Capitanio et al 2009, ApJ
690, 1621). Similarly low-frequency oscillations have been seen in
the BHC GRS 1915+105 (Morgan et al. 1997, ApJ, 482, 993). However, in
that source the mHz QPO was seen together with strong (>20 %) 0.1-50
Hz broadband noise, which is not the case in our observation (<12%).
The mHz QPO from IGR J17098-3628 has also different properties than
the so-called Type C QPOs (e.g., Casella et al. 2005, ApJ, 629, 403),
which are also observed together with strong broadband noise and
at higher frequencies.
We note that mHz QPOs have been reported in 4 neutron star systems
(Revnivtsev et al, 2001, A&A, 372, 138; Linares et al., 2010, ATEL #2958).
However, the fractional rms amplitude of those oscillations typically
decreases with energy, opposite to what we find in the present work.