# 0.1 Hz QPOs during RXTE observations of IGR J17091-3624

ATel #3168; * ***J. Rodriguez, S. Corbel (UMR AIM, CEA-Saclay, University Paris 7, CNRS, France) J. A. Tomsick (SSL Berkeley, USA), A. Paizis (INAF, Milano, Italy), E. Kuulkers (ESA/ESAC, Madrid, Spain)**

on **15 Feb 2011; 19:42 UT**

Distributed as an Instant Email Notice Transients

*Credential Certification: S. CORBEL (corbel@discovery.saclay.cea.fr)*

Subjects: X-ray, Transient

After the report of renewed activity of IGR J17091-3624 as seen
with Swift (ATel #3144, #3148, #3167), with the confirmation of the nearby
source IGR J17098-3628 being dormant, we observed this region with RXTE.
4 pointings have been performed on Feb 9, 10, 12, and 14, 2011.

Inspection of the PCA spectra show some contamination by the nearby (0.67 deg away)
X-ray binary GX 349+2. We roughly estimate the contribution of this source
to be about 287 cts/s over the ~2-60 keV PCA range. We assume a constant rate over all
our observations.

The net ~2-60 keV count rate of IGR J17091-3624 increased from ~82cts/s to ~278cts/s,
but then decreased to ~121 cts/s from the first to the third obs. In the last observation it
increased again to ~308 cts/s.

We analysed the Good Xenon data and extracted ~2-60 keV light curves with a
time resolution of ~1ms (2^(-10) s). In the first observation
the power density spectrum (PDS) is consistent with Poisson noise
above ~1Hz. It shows large variability below this frequency. A single
zero-centred Lorentzian is sufficient to account for the continuum.
The total amplitude is estimated to be 26% although the uncertainties here
are large.

In the 2nd observation the PDS is consistent with Poisson noise above 10 Hz.
The 0.01-10 Hz PDS is well represented (red. chi square=1.21 for 159 dof)
by the sum of 3 Lorentzians, all zero centred, with a total power
of about 15% RMS over this frequency range.
Large residuals are, however, present at around 0.1 Hz. Adding
another Lorentzian improves the fit to 1.02 for 156 dof (chance probability of
1.7e-06 according to an F-test).
The last feature has a frequency of 9.4+/-0.3 e-2 Hz, a
quality factor Q~9.1, and an RMS amplitude of 3.2+/-0.2%.

In the third observation, the PDS is consistent
with Poisson noise above typically 5 Hz. Two broad Lorentzians are sufficient
to represent the continuum. The total RMS amplitude is ~15%.
A thin feature is also present in the residuals.
A Lorentzian with freq=0.105 -0.003 +0.004 Hz, Q=7.4 ,A=3.4 (-0.3 +0.2)%
improves the fit (chance probability of 2.3e-4 according to an F-test).

The PDS of the 4th observation is consistent with Poisson noise above
1 Hz (the observation is much shorter). Below 1 Hz the continuum is well
represented by the sum of 2 zero-centred Lorentzians with a total
RMS amplitude 12.3%. The fit also requires the addition of a QPO for a
good fit to be achieved (chance probability of 2.2e-4 according to an F-test).
The QPO has the following parameters: freq=0.13+/-0.01, Q=3.5, and
A=4.5 (+/-0.3) %.

We note that the uncertainties quoted do not take into account the uncertainties
in the estimate of the flux from GX349+2.
A ~0.1 Hz feature has never been reported for GX 349+2 despite
the huge number of observations dedicated to this source. We, therefore, attribute
the QPO to IGR J17091-3624.

This is the first report of a low frequency QPO in this source. This and
the increasing frequency in correlation with the increase of flux, is consistent
with a black hole binary in its hard state. More observations of this source in its outburst are encouraged.