INTEGRAL detects renewed activity from IGR J19294+1816
ATel #4135; M. Fiocchi (INAF-IAPS, Roma, Italy), S. P. Drave (Southampton, UK), J. Chenevez (DTU Space, Denmark), L. Sidoli (INAF-IASF, Milano, Italy), Sguera (INAF-IASF; Bologna, Italy), A. J. Bird (Southampton, UK), E. Kuulkers (ESA/ESAC, Spain), L. Natalucci (INAF-IAPS, Roma, Italy), A. Tarana (INAF-IAPS, Roma, Italy)
on 29 May 2012; 11:36 UT
Credential Certification: mariateresa fiocchi (email@example.com)
Subjects: X-ray, Gamma Ray, Binary, Variables
Referred to by ATel #: 4136
During recent INTEGRAL Galactic Plane Scanning observation (PI: A. Bazzano),
starting 2012 may 26 at 10:38 UTC (total exposure time ~36.3 ks), IBIS/ISGRI detected renewed activity from the transient binary system IGR J19294+1816 (Atel #1997).
This hard X-ray transient was detected at about 9 sigma in the IBIS map 18-40 keV, with a flux of 18+/-2 mCrab (uncertainties at 90% c.l.).
Its 18-60 keV spectrum is well fitted by a power law model with photon index of 3.6(+0.8,-0.7) and reduced chi-squared of 0.97 (15 d.o.f.).
The source was inside the field of view of the JEM-X monitor during two pointings for a total of ~2.3 ks effective exposure and the estimated 3-10 keV flux is 13+/-3 mCrab.
This source is an X-ray transient accreting pulsar, with an outburst period of around 117 days (likely the binary orbital period; Corbet and Krimm 2009, ATel #2008)
and a spin period of about 12.44 seconds (Strohmayer et al. 2009, Atel #2002; Rodriguez et al. 2009).
Whilst the system is likely a Be X-ray Binary further observations are required to explain the short, intense SFXT-like flaring episodes observed in this source (Rodriguez et al. 2009).
The last reported outburst occurred on February 7, 2012 (Finger et al., 2012, Atel #3917), so the INTEGRAL detection is consistent
with the rise to a new outburst, actually expected in the first days of June 2012.
A Swift ToO follow-up has been approved and the data analysis will soon be performed.
Results from the Galactic Plane Scanning are made publicly available at: http://gpsiasf.iasf-roma.inaf.it/ .