| Miscellaneous :
| Tuerler et al. 2009 ATel 1997:
- 20-40 keV flux of ~14 +/- 2 mCrab, not detected at higher energies
- Averaged spectrum of the source is consistent with a single powerlaw in Γ= 4.0=>20-40 keV flux =1.1 E-10 erg/cm^2/s.
- Do not exclude an association with 2E 1927.5+1805
| Rodriguez et al. 2009 ATel 1998:
- Analyses of Swift archival observations performed on 2007 december 9 and 13.
- Source = Swift 1929.8+1821 at position inconsistent with that of the 2E 1927.5+1805
- 2MASS J19295591+1818382 is counterpart with infrared magnitudes J=14.56 ±0.03, H=12.99 ±0.02 and Ks=12.11±0.02.
- Swift spectrum is well fitted with an absorbed power law, or an absorbed black body
- NH=3.7x1022 cm-2, Γ=0.8,
F2-10 keV, unabs=3.6e-11 erg/s/cm-2 (power law)
- kTbb=2.1 keV F2-10 keV, unabs.=3.0e-11 erg/s/cm2 (BBody), with size
RBB=(0.46 * D10 kpc) km (D10 kpc distance to the source in units
of 10 kpc)
- Feature at 8.0e-2Hz in the power spectrum, could be a coherent pulsation
although nothing seen in folded light curve
- IGR J19294+1816 is more likely associated to Swift J1929.8+1821
- Possible X-ray binary possibly containing a pulsar
| Krimm et al. 2009 ATel 1999:
- Detection in Swift/BAT archival observations
- Earliest detection reported: January 13, 2006, 6 additional detections since then
- Recent increased activity seen on March 23, 2009 (NOT
2008 as reported in the ATel), after March 28 the
source has faded below detectability.
- Possible sort of periodicity in the system at a period of ~56 days as seen from
the period of detections with the BAT.
| Strohmayer et al. 2009 ATel 2002:
- RXTE Observation show pulsation at 12.44s and harmonics
- Amplitude of pulse 37%
- Highly variable phase average flux, possible quasi period of 190 s
- Confirms the object is a possible pulsar
| Corbet and Krimm 2009 ATel 2008:|
- Analysis of the Swift/BAT light curve covering the
period Jan 1st 2006 to April 2 2009
- Strong peak in the powe spectrum of the source at a period of 117 days<=>
associate with the orbital period of the source
- Occurrences of high flux at half this period=>interaction of the neutron star with the disk of the donor star.
Tpeak (MJD) = 54,680.3 (+/- 0.6) + n x 117.2 (+/- 0.2)
- Region of Be systems in the Corbet Diagram, compatible with the transient nature of this system.
| Rodriguez et al. 2009 A&A:|
- Multi-instrumental (Swift, INTEGRAL, RXTE) analysis
- 2MASS J19295591+1818382 has J=14.56, H=12.99 and Ks=12.11.
- Swift and RXTE spectral analysis => rather hard source / evidence for local absorption in one observation
- Timing study => barycentred period of 12.43781 s <=> spin period of a pulsar binary
- Results compatible with a Be-HMXB but INTEGRAL => occurrences of short and intense flares
reminiscent of SFXT ie system with a supergiant companion.
- Definitive conclusion on the nature Be vs Sg not possible
| Bozzo et al. 2010
- ISGRI detection of a new outburst
- Spectrum can be fit with a blackbody at a temperature of 4.8 keV.
| Jenke et al. 2010
- Fermi-GBM. The barycenter-corrected pulse frequency is 80.3111(4) mHz for data corresponding to 27-29 October, 2010
| Bozzo et al. 2011 A&A :|
- INTEGRAL and Swift observations during 2010 outburst
- Source flux decayed smoothly over a period of 2 months without spectral changes
- Pulsations at 12.5s up to 50 keV
- Marginal detection of the ~116d period
- Very probably a Be-HMXB rather than an SFXT
| Finger et al. 2012 ATel 3917 :|
- Detection of pulsed flux with Fermi GBM
- Pulsed flux ~15 mCrab in the 12-50 keV range
- Pulsation has a barycentric frequency of 80.2754 mHz
| Fiochi et al. 2012 ATel 4135 :|
- Renewed activity with INTEGRAL/IBIS on may 26 2012
- 18-60 keV spectrum is well fitted by a power law model with Gamma~3.6
- Detection consistent with the rise of a new outburst and compatible
with the known orbital period of 117 days.
| Sidoli et al. 2012 ATel 4136 :|
- Swift observations after renewed activity
- XRT spectrum well described by absorbed power law model,
with Γ~1.25 and NH~ 8 x 1022 cm-2
- 2 keV absorbed (NH~ 4 x1022 cm-2) black body provides a good fit
- Detection of X-ray pulsations at P=12.457 at a fraction
of ~ 60%.