D. Porquet

X-ray flares reveal mass and angular momentum of the Galactic Center black hole

We have analysed the light curve of the two brightest X-ray flares from the Galactic Center black hole, one flare observed by XMM-Newton on Octoberxa03,xa02002 (Porquet etxa0al. [CITE]), and the other flare observed by Chandra on Octoberxa026,xa02000 (Baganoff etxa0al. [CITE]). The power density spectra show five distinct peaks at periods ofxa0~100u2009s, 219u2009s, 700u2009s, 1150u2009s, andxa02250u2009s common to both observations within their estimated measurement uncertainties. The power density spectrum of the recently reported infrared flare of Junexa016,xa02003 (Genzel etxa0al. [CITE]) shows distinct peaks at two, if not three, periods (including the

XMM-Newton observation of the Seyfert 1.8 ESO 113-G010: Discovery of a highly redshifted iron line at 5.4 keV

1008 pm 120

Discovery of a bright X-ray transient in the Galactic Center with XMM-Newton

u2009s infrared period), which are consistent with the X-ray periods. The remaining two periods could not be covered by the infrared measurements. Each period can be identified with one of the characteristic gravitational cyclic modes associated with accretion disks, i.e. either Lense-Thirring precession, Kepler orbital motion and the vertical and radial epicyclic oscillation modes, in such a way that a consistent value for the black hole mass ofxa0

Discovery of X-ray eclipses from the transient source CXOGC J174540.0-290031 with XMM-Newton

Msb{rm{BH}} = 2.72sp{+0.12}sb{-0.19}times 10sp 6~M_odot

The surprising Far-UV spectrum of the polar BY Camelopardalis

and the angular momentum

An XMM-Newton view of the X-ray flat radio-quiet quasar PG 1416 129

a = 0.9939sp{+0.0026}sb{-0.0074}

Far-UV FUSE Spectra of Peculiar Magnetic Cataclysmic Variables

is obtained. The available data onxa0

Abnormal CNO abundances in magnetic cataclysmic variables

Msb{rm{BH}}

The highly red-shifted FeKα line in ESO 113-G010

derived from studies of the orbital motion of the S2xa0(S0-2) star (Schodel etxa0al. [CITE]; Ghez etxa0al. [CITE]) agree with our findings. Finally we discuss some implications of the fairly high value for the angular momentum.

Discovery of X-ray eclipses from the transient source located at only 0.1PC from SGR A*

We present a spectral analysis of the Seyfert 1.8 ESO 113-G010 observed with XMM-Newton for 4 ks. The spectrum shows a soft excess below 0.7 keV and more interestingly a narrow emission Gaussian line at 5.4 keV (in its rest-frame), most probably originating from a redshifted iron Kα line. No significant line at or above 6.4 keV is found contrary to other objects showing redshifted lines, ruling out a strong blue-wing to the line profile. The line is detected at 99% confidence, from performing Monte Carlo simulations which fully account for the range of energies where a narrow iron line is likely to occur. The energy of the line could indicate emission from relativistic (0.17-0.23 c) ejected matter moving away from the observer, as proposed for Mrk 766 by Turner et al. (2004, ApJ, 603, 62). Alternatively, the emission from a narrow annulus at the surface of the accretion disk is unlikely due to the very small inclination angle (i.e. less than 10 ◦ ) required to explain the narrow, redshifted line in this intermediate Seyfert galaxy. However emission from a small, localized hot-spot on the disk, occurring within a fraction of a complete disk orbit, could also explain the redshifted line. This scenario would be directly testable in a longer observation, as one would see significant variations in the energy and intensity of the line within an orbital timescale.