The micro Seyfert galaxy NGC-4395 hosts a supermassive black hole at its center that
actively accrete matter and thus radiates very strongly in the X-ray range. Denoted
the active galactic nucleus this thesis focuses on determining its spin. The spin parameter
corresponds to the angular momentum of the black hole and the properties of the
accretion disk surrounding the black hole.
Our spectrum was obtained from satellite telescope XMM-Newton and was analysed
in the range of
3 to 10 keV using the X-ray spectral fitting software XSPEC with the
standard models provided. A good fit was found, and therefore a good description of the
parameters describing the black hole and its disk. These start values were used for the
far more advance model
KERRCONV*REFLIONX which contains the spin.
Specially noteworthy is the broad and narrow Iron
Kemission lines normally occurring
6:4 keV whose form tells which different relativistic or gravitational effects that
affects the emissivity. In our spectrum both the broad and narrow Fe emission lines were
prominent as shown by the significant improvement in
2. Furthermore the reflected
component of our fit completely dominated our spectra and a majority of the emission
originates from the innermost regions of the disk, probably caused by strong gravitational
light bending revealing a closely positioned corona. The high value obtained on the spin
parameter seems to be consistent with the relatively low mass and possibly implies a
coherent accretion during the black holes formation.
2013. , 29 p.