skip to content
 
ASCA Guest Observer Facility

MCG-6-30-15

MCG-6-30-15

Image Credit: Tanaka et al., Copyright: Nature, 375, 659, 1995
Image generated by Dr. Paul Nandra NASA/GSFC

The line profile of iron K-alpha from MCG-6-30-15 observed by the ASCA satellite (Tanaka et al, 1995, Nature, 375, 659). The emission line is extremely broad, with a width indicating velocities of order one-third of the speed of light. There is a marked asymmetry towards energies lower than the rest-energy of the emission line (6.4 keV). This asymmetry is most likely caused by gravitational and relativistic-Doppler shifts near the black hole at the center of the galaxy. The solid line shows the model profile expected from a disk of matter orbiting the hole, extending between 3 and 10 Schwarzschild radii.
Get the Color Postscript image. of this spectrum.

For more information see:
"On the dependence of iron K-line profiles with luminosity in Active Galactic Nuclei"; Nandra, K., Mushotzky, R.F., George, I.M., Turner, T.J. , Yaqoob, T. 1997, ApJ, 488, L91

There is also a simulation of a black hole that may explain this result.


This file was last modified on Wednesday, 16-Feb-2005 12:04:47 EST
Curator: Michael Arida (SP Sys); arida@milkyway.gsfc.nasa.gov
HEASARC Guest Observer Facility


If you have any questions concerning ASCA, visit our Feedback form.

This file was last modified on Wednesday, 16-Feb-2005 12:04:47 EST

NASA Astrophysics

  • FAQ/Comments/Feedback
  • Education Resources
  • Download Adobe Acrobat
  • A service of the Astrophysics Science Division (ASD) at NASA/ GSFC

    ASCA Project Scientist: Dr. Nicholas E. White

    Responsible NASA Official: Dr. Andy Ptak

    Privacy Policy and Important Notices.