High Resolution X-ray Spectroscopy of the Fe K complex in IC 4329A
  We report the detection of complex Fe K line emission from a Chandra High Energy Transmission Grating Spectrometer observation of the Seyfert 1 galaxy IC 4329A. The line emission is double-peaked, one peak centered at ~6.3 keV, and the other at ~6.9 keV in the source rest frame. When modeled by Gaussians, the lower energy peak is resolved by the HEG at >99% confidence, whilst the higher energy peak is resolved at only <90% confidence. The best-fitting widths are \~21,000km/s and ~4000km/s FWHM for the ~6.3 keV and ~6.9 keV peaks respectively. If the peaks correspond to two distinct emission lines, then the peak energies are redshifted with respect to the expected line energies of Fe I Ka and Fe XXVI Lya by at least 650 km/s and 950 km/s respectively. Alternatively, the Fe K line profile may be due to a single line from a relativistic accretion disk. In that case the inclination angle of the disk is required to be 24^{+9}_{-1} degrees, the outer radius constrained to several tens of gravitational radii, and the radial line emissivity flatter than r^{-0.7}. Another possibility is that both peaks are due to distinct lines but each one relativistically broadened by a disk. In that case the lower energy peak could correspond to emission from Fe in a low ionization state, and the high-energy peak to Fe XXVI Lya emission. Then, the inclination angle is even less, restricted to a few degrees. However, the radial emissivity law is allowed to be steeper (~r^{-2.5}) and the outer radius does not have to be fine-tuned. Yet another scenario is that the lower energy peak originates in a disk but the higher energy peak originates in more distant matter. 
B.McKernan (1) and T.Yaqoob (2,3) ((1)University of Maryland, College   Park, (2) Johns Hopkins University, (3) NASA/GSFC)