Proposals from the following XMM scientific categories were
awarded Chandra time by the XMM-Newton AO4 peer review as part of
the CXO/XMM-Newton joint proposal program:
Active Galactic Nuclei, Quasars, BL-Lac Objects and X-ray Background
White Dwarf Binaries, Neutron Star Binaries, Cataclysmic Variables, ULXs and Black Holes
| PI Name | Proposal # | Title | XMM Priority | Chandra time | Targets |
|---|---|---|---|---|---|
| Reeves | 06701082 | Revealing the Relativistic Iron line in the Seyfert 1.9 Galaxy, MCG-5-23-16 | B | MCG -5-23-16 | |
| Wijnands | 06401083 | Monitoring observations of the Galactic Center region | B | GC-1,GC-2,GC-3,GC-7,GC-8,GC-9,GC-10 |
Scientific Category: ACTIVE GALAXIES AND QUASARS
Title: Revealing the Relativistic Iron line in the Seyfert 1.9 Galaxy, MCG-5-23-16
PI: Reeves
Approved Chandra Time (Ksecs): 50.0
Abstract:
We propose a 130ks observation of the X-ray bright Seyfert 1.9 galaxy MCG -5-23-16 with XMM-Newton. Our present analysis of the short XMM observations of MCG-5-23-16 reveals one the best known examples of a relativistically broadened iron K line, with the red-wing of the line extending down to 5keV in the EPIC data. Indeed MCG-5-23-16 is one of only a handful of objects that clearly show a broad iron line with XMM-Newton. Therefore it is imperative that we study the iron K line emission in this Seyfert galaxy in much greater detail. We also propose for a simultaneous 50ks Chandra/HETGS observation, to constrain the narrow core of the line. These observations will not only confirm the existence of the broad disk line, but also enable us to determine the accretion disk geometry.
Scientific Category: BH AND NS BINARIES
Title: Monitoring observations of the Galactic Center region
PI: Wijnands
Approved Chandra Time (Ksecs): 70.0
Abstract:
We propose a monitoring campaign using XMM-Newton and Chandra of a 2 by 1 degee region centered on the Galactic Center. We will be able to detect transients which occur near the Galactic Center with a peak luminosity of 1E33-1E35 ergs/s, 10 to 1000 times more sensitive than what is possible with other satellites (i.e., RXTE and INTEGRAL). This allows us to observe a very poorly studied group of X-ray transients and to follow the luminosity behavior of weak (<1E36 ergs/s) persistent sources.