| PI Name | Title | Chandra time | Targets |
|---|---|---|---|
| Aaron Barth | A Multiwavelength Study of POX 52, A dwarf Seyfert Galaxy with an Intermediate-Mass Black Hole | POX 52 | |
| John Biretta | HST/Chandra Monitoring of a Dramatic Flare in the M87 Jet | NGC 4486 |
Scientific Category: AGN/Quasars
Title: A Multiwavelength Study
of POX 52, A dwarf Seyfert Galaxy with an Intermediate-Mass
Black Hole
PI: Aaron Barth
Approved Chandra Time (Ksecs): 25
Abstract:
We propose a comprehensive optical, UV, and X-ray investigation of the
unique galaxy POX 52. POX 52 is a Seyfert 1 galaxy with
unprecedented properties: its host galaxy appears to be a dwarf
elliptical, and its stellar velocity dispersion is only 36
km/s. The stellar velocity dispersion and the broad
emission-line widths both suggest a black hole mass of order
10^5 solar masses, placing POX 52 in a region of AGN parameter
space that is almost completely unexplored at present. We
request ACS/HRC imaging to perform a definitive measurement of
the host galaxy structure; STIS UV and optical spectroscopy to
study the nonstellar continuum and the structure of the
broad-line region; and Chandra ACS imagin to detect the X-ray
emission from the nucleus and investigate its spectral and
variability properties. The results of this program will give a
detailed understanding of the host galaxy and accretion
properties of one of the very few known black holes in the mass
range around 10^5 solar masses.
Scientific Category: Jets, AGN Physics, BL LAC Objects and Blazars
Title: HST/Chandra Monitoring
of a Dramatic Flare in the M87 Jet
PI: John Biretta
Approved Chandra Time (Ksecs): 60
Abstract:
As the nearest galaxy with an optical jet, M87 affords an unparalleled
opportunity to study extragalactic jet phenomena at the highest
resolution. During 2002, HST and Chandra monitoring of the M87
jet detected a dramatic flare in knot HST-1 located ~1" from the
nucleus. As of late 2003 its brightness has increased
twenty-fold in the optical band, and continues to increase
sharply; the X-rays show a similarly dramatic outburst. In both
bands HST-1 now greatly exceeds the nucleus in brightness. To
our knowledge this is the first incidence of an optical or X-ray
outburst from a jet region which is spatially distinct from the
core source; this presents an unprecedented opportunity to study
the processes responsible for non-thermal variability and the
X-ray emission.
We propose seven epochs of HST/STIS monitoring during Cycle 13, as
well as seven epochs of Chandra/ACIS observation (5ksec
each). We also include a brief HRC/ACS observations that will be
used to gather spectral information and map the magnetic field
structure. This monitoring is continued into Cycles 14 and 15.
The results of this investigation are of key importance not only for
understanding the nature of the X-ray emission of the M87 jet,
but also for understanding flares in blazar jets, which are
highly variable, but where we have never before been able to
resolve the flaring region in the optical or X-rays. These
observations will allow us to test synchrotron emission models
for the X-ray outburst, constrain particle acceleration and loss
timescales, and study the jet dynamics associated with this
flaring component.