Chandra X-Ray Observatory
	(CXC)

Cycle 2 Accepted Archive Proposals

Proposal NumberPI NameTitle
02300855 Jonathan Grindlay Archival Deep Chandra Galactic Fields: ChaMPlane
02900722 Fiona Harrison A Serendipitous Extragalactic X-ray Source Identification (SEXSI) Program
02800373 Joseph Mohr Galaxy Cluster Scaling Relations:
Structural Evolution and Distance Measurements
02910630 Randall Smith An X-ray Halo Survey: Measuring Dust Grain Size, Composition and Position
02910391 Barbara Whitney Outflows Associated with X-ray Protostars In Rho Oph:
Observational Constraints to the X-ray/Outflow Connection
02900647 Belinda Wilkes The Chandra Multi-wavelength Project (ChaMP):
A Serendipitous X-ray Survey Using Chandra Archival Data



Proposal Title: ARCHIVAL DEEP CHANDRA GALACTIC FIELDS: CHAMPLANE

PI: JONATHAN GRINDLAY               Observer: 
Subject Category: WD BINARIES AND CV

Abstract: 

We propose to conduct analysis of archival deep ~30 ks galactic fields
(b < 10 deg) imaged by Chandra to conduct the Chandra Multiwavelength Plane
(ChaMPlane) Survey. Our primary goal is to identify CVs, quiescent LMXBs, and
black hole x-ray novae in quiescence, in order to constrain and ultimately
measure the luminosity functions of each. The ChaMPlane survey offers the best
chance for constraining the formation/evolution of CVs and LMXBs and the stellar
BH content of the Galaxy. CVs and qLMXBs will be identified by their Halpha
excess as `blue' objects in the R vs. (Halpha - R) plane down to R ~ 24 with our
recently approved NOAO Long Term Survey program. Support is requested for the
x-ray analysis and creation of galactic survey databases and catalogues.

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Proposal Title: A SERENDIPITOUS EXTRAGALACTIC X-RAY SOURCE IDENTIFICATION (SEXSI) PROGRAM

PI: FIONA HARRISON                  Observer: 
Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Abstract: 

We propose to continue our program of identifying hard X-ray sources
discovered in high-latitude Chandra PV and GO observations. We are performing
systematic deep optical and IR imaging and spectroscopy of serendipitous sources
detected of medium and deeply exposed fields, with the ultimate goal of making a
complete census of a large area (several square degrees) of the extragalactic
hard X-ray sky. We are proposing here to obtain suport for analysis of the
Chandra X-ray images.

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Proposal Title: GALAXY CLUSTER SCALING RELATIONS: 
                STRUCTURAL EVOLUTION AND DISTANCE MEASUREMENTS

PI: JOSEPH MOHR                     Observer: 
Subject Category: CLUSTERS OF GALAXIES

Abstract: 

We propose to study cluster structural evolution and measure distances
with archival observations of 39 intermediate and high redshift clusters; we
will study the relation between X-ray isophotal size and intracluster medium
(ICM) temperature (Tx) and the relation between ICM mass and Tx (S-T and M-T,
repsectively). We have studied these relations locally (PSPC data) and at
intermediate redshift (ROSAT HRI data); with Chandra data we can precisely
compare local and high z relations, and we can measure relative distances to
z=0.8. In contrast to the high scatter luminosity-temperature relation, the S-T
and M-T relations are ideally suited to studying the structural evolution of the
cluster virial region.


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Proposal Title: AN X-RAY HALO SURVEY: 
                MEASURING DUST GRAIN SIZE, COMPOSITION AND POSITION

PI: RANDALL SMITH                   Observer: 
Subject Category: GALACTIC DIFFUSE EMISSION AND SURVEYS

Abstract: 

X-ray halos, created by interstellar dust grains, can be seen with
Chandra when a bright source is only moderately absorbed. The halos are quite
sensitive to the grain properties, especially the size distribution and
composition. X-ray halos are most sensitive to the largest grains, about which
little is known from other wavelengths. Using a survey of 20 sources from AO-1,
we will use Chandra's superior angular resolution to measure the extent of the
large dust size distribution and the composition of the dust in the ISM; in
addition we will be able to measure the relative position of grains along the
line of sight. Since the larger grains contain much of the mass, our results
will address questions in the ongoing controversy over interstellar abundances,
especially for carbon.

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Proposal Title: OUTFLOWS ASSOCIATED WITH X-RAY PROTOSTARS IN RHO OPH:
                OBSERVATIONAL CONSTRAINTS TO THE X-RAY/OUTFLOW CONNECTION

PI: BARBARA WHITNEY                 Observer: 
Subject Category: GALACTIC DIFFUSE EMISSION AND SURVEYS

Abstract: 

We propose to examine the link between hard X-ray emission and
outflows in protostars by searching for X-ray emission in two dense cores of the
Rho Oph cloud that harbor 60 young stellar objects. Our statistical analysis of
deep Chandra archive data will yield limits on the frequency X-ray emission
emanating from protostars and will provide insights into the mechanism that
drives outflows. We will combine deep ACIS-I data with near-IR and optical
imagery, and CO data from the literature. We expect to trace the morphology of
these emissions, from the faster moving material at X-ray wavelengths to the
large-scale and slowly moving molecular outflows. We will obtain the first
correlation between X-ray emission and outflows for the youngest stars in the
closest stellar nursery.

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Proposal Title: THE CHANDRA MULTI-WAVELENGTH PROJECT (CHAMP): 
                A SERENDIPITOUS X-RAY SURVEY USING CHANDRA ARCHIVAL DATA

PI: BELINDA WILKES                  Observer: 
Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Abstract: 

We are performing a serendipitous X-ray survey (ChaMP) of 8 sq deg of
sky to flux limits intermediate between previous surveys and small area Chandra
deep surveys (10E-13<F(2-10)<6E-16 erg/cm**2/s). We predict ~3000 sources, ~2000
of which are active galactic nuclei (AGN). Optical imaging is in progress using
SDSS g,r,i filters to flux limits matched to the X-ray data. ChaMP: 1) requires
no new X-ray data 2) provides a large, uniform, multi-wavelength, public
database allowing the community to address a wide variety of scientific
questions 3) covers sufficient area to fill in the gaps left by deep surveys at
bright flux levels We request funding for 2 research assistants to facilitate
our analysis and identification thus providing earlier (~6 months) public access
to our results.

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Last modified: 12/02/10

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