HST Imaging in the Chandra Deep Field South: III. Quantitative Morphology of the 1 Msec Chandra Counterparts and Comparison with the Field Population

Details HST Imaging in the Chandra Deep Field South: III. Quantitative Morphology of the 1 Msec Chandra Counterparts and Comparison with the Field Population HST Imaging in the Chandra Deep Field South: III. Quantitative Morphology of the 1 Msec Chandra Counterparts and Comparison with the Field Population

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...20110706g&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #107.06; Bulletin of the American Astronomical Society, Vol. 34, p.1275

Mathematics

Logic

Scientific paper

We present a quantitative morphological analysis of the 37 HST/WFPC2 counterparts we identified (Koekemoer et al. 2002) in the 1 Msec Chandra Deep Field South (CDFS). We investigate: 1) 1-D surface brightness profiles from isophotal ellipse fitting; 2) 2-D, PSF-convolved, bulge+disk+nucleus profile-fitting to determine the optical flux from the central engine alone; 3) asymmetry and concentration indices for all 3000 sources in our three WFPC2 pointings to look for systematic bias in these shape parameters for the CDFS counterparts; and 4) near-neighbor galaxy counts to compare the local environments of the X-ray sources versus the field control sample. Our 2-D profile fitting reveals a significant nuclear point-source component in ~ 1/2 of the resolved HST/WFPC2 counterparts. This fraction is comparable for analogous low-redshift samples of moderate-luminosity AGN, suggesting no evidence for evolution in their optical obscuration out to z ~ 0.5-1, typical of our sources. The nuclear components of the resolved CDFS sources exhibit a narrow range of FX/Fopt,nuc which is consistent with the several HST-unresolved X-ray sources in our fields. The asymmetry index distribution of the 21 CDFS sources at I<23 is indistinguishable from the I<23 field. Similar findings for local AGN samples suggest no close connection between galaxy mergers and AGN activity - our results extend this counterargument to z ~ 0.5-1. Moreover, the frequency of I<23 near neighbors around the CDFS counterparts is not significantly different from the field sample. By contrast, the concentration indices for the CDFS counterparts are clearly skewed towards larger values - inconsistent with the field distribution at 5-sigma. A plausible inference is that the strong correlation between black hole mass and host galaxy concentration index observed in nearby galaxies is already evident by z ~ 0.5-1. We also highlight preliminary results from the successor ACS GOODS morphological analyses of the same field.

Affiliated with

Also associated with

No associations

Rating

HST Imaging in the Chandra Deep Field South: III. Quantitative Morphology of the 1 Msec Chandra Counterparts and Comparison with the Field Population does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with HST Imaging in the Chandra Deep Field South: III. Quantitative Morphology of the 1 Msec Chandra Counterparts and Comparison with the Field Population, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and HST Imaging in the Chandra Deep Field South: III. Quantitative Morphology of the 1 Msec Chandra Counterparts and Comparison with the Field Population will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1891011