0
Assigned ID: 203
----- Attempting Submission 1 (Thu Apr 06 09:07:45 GMT 2017) -----
HST Phase I Proposal 203 (jsilverman_v2.apt) successfully submitted.
Receipt: # 203-1
----- Attempting Submission 2 (Fri Apr 07 04:51:41 GMT 2017) -----
Resubmission after all target changes have been accepted by STSCI. I made a very minor change due to a typo. The name of target #17 COSMOS-XID454
was changed to COSMOS-CID454.
2109637080
----- Attempting Submission 1 (Thu Jul 20 08:58:36 GMT 2017) -----
HST Phase II Proposal 15115 (jsilverman_phaseII_v3.apt) successfully submitted.
Receipt: # 15115-1
----- Attempting Submission 2 (Tue Aug 01 05:52:17 GMT 2017) -----
----- Attempting Submission 3 (Tue Oct 24 01:11:48 GMT 2017) -----
Emergence of the supermassive black hole - galaxy mass relations at z > 1
Our aim is to establish, in an unbiased manner, whether local fundamental relations between the mass of supermassive black holes (SMBHs) and that of their host galaxies (M_BH vs. L_host, M_BH vs. M_stellar) evolve with cosmic time. We will answer one of the outstanding key questions in astrophysics, "Are galaxies built up around the massive potential wells of mature SMBHs or does the growth pathway of galaxies precede that of their central SMBH?" Current simulations predict a strong evolution in the M_BH vs. L_host relation with SMBHs more massive by 0.5 dex at z~1.4 as compared to z=0. To test this, we have constructed a uniformly-selected sample of broad-line AGN in deep survey fields with black hole mass estimates (7.5<log M_BH<8.5) falling below the knee of the black hole mass function (significantly reducing biases) and derived from Balmer lines (i.e., Halpha), the same virial mass indicator used for calibrating local relations thus further lessening biases. We request to use HST/WFC3 to measure the total stellar mass of 36 AGN host galaxies at 1.2<z<1.7 (4x current samples), in the rest-frame V/R-band using F125W and F140W filters (dependent on the target). This sample size is required to be sensitive to an offset in the mass relations of >=0.23 dex to confirm (or rule out) the expected evolution. To date, no effort has been achieved with HST to measure the stellar mass of broad-line AGN hosts with black hole masses at intermediate levels and having sufficient statistics at z>1. We will also measure the scatter in the mass relations at early epochs thus constraining the strength of coupling between black holes and their hosts.
We are using HST/WFC3 IR imaging to detect the host galaxies of 32 Active Galactic Nuclei (1.2 < z < 1.7), already identified by their broad Halpha emission lines through ground-based NIR spectroscopy, in key survey fields (COSMOS, E-CDF-S and SXDS). The F125W (1.2 < z < 1.44) and F140W (1.44< z < 1.7) filters are implemented, while specifically chosen based on the redshift of each target as indicated in parenthesis, to measure the total stellar mass of the underlying host galaxy by sampling the spectral energy distribution above 4000 Angstroms. We further ensure that the broad Halpha line is not present in the bandpass since its presence can contaminate stellar mass estimates due to the broad wings of the PSF.
The detection of the host galaxy requires accurate characterization and modeling of the point spread function to decompose the total NIR emission into that of an unresolved central AGN and the extended host galaxy that is expected to dominate the total emission beyond 0.3" based on an analysis of a representative AGN that falls within the CANDELS (WFC3) footprint. For all 32 targets, we have set a fixed position (geometric center; Aperture: IR-FIX) of WFC3 to include the target of interest and a sufficient number of stars (~ 4 - 5) used to constrain the modeling of the PSF. As a result, the center pointing of WFC3 does not correspond to the target position but offset by an amout less than 80". To improve the sampling of the PFS for each target, we choose to have a dither pattern (WFC3-IR-DITHER-BLOB) with six different positions separated by the default 5.18".
A single orbit of exposure per target is sufficient to detect the host galaxy at a significance level of 5sigma with either the F125W and F140W bands for all 32 AGNs. This estimate is based on a determination of the expected nuclear-to-host ratio (found to typically range from 0.3-7) of the IR emission using the existing HST/F814W (Scoville et al. 2007) and ground-based IR (McCracken et al. 2012) imaging in COSMOS.
Massive Black Holes And Their Host Galaxies
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