Probing Quasar Host Galaxy of a Quasar at z=2.1 with Damped Lyman Alpha System as Coronagraph

0 Assigned ID: 374 ----- Attempting Submission 1 (Fri Apr 11 05:47:07 GMT 2014) ----- HST Phase I Proposal 374 (HST_cycle22_Cai.apt) successfully submitted. ----- Attempting Submission 2 (Fri Apr 11 06:32:42 GMT 2014) ----- HST Phase I Proposal 374 (HST_cycle22_Cai.apt) successfully submitted. ----- Attempting Submission 3 (Fri Apr 11 17:12:43 GMT 2014) ----- HST Phase I Proposal 374 (HST_cycle22_Cai.apt) successfully submitted. ----- Attempting Submission 4 (Fri Apr 11 21:06:32 GMT 2014) ----- HST Phase I Proposal 374 (HST_cycle22_Cai.apt) successfully submitted. ----- Attempting Submission 5 (Fri Apr 11 21:08:50 GMT 2014) ----- HST Phase I Proposal 374 (HST_cycle22_Cai.apt) successfully submitted. ----- Attempting Submission 6 (Fri Apr 11 21:16:25 GMT 2014) ----- This pattern is not used in this proposal. POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures. 0 ----- Attempting Submission 1 (Thu Jul 24 16:46:28 GMT 2014) ----- HST Phase II Proposal 13818 (HST_13818_July24_PhaseII.aptbackup) successfully submitted. ----- Attempting Submission 2 (Thu Jul 24 17:01:57 GMT 2014) ----- ----- Attempting Submission 3 (Thu Oct 02 16:29:25 GMT 2014) ----- We have checked the warnings. The target is indeed in the center of the detector, and we won't worry too much of the low efficiency in the edge because of the narrowband of the WFC3/UVIS Probing Quasar Host Galaxy of a Quasar at z=2.1 with Damped Lyman Alpha System as Coronagraph Fully resolving high-redshift quasar host galaxies is crucial for understanding how massive galaxies and their central black holes form and evolve. However, studies of high-redshift quasar host galaxies are hindered by difficulties in isolating the hosts and accurately subtracting the strong emission from quasar nuclei. From the SDSS-III quasar spectra library, we have discovered a number of rare occurrences where strong damped Lyman alpha absorbers (DLAs) completely block the nuclear emission from the quasar; they act as a natural coronagraph and reveal narrow Ly-alpha emission from the quasar host galaxies. We propose to carry out HST/WFC3 narrow-band imaging of one such system, J1154-0215, at z=2.1. At this redshift, the WFC3/UVIS narrow-band filter FQ387N lies perfectly within the DLA dark trough, thereby enabling us to image the quasar host galaxy without the need for PSF subtraction. The FWHM and luminosity of the narrow Ly-alpha emission detected in this DLA trough are consistent with that of Lyman break galaxies. Our ground-based deep 2-D spectrum indicates that the Ly-alpha emission is marginally resolved under the seeing of 0.6'', suggesting that it is most likely powered by star formation from the quasar host galaxies. High resolution HST imaging, for the first time, will enable us to fully measure the morphology and physical properties of a type-1 quasar host down to the inner 1 kpc scale at z>2, free of PSF subtraction systematics. It will also probe florescent Ly-alpha emission from cool gas associated with the DLA, and study the gas inflows/outflows in the quasar environment to test models of feedback in quasar host galaxies and massive galaxy formation. We will use one narrowband filter FQ387N to image one quasar J1154-0215. The quasar J1154-0215 has a strong Damped Lyman Alpha (DLA) system which completely blocks the strong nuclear emission from the quasar. The DLA acts as a natural coronagraph and will reveal the Lyman alpha (Lya) emission from the quasar host galaxies. We will observe this program with two-visit. The first visit contains 3-orbit. The second visit contains 3-orbit. (1) In the first visit, we do a three-point-dither to populate the first 3-orbit. We split each orbit into two sub-exposure using CR-SPIT=2 (2) In the second visit, we use a same three-point-dither to populate the next 3-orbit. We split each orbit into two sub-exposure using CR-SPIT=2. We will first do a small POS-TARG offset of delta_x= 0'', delta_y=-0.135 when we start the second visit. We found that even with orbit-long individual exposure, the sky background of FQ387N narrowband will be much lower than the recommended threshold of 12e-/pixel. This low sky background will strong affect the charge transfer efficiency of the WFC3 UVIS detector. In order to obtain a threshold of 12e-/pixel background level which will improve the charge transfer efficiency, we will use a post-flash illumination with a intensity of 10e- for our 6-orbit observations. AGN/QUASARS 12 false false false false false SUPPORTED GALAXY LYMAN ALPHA CLOUD QUASAR J2000 J2000 WFC3/UVIS Imaging No No FQ387N POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 1

false

POS-TARG DITHER DITHER 2 0.135 WFC3-UVIS-DITHER-LINE false false 0.145 3 46.84 POS-TARG LINE 46.84 2

true

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