Host galaxy properties of z>~0.3 broad-line AGN with direct black hole masses from reverberation mapping

0 Assigned ID: 608 ----- Attempting Submission 1 (Fri Apr 10 17:41:08 GMT 2015) ----- FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser Dear PC, I am submitting the Phase II file for program GO-14109. Please see "Proposal Description" for notes on the observations. I have two questions/comments: 1. For the UVIS orbit for target RM775, I used 3 sub-exposures at each dither position, with one 60s exp and two 242s exp to avoid target saturation. However, I didn't use post-flash for the short 60s exposures as the target is bright. Let me know if this is OK. 2. For target RM767, there is a nearby star that will cause extreme saturation in the STEP25 IR exposures. However, this star is near the edge of the IR512 detector (~30" from the science target), so I was wondering if we can rotate the detector or shift the center of the detector to avoid this bright star. If you find any other potential issues, please let me know as well. Thank you very much for your help! Yue -838285225 ----- Attempting Submission 1 (Fri Jul 17 22:57:48 GMT 2015) ----- Please see my submission comments regarding this warning (post-flash not used for short UVIS exposures of Target RM775). Host galaxy properties of z>~0.3 broad-line AGN with direct black hole masses from reverberation mapping We propose WFC3 IR and UVIS imaging for a unique sample of ten z>~0.3 broad-line AGN with direct black hole (BH) mass measurements from reverberation mapping (RM), resulting from the ongoing Sloan Digital Sky Survey Reverberation Mapping (SDSS-RM) project. Our sample is the first sample of z>~0.3 AGN with direct BH masses from RM rather than the less reliable BH mass estimates from single-epoch spectroscopy. The 2-band HST imaging will be used to measure host galaxy properties such as the bulge luminosity and stellar mass in these AGN as well as to quantify the host-free AGN luminosity at rest-frame optical wavelengths, important for measuring the first broad-line region size-AGN luminosity relation at z>~0.3. The measured host properties combined with the RM BH masses from SDSS-RM will be used to investigate the possible evolution of the correlations between BH mass and bulge properties and compared to earlier evolutionary studies based on single-epoch BH masses. The proposed HST imaging, combined with ground-based spectroscopy from the SDSS-RM project, will provide new perspectives on the co-evolution of BHs and host galaxies and the role of AGN feedback in galaxy formation models, and improve the utility of RM on measuring BH masses in broad-line AGN at z>0.3. We will observe 10 science targets (1 visit per target). Each visit will have two orbits (one for WFC3-UVIS observation and one for WFC3-IR observation). The 10 science targets are grouped togther within a window of 3 days, along with one visit/orbit for a PSF star (GRW+70D5824). For the PSF star observation, the UVIS and IR observations are combined in a single orbit. This stragety is to facilitate PSF reconstruction for our science targets by observing the PSF star quasi-simultaneously. The total number of orbits is therefore 21. Note that all our science targets have similar RA/DEC, and they have the same visibility window. For the UVIS observations, we will use the 2k (2K2C) subarray with the F606W filter, and the three-point line dither pattern. At each dither position we will take 2 sub-exposures (CR-SPLIT=2), totaling 6 sub-exposures to fill the orbit. The only exception is target RM775 (SDSS r=18.3) for which we will use 3 sub-exposures at each dither position: one 60s exposure and two 242s exposures to avoid saturation. No post-flash is applied to the 60s exposures, but that should be OK given that the target is bright. For the IR observations, we will use the 512 (SUB512) subarray with the F110W filter, and the four-point box dither pattern. Two exposures are used: a STEP25 (NSAMPLE=11) sequence with 4 sub-exposures at each dither position (16 sub-exposures in total), and a SPARS5 (NSAMPLE=7) sequence with 1 sub-exposure at each dither position (4 sub-exposures in total). The two exposures will fill the IR orbit. The PSF star observations use the same WFC3 configurations and dither patterns as for our science targets, but with different exposure times to avoid saturation. Post-flash is set to FLASH=12 for these relatively short UVIS exposures. -------- Realtime Justification -------- Special Scheduling Requirements We request our grouped targets (including the PSF star) be observed within a 3-day window. This is to ensure a stable PSF over this short period. Delayed scheduling due to this restriction is OK. AGN/QUASARS 12 false false false false false false SUPPORTED GALAXY QUASAR J2000 J2000 r=18.3 GALAXY QUASAR J2000 J2000 r=18.9 GALAXY QUASAR J2000 J2000 r=19.6 GALAXY QUASAR J2000 J2000 r=20.1 GALAXY QUASAR J2000 J2000 r=19.0 GALAXY QUASAR J2000 J2000 r=20.7 GALAXY QUASAR J2000 J2000 r=20.7 GALAXY QUASAR J2000 J2000 r=19.9 GALAXY QUASAR J2000 J2000 r=21.9 GALAXY QUASAR J2000 J2000 r=20.5 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W POS-TARG DITHER 0.572 LINE 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 1

false

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

false

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