0Assigned ID: 1751
----- Attempting Submission 1 (Fri Mar 01 20:49:02 GMT 2013) -----
HST Phase I Proposal 1751 (MgII_imaging_WFC3.apt) successfully submitted.
----- Attempting Submission 2 (Sat Mar 02 00:13:58 GMT 2013) -----At the time that the long range plan is developed or walkthroguh scheduled, we would
very much value a short meeting with the PC and contact scientist to discuss our
non-conventional dither patterns. We spent a large amount of time reviewing documentation
and considering the tradeoff between saturation, bad pixel removal, and PSF sampling while
developing this strategy. If there is a consideration we've missed it would be good to catch
this before observations are too far underway, and to access data on the first fields observed
promptly in case any corrections must be made to the strategy. The changes would not affect
programming as they would only modify the distance of subpattern dithers, and even then
by a small amount.-300642401----- Attempting Submission 1 (Thu Jun 27 19:49:09 GMT 2013) -----The Structure of MgII Absorbing Galaxies at z=2-5: Linking CGM Physics and Stellar Morphology During Galaxy AssemblyUsing Magellan/FIRE, we have completed the first infrared survey for MgII absorption systems in the z>2 universe. At z<0.5, such MgII absorbers are almost universally associated with ~L* galaxies. Morphological studies of these host galaxies indicate that MgII traces inflowing gas accretion and outflowing galactic winds in the circum-galactic medium (CGM); both processes are critical to the regulated growth of stellar mass. We propose a deep WFC3 imaging survey toward 9 of our survey sightlines hosting 44 MgII absorbers to investigate the morphology-absorber connection in a unique sample spanning 2<z<5. Only HST is capable of delivering the deep, spatially resolved rest-frame optical imaging needed to measure morphological parameters and orientations of these galaxies, connecting our work directly to what has been achieved in the local universe.Our program requires a single observing setup, incorporating the F160W IR filter to capture rest frame optical emission from the MgII host sample galaxies (or rest frame near-UV for the highest redshift examples). Our observing strategy is modeled after the similar WFC3 survey of Law et al. (2012), who studied the rest frame optical properties of galaxies selected generally from the field, over a similar redshift range. However we employ a slightly different, customized dithering pattern.
Each of the 9 fields is scheduled for one visit consisting of 3 orbits. Our primary targets of interest are faint galaxies (H_AB=23-25 magnitudes) that are typically located within ~15 arcseconds of a bright background quasar (H_AB=19).
We are not interested in photometry for the quasar itself, but given our long integrations (7835 seconds/field, split into 650 second SPARS50 ramps), we are concerned about saturation and persistence from the QSO which is by construction near the science targets. Accordingly we designed a specailized dither pattern to mitigate the effects that saturation and persistence would have on our ability to identify galaxies at small angular separation.
The dither pattern consists of three pointings on a spiral pattern (effectively an "L"), separated by 16 arcseconds. This ensures that any persistence image from the saturated QSO is placed >15" away from the new position of the QSO at the start of each orbit. At each of these three locations, we perform a 2.5 pixel, 4-point box subpattern dither to sample the PSF. Our choice of 2.5 pixels provides full PSF sampling, and just exceeds the minimum recommended dithering distance of 2 pixels to recover operability from hot pixels. The 16" dithers between orbits will span clustered artifacts on the detector.
Our SPARS50 x 14 or 15 exposures were chosen to pack a self contained 4-pont sample of the PSF in each orbit. Also, this provides exposures long enough to be background-dominated even for a 14 read ramp, yet short enough to avoid deep saturation (we hope) for most of our QSOs. We anticipate saturation in the central few pixels in some cases but hope to avoid saturation in the PSF wings.Please note that for several of our targets, most notably numbers 6, 7, 8 and 9, there will be no flux from the quasar at optical wavelengths - they are at very high redshift and therefore only visible in the IR. This is why there is no target in the finding chart crosshairs for several examples. However we have verified independently that the pointings are all correct using our own IR images.
Also, the science fields are centered around known quasars which constitute the "targets," but the actual sources of interest are faint galaxies near the quasar on the sky - not the quasar itself (see the Observing Description for details).QUASAR ABSORPTION LINES AND IGM12falsefalse0.00.0falsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF160WPOS-TARGDITHERDITHER416This is a 3 point "L" with spacing 16 arcseconds between the end points. The strategy here is to hop over bad pixel regions but more importantly to move the (possibly) saturated core from the central quasar >=15 arcseconds (~100 kpc). in each large dither. We wish to avoid the possibility of persistence images in dithered sequences near the bright QSO, becuase we are looking for faint galaxies within a circle of 15" radius.
Within each large dither, we perform a small dither pattern (2.5 pixel square box) for the purpose of PSF sampling. However we keep this dither small so as not to smear out possible persistence images within the subpattern.WFC3-IR-DITHER-BOX-MINfalse90true0.3030.3383221.788POS-TARGSPIRAL03truePOS-TARGDITHERDITHER416This is a 3 point "L" with spacing 16 arcseconds between the end points. The strategy here is to hop over bad pixel regions but more importantly to move the (possibly) saturated core from the central quasar >=15 arcseconds (~100 kpc). in each large dither. We wish to avoid the possibility of persistence images in dithered sequences near the bright QSO, becuase we are looking for faint galaxies within a circle of 15" radius.
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