0 Assigned ID: 4247 ----- Attempting Submission 1 (Wed May 24 04:09:59 GMT 2023) ----- HST Phase I Proposal 4247 successfully submitted. Receipt: # 4247-1 ----- Attempting Submission 2 (Wed May 24 08:08:36 GMT 2023) ----- HST Phase I Proposal 4247 successfully submitted. Receipt: # 4247-2 Hi, I've updated the phase II based on instrument scientist Amanda Pagul advice and guidance on how to achieve 4 exposures for both each filter spread across two orbits (so two exposures per filter per orbit). I've adopted two-point dither patterns with a POS TARG offset to try and mimic a box dither pattern. 1260465678 ----- Attempting Submission 1 (Tue Sep 12 05:57:11 GMT 2023) ----- ----- Attempting Submission 2 (Tue Nov 14 08:00:50 GMT 2023) ----- The stellar initial mass function (IMF) is a critical assumption underlying nearly every galaxy observable, yet it remains poorly constrained at high (z>0) redshift. The low-mass end in particular (M<0.4 Msun) significantly affects the mass-to-light ratio, and therefore measurements of key galaxy properties including the stellar mass and dark matter content are highly sensitive to its assumed shape. Thanks to upcoming cycle 2 JWST/NIRSpec IFU observations of 2 massive lensed quiescent galaxies at z~1, a precise measurement of the IMF at z~1 using spectral lines sensitive to low-mass stars will be possible for the first time. However, this forthcoming JWST IFU data has far more potential than solely measuring the IMF spectroscopically. This proposal will significantly expand the science available from this dataset by using only 2 orbits of HST/WFC3 to build a precise lens model of the one target without pre-existing WCF3 images and reconstruct the source galaxy's morphology. The high spatial resolution imaging from HST will open the door for spatially resolved studies of the target, allowing us to use the JWST data to its full capacity. With the combined HST imaging and JWST spectra we can then make an independent measurement of the IMF normalisation from dynamical modeling, a method which is in tension with results from stellar spectral features. Additionally, the dynamical models will provide a measure of the total mass density slope at an epoch where simulations and observations differ significantly in their predictions. This analysis will be the first of its kind and will provide a key test for galaxy formation and evolution theories. For the IR/F140W we find that with 4 dithers of total exposure time ~900s, for an extended 3" source with 1x1 pixel binning, assuming a flat continuum in F\lambda and standard background levels we obtain a S/N ~ 10 per pixel. For the UVIS/F814W we find that in 4 frames of total exposure time ~3000s, for an extended 3" source with 2x2 pixel binning, assuming a flat continuum in F\lambda and standard background levels we obtain a S/N~ 5 per pixel. Based on the instrument overheads listed in the WFC3 user documentation, the total time required comes to 2 orbits. Increasing from 3 to 4 dithers for each filter has a negligable change on the S/N as estimated by the ETC, but will improve the spatial sampling in the dithered images. All CoIs have substantial experience in optical and near-infrared observations of quescent galaxies, with senior members considered leaders in this field. PI Barone is an expert on the stellar populations of quiescent galaxies from IFU observations. Vaughan is an expert on the low-mass end of the IMF and the stellar populations of quiescent galaxies. Glazebrook is a leading expert on high redshift quiescent galaxy evolution and has over 30 years of experience in optical and near-infrared observations, data reduction, and analysis. Nanayakkara is an expert in high redshift stellar populations and has extensive experience in optical and near-infrared observations, data reduction, and analysis. Tran is a recognized world expert in galaxy evolution who has helped lead multiple extragalactic surveys, and currently leads the ASTRO 3D Galaxy Evolution with Lenses (AGEL) survey. Vasan is a PhD student supervised by CoI Jones and has expertise on using lenses to study the high redshift sources for their gas-phase kinematics. Kirby is expert in using stellar spectroscopy to measure the chemical abundances and stellar populations of nearby galaxies. Leethochawalit is an expert in high redshift galaxy observations from ground and space based observations. Zhuang is a PhD student supervised by CoI Kirby and has expertise in the stellar populations of z=1 quiescent galaxies. Zhuang led the analysis of the stellar populations of AGEL0014 and AGEL1323 from the ground-based rest-frame optical spectroscopy. Jones is expert on the abundances and kinematics of the interstellar medium of high-redshift galaxies, and has published numerous studies of lensed galaxies. Kacprzak is an leading expert on circumgalactic medium physics and how it influences galaxy evolution from 0<z~2. Nightingale is an expert on galaxy-galaxy scale strong lens modelling and source reconstruction from HST imaging. Shajib is an expert on galaxy-scale strong lens modelling and observational cosmology from lensing. Mendel is an expert on high redshift galaxy evolution in particular their kinematics and dynamics. Sahu is a postdoctoral researcher working with Tran on lens modelling of strongly lensed galaxies and the analysis of their dark matter profiles. Galaxies Stellar Populations and the Interstellar Medium 6 false false false false false false false false SUPPORTED GALAXY GRAVITATIONAL LENS DESJ0014+0041 J2000 J2000 WFC3/IR Imaging No No F140W WFC3/UVIS Imaging No No F814W POS-TARG DITHER DITHER 4 5.183 WFC3-IR-DITHER-BOX-MIN false 74.653 false 0.365 0.572 2 41.859 POS-TARG WFC3-IR-DITHER-BLOB 18.528 2 false POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 3 false POS-TARG DITHER DITHER 4 5.183 WFC3-IR-DITHER-BOX-MIN false 74.653 false 0.365 0.572 2 41.859 POS-TARG WFC3-IR-DITHER-BLOB 18.528 4 false POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 5 false 1699948009013 The scheduling data was generated by CASM 31.1. CASM was run in Phase II mode. /private/var/folders/l3/ndzrxs1j3sng7pc39xhjh1fwcfnqz3/T/OPVisit1267517191007768293.xml Sequence as decided by ETC: - For the IR/F140W 4 dithers of total exposure time 900s - For the UVIS/F814W 4 frames of total exposure time 3000s (Tic-Visit :proposal-id 17437 :visit-id "01" :proposal-version -1 :trans-version "20230626" :date "14-Nov-2023 18:46:39.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2129872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17437 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17437 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2752 :al-overhead-at-end 116 :internal-dur-at-end 31 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3136 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17437 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2720 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3136 :pcs-gap 0 ) true 2 0