0 Assigned ID: 5492 ----- Attempting Submission 1 (Tue Mar 26 17:04:27 GMT 2024) ----- HST Phase I Proposal 5492 successfully submitted. Receipt: # 5492-1 ----- Attempting Submission 2 (Tue Mar 26 22:37:42 GMT 2024) ----- HST Phase I Proposal 5492 successfully submitted. Receipt: # 5492-2 ----- Attempting Submission 3 (Tue Mar 26 23:53:04 GMT 2024) ----- HST Phase I Proposal 5492 successfully submitted. Receipt: # 5492-3 ----- Attempting Submission 4 (Tue Mar 26 23:55:32 GMT 2024) ----- POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. This is a resubmission for this program's Phase II after switching to mostly 4-orbit visits (instead of mostly 5-orbit visits) to improve the ease of scheduling. -217894169 ----- Attempting Submission 1 (Tue Aug 13 14:08:32 GMT 2024) ----- HST Phase II Proposal 17728 successfully submitted. Receipt: # 17728-1 ----- Attempting Submission 2 (Tue Aug 13 17:44:06 GMT 2024) ----- HST Phase II Proposal 17728 successfully submitted. Receipt: # 17728-2 ----- Attempting Submission 3 (Wed Aug 14 21:13:04 GMT 2024) ----- We are aware of the small monochromatic FoV for the ramp filters and have selected dither and target offsets that are small (never more than a few arcseconds) to ensure that our target is always within the optimal region on the ACS/WFC detector. Spatially Resolving Highly Ionized Channels of Lyman Continuum and Lyman Alpha Escape on 10's of Parsecs Scales In A Strongly Lensed Galaxy Our understanding of the EOR will be limited by our ability to directly study the physical mechanisms that regulate LyC escape in galaxies where LyC escape can be directly measured. However, revealing the physics of LyC requires resolving the relevant physical scales, which are increasingly believed to be small, i.e. on the order of the size of individual compact star clusters (~10-100 pc). This work can only be performed with detailed studies of bright, highly magnified LyC leaking systems, but currently there is only one such system known (the Sunburst Arc). We propose UV/blue HST imaging of LyC and LyA of SGAS1110, an exceptionally magnified strongly lensed galaxy at z=2.48. The proposed data will spatially resolve escaping LyC and LyA radiation down to ~30 pc scales, identifying channels of extremely low HI column density. The target galaxy has a double-peaked LyA emission profile observed from galaxy-integrated ground-based spectroscopy, as well as JWST/NIRSpec IFU spectroscopy that identifies multiple compact star forming regions with extreme ionization (O3/O2 >11 and Ne3/O2 > 1.5; implying log(U) of ~ -1). These regions have nearly identical properties to the extreme LyC leaking region in the Sunburst Arc, which is associated with a single compact star cluster, ~<10 pc in size. This program would provide the crucial missing piece (direct imaging of spatially resolved LyC and LyA escape) to use SGAS1110 as a new laboratory for understanding the relationship between ionizing photon escape and spatially resolved physical properties on the physical scales of individual star clusters, as well as role that complex galaxy and ISM geometries play in enabling LyC escape. This program will measure rest-frame Lyman Continuum (LyC; lambda < 912A) and Lyman-Alpha (lyA; rest-frame lamba = 1216A) emission from a bright, strongly lensed galaxy at z=2.481. The WFC3/UVIS F275W filter captures the LyC emission and the ACS/WFC FR423N tunable narrowband ramp filter captures the LyA emission. We note that in the event that ACS/WFC becomes decommissioned, the FR423N observations can also be performed using the FQ423M (a very narrow medium band) filter on WFC3/UVIS. Observations in both filters are deep -- 29 orbits in F275W and 15 orbits in FR423N -- and so idividual exposures will span an entire orbit, with orbits grouped into separate visits that each consist of 3, 4 or 5 orbits to facilitate shedulability. We will reconstruct the undersampled PSF by dithering exposures using 3-pt line, 4-pt box, or 5-pt line sub-pixel dither patterns within each visit, where the number of positions match the number of orbits in a given visit. We also adjust the main target coordinates slightly (by a few arcseconds) between visits to provide larger offsets to fill in chip defects and to fill in the WFC3/UVIS chip gap. Our aperture selections are chosen to optimize the signal-to-noise of our primary target, which is quite small -- the three bright images of the lensed galaxy all fall within a ~7x20 arcsecond region of the sky. The primary target is the central (most magnified) image of the galaxy which covers a region on the sky ~3x9arceseconds. For the F275W observations we use the UVIS2-C1K1C-CTE aperture, which places the target in the corner of chip 2 near the readout, thus minimizing CTE losses. The target is small enough (maximum extent ~7x20arcsec) that it will easily fall onto the detector (>~ 15 arcsec from the edge) regardless of the position angle of the observation. For the FR423N observations we use the WFC1-IRAMP aperture, which is matched to the FR423N ramp filter being located on the inner part of the ramp filter wheel. The FOV of the monochromatic inner ramp filter region (~25x75 arcseconds). These observations will comfortably fit three bright images of the lensed galaxy (as well as the higheest priority central image that is most highly manified) within the ACS/WFC ramp filter field of view at any position angle. Members of this proposal team have extensive expertise working with massive galaxy clusters and using strong lensing to study the properties of highly magnified galaxies across the entire observable electromagnetic spectrum. Prof. M. Bayliss is an expert on multi-wavelength studies of star formation, gravitational lensing, and galaxy clusters. He has worked with imaging and spectroscopic data from the X-ray to the near infrared, and is an experienced user of Hubble, Chandra, JWST, and numerous 6-10m class ground based telescopes. Prof. Bayliss has led 6 HST observing programs, all studies of highly magnified strong lensing systems, and will serve as the overall project lead. All CoIs below will also contribute to some or all of: data reduction, analysis, and paper-writing. Co-I Florian is an expert in the morphologies, stellar populations, and physical conditions inside distant galaxies, particularly in those that have been gravitationally lensed and has extensive experience working with HST imaging data. He will contribute to the morphological analysis of the spatially resolved analysis of SGAS1110. Dr Gourav Khullar has extensive experience with stellar populatoin modeling, and has applied SPS models to a variety of high-redshift galaxies. He will contribute to the SPS modeling effort for SGAS1110, incorporating both broadband SED and emission line spectroscopic constraints. Prof. Michael Gladders is a galaxy cluster and strong lensing expert, with extensive experience in data handling and analysis (spectroscopic and photometric). Prof. Sharon leads the lensing analysis of several ongoing lensing survey. Sharon and her research group, including Remolina Gonzalez and Mahler, have ample experience in lens modeling and analysis of cluster lenses of all scales (including Frontier Fields, Johnson et al. 2014, Remolina Gonzalez et al. 2018; RELICS, Cerny et al. 2018, Paterno-Mahler et al. 2018; and SGAS, Sharon et al. 2019) Co-I Dahle is an observational astronomer, with a focus on gravitational lensing (both strong and weak). Dr. Rigby is the Semior JWST Project Scientist and an expert on studying distant star-forming galaxies magnified by gravitational lensing. Dr. Keuhno Kim has expertise analyzing extreme star forming galaxies in the local universe, and also ditting the morphological properties of galaxy samples across a wide range of redshifts. Dr. Emil Rivera-Thorsen is an expert on the properties of Lyman-alpha and Lyman continuum emitting galaxies, as well as on spatially resolved properties of starburst galaxies. Galaxies Intergalactic Medium and the Circumgalactic Medium 6 false false true false false false true false false false false false SUPPORTED GALAXY GRAVITATIONAL LENS HIGH REDSHIFT GALAXY STAR FORMING REGION SDSSJ1110+6459 J2000 J2000 GALAXY GRAVITATIONAL LENS HIGH REDSHIFT GALAXY STAR FORMING REGION SDSSJ1110+6459 J2000 J2000 GALAXY GRAVITATIONAL LENS HIGH REDSHIFT GALAXY STAR FORMING REGION SDSSJ1110+6459 J2000 J2000 WFC3/UVIS Imaging No No F275W ACS/WFC RampFilter No No FR423N POS-TARG DITHER 0.2637 This 4-pt box dither pattern is intended to provide sub-pixel dithers to support PSF reconstruction in the ACS ramp filter data taken on visits containing four orbits (one dithered exposure per orbit). LINE 0.1856 false false 69.02 4 20.7 ACS-WFC-DITHER-BOX 2 false POS-TARG DITHER 0.173 This 4-pt box dither pattern is intended to provide sub-pixel dithers to support PSF reconstruction in the WFC3/UVIS F275W data taken on visits containing four orbits (one dithered exposure per orbit). LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 3 false POS-TARG DITHER 0.145 This 5-pt line dither pattern is intended to provide sub-pixel dithers to support PSF reconstruction in the WFC3/UVIS F275W data taken on visits containing five orbits (one dithered exposure per orbit). LINE false false 5 46.84 WFC3-UVIS-DITHER-LINE 4 false POS-TARG DITHER 0.187 This 3-pt line dither pattern is intended to provide sub-pixel dithers to support PSF reconstruction in the ACS ramp filter data taken on visits containing three orbits (one dithered exposure per orbit). 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 17728 :visit-id "08" :proposal-version -1 :trans-version "20240627" :date "13-Aug-2024 13:28:20.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1154976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17728 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17728 :visit-id "08" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "08" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "08" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "08" :orbit-number 4 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) true 4 0 /Users/mbayliss/astro/observing/hst/cycle32/OP-cache/HST-GO-17728_PhaseII-v09.xml The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17728 :visit-id "09" :proposal-version -1 :trans-version "20240627" :date "13-Aug-2024 13:28:21.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1154976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17728 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17728 :visit-id "09" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "09" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "09" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "09" :orbit-number 4 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) true 4 0 /Users/mbayliss/astro/observing/hst/cycle32/OP-cache/HST-GO-17728_PhaseII-v11.xml The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17728 :visit-id "11" :proposal-version -1 :trans-version "20240627" :date "13-Aug-2024 13:43:03.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1443728 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17728 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17728 :visit-id "11" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "11" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "11" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "11" :orbit-number 4 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17728 :visit-id "11" :orbit-number 5 :pcs-time 380 :si-vis-utilization 2739 :al-overhead-at-end 123 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) true 5 0