0 Assigned ID: 200 ----- Attempting Submission 1 (Thu Mar 05 01:07:49 GMT 2020) ----- HST Phase I Proposal 200 successfully submitted. Receipt: # 200-1 ----- Attempting Submission 2 (Fri Mar 06 19:08:58 GMT 2020) ----- HST Phase I Proposal 200 successfully submitted. Receipt: # 200-2 FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser 0 ----- Attempting Submission 1 (Fri Jun 26 01:27:04 GMT 2020) ----- HST Phase II Proposal 16226 successfully submitted. Receipt: # 16226-1 ----- Attempting Submission 2 (Mon Jun 29 04:18:36 GMT 2020) ----- HST Phase II Proposal 16226 successfully submitted. Receipt: # 16226-2 ----- Attempting Submission 3 (Thu Jul 16 20:12:55 GMT 2020) ----- HST Phase II Proposal 16226 successfully submitted. Receipt: # 16226-3 ----- Attempting Submission 4 (Thu Sep 24 17:47:22 GMT 2020) ----- We are adopting the new recommended FLASH level of 20e-/pixel for our WFC3/UVIS primary exposures. Metallicity Distribution Functions of Quenched Field Dwarf Galaxies Environment is thought to play a central role in quenching low-mass dwarf galaxies. However, an increasing number of dwarf galaxies discovered in isolation suggest that mechanisms other than environment can quench dwarf galaxies. Here, we propose deep WFC3/F395N (Ca H & K) imaging to measure metallicites (~0.1-0.2 dex) for hundreds of individual stars in Cetus and Tucana, the two nearest examples of isolated quenched dwarf galaxies. Our Ca H & K photometry will provide an order-of-magnitude increase in the number of stars in each systems with reliable metallicities (from ~40 to 400), enabling the first detailed study of the metallicity distribution functions (MDFs), and the physics they encode, in isolated quenched dwarf galaxies. Specifically, we will (1) construct and characterize detailed MDFs for Cetus and Tucana from a number of stars comparable to MW satellites; (2) use our MDFs to differentiate between signatures of external vs internal quenching in low-mass galaxies; and (3) combine our MDFs, HST-based SFHs, and HST-based proper motions (and orbital histories) to complete our knowledge of these enigmatic galaxies' formation histories. This program will provide qualitatively new insight into how and why isolated low-mass galaxies stop forming stars. The construction of MDFs in such distant systems is only possible due to the excellent blue-sensitivity and angular resolution of HST -- no other ground- or space-based facility can acquire this data. This novel use of HST will establish it as a leader for measuring stellar metallicities in galaxies located at large distances from the Milky Way. The goal of this program is to obtain F395N imaging with S/N > 10 for the Cetus and Tucana dwarf galaxies down to F475W ~ 25. We aim to combine this data with existing F475W and F814W archival imaging (GO-10505) of each dwarf to construct their metallicity distribution functions and infer their quenching mechanisms. Accordingly, we extensively reference GO-10505 for program design. Most of the visits in this program are two orbits. In each orbit, there are 2 F395N exposures taken per orbit in wFC3/UVIS, and no CR-splits.We follow the dither pattern from proposal GO-10505 using POS-TARG. For Tucana and Cetus respectively, there are 12 and 11 unique dither pointings, one per orbit. Coordinated parallel exposures are obtained using WFC/ACS in F475W and F814W filters. For the first visit to each galaxy, we impose orientation requirements so that our parallel exposures overlap with parallel fields targeted in GO-10505. Those fields were designed to avoid bright foreground stars, and also, to target scientifically valuable portions of each object's galactic halo. Subsequent visits to the object follow the same orientation to maximize the sky area covered in full depth in both the prime and parallel fields. A graduate student working with Dr. Daniel Weisz, Sal Wanying Fu (program PI) has led mutiple papers on stellar spectroscopy in Local Group dwarf galaxies. As program PI, Fu will lead analysis and oversee execution of this program. Dr. Daniel Weisz (Co-I) is an expert on resolved stellar populations with HST, the Local Group, color-magnitude diagrams, star formation histories, and the formation and evolution of dwarf galaxies. He has worked on over 1500 orbits of HST data of resolved stellar populations, and has been first author of 10 papers using HST observations of nearby galaxies in the past decade. Dr. Else Starkenburg is a co-PI of the PRISTINE CaHK survey of the MW and an expert in both theory and observations of theory and observations of metal-poor stars, the Galactic halo, and dwarf galaxies. Dr. Starkenburg will oversee theoretical interpretation of our results. Dr. Nicolas Martin is a co-PI of the PRISTINE CaHK survey of the MW and is an expert in observations of metal-poor stars and satellite galaxies around the MW and M31, particularly with SDSS, Pan-STARRS, and Keck/DEIMOS. Dr. Mario Mateo is the principle investigator of Magellan/M2FS spectrograph, is an expert in all types of observations of dwarf galaxies, and wrote the seminal annual review (Mateo 1998) on dwarf galaxies in the Local Group. Dr. Patrick Cote is an expert on ground-based observations of nearby galaxies and galaxy groups, particularly with the CFHT. Dr. Andrew Dolphin is an expert on resolved stellar populations, is the author of DOLPHOT, the most widely used PSF photometry reduction routine for HST, and is also author of MATCH, the CMD fitting package that we will use to measure SFHs in this program. Prof. Michael Boylan-Kolchin is a theorist with particular expertise in dwarf galaxies and dark matter, and is a member of the FIRE collaboration. He will help facilitate theoretical interpretation of our findings. Mr. Nathan Sandford is a graduate student working with Dr. Daniel Weisz on stellar spectroscopy and the chemical information content of spectral features. Stellar Populations and the Interstellar Medium 6 false false false false false false false SUPPORTED GALAXY DWARF SPHEROIDAL This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY DWARF SPHEROIDAL J2000 J2000 WFC3/UVIS Imaging No No F395N ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F814W WFC3/UVIS Imaging No No F395N ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F814W Hst Same orient constraint links visits (01 02 03 04 05 06) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v01.xml This is the first visit to Tucana. We do not require orient restrictions in order to maximize schedulability for the field in the primary exposure. Each visit to Tucana consists of two orbits. In each orbit, we will acquire two primary exposures in F395N using WFC3/UVIS (no CR-splits). The coordinated parallel exposures are divided into F475W and F814W using ACS/WFC (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "01" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:26:15.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2861 :al-overhead-at-end 127 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2851 :al-overhead-at-end 127 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 2 0 Hst Same orient constraint links visits (01 02 03 04 05 06) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v02.xml The visits after the first visit to Tucana will require the same orientation as the first visit. Similarly to the first visit, each visit will consist of two orbits. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "02" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:26:13.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "02" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2861 :al-overhead-at-end 127 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2851 :al-overhead-at-end 127 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 2 0 Hst Same orient constraint links visits (01 02 03 04 05 06) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v03.xml The visits after the first visit to Tucana will require the same orientation as the first visit. Similarly to the first visit, each visit will consist of two orbits. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "03" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:32:29.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "03" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2861 :al-overhead-at-end 127 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "03" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2851 :al-overhead-at-end 127 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 2 0 Hst Same orient constraint links visits (01 02 03 04 05 06) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v04.xml The visits after the first visit to Tucana will require the same orientation as the first visit. Similarly to the first visit, each visit will consist of two orbits. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "04" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:32:36.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "04" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2861 :al-overhead-at-end 127 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2851 :al-overhead-at-end 127 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 2 0 Hst Same orient constraint links visits (01 02 03 04 05 06) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v05.xml The visits after the first visit to Tucana will require the same orientation as the first visit. Similarly to the first visit, each visit will consist of two orbits. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "05" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:32:43.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "05" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2861 :al-overhead-at-end 127 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "05" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2851 :al-overhead-at-end 127 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 2 0 Hst Same orient constraint links visits (01 02 03 04 05 06) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v06.xml The visits after the first visit to Tucana will require the same orientation as the first visit. Similarly to the first visit, each visit will consist of two orbits. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "06" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:32:54.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "06" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2861 :al-overhead-at-end 127 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "06" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2851 :al-overhead-at-end 127 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 2 0 /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v07.xml Hst Same orient constraint links visits (07 08 09 10 11 12) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. This is the first visit to Cetus. We require constraints on orientation, and for remaining visits to this galaxy, we request the same orient as in this visit. That way, coordinated parallels with ACS/WFC will always fall in the same field. Each visit to Cetus except the final consists of two orbits; the final visit is one orbit only. In each orbit, we will acquire two primary exposures in F395N using WFC3/UVIS (no CR-splits). The coordinated parallel exposures are divided into F475W and F814W using ACS/WFC (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "07" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:32:57.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "07" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2766 :al-overhead-at-end 94 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "07" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2756 :al-overhead-at-end 124 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) true 2 0 /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v08.xml Hst Same orient constraint links visits (07 08 09 10 11 12) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. The visits after the first visit to Cetus will require the same orientation as the first visit. Similarly to the first visit, each visit will consist of two orbits. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "08" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:33:00.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "08" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2766 :al-overhead-at-end 94 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "08" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2756 :al-overhead-at-end 124 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) true 2 0 /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v09.xml Hst Same orient constraint links visits (07 08 09 10 11 12) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. The visits after the first visit to Cetus will require the same orientation as the first visit. Similarly to the first visit, each visit will consist of two orbits. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "09" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:33:03.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "09" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2766 :al-overhead-at-end 94 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "09" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2756 :al-overhead-at-end 124 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) true 2 0 /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v10.xml Hst Same orient constraint links visits (07 08 09 10 11 12) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. The visits after the first visit to Cetus will require the same orientation as the first visit. Similarly to the first visit, each visit will consist of two orbits. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "10" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:33:06.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "10" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2766 :al-overhead-at-end 94 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "10" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2756 :al-overhead-at-end 124 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) true 2 0 /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v11.xml Hst Same orient constraint links visits (07 08 09 10 11 12) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. The visits after the first visit to Cetus will require the same orientation as the first visit. Similarly to the first visit, each visit will consist of two orbits. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "11" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:33:26.0" :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 2291872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "11" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2766 :al-overhead-at-end 94 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16226 :visit-id "11" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2756 :al-overhead-at-end 124 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) true 2 0 /Users/swfu/research/proposals/cycle28_cetustucana/OP-cache/Cetus_Tucana_APT-v12.xml Hst Same orient constraint links visits (07 08 09 10 11 12) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. The visits after the first visit to Cetus will require the same orientation as the first visit. In the final visit to Cetus, we require only one orbit for a total of 11 orbits for this galaxy in this proposal. We will take two exposures in F395N per orbit (no CR-splits) with WFC3/UVIS. The coordinated parallel exposures are taken with ACS/WFC, and each orbit is divided into one F475W and one F814W exposure (no CR-splits). (Tic-Visit :proposal-id 16226 :visit-id "12" :proposal-version -1 :trans-version "20200619" :date "24-Sep-2020 10:33:12.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1145936 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16226 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16226 :visit-id "12" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2766 :al-overhead-at-end 94 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) true 1 0