0Assigned ID: 4505
----- Attempting Submission 1 (Wed May 24 18:50:55 GMT 2023) -----
HST Phase I Proposal 4505 successfully submitted.
Receipt: # 4505-1Unschedulable Visit
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Unschedulable VisitWe have manually combined the recommended POS-TARGS from ACS ISR 2023-4 with the (slightly larger) 20 pixel box patttern between visits for each primary+parallel group. Note that the Target confirmation charts will not show 4 of the 5 galaxies due to being extremely LSB objects. If deeper image cutouts that clearly show the faint targets are needed to re-create these charts, please let us know.
We want to thank Christian Soto for the usual help with phase II, and Debopam Som for help with the WFC3 backgrounds
Also thanks to Shelly Meyett for additional help re: working in RGM mode.
Resubmission (V3) 07/01/2024 - reworked phase II due to RGM mode. SOme targets moved to other ACS chip. Redone without LOWSKY constraint due to 10% loss in esposure time and extreme difficulties in scheduling
schedulability issues with series of visits with SAME ORIENT AS. Program now much easier to schedule, with perhaps only a much of a 0.1 mag drop in photometric depth.
Resubmission (V4) 07/05/2024 - changes ORIENT angles for two targets to facilitate guide star acquisition. Added preferred dates for same two targets in the first half of year to
mimize sky background without LOWSKY. Schedulability still over 4-5 weeks per target per year
Resubmission (V5) 08/12/2024 - changed one parallel target in Visit04 from ANTI-SUN to 'ANY", as the rest of them are.
Resubmission (V6) 1/9/2025 - Created duplicate of failed VIsit 15 = Visit 21
Resubmission (V7) 1/14/2025 - removed BETWEEN constaint for Visit 21 for schedulability
Resubmission (V8) 1/17/2025 - 4 more orbits to be rescheduled due to guide star failures. VIsit 22 is a duplicate of failed VIsit 16, and VIsit 23 is a
\combination of the 3/4th images=Orbit 2 from each of Visits 13 and 14 .
IMPORTANT: If duplicating Visit 13/14 orbits should be done as two single orbit visits (rather than a single 2 orbit visit), please advise.
Resubmission (v9) - increased ORIENT range of VIsit 22 and 23 (to 275-305) to potentiallyallow imprived schedulability. Note: VIsit 23 is SAME ORIENT as Visit 22. If that constrains things too much, we can revise.
Resubmission (v10) - added VIsit 24 = single orbit visit (F814W only) from failed Visit 22. Changed ORIENT to 160-169 to allow for possible scheduling in April 2025, but ACS field less than 1' from a bright (V=11) star. Moving to a different ORIENT to increase this distance would mean a different schedule.2045274591----- Attempting Submission 1 (Thu Sep 14 17:49:51 GMT 2023) -----
HST Phase II Proposal 17528 successfully submitted.
Receipt: # 17528-1
----- Attempting Submission 2 (Thu Sep 14 19:03:32 GMT 2023) -----
----- Attempting Submission 3 (Mon Jul 01 18:46:08 GMT 2024) -----
HST Phase II Proposal 17528 successfully submitted.
Receipt: # 17528-3
----- Attempting Submission 4 (Fri Jul 05 13:58:04 GMT 2024) -----
----- Attempting Submission 5 (Mon Aug 12 18:50:49 GMT 2024) -----
----- Attempting Submission 6 (Thu Jan 09 18:49:36 GMT 2025) -----
----- Attempting Submission 7 (Tue Jan 14 23:16:06 GMT 2025) -----
----- Attempting Submission 8 (Fri Jan 17 18:33:54 GMT 2025) -----
HST Phase II Proposal 17528 successfully submitted.
Receipt: # 17528-8
----- Attempting Submission 9 (Thu Jan 23 19:40:39 GMT 2025) -----
----- Attempting Submission 10 (Tue Mar 04 18:30:25 GMT 2025) -----Resubmitted Phase II for a single replacement orbit (VIsit 24) pervious observations already catrried out, so show up as unschedulable in VIsit PlannerUltradiffuse Galaxies in the Virgo ClusterThe "ultradiffuse galaxies" (UDGs) found within galaxy clusters present challenges to models of galaxy formation and evolution. They may be diffuse field galaxies only now falling into the cluster, post-infall galaxies undergoing rapid transformation, or long-lived cluster galaxies stabilized against disruption by massive dark halos. Recent observations also suggest systematic differences between their globular clusters (GCs) and those of normal galaxies. Unfortunately, large uncertainties in the distances, dynamics, and GC populations of UDGs continue to complicate our understanding of these galaxies.
We propose deep imaging of five Virgo Cluster UDGs to pinpoint their positions within Virgo via accurate tip of the red giant branch (TRGB) distances, allowing us to quantify their local environments: in the Virgo core, the cluster outskirts, or intervening field. Coupled with published kinematic data, we will determine if they are infalling objects or ones that have already passed through the Virgo core. Using imaging that probes three magnitudes below the GC luminosity function turnover, we will construct larger and cleaner GC samples than possible from the ground, allowing us to measure the physical sizes and luminosities of their GCs to test for systematic differences between GCs in UDGs and those in normal galaxies. Finally, we will compare the properties of their compact nuclei to ultracompact dwarf galaxies (UCDs) in Virgo to test the evolutionary link between UDGs and UCDs. The information provided by HST will be used in conjunction with simulations to study cluster-driven evolution and transformation of low density galaxies.The program is to obtain deep F814W images of a sample of five ultra-diffuse galaxies (UDGs) in the Virgo cluster, and to obtain photometry of very faint point sources over the entire FOV. We are using ACS as primary to get the larger FOV on the target galaxy, and using WFC3 in parallel to obtain a 'background' field necessary for our science goals. There are also single orbit F475W visits in order to get photometry for any marginally resolved globular clusters wihtin each galaxy. We have used different ACS apertures and offset coordinates for our targets in order to get as much of the target galaxy in the ACS FOV, whilst still availding bright stars in either the ACS primary iomages or the CPAR WFC3 images, which we are using for background estimation.
F814W - we have 7 orbits (split into 4 visits) in this filter for each of the five targets. For each of the three 2-orbit visits, we are using a small custom 4 point dither-box to best sample the PSF in the ACS primary exposures AND the WFC3/UVIS parallels. We have used the POS-TARGS from Anderson (2023) ISR ACS 2023-04 for ACS primary, and WFC3/UVIS in parallel. Between visits, we are using POS-TARGs to create a slightly larger (~20 pixels) box pattern to assist with hot-pixel removal. As per suggestion from instrument scientists, we have combined the small and large POS-TARGs and defined each ACS+WFC3 exposure as an individual group.
The 4th part of this larger box (location 4) is a single orbit (2 exposures only), so we only use the first two points in the small dither pattern used in the 3 preceding visits. We are not trying to cover the ACS chip gap, and the box sizes we are using (4 to 20 pixels) should be small enough allow for decent sub-pixel dithering over as much of the ACS /WFC3 FOV as possible.
F475W - here we are taking 3 exposures over the single orbit in a single visit. There is no clear best way to dither 3 exposures to fill out the PSF, so we have used the first 3 POS-TARGS from the custom box pattern used above, and have each ACS+WFC3 exposure done at each specific POS-TARG. We have added this single oprbit to the single $814W orbit noted above to get a 4th visit.
Exposure times: All of our F814W observations (ACS and WFC3) are 2 images per orbit -- there will be a total 14 individual F814W images per target, so CR removal in construction of a single deep image will be straightforward. We have anywhere from 30-45 days of scheduability for all of our visits. The single orbit in F475W will employ 3 primary+parallel images; although not optimal for PSF re-contruction, the sky background should be high enough ACS that we do not require any FLASH for these ACS+F475W images.
Roll Angles: All Visitis for a given target to be made at the same roll angle as the first Visit. For each target, we have chosen ORIENT ranges that (a) allow for as much schedule-ability as is possible, (b) avoid bright stars in the primary ACS FOV, and (c) place the WFC3 parallel fields in a location from of bright stars and/or other galaxies. For two objects the roll angles are further constrained to be sure the center of the galaxy does not approach the chip gap (both galaxies nearly fill the entire ACS FOV) -- on those cases (VCC 1052 and VCC 1448) the small ORIENT ranges did NOT result in reducing schedueability.
LOW-SKY: We had originally requested LOW-SKY for our observations, as our targets are ~15 degrees from the ecliptic, and we want as low a sky background as possible for the deep F814W images. However, with RGM mode, the strong cuts to exposure times and reducgtion in availble dates made this unfeasible. We have thus dropped the LOWSKY requirement (for RGM mode), and worked the schedule of the observations and ORIENT values to minimize the zodiacal light background of our images (using the ETC as a guide) while retaining most on-orbit visiility and much for flexability for scheduling. (these dates are Jan-May in any given year) This will only make our photometric limits 0.1 mag brighter that originally planned, which will not have an adverse effect on our science goals.
FLASH? To maximize sky backgrounds to reduce CTE effects, we are using long exposures : 1/2 orbit images in F814W, and 1/3 orbit images in F475W for both cameras. With our 1/2 orbit exposures in F814W for both ACS and WFC3, we will not need any post-FLASH for any exposures. For the shorter (~715s) F475W exposures, we will have high enough sky backgrounds in ACS (~30-40e- at lowest using plots from Anand et al 2022, and ETC https://etc.stsci.edu/etc/results/ACS.im.1889538/ ) to not require any post-FLASH.
For WFC3, the ~715s F475W exposures are predicted (via the APT) to have sky backgrounds of 12e-/pixel Thus we may need a FLASH of (at most) 8e- for these shorter F475W exposures for WFC3 only to reach the 20e- background. Most other CTE reduction strategies will not work here as our sources cover the entire FOV.Our team is comprised of key members of the ground-based Next Generation Virgo Survey (NGVS) and Hubble ACS Virgo Survey (ACSVCS). We have extensive experience working with HST imaging data, and studying the Virgo Cluster from ground and space, using both resolved and integrated stellar populations. We also have a strong track record of spectroscopic followup of Virgo galaxies and their globular clusters using large ground-based telescopes.
Patrick Cote has expertise in the study of galaxy structure and evolution, star clusters, and galactic nuclei. He was the principal investigator of the ACSVCS.
Patrick Durrell has extensive experience in data reduction and point-source photometry of faint stellar populations on both ACS and WFC3 images, including multiple projects over the past decade studying the RGB populations in nearby galaxies.
Laura Ferrarese is the PI of the NGVS and a key member of ACSVCS and the ACS Fornax Cluster Survey. She has expertise in the structure and kinematics of galaxies and their nuclei, including the study of supermassive black holes.
Raja Guhathakurta has worked extensively on the formation and evolution of galaxies and has been a leader in the spectroscopic components of the PISCeS and NGVS surveys, and well as the the spectroscopic supplement to PHAT, the HST multi-cycle treasury survey of M31.
Sungsoon Lim works on the stellar populations of nearby galaxies, and has led the effort to find UDGs in the NGVS imaging, cuminating in the Virgo UDG catalog that shapes our sample. He recently led a paper on globular clusters and nuclear star clusters in Coma cluster UDGs based entirely on HST imaging (GO-14658).
Chris Mihos has worked extensively on deep imaging of galaxies and clusters, having led the Burrell Schmidt Virgo Survey which discovered many of these UDGs. He is PI on several recent HST studies of resolved stellar populations in external galaxies, including the pilot project for this study in which the TRGB distance estimate and dynamical history of the Virgo ultradiffuse galaxy VCC 615 (Mihos+22) was derived. He also has expertise in numerical simulations of interacting galaxies and galaxy clusters.
Eric Peng has deep experience studying extragalactic globular cluster systems and dwarf galaxies, and has led two recent HST programs studying GCs in UDGs (GO-14658 and GO-15417). Dr. Peng has played a key role in the identification and ground-based follow-up of Virgo cluster UDGs.
Laura Sales has expertise in dynamical simulations of galaxies and galaxy clusters, including her most recent works studying the formation and evolution of ultradiffuse galaxies in field and cluster environments.
Dr. Elisa Toloba has led many spectroscopic studies of galaxies and their globular clusters systems, and has expertise in developing dynamical mass estimates using sparse tracers. She led the recent Keck campaign to estimate dynamical masses for three of the Virgo UDGs in our sample (Toloba+18, 23).Galaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYLSBYESJ2000J2000GALAXYLSBJ2000J2000GALAXYLSBJ2000J2000GALAXYLSBJ2000J2000GALAXYLSBJ2000J2000ACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF475WWFC3/UVISImagingNoNoF475WACS/WFCImagingNoNoF475WWFC3/UVISImagingNoNoF475WACS/WFCImagingNoNoF475WWFC3/UVISImagingNoNoF475WACS/WFCImagingNoNoF475WWFC3/UVISImagingNoNoF475WACS/WFCImagingNoNoF475WWFC3/UVISImagingNoNoF475WHst Same orient constraint links visits (01 02 03 04)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 1 of 4 different POST TARGS for each of the 4 F814W-related visits. ORIENT range chosen by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. Restricted ORIENT here to avoid bright stars (brighter than V=15) in the WFC3 parallel field, which is to be used as a background. Even with this, can schedule for over 5 weeks/yr.
Note: the schedulable dates for this ORIENT range also co-incides with with lowest zodiacal light values MU_V>22.2 (using the ACS ETC to calculate), which will maximize the S/N of faint sources on the deep images.1740308480000262.0(Tic-Visit
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Second orbit has three shorter F475W images (again, using a custom POS-TARG pattern) to be used for studies of brighter objects (globular clusters). FLASH will be required on the F475W CPAR WFC3 images to reach the 20 e- level required to reduce CTE effects.1735863484000292.95222(Tic-Visit
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)true20Hst Same orient constraint links visits (09 10 11 12)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 3 of 4 different POST TARGS for each of the 4 F814W-related visits. ORIENT range chosen by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. Small ORIENT range does not significantly hurt schedulability. SAME ORIENT as previous visit1736646096000289.08585(Tic-Visit
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(Tic-Obset
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)true20Hst Same orient constraint links visits (09 10 11 12)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W image, 2 exposures in first orbit in box pattern using POS-TARGS pattern. Location 4 of 4 different 20 pixel dithers). Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. SAME ORIENT as first visit in series
Second orbit has three shorter F475W images (again, using a custom POS-TARG pattern) to be used for studies of brighter objects (globular clusters). FLASH will be required on the F475W CPAR WFC3 images to reach the 20 e- level required to reduce CTE effects.1736634755000289.08585(Tic-Visit
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)true20Hst Same orient constraint links visits (13 14 15 16 21)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 1 of 4 different POST TARGS for each of the 4 F814W-related visits. ORIENT range chosen by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. Chosen ORIENT to gain access to guide stars. Chosen dates after Jan 1 2025 to obtain zodiacal light values MU_V>22.2 (using the ACS ETC to calculate), which will maximize the S/N of faint sources on the deep images. V=11.3 star located about 1' from ACS field; can shift field slightly further N if problematic. Tasrgrt schedulability about 5 weeks1736657306000298.0(Tic-Visit
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(Tic-Orbit
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:max-dark-utilization 1920
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)true20The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 1 of 4 different POST TARGS for each of the 4 F814W-related visits. ORIENT range chosen by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. Chosen ORIENT to gain access to guide stars. Chosen dates after Jan 1 2025 to obtain zodiacal light values MU_V>22.2 (using the ACS ETC to calculate), which will maximize the S/N of faint sources on the deep images. V=11.3 star located about 1' from ACS field; can shift field slightly further N if problematic. Tasrgrt schedulability about 5 weeks
Visit 23 is a 2-orbit visit that combines the second failed orbit of VIsit 13, and the second failed orbit of Visit 14. In order to ease scheduabaility, VIsit 23 is same ORIENT as Visit 22, which has a more relaxed ORIENT range of 275-305 degrees compared to the successful images in VIsits 13, 14 and the scheduled VIsit 21.1739894751000291.38931(Tic-Visit
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)true20Hst Same orient constraint links visits (13 14 15 16 21)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 2 of 4 different POST TARGS for each of the 4 F814W-related visits. Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. For VLSB-D, the elongated nature of this galaxy necessitates a smaller ORIENT range (very schedule-able) to maximize TRGB stars in the WFC1 chip. V=11.3 star located about 1'; from ACS field; can shift field slightly further N if problematic.1736566584000298.0(Tic-Visit
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)true20Hst Same orient constraint links visits (13 14 15 16 21)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 3 of 4 different POST TARGS for each of the 4 F814W-related visits. Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. For VLSB-D, the eklongated nature of this galaxy necessitates a smaller ORIENT range (very schedule-able) to maximize TRGB stars in the WFC1 chip. V=11.3 star located about 1'; from ACS field; can shift field slightly further N if problematic.1736197974000298.0(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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:max-dark-utilization 1920
:low-sky "N"
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)true20Hst Same orient constraint links visits (13 14 15 16 21)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W image, 2 exposures in first orbit in box pattern using POS-TARGS pattern. Location 4 of 4 different 20 pixel dithers). Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. For VLSB-D, the elongated nature of this galaxy necessitates a smaller ORIENT range (very schedule-able) to maximize TRGB stars in the WFC1 chip. V=11.3 star located about 1'; from ACS field; can shift field slightly further N if problematic.
Second orbit has three shorter F475W images (again, using a custom POS-TARG pattern) to be used for studies of brighter objects (globular clusters). FLASH will be required on the F475W CPAR WFC3 images to reach the 20 e- level required to reduce CTE effects.1736702668000298.0(Tic-Visit
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:data-volume 2864864
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(Tic-Obset
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(Tic-Orbit
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:max-dark-utilization 1920
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)true20Hst Same orient constraint links visits (13 14 15 16 21)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 3 of 4 different POST TARGS for each of the 4 F814W-related visits. Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. For VLSB-D, the eklongated nature of this galaxy necessitates a smaller ORIENT range (very schedule-able) to maximize TRGB stars in the WFC1 chip. V=11.3 star located about 1'; from ACS field; can shift field slightly further N if problematic.
Note- duplicate of Visit 15, which failed guidestar lock1738438016000298.0(Tic-Visit
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:data-volume 2291872
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(Tic-Obset
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(Tic-Orbit
:proposal-id 17528
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:si-vis-utilization 2634
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(Tic-Orbit
:proposal-id 17528
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:si-vis-utilization 2634
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:dark-offset NIL
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)true20The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W image, 2 exposures in first orbit in box pattern using POS-TARGS pattern. Location 4 of 4 different 20 pixel dithers). Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. For VLSB-D, the elongated nature of this galaxy necessitates a smaller ORIENT range (very schedule-able) to maximize TRGB stars in the WFC1 chip. V=11.3 star located about 1'; from ACS field; can shift field slightly further N if problematic.
Second orbit has three shorter F475W images (again, using a custom POS-TARG pattern) to be used for studies of brighter objects (globular clusters). FLASH will be required on the F475W CPAR WFC3 images to reach the 20 e- level required to reduce CTE effects.
NOTE: Visit 22 is a duplicate of the failed VIsit 16 - in order to aid rescheduling schedule, expanded ORIENT range to 275-3051739724708000291.38931(Tic-Visit
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:data-volume 2864864
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(Tic-Obset
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(Tic-Orbit
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)true20The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode./private/var/folders/ny/3pp1x6l94l58lsgpvwnw0hv40000gn/T/OPVisit332408579042694273.xmlF814W image, 2 exposures in first orbit in box pattern using POS-TARGS pattern. Location 4 of 4 different 20 pixel dithers). Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. For VLSB-D, the elongated nature of this galaxy necessitates a smaller ORIENT range (very schedule-able) to maximize TRGB stars in the WFC1 chip.
NOTE: V=11.3 star located less than 1' from ACS field.\ -- if any issue we may need to consider a different ORIENT.
NOTE: Visit 24 is a duplicate of the failed F814W orbit (2 exposures= first orbit) from Visit 22 - in order to aid rescheduling, changed ORIENT range based on availability for mid April 2025 observationsi Maintains center of galaxy at some location/chip as previous observations.(Tic-Visit
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)true10Hst Same orient constraint links visits (17 18 19 20)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 1 of 4 different POST TARGS for each of the 4 F814W-related visits. Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars (some V=15 stars near ACS FOV), and (c) placement of parallel WFC3 field to maximize scientific yield.VCC 1448 is one of the largest galaxies in our sample; we have offset the center of the galaxy slightly W of the WFC aperture center to maximize the amount of the galaxy in the ACS FOV, whilst still keeping the nucleus and the inner ~20" from the chip gap. We have chosen a restricted ORIENT to be sure the galaxy core does not approach the chip gap, but this restricted range does NOT compromise scheduleability, which remained unchanged. All scheduleable dates within requested ORIENT range fall with zodiacal light values MU_V>22.2 (using the ACS ETC to calculate), which will maximize the S/N of faint sources on the deep images.1735772743000285.0(Tic-Visit
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)true20Hst Same orient constraint links visits (17 18 19 20)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 1 of 4 different POST TARGS for each of the 4 F814W-related visits. Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield.VCC 1448 is one of the largesst galaxies in our sample; we have offset the center of the galaxy slightly E of the WFC aperture center to maximize the amount of the galaxy in the ACS FOV, whilst still keeping the nucleus and the inner ~20" from the chip gap. We have chosen a restricted ORIENT to be sure the galaxy core does not approach the chip gap, but this restricted range does NOT compromise scheduleability, which remained unchanged. All scheduleable dates within requested ORIENT range fall with zodiacal light values MU_V>22.2 (using the ACS ETC to calculate), which will maximize the S/N of faint sources on the deep images.1736107380000285.0(Tic-Visit
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(Tic-Orbit
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)true20Hst Same orient constraint links visits (17 18 19 20)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W images, 2 exposures per orbit in custom dither-box pattern using POS-TARGs. Location 1 of 4 different POST TARGS for each of the 4 F814W-related visits. Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. VCC 1448 is one of the largesst galaxies in our sample; we have offset the center of the galaxy slightly E of the WFC aperture center to maximize the amount of the galaxy in the ACS FOV, whilst still keeping the nucleus and the inner ~20" from the chip gap. We have chosen a restricted ORIENT to be sure the gtalaxy core does not approach the chip gap, but this restricted range does NOT compromise scheduleability, which remained unchanged. All scheduleable dates within requested ORIENT range fall with zodiacal light values MU_V>22.2 (using the ACS ETC to calculate), which will maximize the S/N of faint sources on the deep images.1735852152000285.0(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
:proposal-id 17528
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:orbit-number 2
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:si-vis-utilization 2634
:al-overhead-at-end 0
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)true20Hst Same orient constraint links visits (17 18 19 20)The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.F814W image, 2 exposures in first orbit in box pattern using POS-TARGS pattern. Location 4 of 4 different 20 pixel dithers). Small ORIENT range dictated by (a) maximizing schedule-able roll angles, (b) avoidance of bright stars, and (c) placement of parallel WFC3 field to maximize scientific yield. VCC 1448 is one of the largest galaxies in our sample; we have offset the center of the galaxy slightly E of the WFC aperture center to maximize the amount of the galaxy in the ACS FOV, whilst still keeping the nucleus and the inner ~20" from the chip gap. We have chosen a restricted ORIENT to be sure the galaxy core does not approach the chip gap. Small ORIENT range does not significantly change schedulability.
Second orbit has three shorter F475W images (again, using a custom POS-TARG pattern) to be used for studies of brighter objects (globular clusters). FLASH will be required on the F475W CPAR WFC3 images to reach the 20 e- level required to reduce CTE effects.1735348567000285.0(Tic-Visit
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