0Assigned ID: 845
----- Attempting Submission 1 (Fri Apr 05 22:05:46 GMT 2019) -----
HST Phase I Proposal 845 (gd1.apt) successfully submitted.
Receipt: # 845-1
----- Attempting Submission 2 (Fri Apr 05 23:44:38 GMT 2019) -----FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browserAug 9, 2023: Resubmitted for the re-observations of failed visits 02, 03, 05, 06, 09. Replaced visits are 52, 53, 55, 56, 59.
Initial submit for the second-epoch program 16791.
Re-submitted after cutting down orbital lengths to allow wider windows in Visit Planner + splitting original Visits 05 and 08 each into 3 single-orbit visits.258337921----- Attempting Submission 1 (Tue Jul 23 14:02:22 GMT 2019) -----
----- Attempting Submission 2 (Wed Jul 24 17:35:20 GMT 2019) -----
----- Attempting Submission 3 (Wed Sep 18 18:37:07 GMT 2019) -----
----- Attempting Submission 4 (Mon Sep 23 17:10:13 GMT 2019) -----
HST Phase II Proposal 15930 (PID15930.apt) successfully submitted.
Receipt: # 15930-4
----- Attempting Submission 5 (Mon Sep 23 17:43:02 GMT 2019) -----
----- Attempting Submission 6 (Thu Dec 12 14:20:19 GMT 2019) -----
----- Attempting Submission 7 (Mon Jul 19 15:39:00 GMT 2021) -----
HST Phase II Proposal 16791 successfully submitted.
Receipt: # 16791-7
----- Attempting Submission 8 (Mon Jul 19 23:29:24 GMT 2021) -----
----- Attempting Submission 9 (Wed Aug 09 19:38:35 GMT 2023) -----Resubmitting for re-observations of failed visits. All errors/warnings pertain to completed or failed visits. Newly created visits (52, 53, 55, 56, 59) do not result in any error/warning.Cold Dark Matter and the GD-1 Stellar StreamWe propose to use HST to characterize a dark-matter subhalo in the Milky Way. Tidally disrupted globular clusters create thin and kinematically cold stellar streams that are extremely sensitive to any gravitational perturbation. Orbiting in the Milky Way halo, these streams provide a unique opportunity to test for the presence of perturbing dark-matter subhalos. Gaps discovered along streams provide tentative evidence for dark matter influence, but their origin remains uncertain as stream gaps alone can be due to baryonic effects as well. Recently, Gaia observations of the GD-1 stellar stream have revealed a spur of stars associated with one of the gaps in the stream. Such features naturally arise when a stream encounters a massive perturber, and have a unique 3D kinematic signature. We propose here to measure precise proper motions in the perturbed region of GD-1. We will target eight fields with ACS/WFC and parallel-observe with WFC3/UVIS in two epochs. Proper motion accuracies near 3 km/s will be achieved by measuring the relative motion between stream stars and background galaxies using established techniques that have already been successfully applied to other objects in the Local Group (e.g., LMC/SMC, Leo I, M31, Sgr and Lethe streams). A passing subhalo is expected to introduce differences in tangential velocity between the stream and the spur, and our data will have the precision to resolve these kinematic offsets. Our results will definitively establish whether GD-1 features are a signature of a dark matter subhalo. If HST confirms the subhalo origin of the gap, it will measure the physical properties of the subhalo and rule out all reasonable alternatives.The ultimate goal of this multi-cycle program (GO-15390 & 16791) is to obtain sets of images separated by 3 years in time for measuring absolute proper motions of individual stars along the GD-1 stellar stream. As part of the Cycle 27 program GO-15930, the first-epoch data for 16 (8 primary ACS/WFC + 8 parallel WFC3/UVIS) target fields were obtained on Feb 2020 using F606W and F814W filters. For this Cycle 29 program GO-16791, we will obtain the second-epoch data for the same 16 target fields using the same telescope configurations (pointings and orientations) as in the first-epoch observations. The second-epoch data will be primarily used for measuring motions of stars against background galaxies, so we only use the F606W filter. We added "Orient Ranges" special requirements for each visit to align our second-epoch observations with the first-epoch ones as closely as possible. We also added "Timing Requirements" to allow time baselines to be in accordance with our request in the Phase 1 proposal. Each visit has 3 orbits, and each primary or parallel orbit has 1 short + 2 long F606W exposures.PI Ana Bonaca is an expert in tidal streams, having discovered one of the most distant cold streams and also theoretically explored what aspects of the Milky Way can be constrained from observations of tidal streams. Together with CoI Price-Whelan, she most recently discovered a sign of perturbation in the GD-1 stream using Gaia data. As a follow-up, she dynamically modeled the observed GD-1 features and showed they can be caused by a massive object passing by a stellar stream, which inspired this proposal.
CoI Charlie Conroy is an expert in stellar population studies on scales from individual stars to most massive galaxies in the universe. He has plentiful experience with HST observations, and has most recently published a study of stellar variability in M51 from the ongoing HST project GO 14704.
CoI David W. Hogg is an expert in data analysis, including experimental design and modeling of dynamical systems with noisy stars and complex selection functions, as well as precision imaging analysis. He was a part of the groundbreaking effort in understanding the dynamical theory of dark-matter interactions with cold stellar structures.
CoI Nitya Kallivayalil is an expert in astrometry, whose inventive use of HST to measure proper motions of the LMC/SMC system has revolutionized our understanding of these objects. She has a career of experience in measuring proper motions with HST, and is the PI of an ongoing effort to measure precise proper motions for all satellites of the Milky Way (GO 14734).
CoI Adrian Price-Whelan is an expert in the Milky Way dynamics, and has worked in areas spanning from signatures of orbital chaos in tidal streams to identification of binaries from sparse radial velocity data. Together with PI Bonaca, he most recently discovered a sign of perturbation in the GD-1 stream using Gaia data that inspired this proposal.
CoIs Sangmo Tony Sohn and Roeland van der Marel have together with CoI Kallivayalil developed a set of techniques for obtaining proper motions with HST that will be used in executing this project.Stellar Populations6falsetruefalsefalsefalsefalsefalsefalseSUPPORTEDSTELLAR CLUSTERGLOBULAR CLUSTERTIDAL TAILNOJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERTIDAL TAILNOJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERTIDAL TAILNOJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERTIDAL TAILNOJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERTIDAL TAILNOJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERTIDAL TAILNOJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERTIDAL TAILNOJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERTIDAL TAILNOJ2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WThe scheduling data was generated by CASM 31.0.CASM was run in Phase II mode./private/var/folders/7q/8p7_k1q56vlfhxhm_v9tnb6m0004ph/T/OPVisit8786419027437349855.xmlThis is a 3-orbit visit for the SPUR1 target field. We will observe this field using the F606W filters. We request a specific orient range to match the first-epoch's telescope orientation. Inidivual exposures will be dithered using a customized dither pattern designed for optimizing pixel-phase coverage via the POS TARG arguments. To fulfill our scientific goals, we require at least 3 years of time baseline as stated in our Phase 1 proposal. Since the first-epoch data for this field were obtained in Feb 2020, we added Timing Requirements of "After 01-AUG-2022:00:00:00".1676116825000182.93(Tic-Visit
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