Supposed to be the final version1007103500Assigned ID: 947
----- Attempting Submission 1 (Fri Mar 06 23:38:51 GMT 2020) -----
HST Phase I Proposal 947 successfully submitted.
Receipt: # 947-1
----- Attempting Submission 2 (Sat Mar 07 00:43:30 GMT 2020) -----
HST Phase I Proposal 947 successfully submitted.
Receipt: # 947-2
----- Attempting Submission 3 (Sat Mar 07 00:59:48 GMT 2020) -----
HST Phase I Proposal 947 successfully submitted.
Receipt: # 947-3
----- Attempting Submission 4 (Sat Mar 07 01:06:00 GMT 2020) -----The number of orbits used exceeds the number allocatedJan 04, 2022
Added visit 54 which is the approved re-observation of the four orbits of Visit 04.
Added visit 51 which is the approved re-observation of the two orbits of Visit 01.-1234465503----- Attempting Submission 1 (Wed Jun 03 20:39:58 GMT 2020) -----
----- Attempting Submission 2 (Thu Jun 04 19:45:53 GMT 2020) -----
----- Attempting Submission 3 (Mon Aug 16 20:08:06 GMT 2021) -----
----- Attempting Submission 4 (Tue Jan 04 21:26:09 GMT 2022) -----Visit 04 should be flagged as FailedResolved Proper Motions of M33As the only low-mass disk galaxy in the Local Group, M33 is one of the most important and best-studied galaxies on the sky. It is also one of the most confusing: since it is nearly bulgeless, it is unclear what makes it stable to formation of a strong bar. One stabilizing factor may be the existence of dynamically hot components such as a thick disk or halo, but these have long been controversial and hard to detect. Recent individual-star spectroscopy now gives clear evidence of a halo component, but its structural properties, its origin, and its dynamical effects are not yet clear. We propose to use proper motions with 16-year baselines to measure the kinematics of stars in five fields at the edge of the M33 disk. We will probe the relative rotational lag of the hotter components (the halo and a possible thick disk) versus the young, thin disk. We will measure the dispersions in the planar and vertical directions separately, using dispersions measured directly from proper motions as well as the correlation between the proper motions and LOS velocities from spectroscopy. We will check the halo for non-equilibrium flows indicating a possible origin in a recent merger. We will also provide an independent and more precise measurement of M33's center-of-mass proper motion. These observations are only feasible now because of the longevity of HST. They will yield a dataset completely unique in nature for any galaxy like M33, which will shed new light on the structure and dynamical history of this important galaxy.The primary goal of this program is to measure the proper motion (PM) of M33 stars using multi-epoch HST imaging. We will target 5 fields in total that have existing deep ACS/WFC imaging data. These are DISK2, DISK3, DISK4, M9, and U49. Each target field will be re-observed for 5 orbits with ACS/WFC using the same field locations and telescope orientations as the first-epoch observations. We will image all primary ACS/WFC target fields using F814W ro measure PMs. The parallel WFC3/UVIS fields will be observed using F606W and F814W to study the stellar populations and number density of M33 stars that are 6 arcmin away from our primary target fields.The majority of the investigators are members of the HSTPROMO group, led by co-I van der Marel, which has published numerous papers reporting proper motion measurements of dwarf galaxies, globular clusters, individual stars along stellar streams, and distant Milky Way (MW) halo stars.[*] PI Sohn has led many HST programs over the past decade for measuring proper motions of M31, dwarf spheroidal galaxies in the Milky Way halo (Leo I, Draco, and Sculptor), stars along stellar streams such as Sagittarius, Orphans, and Lethe, distant Milky Way globular clusters, and M31 satellites NGC 147 and 185. He has been the PI for several of these programs, and will oversee this entire program as well. Co-PI Fardal is an expert in dynamical analysis of stellar streams and galaxies in the Local Group. Co-I Watkins is an expert in velocity anisotropy analysis and dynamical mass estimation, and has particularly published papers studying the M31 galaxy and its satellites. Co-Is Besla, Patel, and van der Marel are experts in dynamical analysis of Local Group galaxies. CoI del Pino Molina is an expert in analysis of internal dynamics of galaxies in the Local Group. Co-I Tollerud is an expert in observations of the internal dynamics of M31 satellites and techniques. Co-Is Guhathakurta, Gilbert, and Quirk are experts in stellar spectroscopy and the structural components of M33. [*] See list of refereed publications by the HSTPROMO group at http://www.stsci.edu/~marel/hstpromo.html#PapersGalaxiesStellar Populations and the Interstellar Medium6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDISKHALOSPIRALJ2000J2000GALAXYDISKHALOSPIRALJ2000J2000GALAXYDISKHALOSPIRALJ2000J2000GALAXYDISKHALOSPIRALJ2000J2000GALAXYDISKHALOSPIRALJ2000J2000ACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WThe scheduling data was generated by CASM 29.2.CASM was run in Phase II mode./private/var/folders/7q/8p7_k1q56vlfhxhm_v9tnb6m0004ph/T/OPVisit8014317918401597484.xmlThis is the visit for imaging the M33-DISK2 field with ACS/WFC as primary and WFC3/UVIS as parallel. 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)
(Tic-Orbit
:proposal-id 16274
:visit-id "54"
:orbit-number 4
:pcs-time 392
:si-vis-utilization 2788
:al-overhead-at-end 0
:internal-dur-at-end 1015
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true40