Submission 2, minor text changes914748237Assigned ID: 5974
----- Attempting Submission 1 (Thu Nov 07 13:23:23 GMT 2024) -----
HST Phase I Proposal 5974 successfully submitted.
Receipt: # 5974-1
----- Attempting Submission 2 (Thu Nov 07 23:02:16 GMT 2024) -----Phase II for GO-17926. Observing Draco and NGC2419 for proper motion cross calibration between ACS, WFC3 and NIRCam.1093971711----- Attempting Submission 1 (Wed Jan 29 19:42:23 GMT 2025) -----Enabling cross instrument proper motions with Draco dSph and NGC 2419An unexpected way that ACS/WFC has transformed our knowledge of the Universe is through kinematics, especially via the measurement of proper motions (PMs) for galaxies and star clusters across the Local Group (LG) and beyond. This work requires extremely high precision astrometry and relies on long time baselines. Together, these requirements have made ACS the best, and in many cases, the only instrument for this type of work. Through observations of the Draco and NGC 2419, this proposal aims to cross-calibrate ACS/WFC with WFC3/UVIS and JWST/NIRCam to enable this important science to continue after ACS/WFC is decommissioned. We will also improve the determination of the type of dark matter halo in the Milky Way satellite galaxy Draco dwarf spheriodal, core or cusp, to a limit of 10 sigma. This will be the best data to date for resolving the tension of the core-cusp problem in Lambda CMD. We will also investigate the kinematic properties of the known multiple populations in the distant massive Milky Way Globular cluster NGC 2419 , which will help constraints its formation and evolution.We propose to observe Draco dSph and the Milky Way globular cluster NGC 2419 in order to cross match the astrometric results with near simultaneous HST/ACS and HST/WFC3 observations of these targets. This will allow us to astrometrically calibrate these instruments to enable future proper motion measurements using cross observatory and cross instrument calibrations we derive. This will enable to use of ACS images as first epochs even after ACS is decommissioned, something that is not currently possible without a second epoch of ACS measurements. We will also compare with JWST NIRCam.Team Expertise:
PI Dr Paul Bennet is an expert in satellites inside and outside of the LG. He has had previous experience leading successful HST programs, e.g GO-15858 (Bennet et al. 2020). Dr Bennet has also succesfully led multiple HST programs related to the photometry and astrometry of dwarf galaxies using ACS (e.g. GO-15858, GO-17174 and GO-17501) including looking at orbital histories, dwarf galaxy quenching and the links between them. He is also a member of the NIRCam instrument team which will be highly useful in this cross-calibration work. Dr Bennet will lead and perform the majority of the work for this project.
Co-I Dr Tony Sohn is an expert in measuring HST proper motions, his past measurements include M31, bulk proper motions of dwarf spheroidal galaxies in the Milky Way halo (Leo I, Draco, and Sculptor), individual proper motions of stars along stellar streams such as Sagittarius, Orphan, and Lethe, distant Milky Way globular clusters, and M31 satellites NGC 147 and 185. Dr Sohn will contribute to the PM measurements part of this work.
Co-I Dr Ekta Patel is an expert in orbital modelling and mass modelling in the Local Group. Dr Patel will contribute to the orbital history of our targets based on the PMs found in this program and contribute to the MW mass estimation.
Co-I, Dr K. McKinnon is an expert in rigorous statistical combinations of HST images with Gaia data, which enables significantly improved measurements of astrometry than either dataset can measure alone.
Co-I, Dr Eduardo Vitral, is an expert in the intepretation of internal proper motions and mass modeling using 3D kinematic data.
Co-Is Dr Mark Fardal, Dr. Andrea Bellini, Dr. Erik Tollerud, Dr. Mattia Libralato, Dr. Andrew Pace, Dr. Christopher Garling, Dr Roeland van der Marel, Dr Nitya Kallivayalil, Dr Laura Watkins and Mr Jack Warfield are experts in HST kinematic analysis, dynamical mass estimation, and dynamical modeling of Local Group galaxies including both equilibrium and N-body modeling. They will contribute to the calculations and interpretation of the results.
See list of refereed publications by the HSTPROMO group at http://www.stsci.edu/~marel/hstpromo.html#PapersStellar Populations and the Interstellar MediumGalaxies6falsefalsefalsefalsefalsefalsetruePRIMARY2.4trueSUPPORTEDGALAXYDWARF ELLIPTICALJ2000J2000EXT-CLUSTERGLOBULAR CLUSTERJ2000J2000ACS/WFCImagingNoNoF606WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF814W/private/var/folders/w_/jnjpw_kd2_dgbfb8dt29vldc0002m5/T/OPVisit10940531785385998520.xmlTiming link suitability includes constraints ([Group (01 02) Within 90.0 days])The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.(Tic-Visit
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