ORBITAL VISIBILITY OVERRUNAdded Visit 52 to reobserve QSO2. This is for HOPR 89178.-1564465948----- Attempting Submission 1 (Fri Jul 15 20:27:49 GMT 2016) -----
----- Attempting Submission 2 (Sun Jul 17 02:18:11 GMT 2016) -----
----- Attempting Submission 3 (Thu Oct 27 13:08:38 GMT 2016) -----
----- Attempting Submission 4 (Mon Oct 23 18:14:55 GMT 2017) -----Visit 02 failed due to FGS not being able to lock on guide stars. We were approved to reobserve this target as per HOPR 89178.The Proper Motion Field along the Magellanic Bridge: a New Probe of the LMC-SMC interactionOur HST PM measurements of the LMC and SMC have revolutionized our understanding of the Magellanic System, and have spurred new research on its use as a cosmological probe of galaxy formation. The PMs imply that the Magellanic Clouds are likely on their first infall towards the Milky Way (MW). The disturbed nature of the Magellanic System is therefore likely due to the LMC-SMC interaction, and not to the MW influence. This has emphasized the importance of dwarf galaxy interactions for galaxy evolution. The Clouds are connected by a complex of gas and stars called the Magellanic Bridge. We will map the stellar PM field of the Bridge, similar to our prior HST mapping of the LMC PM rotation field. Our state-of-the-art N-body simulations show that the PM field will tightly constrain the impact parameter of LMC-SMC orbit at its last pericenter 100-300 Myr ago, which is the main uncertainty in our understanding of the LMC/SMC interaction history. This will test whether the tidal debris between the galaxies is due to a recent direct-hit collision. It will also test models in which the tidal debris is responsible for the observed microlensing events. For each of the 8 target fields in the Magellanic Bridge, we expect to achieve PM accuracies of 10-25 km/s per field, well below the 130 km/s velocity difference between the Clouds. This will yield the best constraints to date on the LMC/SMC interaction, and will further test the importance of dwarf-dwarf interactions for galaxy evolution. We will also model the CMDs for all 16 (8 primary and 8 coordinated-parallel) fields, to better determine the stellar population properties of the Magellanic Bridge, and its spatial variation. The age and metallicty of the stars will further constrain the N-body models and the scenarios for the formation of the Magellanic Bridge.To measure the absolute proper motion of stars in the program fields, we will use quasars as stationary reference sources. This Cycle 24 GO-14775 program is for obtaining the second-epoch images of the quasar fields in the Magellanic Bridge. The first-epoch images for the same fields have already been obtained through the Cycle 22 GO-13834 program. We will largely use the same strategy used in our first-epoch observations, but use the F606W as the primary filter in this epoch. In addition, we added one long F606W and one long F814W exposures to construct deep CMDs in our field that will help with the identification of Magellanic Bridge stars. Each field in this epoch will consist of a single orbit observation, obtaining multiple dithered WFC3/UVIS exposures in a POSTARG pattern to optimize PSF sampling.RESOLVED STELLAR POPULATIONS6falsefalsefalsefalsefalsefalseSUPPORTEDGALAXYQSOB0202-765J2000J2000GALAXYQSOB0242-7229J2000J2000GALAXYQSOB0251-675J2000J2000GALAXYQSOESO31-8J2000J2000B = 15.5GALAXYQSOESO55-2J2000J2000B = 15.7ACS/WFCImagingNoNoF775WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF775WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF775WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode./private/var/folders/7q/8p7_k1q56vlfhxhm_v9tnb6m0004ph/T/OPVisit4980162471021074165.xmlThis is the visit for second-epoch observation of MCBRIDGE-QSO1.(Tic-Visit
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