0Assigned ID: 151
----- Attempting Submission 1 (Wed Apr 06 18:39:25 GMT 2016) -----
HST Phase I Proposal 151 (la24.apt) successfully submitted.
Receipt: # 151-1
----- Attempting Submission 2 (Fri Apr 08 14:18:10 GMT 2016) -----This submission contains a target not contained in the Phase I proposal.
We requested a target switch from SPM4.0-0390226948 to CD14-A05 in
HOPR 85049, approved by the TTRB on 7/7/16.
Second submission (7/20/16): we have updated the acquisition in both visits to incude an ACQ/SEARCH (2x2)
before the ACQ/IMAGE.667470416----- Attempting Submission 1 (Tue Jul 12 19:42:06 GMT 2016) -----
----- Attempting Submission 2 (Wed Jul 20 14:52:37 GMT 2016) -----The Origin of the Leading Arm of the Magellanic StreamA vast debris field of gas connects the Magellanic Clouds and the Milky Way. Known as the Leading Arm (LA), this structure is actively feeding the Galactic disk with new fuel for star formation. Three main concentrations of gas exist, named LA I, LA II, and LA III, but the metallicity has only been measured in one of these three (S/H=0.25+/-0.07 solar in LA II), and the physical connections between the regions are unclear. Here we propose COS FUV spectroscopy of two additional targets (one star and one QSO) that probe LA I and LA III, to map the LA metallicity as a function of position. By comparing the LA chemical abundances in each region we will directly test models of LA formation (single stripping event vs multiple episodes) and therefore constrain the dynamics of the Magellanic System. The observations will also provide measurements of the dust content of the LA via the S/Fe ratio, and the high-ion content via the Si IV doublet, which traces the interaction between the LA and the hot halo of the Milky Way.
Overall, this program will form a case study of the only gas structure accreting onto the Milky Way that can be traced to a neighboring galaxy, and will therefore explore the mechanisms by which galaxies fuel their star formation.This is a 6-orbit proposal to observe two targets (one star and one QSO) in the direction of the Leading Arm of the Magellanic Stream.
V01 observes a QSO (UVQSJ101629.20-315023.6, z=0.24) with the G130M/1291 setting, for four orbits. It uses an ACQ/SEARCH (2x2) and an ACQ/IMAGE, both with MIRRORB.
V02 observes a B V star (CD14-A05, T_eff=15000; spectral type B5 IV, this target is not in SIMBAD since it was discovered and characterized by members of our team), for two orbits total, one with G130M/1291 and one with G160M/1600. This also uses an ACQ/SEARCH (2x2) and ACQ/IMAGE, both with MIRRORB.
Note that CD14-A05 was not in the original Phase I proposal. Our original stellar target was SPM4.0. However, observations obtained after the Phase I deadline revealed that this target was a sub-dwarf, much closer than previously thought, and of no connection to the Leading Arm. Therefore we requested a target switch to CD14-A05 in HOPR 85049, approved by the TTRB on 7/7/16.Stellar Physics12falsetruefalsefalsefalsefalseSUPPORTEDISMABSORPTION LINE SYSTEM - GALACTICHIGH VELOCITY CLOUDTIDAL TAILNOJ2000J2000FUV=17.32, NUV=17.13, Magnitude given above is B (V unavailable)STARB3-B5 V-IVNOJ2000GALEX NUV=16.83, FUV=16.70COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600/private/var/folders/tk/3gx7p0k112l_9pg4glzb8hhh00015x/T/OPVisit517207729150543315.xmlThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.(Tic-Visit
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