0 Assigned ID: 1324 ----- Attempting Submission 1 (Tue Jan 31 00:52:56 GMT 2017) ----- HST Phase I Proposal 1324 (test1.apt) successfully submitted. Receipt: # 1324-1 ----- Attempting Submission 2 (Tue Jan 31 16:42:34 GMT 2017) ----- HST Phase I Proposal 1324 (submitted version 1.apt) successfully submitted. Receipt: # 1324-2 ----- Attempting Submission 3 (Tue Jan 31 22:36:16 GMT 2017) ----- HST Phase I Proposal 1324 (submitted version 2.apt) successfully submitted. Receipt: # 1324-3 ----- Attempting Submission 4 (Wed Feb 01 02:14:24 GMT 2017) ----- HST Phase I Proposal 1324 (submitted version 2.apt) successfully submitted. Receipt: # 1324-4 ----- Attempting Submission 5 (Wed Feb 01 02:27:23 GMT 2017) ----- INEFFICIENT ORDERING OF FP-POS POSITIONS The FP-POS inefficiency warnings may be disregarded because the exposures are organized to go through all positions sequentially as suggested by the Contact Scientist for efficiency. 1633612453 ----- Attempting Submission 1 (Thu Mar 30 17:02:03 GMT 2017) ----- ----- Attempting Submission 2 (Mon Apr 17 03:29:03 GMT 2017) ----- ----- Attempting Submission 3 (Thu Apr 20 04:42:32 GMT 2017) ----- HST Phase II Proposal 14919 (14919-modified-2.apt) successfully submitted. Receipt: # 14919-3 ----- Attempting Submission 4 (Fri Apr 21 19:43:06 GMT 2017) ----- The FP-POS inefficiency warnings have been noted and I do not consider it a serious problem for this program. Stellar mergers between nondegenerate stars have long been thought to have an important influence on stellar clusters, and perhaps be the origin of a number of types of peculiar stars. It is estimated that a significant fraction of stars eventually undergo a merger. No spectroscopic observations of a pre-merger system in its final interacting phase have ever been obtained. Models of the merger process are in wide disagreement. They predict a number of observable effects leading up to the merger, some of which can affect the merger process itself. Mergers, and the final common-envelope binary phase of stars, are not well understood, partly because the models have not been well tested. We propose to obtain the first UV spectroscopy of a Kepler contact binary system which will merge in about 2022. These observations will provide crucial constraints on merger models for the first time. Our observations will also determine the nature of the UV excess of this system already detected by broadband UV photometry. Whether the UV excess comes from a white dwarf companion or from some other process, knowing its nature is essential to understanding this system and its forthcoming merger. We wish to obtain a series of spectra in a single visit in order to cover a complete period of the target. Stellar Physics 6 false true false false false false SUPPORTED EXT-STAR ACCRETION DISK CIRCUMSTELLAR MATTER G V-IV NO J2000 J2000 COS/NUV Spectroscopic No No G230L 2635 COS/FUV Spectroscopic No No G140L 1280 1492704934613 C:\Users\Zeke\Desktop\2017 HST mid-cyc KIC\OP-cache\14919-modified-3-v01.xml The scheduling data was generated by CASM 25.0. CASM was run in Phase II mode. 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