0 Assigned ID: 1689 ----- Attempting Submission 1 (Thu Apr 08 19:27:31 GMT 2021) ----- Updated to cycle through FP-POS for each orbit as suggested by Ravi Sankrit. 1384642424 ----- Attempting Submission 1 (Thu Jul 08 20:59:04 GMT 2021) ----- ----- Attempting Submission 2 (Tue Sep 28 17:21:29 GMT 2021) ----- The Missing Piece of the IC 10 X-1 Puzzle: What is the Mass of the Black Hole? IC 10 X-1 belongs to the extremely rare class of Wolf-Rayet + black hole binary stellar system, and is a valuable laboratory for understanding massive star evolution, black hole formation, and the effects of X-ray irradiation on stellar winds - but only if we know the mass of the black hole. Black hole masses in these systems have proven notoriously difficult to measure with ground-based optical spectroscopy; only Hubble FUV spectroscopy currently capable of achieving a black hole mass measurement, as was demonstrated for the twin system NGC 300 X-1 (HST program #15999). With a well-constrained orbital period (1.45175d), full X-ray coverage with Chandra, XMM-Newton, and NuSTAR, and copious quantities of archival Gemini spectroscopy available, FUV spectroscopy that samples the binary orbital period is the only missing piece of the black hole mass-puzzle for IC 10 X-1. We request 10 orbits with COS/G140L to constrain the mass of the black hole in IC 10 X-1, which will have far-reaching consequences for understanding black formation and for constraining future evolutionary pathways (including the possibility of compact object-merger events) of massive binary stellar systems. We will collect COS spectra for the Wolf-Rayet + black hole binary IC 10 X-1 at five different orbital phases (with 2 orbits per visit). The instrument settings for all four visits is identical: IC 10 X-1 (5 x 2 orbits): COS/FUV G140L. The best measurement of the binary orbital period is 1.45175 +/- 0.00001 d, with a zero-point time corresponding to phase=0.5 (e.g., the deepest part of the X-ray dip) on MJD 54040.87. The Hubble visits should roughly sample the entire binary orbital period, although they need not be taken during a single orbital cycle. However, to keep the orbital phase uncertainty to a minimum, all HST visits should be completed within roughly two months of one another. Dr. Breanna Binder led the successful joint Chandra-Hubble program (HST program #15999) that led to the improved black hole mass estimate of the ``twin'' Wolf Rayet + black hole system NGC 300 X-1. She is an expert in both NGC 300 X-1 and IC 10 X-1, and has extensive experience observing both systems across multiple wavelength regimes. Drs. Laycock and Christodoulou are experts on IC 10 X-1, and have published numerous studies of the multiwavelength properties of the source. Mr. Bhattacharya is a graduate student under Drs. Laycock and Christodoulou who will be writing his dissertation on observations of IC 10 X-1 and other similar X-ray binary systems. Dr. Chene is an expert in analyzing Gemini spectroscopy, and has been collaborating extensively with Mr. Bhattacharya on analyzing archival Gemini spectroscopy of IC 10 X-1. Stellar Physics and Stellar Types 6 false false false false false false false false SUPPORTED STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 Timing link suitability includes constraints ([Group (01 02 03 04 05) Within 75.0 days]) The scheduling data was generated by CASM 29.2. 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