0 Assigned ID: 1887 ----- Attempting Submission 1 (Fri Apr 09 12:17:05 GMT 2021) ----- HST Phase I Proposal 1887 successfully submitted. Receipt: # 1887-1 ----- Attempting Submission 2 (Fri Apr 09 12:25:52 GMT 2021) ----- HST Phase I Proposal 1887 successfully submitted. Receipt: # 1887-2 ----- Attempting Submission 3 (Fri Apr 09 19:41:40 GMT 2021) ----- 0 ----- Attempting Submission 1 (Fri Jul 02 13:56:59 GMT 2021) ----- ----- Attempting Submission 2 (Mon Sep 06 11:18:14 GMT 2021) ----- A dormant black hole or a stripped Helium star in a massive binary system The quest for dormant stellar-mass black holes (BHs) in massive binaries (i.e., OB+BH systems) is raging. All the candidates proposed so far have been heavily disputed in the weeks following their report. Combining a literature search and archival spectroscopic data with innovative analysis techniques, we have identified two promising massive binaries harboring unseen companions with masses above the BH-mass limit, and for which simulations could discard the presence of a 5Msun main-sequence stellar companion. Here we request STIS/FUV spectroscopy of the best candidate (that with the heaviest companion mass) to unveil or discard the presence of a hot, Helium stripped star as the unseen companion. A Helium stripped star would indeed contribute very little to the system optical flux, but its contribution would become more significant in the far-UV. Should the proposed observations fail to reveal such hot companion, this project will prove beyond doubt the presence of a BH, with important consequences on the evolution of gravitational-wave progenitors and the debated presence of a kick accompanying BH formation. Either outcome -- either a Helium stripped star or a dormant BH -- will result in a significant leap forward in our understanding of the evolution of massive stars, but only the FUV capabilities of HST can discriminate between both scenarios. 8-epoch FUV/STIS spectroscopy of a single target. 8 visits (1epoch per visit). Phase constraint are given for each observations of this 14d-period binary GA WAVECAL have been manually placed after the science exposure to optimize science exposure duration Impact of reduced-gyro operations on the program: none expected unless the visibility of the visits are strongly reduced BOT: Galex observations are available. Both the GSC&Galex BOT as well as ETC computations confirm the target is safe Our team is composed of observers expert in multiwavelength spectroscopy of massive stars, including in UV and optical high resolution spectroscopy, in UV-optical atmosphere modelling of massive stars (incl. codes such as CMFGEN, FASTWIND and POWR) and in massive stellar evolution and GW progenitors. Members of our team mastered the techniques needed to reach the objectives of this project: STIS instrument (Sana is a former instrument scientist in the COS/STIS team), orbital analysis (Sana, Mahy, Fabry; see the many publication on binaries in ADS), spectral disentangling (Mahy, Shenar; see e.g., Mahy et al. 2020a,b; Shenar et al. 2020), analysis of stellar atmosphere and stellar winds of O-type stars (Abdul-Masih, Mahy, Shenar, see e.g., Abdul-Masih 2019 displaying the first spectral disentangling of COS UV spectroscopy of an O-type binary). The high degree of expertise and a full description of the advanced disentangling methods needed for this specific project have been developed to check and refute earlier claims of the presence of black holes (BHs) in OB+BH systems (Abdul-Masih et al. 2020, Nature; Bodensteiner et al. and Shenar et al. 2020, A&A). Our team further includes theoreticians (Langer, Marchant) who have predicted the occurance of OB+BH systems (Langer et al. 2020, includig several other coIs of this proposal) as well as studied various patways to produce BH binaries (e.g., Marchant et al. 2016). They will lead the analysis of the kick velocities should we confirm the OB+BH nature of the object. The feasibility of retrieving direct constraints on the kick velocity is demonstrated at the end of the proposal. As ESA investigators, we are not elligeable for HST funding, however, the Leuven team is currently funded by the ERC-Consolidator Grant MULTIPLES that runs until 2023 so that there is enough funds to guarantee the availability and sustainbility of the team for the entire duration of the project. Stellar Physics and Stellar Types 6 false false true false false false false false SUPPORTED STAR GIANT O NO J2000 J2000 U=9.14, G=9.1143 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 /private/var/folders/fk/cphy05pn5jvgyrcz6vtfchzwdpknxl/T/OPVisit5076385122349295343.xml The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. 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