0 Assigned ID: 2395 ----- Attempting Submission 1 (Fri Apr 09 22:54:02 GMT 2021) ----- HST Phase I Proposal 2395 successfully submitted. Receipt: # 2395-1 ----- Attempting Submission 2 (Fri Apr 09 23:15:06 GMT 2021) ----- HST Phase I Proposal 2395 successfully submitted. Receipt: # 2395-2 ----- Attempting Submission 3 (Fri Apr 09 23:18:54 GMT 2021) ----- When I checked the BOT, it showed few safety warnings in GSC but no issues are found while using the GALEX catalog. Since it assumes a spectral type of O5, where as the actual targets have later spectral types, I hope this will not make any problems. 1887406469 ----- Attempting Submission 1 (Wed Jul 28 06:44:48 GMT 2021) ----- The HST probes the winds and feedback of metal poor OB stars in the tidally stripped Magellanic Bridge\ Metallicity is one of the most fundamental parameters governing both stellar and galactic evolution. However, the impact of metallicity on the physics of massive stars and their feedback is empirically not well constrained at low metallicities. The Magellanic Bridge, which is our nearest tidally interacting environment with significantly low mean metallicity Z<~0.1Zsol, offers a unique laboratory for this study. Recently three O-type and few early B-type stars in the Bridge were identified via optical spectroscopy. This newly discovered sample will allow to characterize the winds of metal-poor massive stars and to empirically establish the scaling of mass-loss with metallicity, which cannot be done by using optical data alone. We selected 6 UV brightest OB stars as targets to obtain COS FUV spectra. The spectra will be analyzed using advanced non-LTE stellar atmosphere models, thereby determining the stellar, wind parameters, and Fe abundances of individual massive stars in the Bridge. The empirical mass-loss rates at low metallicity will be used to constrain stellar evolution models. Two B stars in our sample showing high UV excess are suspected to be binaries and might hide a hot companion. The far UV spectra are crucial to identify and characterize the stripped He companions of B stars which are not found yet at low metallicity. The UV + optical spectral analysis is essential to quantify ionizing fluxes as well as mechanical energy provided by OB stars at low metallicity. Together with physics and abundances of diffuse gas from ISM lines, our study will shed light on stellar feedback and star formation, as well as constrain the formation history of the Bridge. The coordinates and proper motions of the targets are taken from GAIA DR2 catalog. We adopted different observing strategies depending on the spectral type. For O stars we use only COS-FUV and for B stars we use both FUV and NUV. In COS-FUV, we use G130M with cenwave 1291 with two allowed FP-POS, and G160M cenwave 1611 with ALL FP-POS. In COS-NUV, we use G185M with two settings cenwave 1913 and 1953, with ALL FP-POS. In the case of WDG-8, both NUV and FUV observations are planned in a sigle orbit. For other two B stars (S0XA000379, S0XA000375), FUV and NUV obesrvations will be in two consecutive orbits. The team consists of experts in all subjects relevant for the proposal. Dr. W.-R. Hamann is a leading experts in UV spectroscopy of massive stars and stellar wind modeling. Prof. Gallagher is a leading expert in observations of stellar populations in star forming galaxies. Drs. T. Shenar, A. Sander, L. Oskinova, R. Hainich and V. Ramachandran have large experience with studies of massive stars in the Magellanic Clouds. Dr. Ramachandran (PI) has published spectroscopic studies of OB stars in the SMC, LMC and the Magellanic Bridge. Dr. Hainich has recently published grids of spectral models for OB-type stars in the SMC. Dr. Oskinova is the PI of large observing campaigns in optical to spectroscopically study OB stars in the SMC, and of the HST UV spectroscopic observations of the most massive stars in the SMC and star cluster NGC 346. Dr. Shenar is an expert in binary analysis of massive stars, and has published tools for spectral deconvolution of binary star spectra. Dr. Sander is an expert in hydrodynamic modeling of stellar winds, including winds from metal poor stars. The Co-Is have large experience in developing the models and theory of stellar winds, and in mass loss diagnostics in clumped winds based on UV spectroscopy. The primary modeling tools for the analysis of the observations will be the PoWR non-LTE stellar atmosphere model which is actively used for the analysis of metal poor OB stars. Recent publications include: Ramachandran, V., Oskinova, L. M., & Hamann, W.-R. 2021 A&A, 646, 16 Discovery of O stars in the tidal Magellanic Bridge. Stellar parameters, abundances, and feedback of the nearest metal-poor massive stars and their implication for the Magellanic System ecology Gilkis, A., Shenar, T., Ramachandran, V., et al. 2021 MNRAS 603, 1884 The excess of cool supergiants from contemporary stellar evolution models defies the metallicity-independent Humphreys-Davidson limit J.S. Vink & A.A.C. Sander 2021 MNRAS (in press) Metallicity-dependent wind parameter predictions for OB stars Fulmer, L. M., Gallagher, J. S., Hamann, W.-R., et al. 2020 A&A, 633, 164 Testing massive star evolution, star-formation history, and feedback at low metallicity. Photometric analysis of OB stars in the SMC Wing Ramachandran, V.; Hamann, W. -R.; Oskinova, L. M. et. al., 2019 A&A 625, 104 Testing massive star evolution, star formation history, and feedback at low metallicity. Spectroscopic analysis of OB stars in the SMC Wing Hainich et al., 2019, A&A 621, 85 PoWR grids of non-LTE model atmospheres for OB-type stars of various metallicities Ramachandran, V.; Hamann, W.-R.; Hainich, R.; et al, 2018, A&A 615, 40 Stellar population of the superbubble N 206 in the LMC. II. Parameters of the OB and WR stars, and the total massive star feedback Hainich, R.; Oskinova, L. M.; Shenar, T.; et al., 2018, A&A, 609, 94 Observational properties of massive black hole binary progenitors Ramachandran, Varsha; Hainich, R.; Hamann, W.-R.; et al., 2018, A&A 609, 7 Stellar population of the superbubble N 206 in the LMC. I. 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