0 Assigned ID: 139 ----- Attempting Submission 1 (Thu Aug 16 12:43:38 GMT 2018) ----- ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN approved HOPR 1626738962 ----- Attempting Submission 1 (Wed Dec 05 17:26:46 GMT 2018) ----- HST Phase II Proposal 15636 (lo-phaseII-x7.apt) successfully submitted. Receipt: # 15636-1 ----- Attempting Submission 2 (Wed Feb 06 16:58:41 GMT 2019) ----- ----- Attempting Submission 3 (Fri Jul 19 21:13:17 GMT 2019) ----- The warnings concern already scheduled exposures. What is on the black hole menu? Joint HST/COS and XMM/EPIC spectroscopy of the X-ray binary M33 X-7. We request 12 HST orbits to obtain the first UV spectra of the most massive known high-mass X-ray binary M33 X-7. This eclipsing system consists of a very massive O-type star and a 16 solar mass black hole immersed in the O star wind and feeding on it. The archival optical spectroscopy does not provide information on wind parameters of the donor star. Our immediate objective is to secure COS spectroscopy of M33 X-7 at different orbital phases. Obtaining these data is imperative to characterize the mass flow in this key system - a likely binary black hole progenitor. M33 X-7 is a strong source of X-rays which influence the donor star wind and affect its dynamics. Therefore, we request 25 ks of XMM-Newton time to obtain X-ray spectroscopy simultaneously with the UV observations. We propose observations at three key orbital phases, tracing the BH eclipse, egress, and inferior conjunction. From the eclipse spectrum we will accurately measure the wind velocity and mass-loss rate of the donor star which has a metallicty ten times lower than solar. Realistic wind parameters are crucially needed to develop the models of massive binary evolution towards binary black holes. Coordinated UV and X-ray measurements in eclipse and egress will describe the gas flows towards the BH and empirically establish its accretion efficiency, thus probing the theories of accretion onto a BH. This innovative study is possible only jointly with the HST and XMM and will have a long lasting science legacy. COORDINATES: Our target has Gaia DR2 coordinates whcih we use in Phase II. These are slightly different from SIMBAD coordinates/ ACQUISITION: The target is located in a relatively crowded field. Within the COS aperture (2.5 arcsec) there is a little cluster of stars, 0.9 arcsec away from the target. This cluster has similar brightness to our target. We are not sure how well the standard ACQ would work in this busy field and can suggest the follwoing strategies 1) We can select a nearby point source which also has GAIA DR2 coordinates. Then we can make offset to our target. Please advise how to do it in the APT? 2) If we center the COS aperture on our source, then the nearby cluster is in the aperture. In this case we need to introduce a roll angle constrain. Please advise how to determine it so that we can well separate the dispersed spectra? 3) May be we can place the aperture such that the nearby cluster is not in the aperture. But then our source will not be in the center. Is it possible and does it make sense at all? PHASE and ROLL ANGLE CONSTRAIN: We are observing an eclipsing binary. The observations are therefore constrained in binary orbit phase. The ephemeris are reaonably well known. We need to introduce a roll angle constrain to be able to separate the spectra of sources which fall in the COS aperture. We would like to discuss this with our Contact and Instrument Scientists to make our program as little constrained as possible, but the same time to be able to extract the spectra. Stellar Physics Massive Black Holes And Their Host Galaxies 6 false false true false false false 25 true SUPPORTED EXT-STAR GIANT O NO This object was generated by the targetselector and retrieved from the SIMBAD database. The coordinates and their uncertainty is updated using GAIA DR2 catalog: source name Gaia DR2 303377286991610752 J2000 ABmag 19.2 in wfc3_uvis_f275w filter STAR B0-B2 III-I NO Coordinates from Gaia DR2 The spectral type is a plausible guess. GAIA-DR2-303377286991607936 J2000 ABmag 19.2 in wfc3_uvis_f275w filter COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 /private/var/folders/z3/xy_g1v_s5fz9yrhzb8thz4cr0001qc/T/OPVisit15761486860886189002.xml The scheduling data was generated by CASM 27.2. CASM was run in Phase II mode. 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