Resubmitting because Col Dr Thomas M. Bown was missing in previous submission. -919107813 Assigned ID: 1109 ----- Attempting Submission 1 (Fri Apr 10 23:55:47 GMT 2015) ----- HST Phase I Proposal 1109 (phase1-FUV.apt) successfully submitted. Receipt: # 1109-1 ----- Attempting Submission 2 (Mon Apr 13 03:00:11 GMT 2015) ----- HST Phase I Proposal 1109 (phase1-FUV.apt) successfully submitted. Receipt: # 1109-2 ----- Attempting Submission 3 (Mon Apr 13 03:22:43 GMT 2015) ----- This is resubmission updates the filters of the imaging observation (as discussed by email). I have made sure the visbility for each orbit remains the same as for the previous submission (by leaving the same amount of "unused" time at the of the orbit). 1060914367 ----- Attempting Submission 1 (Tue Jul 21 09:57:07 GMT 2015) ----- HST Phase II Proposal 14255 (14255.apt) successfully submitted. Receipt: # 14255-1 ----- Attempting Submission 2 (Thu May 05 21:59:56 GMT 2016) ----- A First Look at the Late Stages of Accretion in Tidal Disruption Flares A star that passes too close to a supermassive black hole will be disrupted by the black hole's tidal gravity. The result is an electromagnetic flare that can outshine the optical luminosity of the host galaxy for a few months. The return rate of stellar debris decreases from highly super-Eddington to sub-Eddington in a few years, making stellar tidal disruptions flares (TDFs) a unique laboratory to study accretion physics. Synoptic surveys have so far yielded about 10 strong TDF candidates, and many more (10-100 per month) can be discovered by ongoing and near-future surveys. So far we have only observed the optical/UV emission in the first ~100 days after the discovered event. The luminosity of this emission is too large to be produced in a compact accretion disk, and instead likely originates from ~100s-1000s of gravitational radii from the black hole. After a few years, however, these outer regions will cool significantly, allowing us to directly observe the inner disk with short wavelength observations. Even in the most pessimistic scenario, the flux is readily detected at FUV wavelengths in ~1 HST orbit. Here we propose HST ACS/SBC observations to measure the luminosity and temperature of newly formed accretion disks in a carefully selected sample of 8 known TDFs. These would be the first observations of late-time disk emission from tidal flares, greatly increasing our currently limited understanding of TDF emission mechanisms. In a broader sense, these observations might prove essential to fully realize the potential of TDFs as general tools in the era of time-domain astronomy. ACS SBC observations of eight targets. One orbit per source. Our targets are faint point sources (FUV>20) at the center of resolved galaxies. For the first 3 targets we plan both imaging in two filters (F125LP and F150LP) and slitless spectroscopic observations with PR130L. For these three targets, the spectroscopic observations should be about 25% of the full time for science observations of the orbit. For targets 4 to 8 we request only imaging (again, in F125LP and F150LP). We have decided to use 1x2 (LINE) dithering for the imaging observations and for the PR130L observations. Analysis using BOT revealed no bright targets that yielded warning flags. All our targets are covered by GALEX imaging, no FUV-bright stars are in the field of view. AGN/QUASARS 12 false true false false false false SUPPORTED GALAXY ACCRETION DISK J2000 J2000 GALAXY ACCRETION DISK J2000 J2000 GALAXY ACCRETION DISK J2000 J2000 GALAXY ACCRETION DISK J2000 J2000 GALAXY ACCRETION DISK J2000 J2000 GALAXY ACCRETION DISK J2000 J2000 GALAXY ACCRETION DISK J2000 J2000 GALAXY ACCRETION DISK J2000 J2000 ACS/SBC Imaging No No F115LP ACS/SBC Spectroscopic No No PR130L ACS/SBC Imaging No No F115LP ACS/SBC Spectroscopic No No PR130L ACS/SBC Imaging No No F115LP ACS/SBC Spectroscopic No No PR130L ACS/SBC Imaging No No F115LP ACS/SBC Imaging No No F115LP ACS/SBC Imaging No No F115LP ACS/SBC Imaging No No F115LP ACS/SBC Imaging No No F115LP POS-TARG DITHER 0.472 LINE false false 2 44.4 ACS-SBC-DITHER-LINE 2 false /private/var/folders/66/gcbl87_j2rj5d1c1yf4865h40000gn/T/OPVisit7174337445868663152.xml The scheduling data was generated by CASM 24.0. CASM was run in Phase II mode. 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