Proposal approved through XMM OTAC. Please contact me if this Phase I proposal is incomplete or incorrect. 617761392 Assigned ID: 6050 ----- Attempting Submission 1 (Mon Dec 23 05:54:17 GMT 2024) ----- FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser 0 ----- Attempting Submission 1 (Thu Jan 23 21:24:42 GMT 2025) ----- HST Phase II Proposal 17902 successfully submitted. Receipt: # 17902-1 ----- Attempting Submission 2 (Mon Nov 03 19:28:13 GMT 2025) ----- Flash and dither patterns are as advised by Mitchell Revalski last cycle to use the slightly higher current modes, enabling longer exposure times. On behalf of the EHT's Multiwavelength (MWL) Working Group, we propose a joint campaign on M87* coordinated in part with EHT: 50 ks XMM-Newton, 4 orbits Hubble, & 50 ks NuSTAR. These observations will improve constraints on (1) the SED of M87* and its particle acceleration processes, as well as (2) the variability of the famous jet across the electromagnetic spectrum. The goal of our HST program is to study the optical and UV variability of M87 in conjunction with NuSTAR and XMM-Newton observations. We are particularly interested in tracking the relative flux and SED changes of the core and the knot HST-1 over time. Our observations will occur in two pieces separated by roughly six months and consisting of two orbits each. The first piece should be coordinated with XMM and NuSTAR in June/July 2025; the second will be coordinated with XMM and NuSTAR in December 25/Jan 26. We adopt a modified version of the WFC3/UVIS observing strategy used for historical Hubble M87 monitoring (e.g. PI:Shara). In our analysis, comparable exposures produced to 3-10% uncertainties on the core and HST-1 fluxes after subtracting the host galaxy contribution. Generally each visit consists of two orbits to acquire observations in F275W and F814W (orbit 1) and F390W and F606W (orbit 2) in ACCUM mode. For the summer visit ~contemporaneous with XMM-Newton/NuSTAR, the first orbit consists of three dithered 462 s exposures in F275W and two dithered 348 s exposures in F814W in ACCUM mode, for a total of 2084 s on source; the second orbit has 2x509 s in F390W and 3x348 s in F606W. ETC calculations are given for the nucleus and are approximate as they neglect the host galaxy. The remaining ~1 ks per orbit is covered by overhead (setup, readouts, filter changes, and dithering). We mitigate CTE with a flash to increase the background; sub-exposures reduce cosmic rays. The winter visit ismuch the same, though roll angle constraints make it possible to arrange simultaneous observations with XMM/NuSTAR. Dr. Baganoff is an expert in X-ray observations of Sgr A*. Dr. Balokovic is an expert in X-ray observations of accreting supermassive black holes. Dr. Boyce is an expert in X-ray variability of Sgr A*. Prof. Bower is the Project Scientist for the EHT and is an expert in radio/submm variability of accreting black holes. Prof. Chandra is an expert in accretion and blazars. Dr. Doeleman is the Founding Director of the EHT. Prof. Hada is a member of the EHT Science Council and an expert in VLBI observations of AGN. Prof. Haggard is an expert in X-ray variability and spectroscopy of supermassive black holes. %Dr.\ Jorstad is an expert in multiwavelength variability of blazars. Dr. Johnson is a member of the EHT Science Council and an expert in interferometric imaging of black holes. Dr. Krichbaum is a member of the EHT Science Council and an expert in VLBI. Dr. Kim is an expert in interferometric imaging of jets. Dr. Komossa is an expert in accretion and dynamics in galactic centers. Prof. Lu is an expert in VLBI observations of jets. Prof. Markoff is a member of the EHT Science Council and an expert in the physics of jets and accretion. Prof. Neilsen is an expert in X-ray spectral variability of accreting black holes. Prof. Nowak is an expert in X-ray spectral variability of accreting black holes. Prof. Psaltis is an expert on accretion theory and tests of General Relativity. Dr. Wong is an expert in the theory and interpretation of EHT images. Prof. Zhang is an expert in X-ray observations of galactic nuclei. Balokovic, Boyce, Haggard, Markoff, Neilsen, Nowak, and Zhang will lead the X-ray and optical/UV analysis, with contributions from Komossa, Chandra, and Baganoff. Bower, Hada, Johnson, Krichbaum, Kim, Lu, and Psaltis will contribute to multiwavelength analysis and interpretation of the results. All members of the team are members of the Event Horizon Telescope Collaboration or partners in its Multiwavelength Working Group. Supermassive Black Holes and Active Galaxies 6 false false false false false false true SECONDARY XMM_NEWTON 96139 false SUPPORTED GALAXY ELLIPTICAL JET KNOT NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM. J2000 J2000 WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F390W POS-TARG DITHER DITHER 4 2.414 WFC3-UVIS-DITHER-BOX false 81.785 true 0.112 0.173 3 85.759 POS-TARG WFC3-UVIS-GAP-LINE 23.884 1 false POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 2 false 1737494108841 /Users/jneilsen/Documents/Villanova/Proposals/HST/Cycle32/PhaseII/OP-cache/Untitled-v01.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. This observation should be scheduled to overlap with XMM-Newton observations; the "between" requirement represents the window where XMM observations can occur. 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CASM was run in Phase II mode. This observation should be scheduled to overlap with XMM-Newton observations; the "between" requirement represents the window where XMM observations can occur. 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