0 Assigned ID: 4946 ----- Attempting Submission 1 (Mon Dec 18 18:38:06 GMT 2023) ----- 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 I have updated the aperture to UVIS2 and adjusted the postflash values per guidance from CS Mitchell Revalski. Please let me know if there are any remaining issues here! -151469005 ----- Attempting Submission 1 (Wed Jan 17 20:24:59 GMT 2024) ----- HST Phase II Proposal 17592 successfully submitted. Receipt: # 17592-1 ----- Attempting Submission 2 (Thu Jan 25 01:44:00 GMT 2024) ----- I am following guidance from my contact scientist regarding flash values. On behalf of the EHT's Multiwavelength (MWL) Working Group, we propose a joint campaign on M87: 100 ks XMM, 4 orbits Hubble, and 100 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 2024; the second will be coordinated with XMM and NuSTAR in December 24/Jan 25. 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. The winter and summer observations are similar, with adjustments to compensate for varying orbital visibility of M87. Generally each 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 to be coordinated with NuSTAR and XMM-Newton, the first orbit consists of three dithered 496 s exposures in F275W and two dithered 352 s exposures in F814W in ACCUM mode, for a total of 2192 s on source; the second orbit has 2x 571 s in F390W and 3x 349 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. Reduced visibility in March requires shorter exposures. The first orbit consists of three dithered 438 s exposures in F275W and two dithered 348 s exposures in F814W in ACCUM mode, for a total of 2046 s on source; the second orbit/visit has 2x 482 s in F390W and 3x348 s in F606W. Per our accepted XMM/HST/NuSTAR proposal, this visit should be scheduled within 1 day of a Chandra/EHT observation. Prof. Joey Neilsen, Prof. Daryl Haggard, Prof. Sera Markoff, Prof. Mike Nowak, Dr. Balokovic and Ms. Hope Boyce (a graduate student working with Prof. Haggard) have extensive experience in the multiwavelength monitoring of Event Horizon Telescope targets. Prof. Markoff sits on the EHT Science Council, while Prof. Haggard is a coordinator for the EHT Multiwavelength Working Group. Profs Neilsen and Nowak and Dr. Balokovic were actively involved in construction of an SED for M87 including HST data for the EHT MWL paper on M87. The team also has specific expertise for the HST analysis to be performed. Dr. Svetlana Jorstad and Prof. Sunil Chandra helped lead the analysis of the WFC3 observations for the paper above, including the modeling and subtraction of the host galaxy profile. WIth Dr. Amanpreet Kaur they have also performed detailed comparison of HST imaging to results from Swift/UVOT. For brevity we have not included numerous other co-investigators with expertise in theoretical and observational jet physics, optical and radio astronomy, and AGN. Supermassive Black Holes and Active Galaxies 6 false false false false false false false false SUPPORTED GALAXY ELLIPTICAL JET KNOT NUCLEUS J2000 J2000 WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F606W 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 1720638643834 /private/var/folders/bl/s7q0tqnn5gbcbyvcfnrhj2rh0004nc/T/OPVisit5948044556767733101.xml The scheduling data was generated by CASM 32.1.3. 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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