Science Keywords: Select from 2 to 5 items. Science Keywords is a required field. 0 Assigned ID: 2556 ----- Attempting Submission 1 (Wed Sep 15 12:15:27 GMT 2021) ----- Joint Chandra/HST FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser I choose the UVIS2-C512C-CTE aperture for the UVIS filters to move the target close to readout amp and adopt a lower post-flash level than required by the ETC that assumes the target at the CCD center. There is an error message when running the BOT; I get red lights for the ACS-SBC exposure (orbit 1), as "exceeding Health and Safety limit" based on an assumed total count rate on the chip in the F140LP filter. As explained in the previous 2018 observation, this should be false. I copy below the explanation from beflore by Robert: "However, when looking at the detailed tables of the count rates, I see that the near-UV flux was estimated from the optical flux of the galaxy ESO243-49 in the Guide Star Catalog, extrapolated to the near-UV assuming an O5V spectrum. I know that the O5V spectrum is assumed as worst-case-scenario when no other spectral information is available. However, in this case the assumption of such spectrum is clearly nonsense, because ESO243-49 is an early-type galaxy with an old stellar population and very little emission in the near-UV. So there is absolutely no chance that the near-UV flux will be anywhere near the safety limit. If you don't believe me, you can easily look at the 2010, 2012 and 2013 ACS observations in the same filter and see that it's faint and perfectly safe." 1913735602 ----- Attempting Submission 1 (Thu Oct 14 04:42:16 GMT 2021) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 2 (Thu Apr 21 14:02:03 GMT 2022) ----- There is an error message when running the BOT; I get red lights for the ACS-SBC exposure (orbit 1), as "exceeding Health and Safety limit" based on an assumed total count rate on the chip in the F140LP filter. As explained in the previous 2018 observation, this should be false. I copy below the explanation from beflore by Robert: "However, when looking at the detailed tables of the count rates, I see that the near-UV flux was estimated from the optical flux of the galaxy ESO243-49 in the Guide Star Catalog, extrapolated to the near-UV assuming an O5V spectrum. I know that the O5V spectrum is assumed as worst-case-scenario when no other spectral information is available. However, in this case the assumption of such spectrum is clearly nonsense, because ESO243-49 is an early-type galaxy with an old stellar population and very little emission in the near-UV. So there is absolutely no chance that the near-UV flux will be anywhere near the safety limit. If you don't believe me, you can easily look at the 2010, 2012 and 2013 ACS observations in the same filter and see that it's faint and perfectly safe." For EXP 5-5, there is a warning of flash level, but it is the recommended value from the ETC. We request a Chandra observation (80 ks) of two very rare objects that fall within the same field of view: the strong intermediate-mass black hole candidate ESO 243-49 HLX-1 and a newborn hard tidal disruption event (TDE). For HLX-1, which has been in a prolonged low state for nearly 4 yr, the data will be crucial to measure the current level of the low state and test two competing models for the formation of the system. Five HST orbits are also requested to pin down the host population and age by measuring the host in UV and optical when the contamination from the central source is minimal. For the new hard TDE, our goal is to constrain its long-term X-ray evolution, especially to detect the fast drop, which would be a strong indicator of a jet being shut off. Orbit 1: for ACS SBC F140LP, 4-point box dithering ~2640s of effective exposure time Orbit 2 for WFC3 UVIS F300X, with UV flashing and WFC3-UVIS-DITHER-BOX, 1456s split into 4 exposures of 364s each. Then the last 2 exposures in the F336W filter, also with UV flashing and dithering, 364s each; Orbit 3 for the last 2 exposures in the F336W filter, with UV flashing and dithering, 364s each, total of 1456s (including those of orbit 2). Then, all 4 exposures for F390W, dithered, 365s each, total of ~1460s (no UV flashing needed) Orbit 4 for F555W, 1480s split into 4 dithered exposures of 370s each. Then the first 2 exposures in the F621M filter, also with dithering, 371s each; orbit 5 for the last 2 dithered exposures in the F621M filter,371s each, total of 1484s. Then all 4 dithered exposures for F775W, 363s each, total of ~1452s. n/a Supermassive Black Holes and Active Galaxies 6 false false false false false false false false SUPPORTED STELLAR CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 ACS/SBC Imaging No No F140LP WFC3/UVIS Imaging No No F300X WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F621M WFC3/UVIS Imaging No No F621M WFC3/UVIS Imaging No No F775W POS-TARG DITHER 0.179 LINE 0.116 false false 63.65 4 20.02 ACS-SBC-DITHER-BOX 1 false POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 2 false 1634186209085 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16840 :visit-id "01" :proposal-version -1 :trans-version "20210514" :date "14-Oct-2021 00:36:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 7004096 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16840 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 16840 :visit-id "01" :obset-id "A1" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16840 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2901 :al-overhead-at-end 0 :internal-dur-at-end 117 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16840 :visit-id "01" :orbit-number 2 :pcs-time 383 :si-vis-utilization 2892 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16840 :visit-id "01" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2890 :al-overhead-at-end 125 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16840 :visit-id "01" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2893 :al-overhead-at-end 124 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16840 :visit-id "01" :orbit-number 5 :pcs-time 392 :si-vis-utilization 2891 :al-overhead-at-end 123 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) false 5 0 ACS.im.1011860 ETC run done using the well-determined Vega brightness in the U band and the best-fitting model spectrum. ACS.im.1011865 ETC run done using the observed flux density at 1500 Ang, from 2013. The two runs give essentially the same result, S/N = 10 for the requested exposure time. This is our best estimate of how the source will look like in 6 months' time. However, it could turn out to be a factor of 2 brighter or fainter, so the S/N could be ~7 or ~15.