Following advice from Linda Dressel we have reordered our WFC3 exposures so that the IR orbits do not take place at the end of each visit, have changed the UVIS apertures to UVIS2, and have added post-flash options to 6/7 of our UVIS exposures. ----- Attempting Submission 1 (Tue Jul 10 13:29:46 GMT 2012) ----- ----- Attempting Submission 2 (Wed Sep 26 16:29:52 GMT 2012) ----- The BOT flags an issue with a bright UV source in the field. This is the centre of the host galaxy of HLX-1, and is extended. We have previously observed this source with the ACS/SBC F140LP filter for a similar exposure time and experienced no issues whatsoever with saturation etc. due to the extension of the source. We are therefore confident that there will be no issues observing this target. The Stellar Population Around the Intermediate Mass Black Hole ESO 243-49 HLX-1 We request joint XMM-Newton and HST observations of the best intermediate mass black hole candidate HLX-1. Recent HST and Swift observations found the broadband spectral energy distribution was well described by an irradiated accretion disc plus a stellar population. However, degeneracies in the models resulted in two acceptable solutions with dramatically different parameter values. We request two observations to be performed with XMM-Newton and the HST at different X-ray luminosities in order to break these model degeneracies using the variability of the disc emission. With these two 5 orbit observations we will be able to determine the nature of the environment around the black hole, test formation theories for HLX-1, and rule out beaming as the origin of the extreme luminosities. We have been awarded 10 orbits of HST time with the ACS/SBC, WFC3/UVIS, and WFC3/IR cameras. We will observe the candidate intermediate mass black hole HLX-1 in the galaxy ESO 243-49 with simultaneous X-ray observations to be performed with the XMM-Newton telescope. We will split our orbits as such: 5 orbits during the mid-luminosity X-ray state and 5 orbits during the low-luminosity X-ray state. We request that our HST and XMM-Newton observations be peformed as close together as possible (preferably within +/- 2 days). During a previous set of HST observations of this source with a similar instrument setup, we were advised that there were issues with suitable guide stars in the field for both the ACS/SBC and WFC3/UVIS/IR cameras. To avoid this problem we assigned the ACS/SBC exposure to a separate visit that was performed 10 days apart from the WFC3 exposures. Our previous observation was triggered at short notice following an X-ray outburst. The new observations in this program will not be triggered, but will instead be scheduled during specific time windows when the source is expected to be in the mid and low luminosity X-ray states. We have separated our ACS/SBC and WFC3 exposures in a similar way as previously in order to maximise schedulability, but we request that if possible they be performed within +/- 2 days of each other (i.e. +/-2 days between visit 1 and visit 2, and +/- 2 days between visit 3 and visit 4). If this is not feasible, for example due to a lack of guide stars, please let us know so we can investigate alternative possibilities. UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE 12 false 0.0 186.0 0.0 false false false false SUPPORTED STELLAR CLUSTER ACCRETION DISK STAR FORMING REGION J2000 J2000 far-UV=24.11+/-0.05, H=24.4+/-0.3 ACS/SBC Imaging No No F140LP WFC3/UVIS Imaging No No F300X 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 F775W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W ACS/SBC Imaging No No F140LP WFC3/UVIS Imaging No No F300X 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 F775W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W POS-TARG DITHER 0.179 LINE 0.116 false false 63.65 4 20.02 ACS-SBC-DITHER-BOX 1 false POS-TARG DITHER 0.605 LINE false false 3 41.788 WFC3-IR-DITHER-LINE-3PT 4 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 5 false Timing link suitability includes constraints ([Group (01 02) Within 2.0 days]) The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /Users/saf28/Documents/My Proposals/XMM/XMM A011/HLX-1 HST/HST_phaseII/OP-cache/hlx1_xmmhst_latest_new-v01.xml First far-UV exposure with the ACS/SBV during the mid-luminosity state. 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CASM was run in Phase II mode. /Users/saf28/Documents/My Proposals/XMM/XMM A011/HLX-1 HST/HST_phaseII/OP-cache/hlx1_xmmhst_latest_new-v03.xml First far-UV exposure with the ACS/SBV during the low-luminosity state. 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