LONG SU LIKELY TO INTERSECT THE SAA LONG SU LIKELY TO INTERSECT THE SAA The ACQ/IMAGE target acquisitions for all three visits were accidentally and incorrectly set to use MIRROR B. This is inappropriate, they are supposed to use MIRROR A. I have also updated the relevant ETC field for these TAs. The ACQ/IMAGE is designed to roughly meet a S/N of 40 on the detector. -594262260 ----- Attempting Submission 3 (Wed Feb 12 19:28:21 GMT 2014) ----- ----- Attempting Submission 4 (Tue Mar 04 17:25:04 GMT 2014) ----- Standard Long SU SAA warning. I think this is fine (correct?) Mysterious ionization in cooling flow filaments: a test with deep COS FUV spectroscopy The Cosmic Origins Spectrograph is capable of unraveling a two decade old mystery regarding the filamentary emission line nebulae found in the brightest cluster galaxies (BCGs) of cool core (CC) clusters. These kpc-scale filaments are characterized by elevated H-alpha luminosities and puzzling ionization states that cannot be accounted for by recombination or photionization alone, and are instead excited by an unknown ionization mechanism. The most hotly debated proposed solutions invoke thermal conduction, shocks, or cosmic-ray heating, but progress toward consensus awaits unambiguous spectral discriminants between these models that can only be found in the FUV. We propose deep (9 orbit), off-nuclear observations of two strategically selected BCGs in well-studied cool core clusters with cross-spectrum archival datasets. We also propose a shorter (5 orbit) on-nuclear observation for one of our targets to assess possible AGN contributions to the spectra. These proposed observations represent critical tests that can unambiguously discriminate between the various candidate ionziation models. Constraining the mechanisms by which CC BCG filaments are excited remains one of the most important roadblocks to a better understanding of cooling from hot ambient medium to cold star forming clouds and filaments, a process important for both galaxy and black hole growth. It is therefore important that, before HST ends its mission and we lose FUV capability, we advance our understanding of this decades old mystery. We will obtain deep COS FUV-mode spectroscopy of Abell 2597 (z=0.08) and ZwCl 3146 (z=0.29) with the G140L grating, tuned to a central wavelength of 1280 angstroms. Our goal is to go very deep (9 orbits, roughly 25 ksec) on the off-nuclear filaments in both of these targets. Additionally, we will take a shallower (5 orbit, ~15 ksec) observation of the A2597 nucleus (to assess possible AGN contribution to the spectra). Integration times have been estimated with the COS spectroscopic ETC using a conservative range of surface brightnessess whose median is centered on an inferred C I surface brightness of 1e-16 ersgs/sec/cm2/arcsec2. The ETC suggests that we will reach an SNR of >~ 1 (per 0.08 angstrom pixel wavelength bin) for a 25 ksec exposure using the faintest, most conservative line and continuum cases for both targets. The filaments will fill the COS aperture, spreading over 100 wavelength bins for a combined effective SNR of >8 (on the conservative end), allowing flux measurements to 15% accuracy. Binning over 50 angstroms will allow us to detect the continuum and the lines of interest at an SNR of ~10, even after accounting for vignetting and attenuation due to declining effective area. At shorter wavelengths, we will likely detect more counts allowing for fine-grained definition of the continuum near the short wavelength turnover. After accounting for overheads, we can achieve this 25 ksec exposure time in 9 orbits for each off-nuclear pointing. We further estimate that 5 orbits will be required for the on-nucleus (i.e. significantly brighter) pointing in A2597. We estimate that similar SNR will be reached for both lines and continuum for this on-nucleus observation. With this observing strategy, contaminating geocoronal Ly-alpha emission will fall in the FUV detector gap between segments B and A and will not be recorded in the data. We therefore do not require umbral shadow observations and are not subject to special scheduling constraints for any of our two targets. Our observations are all well below the brightness limits for COS. We will observe using the recommended TIME-TAG mode to allow temporal sampling, improved thermal correction, and exclusion of poor quality data from the final co-addition. All four FP-POS settings will be used, as recommended. ISM IN EXTERNAL GALAXIES 12 false true 0.0 0.0 false false false SUPPORTED CLUSTER OF GALAXIES BCM CONDUCTION FRONT COOLING FLOW EMISSION LINE NEBULA NUCLEUS The listed coorindates are for the desired center of the 4"x4" ACQ/IMAGE search field. We would like the COS Primary Science Aperture to be centered around the brightest region within this field. J2000 J2000 CLUSTER OF GALAXIES BCM CONDUCTION FRONT COOLING FLOW EMISSION LINE NEBULA FILAMENT This is an offset calculated from the brightest FUV knot cospatial with the A2597 nucleus. We wish to acquire on this knot, and then offset to the filament. Positioning of this offset intentionally avoids the rim of likely shocked gas at the northern edge of the radio lobe. J2000 CLUSTER OF GALAXIES BCM CONDUCTION FRONT COOLING FLOW EMISSION LINE NEBULA FILAMENT The listed coorindates are for the desired center of the 4"x4" ACQ/IMAGE search field. We would like the COS Primary Science Aperture to be centered around the brightest region within this field. This pointing intentionally avoids the nucleus (location of the unresolved radio source). J2000 J2000 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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