INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE
INEFFICIENT ORDERING OF FP-POS POSITIONS0----- Attempting Submission 2 (Fri Oct 11 20:16:37 GMT 2013) -----
----- Attempting Submission 3 (Tue May 13 19:42:55 GMT 2014) -----No change, aside from target name.Searching for 300,000 Degree Gas in the Core of the Phoenix Cluster with HST-COSThe high central density of the intracluster medium in some galaxy clusters suggests that the hot 10,000,000K gas should cool completely in less than a Hubble time. In these clusters, simple cooling models predict 100-1000 solar masses per year of cooling gas should fuel massive starbursts in the central galaxy. The fact that the typical central cluster galaxy is a massive, "red and dead" elliptical galaxy, with little evidence for a cool ISM, has led to the realization of the "cooling flow problem". It is now thought that mechanical feedback from the central supermassive blackhole, in the form of radio-blown bubbles, is offsetting cooling, leading to an exceptionally precise (residuals of less than 10 percent) balance between cooling and feedback in nearly every galaxy cluster in the local Universe. In the recently-discovered Phoenix cluster, where z=0.596, we observe an 800 solar mass per year starburst within the central galaxy which accounts for about 30 percent of the classical cooling prediction for this system. We speculate that this may represent the first "true" cooling flow, with the factor of 3 difference between cooling and star formation being attributed to star formation efficiency, rather than a problem with cooling. In order to test these predictions, we propose far-UV spectroscopic observations of the OVI 1032A emission line, which probes 10^5.5K gas, in the central galaxy of the Phoenix cluster. If detected at the expected levels, this would provide compelling evidence that the starburst is, indeed, fueled by runaway cooling of the intracluster medium, confirming the presence of the first, bonafide cooling flow.The primary goal of this program is to obtain spectra of the OVI (1032,1038) doublet, which will be redshifted to 1648,1658A. Our secondary goal is to obtain broad UV continuum coverage.
We are imaging two relatively diffuse/clumpy regions, neither of which are centrally peaked in UV brightness. Thus, pointing revision via ACQ/SEARCH is not possible. We instead must center on a nearby star (~60" away) and perform offsets. According to the COS users manual, such offsets should be accurate enough for our purposes.
All of our observations are done in TIME-TAG mode. This temporal sampling will allow us to exclude poor quality data and get improved thermal correction and background removal. We separate our visits into 7 orbits, where each orbit uses one of four different FP-POS (1,2,3,4,2,3,4). This observing strategy is adopted to reduce the fixed pattern noise and fill up the wavelength hole produced by the chip gap without excessive overheads.
Since our targets are faint (<0.001 cts/s), we use a BUFFER-TIME equal to the exposure time minus 110s, as suggested by Julia Duval for a similar 2012 program.
We choose a central wavelength of 1577 in order to keep the OVI line (1650A) as far from the chip gap as possible. We are open to suggestions on this, if we are pushing the line into a low-sensitivity regime.ISM IN EXTERNAL GALAXIESDefaultfalsefalsefalsefalsefalseSUPPORTEDSTARUNDESIGNATEDJ200020.933 (GALEX NUV)GALAXYCOOLING FLOWELLIPTICALSTARBURSTCenter of galaxy, to be used for COS centroidingJ2000GALAXYCOOLING FLOWELLIPTICALSTARBURSTGALAXYCOOLING FLOWELLIPTICALSTARBURSTCOS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589The scheduling data was generated by CASM 22.0.CASM was run in Phase II mode./private/var/folders/v1/2939dkt15lv0kxn1zxkrlh1m0000gn/T/OPVisit2126213431669792453.xml(Tic-Visit
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