This Phase II proposal has been modified following advice from contact scientist Steve Penton. While Visit 1 is a 6-orbit visit, Steve has cleared this with the HST schedulers, and this reduces the number of visits required to execute the program.
EMAIL FROM STEVE PENTON:
Hi Todd,
I have a much better solution to offer. What if you take the G130M exposure from Visit 02, and tack in onto the end of Visit 01. This will give you an addition ~650 seconds of exposure time. You would obviously just delete Visit 02 and you are good to go.
I have already talked to the schedulers and they are fine with this > 5 orbit visit exception.
Feel free to go ahead and make this change and re-submit.
-Steve P
On Jun 25, 2013, at 4:36 PM, "penton@stsci" <penton@stsci.edu>
wrote:794945491----- Attempting Submission 2 (Tue Aug 06 14:40:54 GMT 2013) -----This proposal has a warning because we use three FP-SPLIT positions instead of four positions. However, we also use two grating central wavelengths in order to fill in the COS detector gap. The combination of two central wavelength settings and multiple FP SPLITS at each central wavelength will be quite adequate for mitigating fixed-pattern noise.WARM AND HOT GASES IN AND AROUND CLUSTER GALAXIES AT Z=0.1-0.2We propose a joint HST/XMM-Newton observing program to study both warm and hot gases in two optically-selected galaxy clusters at z=0.117-0.2108. Each cluster has a UV-bright background QSO projected within the expected strong accretion shock (< 2r_200). We will observe UV absorption lines of the O VI doublet, HI Ly-alpha and Ly-beta, and other ion transitions in the rest frame of the clusters, using the HST/COS G130M grating. These absorption lines are sensitive to the thermal, kinetic, and chemical properties of warm (T < 10^6 K) gas, associated with the halos of individual galaxies and the intracluster medium. Chandra/ACIS observations will be used to measure the luminosity, temperature, and morphology of the hot gas component of the clusters, especially in their core regions. This joint study will thus allow us for the first time to characterize the heating/cooling and dynamic processes of these multiple gas phases in the clusters. The understanding of these processes is essential for understanding cluster galaxy evolution, the correct interpretation of X-ray and Sunyaev-Zeldovich effect measurements, and the use of clusters as cosmology probes.To search for warm-hot cluster gas at log T = 5 - 7, and to generally constrain the thermal, kinetic, and chemical properties of the multiphase intracluster media (ICM), we will observe two QSOs behind the X-ray bright galaxy clusters Abell 1095 (z = 0.206) and Abell 1926 (z = 0.136) with the Cosmic Origins Spectrograph (COS) using the G130M grating. The wavelength range must cover strong resonance lines of species such as OVI, CIII, SiIII, and HI, so we will tilt the G130M grating to cover roughly 1150 to 1450 A. To fill in the chip gap, we will split the exposures (as equally as possible) between the central wavelength = 1309 A and 1327 A settings, and we will use multiple FP split positions to mitigate COS fixed-pattern noise. Both of the target QSOs have been imaged with GALEX, and we have used the GALEX ultraviolet fluxes to calculate exposure times for the target acquisitions and science exposures. In addition, both targets are point souces with accurate coordinates, so we will acquire the targets with the ACQ/IMAGE procedure. SDSS104741.75+151332.3 is marginally too bright to acquire with MIRRORA, so we will use MIRRORB for the target acquisition for this QSO to allow for possible quasar variability that could make the object too bright for MIRRORA.COSMOLOGYDefaultfalsetrue121falsefalsefalseSUPPORTEDEXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICCORONAL GASHOT GASICMJ2000J2000GALEX FUV = 18.20, GALEX NUV = 18.05EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICCORONAL GASHOT GASICMJ2000J2000GALEX FUV = 17.59, GALEX NUV = 17.28COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode./Users/toddtripp/proposals/hst_cyc21/wang/OP-cache/wang_phase2_aug2013-v01.xml(Tic-Visit
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