0Assigned ID: 348
----- Attempting Submission 1 (Fri Apr 08 01:51:05 GMT 2016) -----
HST Phase I Proposal 348 (clusters.apt) successfully submitted.
Receipt: # 348-1
----- Attempting Submission 2 (Fri Apr 08 18:26:31 GMT 2016) -----
HST Phase I Proposal 348 (clusters.apt) successfully submitted.
Receipt: # 348-2
----- Attempting Submission 3 (Fri Apr 08 19:59:57 GMT 2016) -----
HST Phase I Proposal 348 (clusters.apt) successfully submitted.
Receipt: # 348-3
----- Attempting Submission 4 (Fri Apr 08 23:53:56 GMT 2016) -----I am submitting HST phase II proposal 14655. I would like to request the program
coordinator to check the submitted proposal carefully and let me know in case of
any issue.
Thanks,
Sowgat-1629853876----- Attempting Submission 1 (Mon Jul 18 22:38:56 GMT 2016) -----Probing Warm-Hot Gas in the Outskirts of Galaxy Clusters Using Quasar Absorption LinesBy cross-correlating the recently published sample of clusters by Bleem+15 from the 2500 deg^2 South Pole Telescope Sunyaev-Zel'dovich effect survey and the sample of all-sky UV-bright QSOs by Monroe+16, we have constructed a sample of 9 QSO-cluster pairs in the redshift range 0.1<z<0.7. In all cases the QSOs are in the background and at impact parameters of r ~(1-5)r_500 (r_500 being the radius within which the mean matter density is 500 times the critical density of the universe). This sample gives us a unique opportunity to probe unexplored cluster outskirts. Here we propose to obtain 3 QSO spectra as a pilot program that will probe the warm-hot gas, with log (T/K) = 5-6, via the OVI and NeVIII absorption lines, in the outskirts of 3 clusters at z~0.46.
Recent cosmological hydrodynamical simulations suggest that the outskirts of galaxy clusters beyond r >r_500 are ``cosmic melting pots", where galaxies and groups of galaxies are stripped of their metal-rich gas by tidal forces and ram pressure provided by the cluster atmosphere. This enriches the ICM with heavy elements and dissipates heat, thus establishing the overall thermodynamical and chemical structures of galaxy clusters. These simulations predict that the warm-hot gas atmosphere extends out to the accretion shock located at r ~(4-5)r_500, and that it is too cool to be probed via X-ray emission. Detecting this warm-hot gas in the outskirts of galaxy clusters will not only help account for some of the ``missing baryons", but it will also advance our understanding of the physics of galaxy clusters and their use as cosmological and astrophysical laboratories.We propose to observe 3 UV-bright QSOs (GALEX FUV ~ 17.4-17.9) using COS/FUV gratings. For each target we will use both G130M and G160M gratings for a continuous FUV spectral coverage. Each target will be observed for 5 orbits, totalling 15 orbits, in order to achieve a spectral S/N of ~10 per resolution element at the relevant wavelengths. For each target we will allocate 3 orbits for the G130M grating and the remaining 2 orbits for the G160M grating. The G130M observations will use two different central wavelength (cen-wave) settings (i.e. cen-wave 1222 and cen-wave 1309). The cen-wave 1222 setting is particularly needed for covering both members of the NeVIII 770, 780 doublet from the targeted clusters (z = 0.45-0.47). For the G160M observations, cen-wave 1600 and cen-wave 1623 settings will be used. For each cen-wave setting, 4 fixed-pattern positions (i.e. FP-POS=1,2,3,4) will be used in order to minimise the detector's gain sag effect.
For source acquisition, we will do an ACQ/SEARCH with SCAN-SIZE=3, with exposure time calculated with the COS ETC (i.e., obtaining S/N=40 using G130M 1309 grating), using the target flux as found from GALEX. The ETC-run IDs are mentioned for each of the exposures. The ACQ/SEARCH step will be followed by the ACQ/PEAKXD and ACQ/PEAKD steps, respectively, for proper centring of the source. Once the source is rightly centered, TIME-TAG mode will be used for the rest of the observations. Since a maximum of 5 orbits can be used in a given visit, we will observe each target in one visit. Thus, a total of 3 visits are required for completing the program.Intergalactic Medium and Cosmology12falsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSONOJ2000J2000GALAXYQSONOJ2000J2000GALAXYQSONOJ2000J2000COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623/home/sowgat/Work/Cycle-24/14655/OP-cache/14655-v01.xmlThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.(Tic-Visit
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