0 Assigned ID: 950 ----- Attempting Submission 1 (Fri Mar 06 23:42:39 GMT 2020) ----- INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS This is the first version of the proposal. We have attempted to follow the COS2025 policy. Feedback will be greatly appreciated. 552971008 ----- Attempting Submission 1 (Tue Jun 23 21:34:02 GMT 2020) ----- Only one FP-POS setting is used per orbit. Therefore, it is not subject to the overhead loss. Catching radio-mode feedback in action with COS UV absorption spectroscopy A widely accepted tenant of galaxy formation theory is that red-and-dead galaxies maintain their quiescent status through the sustained impact of radio-mode feedback. Driven by an active galactic nucleus, this feedback is purported to heat gas in the galaxy's surroundings to prevent the accretion and cooling of gas onto the galaxy. Moreover, radio-mode feedback drives gas outflows and may remove a substantive amount of gas from galaxies. While radio-mode feedback is now a nearly generic feature of numerical simulations of galaxy formation, the physical mechanisms that drive the interaction between radio jets/lobes and gas in galaxies are still poorly known. With this proposal, we will study a galaxy with bright radio jets (i.e. caught in the act) and therefore putatively exhibiting the radio-mode feedback that sustains its absence of star formation. Fortuitously, a UV luminous quasar lies background to this galaxy with its sightline intersecting the system at an impact parameter R ~ 4 kpc. Existing optical spectra of the quasar shows likely CaII absorption associated with the foreground galaxy, i.e. cool and dense gas. The proposed HST/COS observations will extend the analysis to a diverse set of diagnostics -- HI Lya, OI, SiII, SiIII, SiIV, CII, CIV -- to assess the metallicity, kinematics, and multi-phase nature of gas in the galaxy. These data will provide direct insight into the process of radio-mode feedback and offer tests for current and future models. This observation is designed to obtain COS FUV spectra of a background quasar (z=0.2, FUV=18.3 mag) for probing multiple ISM absorption lines of the targeted foreground galaxy (z=0.0734). We will use two COS FUV settings, 130M (1291 A) and 160 M(1533 A), to obtain the required wavelength coverage for the targeted lines including HI Lya 1215, SII 1250,1253, OI 1302, SiII 1260/1304, SiIII 1206, SiIV 1393/1402, CII 1334, and CIV 1548/1550. The COS FUV settings are designed to follow the COS 2025 policy and to maximize the wavelength coverage for the science at the same time. The total exposure times are chosen to obtain spectra with the two settings both having S/N>10, which results ~11,000 s for 130 M (1291 A) and ~9,100 160 M (1533 A). The corresponding ETC calculations can be found at 130M [http://etc.stsci.edu/etc/results/COS.sa.1448703/](http://etc.stsci.edu/etc/results/COS.sa.1448703/) 160M [http://etc.stsci.edu/etc/results/COS.sa.1423410/](http://etc.stsci.edu/etc/results/COS.sa.1423410/) Following the suggested visit design, we structure our 8 orbits into three visits (3, 3, 2). - 1st visit focuses on obtaining spectra with 130 M (1291 A): 1 orbit - Target acquisition [NUV MIRRORA imaging] + FUV 130M [1291 A] exposure (2436 s) 2 orbit - FUV 130M [1291 A] exposure (2689 s) 3 orbit - FUV 130M [1291 A] exposure (2689 s) - 2nd visit focuses on obtaining spectra with 160M (1533 A): 1 orbit - Target acquisition [NUV MIRRORA imaging] + FUV 160M [1533 A] exposure (2383 s) 2 orbit - FUV 160M [1533 A] exposure (2689 s) 3 orbit - FUV 160M [1533 A] exposure (2689 s) - 3rd visit will obtain spectra with both settings 130M (1291 A) and 160M (1533 A): 1 orbit - Target acquisition [NUV MIRRORA imaging] + FUV 130M [1291 A] exposure (2436 s) 2 orbit - FUV 130M [1291 A] exposure (966 s) + FUV 160M [1533 A] exposure (1485 s) The final science exposure time are 11216 for 130M (1291 A) and 9246 s for 160M (1533A), consistent with the original plan. Dr. Ting-Wen Lan has expertise in galaxy formation and evolution and absorption line measurements with optical spectroscopic datasets. Dr. Jason X. Prochaska is an expert in UV absorption line spectroscopy and data analysis of COS and has led several past HST campaigns. Supermassive Black Holes and Active Galaxies 6 false false true false false false false SUPPORTED ISM ABSORPTION LINE SYSTEM ABSORPTION LINE SYSTEM - EXTRAGALACTIC NO This object was generated by the targetselector and retrieved from the GALEX database. J2000 J2000 Magnitude is FUV COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1533 /Users/tlan/Dropbox/Astro_Research/Proposal/200306_HST_cycle28/PhaseII/OP-cache/my_PhaseII-v01.xml The scheduling data was generated by CASM 28.2. 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. (Tic-Visit :proposal-id 16297 :visit-id "03" :proposal-version -1 :trans-version "20200518" :date "23-Jun-2020 12:16:14.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 95824 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16297 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16297 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2752 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3145 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16297 :visit-id "03" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2753 :al-overhead-at-end 0 :internal-dur-at-end 341 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3145 :pcs-gap 0 ) true 2 0