0 Assigned ID: 1344 ----- Attempting Submission 1 (Fri Jan 29 19:21:52 GMT 2021) ----- HST Phase I Proposal 1344 successfully submitted. Receipt: # 1344-1 ----- Attempting Submission 2 (Sat Jan 30 12:43:59 GMT 2021) ----- POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. 0 ----- Attempting Submission 1 (Fri Feb 05 19:10:48 GMT 2021) ----- These are small enough offsets (<1") that it will not affect the monochromatic area of the ramp filter substantially. In the cores of galaxy clusters, the hot intracluster medium should cool rapidly, leading to "cooling flows" of order ~100-1000 Msun/yr. Our current picture is that AGN feedback is responsible for preventing these runaway cooling events, leading to more typical star formation rates of ~1-10 Msun/yr in the centers of relaxed, cool core clusters. However, recent work suggests that feedback may saturate in the most massive clusters, leading to a cooling imbalance in the most extreme systems. In this proposal, we target one of the most star-forming central cluster galaxies in the Universe (with the other 5 having already been observed), which is forming stars at nearly the classical cooling flow prediction. We will obtain narrow-band [O II] imaging using the ACS ramp filter on this cluster, allowing us to probe the development of thermal instabilities as gas condenses out of the hot phase and ultimately forms stars. Combining these data with the larger sample sample of six massive clusters provides an opportunity to test the limits of AGN feedback, where cooling does not appear to be significantly suppressed. Three of these six clusters also harbor central QSOs, allowing us to probe the different effects of mechanical (radio-mode) and radiative (quasar-mode) feedback in the inner regions of clusters. As the six most star-forming central cluster galaxies, these will make stunning and inspiring images and have tremendous legacy value, as recent Chandra+ALMA and future JWST targets. NOTE: This is a reobservation of a failed visit for a larger approved program. Our goal is to obtain a deep, high-angular resolution maps of [O II]3726,3729 for a single giant elliptical galaxy, following in methodology from HST Proposals 15315 and 15661. This is possible using the ramp filters on ACS, which provide narrow-band filters over the range 3700-10700A. At the redshift of our targets the filter width is ~120A. The width of this filter means that we will (easily) obtain both lines in the [O II] doublet, while avoiding any other strong lines. Given the inherent challenge in flux calibrating and flat fielding HST ramp filter data, achieving a reliable flux map would be challenging even with perfect knowledge of the intrinsic extinction. We will use in-hand broadband filter observations to subtract continuum emission, which will contribute significantly to the narrow bandpass. Broadband filters have been chosen to bracket the 4000A break and avoid emission from Balmer lines and [O III] (5007A). These broadband filters are a factor of ~10x wider than the narrow-band filter, providing similar sensitivity to the continuum in a single orbit as we achieve over 8 exposures in the narrow band. Combining the two bands bracketing the [OII] line, we will have a factor of 5x deeper exposure in the continuum, compared to the narrow-band exposure. Without these deep continuum images, we would add significant amounts of noise during the continuum-subtraction procedure, reducing the effective depth of our narrow-band images. Prof. Michael McDonald has extensive experience with HST data, having PI'd and Co-I'd several proposals over the past several years. The PI has led 7 HST-based publications, and been co- author on tens of such papers. His publications include data from ACS, COS, and WFC3. The PI has three approved programs using the ACS/WFC ramp filter, and has a large amount of experience with both space- and ground-based narrow-band imaging (e.g., McDonald et al. 2010, 2011). The PI has a strong track record of publishing HST data within 1-2 years of acquisition for all successful programs. Beyond HST, the PI is one of the world leaders in the study of warm ionized gas in cool cores, having several successful ground-based campaigns (and publications) studying Halpha emission in nearby systems. The co-I for this proposal (Calzadilla) is a graduate student at MIT who has developed a pipeline for reducing ACS/WFC ramp filter data, and modeling and subtracting continuum emission. He has completed all the analyses to publish this project, and will likely finish the paper this spring. He has the tools in place to convert these new data into results within a matter of hours. In summary, this group is fully capable of reducing, analyzing, and interpreting these data. We have the expertise to supplement these data with data at other wavelengths, and to directly compare to theory/simulations. Galaxies Large Scale Structure of the Universe 0 false SUPPORTED CLUSTER OF GALAXIES COOLING FLOW EMISSION LINE NEBULA NUCLEUS STAR FORMING REGION J2000 J2000 ACS/WFC RampFilter No No FR505N 1612546306024 The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16494 :visit-id "01" :proposal-version -1 :trans-version "20200619" :date "05-Feb-2021 12:31:46.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 568448 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16494 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16494 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2797 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16494 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 347 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) false 2 0 1612552152434 The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16494 :visit-id "02" :proposal-version -1 :trans-version "20200619" :date "05-Feb-2021 14:09:12.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 568448 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16494 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16494 :visit-id "02" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2797 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16494 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 347 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) false 2 0