From Galactic Cores to the Cosmic Web -- A Study of Feedback and Multiphase Galactic Winds with HST and JWST

0 Assigned ID: 3822 ----- Attempting Submission 1 (Thu Oct 20 07:17:18 GMT 2022) ----- HST Phase I Proposal 3822 successfully submitted. Receipt: # 3822-1 ----- Attempting Submission 2 (Fri Oct 21 07:00:23 GMT 2022) ----- HST Phase I Proposal 3822 successfully submitted. Receipt: # 3822-2 ----- Attempting Submission 3 (Fri Oct 21 20:42:55 GMT 2022) ----- HST Phase I Proposal 3822 successfully submitted. Receipt: # 3822-3 ----- Attempting Submission 4 (Fri Oct 21 20:46:08 GMT 2022) ----- 0 ----- Attempting Submission 1 (Tue Dec 13 19:09:23 GMT 2022) ----- From Galactic Cores to the Cosmic Web -- A Study of Feedback and Multiphase Galactic Winds with HST and JWST Feedback plays a pivotal role in regulating the galactic life cycle through its manifestation in shocks and turbulent gas. And yet, the complex interplay between outflows and their host galaxy remains largely unconstrained at relevant physical scales. The lack of direct observational measurements of small-scale energetic properties of the multiphase ISM is a big hurdle for constraining feedback prescriptions for the next generation cosmological models. Since July, new JWST results shed light on the dust-obscured energy sources in nearby (U)LIRGs, prompting the question of what the total contribution to the energy budget from shocks due to said sources across entire galaxies. Here we propose deep narrowband imaging of key near-infrared diagnostic lines for a pilot sample of 3 galaxy mergers with newly published JWST results that represent the best laboratories to explore the starburst-AGN-shocks connection in the nearby universe. Resolving the shocked gas in ionized outflows with wide-field, high-resolution WFC3 images, this study aims to address: 1. How AGN and stellar feedback drive shocks across the ISM; and 2. How winds impact star formation and chemical enrichment within the host galaxy. Our proposed study will tackle complex feedback physics in high gas content environments, commonplace among star-forming galaxies near the cosmic noon. Leveraging a rich ancillary data set including ground-based optical and newly analyzed JWST infrared imaging and integral-field observaions, the new HST observations will yield unique insights into the role of feedback in galaxy evolution and establish the significance of near-infrared diagnostics in the early JWST era. WFC3 provides a set of narrowband filters in the J-band, unavailable to JWST/NIRCam, that is uniquely suited to image [Fe ii] (1.26um) and Pab (1.28um) among nearby objects. We will use a combination of narrow- (F126N, F128N, F130N, F132N) and wide-band (F110W and F160W) filters, since continuum subtraction works better and more efficiently given the color correction as determined from two wide-band images than that from an off-line narrowband filter. We estimated exposure times using ancillary groundbased APO/TripleSpec spectra of our targets, where available, centered on the body of the galaxy with extraction aperture width of 7.5". We estimate that the emission line at the 10 kpc outskirts would be 2 orders of magnitude fainter based on the dynamic range in typical outflows. With the WFC3/IR ETC aiming for a target SNR of 10 per resolution element (2 px x 2 px), we calculate the exposure time needed to reach our S/N limit. We request 3 exposures / dithers per filter for robust cosmic-ray removal. Two of our 3 targets have one narrowband or wideband images available in the archive; we have checked and found that the depth of the archival data sufficient for our study. Therefore, the corresponding narrowband or wideband data will not be requested; instead, we will incorporate the archival data into our analysis to enhance the legacy value of HST data sets. Overhead estimates include setup + filter changes + readout (1 min per each of 3 exposures), dithering (1-6 min per offset), and guide star (re)acquisition (6 min at the first orbit, 5 min after in non-CVZ). These calculations amount to 1-2 orbits being requested for each source. Accounting for orbital visibility, we request a total of 4 new orbits for the complete set of narrow- and wide-band images for our pilot sample. Our Great Observatory All-sky LIRG Survey (GOALS) team has significant expertise in processing, analyzing, and interpreting high-resolution optical and near-infrared imaging, spectroscopic, and integral-field data of nearby galaxy mergers. PI Vivian U, together with Co-PI Jeffrey Rich, co-Is Anne Medling and George Privon, has led large ground-based integral-field surveys of nearby (U)LIRGs in the GOALS sample using Keck, Palomar, VLT, and ANU SSO. They have expertise in analyzing the ionized and molecular gas kinematics in comparison to high-resolution HST images using both near-infrared and optical diagnostics. Co-Is Tanio Diaz-Santos, Kirsten Larson, Sean Linden, Aaron Evans, and Yiqing Song, have all led recent successful HST ACS+WFC3 wide- and narrow-band imaging proposals and subsequently published numerous papers on properties of star clusters and AGN activity in galaxies mergers. PI U, Co-Is Lee Armus, Evans, Privon, Diaz-Santos, and Lai all lead successful JWST ERS or GO-1 proposals, and everyone on the team is involved in one or more of those programs. Co-Is Vassilis Charmandaris, Loreto Barcos-Munoz, Hanae Inami, David Sanders, Sabrina Stierwalt, Jason Surace, Kazushi Iwasawa, Justin Howell, Joseph Mazzarella, Justin Kader, and Marina Bianchin will contribute their multiwavelength expertise on the physical processes within (U)LIRGs toward the interpretation of the proposed analyses. Co-PI Rich and Co-I Privon, with an expansive background in both modeling and observational work of galaxy mergers, will aid in the analysis and interpretation from the multiwavelength and merger modeling perspective. Co-I Claire Max, a pioneer in the adaptive optics field, will contribute her experience in analyzing narrow-band HST images in these systems. Selected relevant GOALS publications by our team: - Armus et al. 2009, PASP, 121, 559; 2020, NatAs, 4, 467; Armus, Lai, U et al. 2022, submitted to ApJL, arXiv:2209.13125 - Barcos-Munoz et al. 2015, ApJ, 799, 10; 2017, ApJ, 843, 117 - Bohn, Inami et al. 2022, ApJL, in review, arXiv:2209.04466 - Evans et al, 2008, ApJL, 675, 69; 2022, ApJL, in press, arXiv:2208.14507 - Diaz-Santos et al. 2010, ApJ, 723, 993; 2011, ApJ, 741, 32; 2013, ApJ, 774, 68; 2014, ApJ, 788, 17; 2017, ApJ, 846, 32 - Haan et al. 2011, AJ, 141, 100; 2013, MNRAS, 434, 1264 - Howell et al. 2007, AJ, 134, 2086; 2010, ApJ, 715, 572 - Inami et al. 2010, AJ, 140, 63; 2013, ApJ, 777, 156; 2018, A&A, 617, 130; 2022, ApJL, in press, arXiv:2208.10647 - Iwasawa et al. 2011, A&A, 529, 106; 2018, A&A, 611, 71 - Kim, Evans et al, 2013, ApJ, 768, 102 - Lai, Armus, U et al. 2022, ApJL, in review, arXiv:2209.06741 - Larson et al. 2016, ApJ, 825, 128; 2020, ApJ, 888, 92 - Linden et al. 2017, ApJ, 843, 91; 2019, ApJ, 881, 70; 2021, ApJ, 923, 278; 2022, submitted to ApJL - Max et al. 2005, ApJ, 621, 738; 2007, Science, 316, 1877 - Medling et al. 2011, ApJ, 743, 32; 2014, ApJ, 784, 70; 2015a, MNRAS, 448, 2301; 2015b, ApJ, 803, 61; 2019, ApJ, 885, 21, 2021, ApJ, 923, 160 - Modica, Evans et al. 2012, AJ, 143, 16 - Privon et al. 2013, ApJ, 771, 120; 2015, ApJ, 814, 39; 2017, ApJ, 835, 213, 2020, ApJ, 893, 149 - Ricci et al. 2017, MNRAS, 468, 1273; 2021, MNRAS, 506, 5935 - Rich et al. 2011, ApJ, 734, 87; 2012, ApJ, 753, 5; 2014, ApJL, 781, 12; 2015, ApJS, 221, 28 - Sanders et al, 2003, AJ, 126, 1607 - Stierwalt et al. 2013, ApJS, 206, 1; 2014, ApJ, 790, 124 - Song et al. 2021, ApJ, 916, 73; 2022, ApJ, in press - Torres-Alba, Iwasawa et al. 2018, A&A, 620, 140 - U et al. 2012, ApJS, 203, 9; 2013, ApJ, 775, 115; 2019, ApJ, 871, 166; 2022a, ApJ, 925, 52; 2022b, Universe, 8, 392 (Invited Review); 2022c, ApJL, in press, arXiv: 2209.01210 Supermassive Black Holes and Active Galaxies 3 false false false false false true false SUPPORTED GALAXY INTERACTING GALAXY SEYFERT This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY INTERACTING GALAXY MULTIPLE NUCLEI STARBURST ULTRALUMINOUS IR GAL This object was generated by the targetselector and retrieved from the SIMBAD database. Given flux is V-band flux in Jy. J2000 J2000 2.489E-02 GALAXY INTERACTING GALAXY MULTIPLE NUCLEI STARBURST ULTRALUMINOUS IR GAL This object was generated by the targetselector and retrieved from the SIMBAD database. Given flux is B-band magnitude. J2000 J2000 14.2 WFC3/IR Imaging No No F128N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F128N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F130N WFC3/IR Imaging No No F132N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W POS-TARG DITHER 0.572 WFC3-IR-DITHER-BOX-MIN 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 1

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