Feedback by the Many or the Few? Surveying Star Cluster Outflows in NGC 4449

0 Assigned ID: 6755 ----- Attempting Submission 1 (Thu Apr 10 22:00:19 GMT 2025) ----- HST Phase I Proposal 6755 successfully submitted. Receipt: # 6755-1 ----- Attempting Submission 2 (Thu Apr 10 23:45:35 GMT 2025) ----- COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS This is an initial draft of the Phase II proposal; the acquisition strategy for several targets in more crowded fields may need to be revised. 999419478 ----- Attempting Submission 1 (Thu Aug 14 15:54:21 GMT 2025) ----- The COS exposure times are given in increments of 0.1 seconds for all targets; the source of this error isn't clear. Feedback by the Many or the Few? Surveying Star Cluster Outflows in NGC 4449 Star clusters are the primary purveyors of stellar feedback in starforming galaxies. Supernovae and stellar winds that are correlated in space and time thermalize their energy to produce hot, expanding bubbles of T ~ 10^7 K gas. When these bubbles merge with others, they can break out of the disk, powering galactic fountains and winds. In starburst galaxies, the star cluster population collaborates to drive kiloparsec-scale outflows. However, how this collaboration occurs remains unclear. It is not known whether galactic winds are driven predominantly by a small number of high-mass clusters (log(M/M_sun) >= 4.5) or by the combined contributions of many lower mass clusters (3 < log(M/M_sun) < 4.5). We propose to answer this question in the nearby dwarf starburst galaxy NGC 4449 (d = 4 Mpc), where we will survey the warm ionized outflows associated with 12 star clusters (11 new and one archival) with 3.4 =< log(M/M_sun) =< 5.4 using "down-the-barrel" COS/G130M spectroscopy. We will measure the metal column densities, traced by N(Si) = N(SiII) + N(SiIII) + N(SiIV), as a function of velocity to constrain the energy and metal mass engaged in galactic fountains (v < v_esc) and winds (v > v_esc) as a function of cluster mass. By quantifying the role of lower mass clusters in driving starburst winds, we will determine the dominant drivers of the large-scale outflows that heat and chemically enrich the circumgalactic and intergalactic medium. We propose a COS FUV survey of warm outflows from 11 young, massive star clusters across the nearby dwarf starburst galaxy NGC 4449 (D = 4 Mpc). The program goal is to determine the feedback contribution, or the amount of outflowing gas in winds (v > v_esc) or fountains (v < v_esc), as a function of cluster mass. We will detect the outflowing gas in absorption from low and intermediate ions against the light of the UV-bright clusters. For each cluster, we will measure the metal column densities associated with warm, diffuse outflows, as traced by the Si column density, N(Si) = N(SiII) + N(SiIII) + N(SiIV). We will use COS/G130M with cenwav = 1291 A to cover the SiII (1190, 1193, 1304 A), SiIII (1206 A), and SiIV (1393, 1402 A) transitions. The exposure time is divided evenly between FP-POS = 3 and 4 to improve the S/N. The medium resolution grating (FWHM = 14 - 19 km/s) is needed to resolve the gas kinematics and determine the column density at v > v_esc. To determine the exposure times, we measured the flux within the COS aperture in an archival HST/WFC3 F218W image (Program 16316, PI Sabbi) and extrapolated to the COS band with the ETC assuming a typical cluster spectral energy distribution and the total (foreground and intrinsic) E(B - V) from Bradley et al. (2020). We validated our exposure time calculation by applying the same procedure to an archival COS spectrum of a star cluster in NGC 4449. We require S/N = 10 at SiIV 1393, 1402 to measure the column density and the velocities to the required precision. This criterion ensures S/N > 10 at SiII and SiIII. This yields total exposure times of t_exp = 1000 - 15500 s, or 1 - 8 orbits per sightline for a total request of 30 orbits. All targets are faint and point-like, and thus a standard target acquisition in ACQ/IMAGE mode is most efficient. The target coordinates are well-known and have been validated using multi-band archival HST/WFC3 imaging of NGC 4449. The ETC and BOT reported no warnings for violations of the bright object limits. Dr. Erin Boettcher is an expert in multiwavelength observations of galactic fountains and winds in nearby galaxies. She has extensive experience analyzing HST/COS observations as a member of the Cosmic Ultraviolet Baryon Survey (Program ID: 15163). Dr. Edmund Hodges-Kluck is an expert in multiwavelength observations of stellar feedback in nearby galaxies, including the formation and evolution of superbubbles and their role in galactic winds. Dr. Mainak Singha is an expert in AGN and stellar feedback and the role of galactic outflows in the baryon cycle. Dr. Mihoko Yukita is an expert in stellar populations and star cluster feedback in nearby galaxies. Intergalactic Medium and the Circumgalactic Medium Galaxies 6 false false false false false false SUPPORTED EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 EXT-CLUSTER STAR FORMING REGION NO J2000 J2000 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. 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(Tic-Visit :proposal-id 18015 :visit-id "13" :proposal-version -1 :trans-version "20250624" :date "14-Aug-2025 10:40:51.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 148112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18015 :visit-id "13" :obset-id "13" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18015 :visit-id "13" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2621 :al-overhead-at-end 0 :internal-dur-at-end 507 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 1 0