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1222044091
----- Attempting Submission 1 (Wed Jul 13 17:51:29 GMT 2022) -----
----- Attempting Submission 2 (Tue Apr 18 03:58:30 GMT 2023) -----
----- Attempting Submission 3 (Fri Jun 30 16:39:21 GMT 2023) -----
----- Attempting Submission 4 (Fri Oct 27 17:59:32 GMT 2023) -----
----- Attempting Submission 5 (Thu Jul 18 23:45:04 GMT 2024) -----
A panoramic study of low-density star formation in XUV disk galaxy NGC 3621: Testing for environmental dependency of clusters, OB associations, and the stellar hierarchy
We propose an efficient yet panoramic UV-optical survey of the extended UV disk galaxy NGC 3621, with the goal of decisively evaluating various environmental dependencies of stellar cluster and OB association populations. Such work is very challenging in the regime of low-density star formation (SF) because large areas must be observed by HST to accumulate statistical samples. Consequently, our knowledge of the SF process, its products, and associated feedback in this extreme, but important, regime is woefully incomplete. Our program addresses this shortcoming in a finely controlled experiment using an otherwise well-studied target. The union of NGC 3621's inner and XUV disks presents an ideal test-bed because the local physical conditions change in a remarkably continuous radial manner, across our ~1400 sq.kpc HST footprint, that fully probes gradients in metallicity, plus stellar mass, gas mass and star formation rate surface density. Cluster and association counts will be high enough to bin versus environment for all our goals: (1) We will test predictions of SF modeling in low-density environments. Our program will provide decisive constraint on the extreme low end of predicted cluster formation efficiency, inform environment-driven models of cluster morphology, and determine whether continually dispersing remnants of SF activity are consistent with expectations. (2) The census of stochastic low-mass clusters and associations will provide a testbed for new models / analysis methods relevant to low-density SF. Our project is a vital step toward a full theoretical picture of SF and galaxy evolution in the vast majority of HI-dominated gas out to high redshift.
We will obtain a ~pc-resolution dataset of truly expansive scope documenting the SF process, its products and their evolution, in the low-density disk regime -- fueling a transformative leap in modelling constraints. HST UV-optical imaging of NGC 3621 is needed to characterise hot, upper MS stars populating hierarchical OB associations and all surviving clusters. Our study is enabled by the efficiency of the F300X NUV filter, halving exposure times vs. workhorse filter F275W, and the acquisition of (B,V,I) with ACS parallels.
Primary+parallel imaging strategy: We will obtain primary NUV data with WFC3 while acquiring optical B,V,I bands with ACS in parallel. Since our survey footprint is large versus the camera separation, we can multiplex and place the parallels over other primary fields, then six months later swap the orientation. The NGC 3621 mosaic consists of a 6x4 tile pattern, split into two opposing regions of 3x4 tiles.
Mosaic and visibility planning: NGC 3621-Region1 has an acceptable ORIENT range of 109-111 and consequently NGC 3621-Region2 must be done at ORIENT 289-291. Within each Region we require SAMEORIENT, so that the mosaic is continuous. Taking all this into consideration, Region-1 can be observed ~40 days/yr and Region-2 for 17 days/yr. We set tighter than default mosaic overlaps in order to provide required parallel coverage (minimizing any gaps).
Orbit planning / filters: Each tile will require one orbit. Primary imaging in F300X WFC3/UVIS will be obtained as three dithered exposures totalling 2475s. Post-flash will be about 13e- depending on specific exposure length. Dithering is accomplished using POSTARGs to subsample the PSF and bridge the chip gap. In the uncrowded outer disk, this will yield a 3.5-sigma point-source detection limit of m(F300X) ~ 26.6 Vega mag. During primary imaging, accounting for all overheads, we are able to accommodate five ACS/WFC exposures with filter changes. Exposures from adjacent ACS tiles yield nearly contiguous overlap, doubling the exposure time (and image count) for nearly all of the footprint, reaching to m(F475W) ~ 27.6, m(F606W) ~ 27.1, m(F814W) ~ 26.3 (except for the mosaic periphery). We will net 1578s (F475W), 680s (F606W) and 1380s (F814W) of total exposure in most regions. For comparison, this will yield NUV-B-V-I images 0.9, 1.4, 0.6 and 1.1 mag deeper than PHANGS-HST, respectively.
Detection limits: At NGC 3621 (7.06 Mpc), our F300X image will recover an 8 M_sun star on the MS with max expected A(V) ~ 0.2 + MW foreground. ACS B, V, I exposure depth is sufficient to recover the aforementioned MS star, a 200 Myr core Helium-burning (HeB) blue loop star, and an RGB star ~ 1.5 mag below the TRGB. F475W was chosen for deeper exposure than F606W, as it will help separate blue loop stars from the MS in the optical CMD. Bootstrapping from LEGUS and PHANGS-HST cluster catalogs, we anticipate cluster detection limits of log M_cl = 2.0, 2.5, 2.9 for ages of 10 Myr, 100 Myr and 300 Myr.
Dr. David Thilker (PI, JHU) is an expert in multiwavelength observational characterization of star formation in nearby galaxies and radio imaging of neutral hydrogen (HI) in circumgalactic environments. He specializes in ultraviolet imaging from HST, GALEX, UVIT, with emphasis on star formation occurring at low density. He is credited with the discovery of extended UV disks (XUV disks). Dr. Thilker has extensive experience with PSF fitting, and clump based, photometry. He is presently most active in the fields of stellar cluster and association populations, working at the forefront of the PHANGS-HST investigations on these topics. He will lead the collaboration, managing or co-leading the team effort on each proposed study.
The team contains world leaders in all relevant subdisciplines required to guarantee success for this project. It is important to note that our project currently includes (and will further involve) junior scientists. Our roster of co-investigators is extensive, so we do not provide detailed qualifications of each person. We have specialists in observational star formation and galaxy evolution (Barnes, Bigiel, Boissier, Cook, Dale, B. Elmegreen, D.Elmegreen, Gallagher, Gil de Paz, Groves, Hunter, Lee, Leroy, MacKenty, Meurer, Rafelski, Roca-Fabrega, Rosolowsky, Thilker, Wofford), resolved stellar populations (Cignoni, Tosi), cluster populations (Cook, Orozco Duarte, Thilker), HST UV-optical imaging (Lee, Thilker), atomic/molecular/dusty ISM (Bigiel, Koch, Koda, Leroy, Pisano, Rosolowsky, Thilker), theoretical astrophysics and modeling (Chevance, B. Elmegreen, Glover, Klessen, Krumholz, Kruijssen) , Bayesian/numerical methods (Krumholz). The team contains numerous members of the LEGUS and PHANGS collaborations -- two of the leading groups currently working on nearby galaxies.
All members of the proposal team will participate in each of the anticipated scientific studies, contributing their expertise as appropriate.
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