0Assigned ID: 2900
----- Attempting Submission 1 (Wed Mar 23 19:51:01 GMT 2022) -----submission following the TTRB acceptance of the repeat of 1 orbit from visits 04 (as of HOPRs 93020).1435098372----- Attempting Submission 1 (Thu Jul 14 21:53:11 GMT 2022) -----
----- Attempting Submission 2 (Wed Nov 23 08:58:59 GMT 2022) -----
----- Attempting Submission 3 (Thu May 18 16:51:54 GMT 2023) -----
----- Attempting Submission 4 (Tue Sep 12 20:59:38 GMT 2023) -----
----- Attempting Submission 5 (Wed Dec 04 09:37:30 GMT 2024) -----Massive star clusters in low star formation regime dwarfs?We propose to determine whether the high end of the star clusters mass function is truncated in low density dwarf galaxies. We will image the cluster populations of 10 nearby dwarfs, aiming at collecting a statistically significant sample of clusters, about 150 across all galaxies, in order to overcome current uncertainties driven by low-number statistics. The proposed 5 bands (NUV-U-B-V-I) observations leverage the UV and high angular resolution capabilities of HST to accurately measure the physical parameters (age, mass, extinction) of the star clusters. We will be able to establish whether and how star formation depends on the local or global galaxy environment, and how much of the star formation in dwarfs takes places in bound clusters, therefore testing whether low-density dwarf galaxies are scaled-down versions of spirals or are instead simply less efficient at forming bound structures. The cumulative star cluster population will provide enough statistics to measure the upper mass truncation with an accuracy of better than 0.5 dex or to robustly rule out its presence, enabling us to determine whether the dearth of observed massive clusters in dwarfs is driven by stochastic sampling at the high mass end (a direct consequence of their low SFRs) or by inhibiting mechanisms driven by physical properties (e.g. the low-density environment in dwarfs).
Young massive clusters can be significant sources of ionizing and mechanical energy. Determining the environmental conditions that favor the formation of massive clusters could help isolate the sources of reionization of the early Universe, one of the key science goals of the just-launched JWST.SAMPLE:
The sample of galaxies was selected from the local (<10 Mpc) LVL sample (Lee+2009); among those galaxies we focus on the ones with the lowest SFR surface density (currently under-represented in cluster studies) but with higher SFR overll, ensuring the presence of numerous clusters.
FILTERS:
We require WFC3/F275W (NUV), F336W (U), F438W (B), F547M (V) and F814W (I). The choice of filters is driven by two main necessities: separating bright stars from faint star clusters and obtaining clusters' ages, masses and extinctions with age accuracy of ~0.2 dex and mass accuracy of 0.3 dex. Part of the galaxies have some of the requested observatiosn (or the corresponding WFC/ACS filters) already available in the HST archive and therefore we simply need to complete the set with the missing filters.
EXPOSURES:
We used as limiting source a 5,000 M_sun, 200 Myr old cluster, with mean A_V(continuum)=0.1 mag, at our maximum distance of 10 Mpc; its apparent AB mag are 25.5, 25.2, 24.0, 24.0 and 23.9 in NUV, U, B, V and I respectively.
When all filters are necessary we use 3 orbits to cover the galaxy, where the first orbit is used for NUV, the second is split between U (~60% of the orbit) and B (~40%), while the third orbit between V (60%) and I (40%). In this way we retrieve a SNR>9 in all filters.
An almost identical orbital strategy (with the same filter set apart from F547W) was carried out successfully by the LEGUS treasury progam (GO 13364).
POSITIONS AND ORIENTATION:
Most of the galaxies are covered with a single pointing; the only one requiring two pointings is NGC2366, where the pointings have been kept separated to maximize the schedulability. The position and orientation of the fields of view were mainly based on maximizing the coverage of the galaxy and avoiding bright stars.
DITHERING:
A 3-pointing pattern [(0,0), (1.34,3.94), (-1.34, -3.94)] is used to both cover the detector's gap and sub-sample the PSF. The offsets of each pattern are given in the POS TARG keyword. We preferred 3 exposures over 4 in order to have longer exposure times, more indicated to reduce CTE limitations.
BRIGHT OBJECTS:
The few sources with warnings of extreme saturation (in NGC4265 and ESO245) were kept them slightly out of the field of views by using orientation constraints on the observations. Those stars have V mag less bright than 11.5 mag and therefore we do not expect them to negatively affect the observation due to dragon breath. The same was done, when possible, for sources with moderate saturation. Some sources with low-to-moderate saturation warning are in the field of view of most of the targets, but saturation is only going to affect the centre or close vicinity of the stars themselvers, without impacting the general study of cluster population in the galaxy.
POSSIBLE IMPACT OF REDUCED-GYRO OPERATIONS:
The orientation constraints of our targets were mainly imposed to maximize the galaxy coverage and keep as much as possible stars with expected moderate-to-high saturation levels outside the FoV. However, in case of reduced observing windows or reduced possible orientation, such constraints can be loosen. The impact on observations would not be catastrofic, as it will still be possible to carry out the main goals of the proposal even in that case. The reduced spatial scan would not impact our observations.Our team is composed of both observational and theoretical experts in the study of star cluster formation and evolution. Most team members are experienced HST users.
D. Calzetti, is an expert on star formation and dust obscuration. She has extensive experience with HST imaging data, and both stellar population and dust modeling. She has modeled spectral energy distributions of both whole star-forming galaxies and clusters within galaxies. She has been/is the PI of multiple HST programs, including the Cycle 21 Treasury project LEGUS (Legacy ExtraGalactic UV Survey).
M. Messa, A. Adamo and L. Smith are experts in cluster spectral analyses of local galaxies and have contributed with key publications to the cluster field of research. They are among key members of the LEGUS Treasury program (leading several publications). Regarding this proposal, they are experts on the analysis of star forming regions using HST imaging, and have developed all the tools necessary to perform cluster detection, photometry, size measurements, SED fitting using different SSP models (Yggdrasil, SLUG, BPASS) thus ensuring a smooth and rapid analysis of the cluster populations in the proposed galaxy sample.
A. Adamo and L. Smith have been the PIs of many HST programs targeting young massive clusters. M.Messa has been Co-I in several HST programs related to the study of star clusters.
B. Elmegreen is an expert on the formation of clusters and on star formation, populations and gas processes in dwarf galaxies.
D. Hunter has many years of experience in the study of dwarf galaxies at multi-wavelengths. She has also used HST for stellar population and cluster studies and was on the original WFPC team.
Mark Krumholz is an expert on theory and simulations of star cluster formation, and recently authored an Annual Reviews of Astronomy and Astrophysics article on star clusters.Galaxies6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYAMORPHOUS IRREGULARMAGELLANIC IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARDWARF COMPACTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARDWARF COMPACTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARMAGELLANIC IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARMAGELLANIC IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WThe scheduling data was generated by CASM 32.1.CASM was run in Phase II mode.1681796744000128.1338432353753(Tic-Visit
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