Probing Multiple Formation Below 1Msun: Towards the Opacity-Limit for Fragmentation from 7.5-150 au in NGC 1333ars

0 Assigned ID: 3483 ----- Attempting Submission 1 (Fri Mar 25 20:02:26 GMT 2022) ----- HST Phase I Proposal 3483 successfully submitted. Receipt: # 3483-1 ----- Attempting Submission 2 (Fri Mar 25 21:42:18 GMT 2022) ----- HST Phase I Proposal 3483 successfully submitted. Receipt: # 3483-2 ----- Attempting Submission 3 (Fri Mar 25 22:05:46 GMT 2022) ----- HST Phase I Proposal 3483 successfully submitted. Receipt: # 3483-3 Unschedulable Visit I checked the pointing to see if there were more favorable observing windows, but Visit 10 was offset by a significant amount. I am resending the observations to make sure that Visit 9 and 10 are schedulable and to see if I need to make any modificaitons. 1616041900 ----- Attempting Submission 2 (Tue Aug 13 02:26:02 GMT 2024) ----- HST Phase II Proposal 17141 successfully submitted. Receipt: # 17141-2 ----- Attempting Submission 3 (Wed Aug 14 03:37:36 GMT 2024) ----- HST Phase II Proposal 17141 successfully submitted. Receipt: # 17141-3 ----- Attempting Submission 4 (Tue Sep 10 01:16:05 GMT 2024) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 5 (Sat Oct 05 20:35:04 GMT 2024) ----- Visit 1 was removed at the very beginning of this process Probing Multiple Formation Below 1Msun: Towards the Opacity-Limit for Fragmentation from 7.5-150 au in NGC 1333ars Multiplicity studies of the Galactic field have revealed important trends in companion frequency, mass ratio, and separation as a function of primary mass, from O-stars to T-dwarfs. Importantly, similar studies in young, star-forming regions have identified an excess of companions to low-mass stars relative to the field in low-density regions, but find a comparable frequency of companions to low-mass stars relative to the field in high-density regions. We propose a small, seven-orbit program with ACS/WFC in parallel with WFC3/UVIS to obtain multi-filter photometry of NGC 1333 (a nearby intermediate density cluster) to perform a multiplicity suvery, characterizing the companion population for primary masses 0.01-1.0 Msun and search for trends based on primary mass and stellar density. Using the empirical PSFs previously derived across the detector for each filter/instrument combination, we will search for close companions with a PSF-fitting technique, proven to detect companions down to 0.5 pixels (0.025") on ACS/WFC, corresponding to 7.5 AU at 300 pc. With the 150 confirmed cluster members within our field of view, we expect to detect 33 companions (if the companion population of NGC 1333 resembles the field) which allows us to place constraints on its mass ratio distribution as a function of primary mass and separation, exploring star formation processes and cluster dynamics in creating and shaping these multiple systems. We propose a small program of seven orbits to observe NGC 1333 in visible wavelengths with the ACS/WFC (hereafter ACS) coordinated in parallel with WFC3/UVIS (hereafter UVIS), as ACS has a field of view 60\% larger than UVIS. Each orbit will observe one ACS and UVIS field, enclosing 150 known members (130 with ACS, 20 with UVIS and some overlap). These seven fields were selected to observe the largest number of sources in the fewest number of frames where any additional field adds a maximum of ten members. To accomplish our science goals, we require short (3s) and long (340s) exposures in the F435W, F606W, and F814W filters that attain S/N > 10 across 12 orders of magnitude with ACS. Sources of 13 (13.7, 12.6) mag in F435W (F606W, F814W) nearly saturate in 3s, and sources of 20.1 (20.1, 19.8) mag achieve a S/N=10 in 3s. Sources of 18.1 (18.8, 17.8) mag in F435W (F606W, F814W) nearly saturate in 340s while sources of 25.3 (25.5, 24.6) mag achieve a S/N=10 in 340s. These limiting magnitudes for F435W and F606W are 4.5 and 5.5 mags deeper than previously attained in the B and R filters (Monet et al. 2003). That of F814W is equivalent to the previous limit in i' and z' filters with Suprime-Cam at the Subaru telescope (Scholz et al. 2009). The data must be unsaturated to apply the PSF-fitting technique and detect companions at 0.5*pixel on ACS. Luhman et al. (2016) were complete down to Ks = 16.2 mas for Aj < 3 mag, 15-20 Mjup for Aj = 3 at a distance of 300 pc using the Ames-Cond and BT-Settl evolutionary models (Allard et al. 2001,2011). Scholz et al. (2009) were complete down to J = 20.8 or 6 Mjup for Aj = 3, while our limit in F814W corresponds to a 8-12 Mjup for Aj = 3. With the median extinction of cluster members (Aj=1.1), our observations can achieve S/N = 10 for 0.09 Msun objects in F435W, 0.015 Msun objects in F606W, and .005 Msun objects in F814W. The short exposures are designed to collect data on the bright stellar members of the cluster without saturating, up to 1 Msun, while the long exposures are designed to collect data on the sub-stellar members of the cluster down to 0.01 Msun. The UVIS parallels can occur within the same orbit if only two images are taken due to the inability to buffer dump to the solid state recorder simultaneously with ACS and UVIS. We select long exposures for F606W and F814W in order to observe sub-stellar members on the outer portion of the star-forming region. Short exposures have low background and suffer significant charge transfer efficiency (CTE) losses, particularly for low S/N, which affect the photometric and astrometric estimates. We combat this effect in two ways: 1) select exposures times with two magnitudes of overlap so low S/N sources in the short exposures will be observed with high S/N in the long exposures, e.g. 18.1-20.1 mag in the F435W filter, 2) invoke a 20e- post-flash for the short exposures of ACS and less post-flash for the long exposures with UVIS which allows for proper pixel-based CTE corrections through the HST pipeline (Anderson & Bedin 2010, Ogaz et al. 2014, Bellini et al. 2017, Miles 2018, Anderson 2020), as recommended by STScI HST help desk. We will take undithered short and long exposures in the F435W, F606W, and F814W filters. The images are undrizzled in accordance with Anderson & King (2006) and Anderson & Bedin (2017) to fit empirical PSFs to the data and avoid interpolated data from drizzle-combined images. Cosmic rays will not be confused with companions within single exposures due to poor PSF fits and their absence in images from other filters. Fields will have a small offset in between exposures of different filters to mitigate hot pixels. Each orbit is made of a 6.5min guide star acquisition, 4min first exposure with ACS, 3s observation in F435W with post-flash (5s), 2.5min overhead, 340s observation in F435W, 5.8min buffer dump, 3s observation in F606W with post-flash (5s), 2.5min exposure overhead, 340s observation in F606W, 5.8min buffer dump, 3s observation in F814W with post-flash (5s), 2.5min exposure overhead, and 340s observation in F814W. co-PI Matthew De Furio has over four years experience in direct imaging surveys in young star clusters with HST where he developed, characterized, and implemented a PSF-fitting routine capable of sub-diffraction limit resolution. He is co-leading the JWST/NIRCam GTO program in NGC 2024 studying the low-mass limit of the initial mass function and the companion population to primaries as low as a few Mjup. co-PI Michael Meyer has over 30 years of experience in infrared astronomy, including development of instrumentation for JWST, and research in star and planet formation, and exoplanets, with a focus on demographic studies based on direct imaging surveys. co-I Aleks Scholz has more than 20 years of experience in observations of very low mass stars and substellar objects. In particular, he has led the survey SONYC that explored the substellar population of NGC1333, the target of this proposal. He is the lead of the JWST/NIRISS GTO program focused on finding brown dwarfs and free-floating planets in the same cluster. co-I Jay Anderson is an expert at PSF-fitting with HST. He created the library of PSFs that will form the basis for this analysis and is able to adjust them to the particular breathing state of the telescope when the new observations get taken. co-I M. Reiter has led star-formation studies with multi-wavelength HST observations and contributed to the development of the PSF-fitting routine. Stellar Populations and the Interstellar Medium 6 false false false false false false false SUPPORTED STELLAR CLUSTER STAR FORMING REGION This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STELLAR CLUSTER STAR FORMING REGION This object was generated by the targetselector and retrieved from the SIMBAD database. 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