0 Assigned ID: 3139 ----- Attempting Submission 1 (Fri Mar 25 05:09:55 GMT 2022) ----- HST Phase I Proposal 3139 successfully submitted. Receipt: # 3139-1 ----- Attempting Submission 2 (Fri Mar 25 17:28:58 GMT 2022) ----- HST Phase I Proposal 3139 successfully submitted. Receipt: # 3139-2 ----- Attempting Submission 3 (Fri Mar 25 22:20:25 GMT 2022) ----- HST Phase I Proposal 3139 successfully submitted. Receipt: # 3139-3 ----- Attempting Submission 4 (Fri Mar 25 22:46:45 GMT 2022) ----- POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE PATTERN POSITION OUTSIDE APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE PATTERN POSITION OUTSIDE APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE 0 ----- Attempting Submission 1 (Thu Jul 14 16:25:04 GMT 2022) ----- I believe all of these warnings are related to the fact that we are creating a 2x2 mosaic of the region surrounding the cluster center. Completing the stellar census of Westerlund 1 We propose to obtain a new epoch of precise astrometry covering a 4'x4' extent of the massive, young cluster Westerlund 1. Previous epochs of HST data have been used to determine cluster membership for the full cluster down to a mass limit of 1.4 Msun using proper motions derived from a combination of optical and near infrared data. By adding an additional epoch of astrometry from WFC3-IR, we will be able to confirm the full membership of the cluster down to 0.1 Msun. These observations will be used to map the full initial mass function (IMF) of the cluster, which we have tentatively found is bottom-light. Furthermore, the additional epoch of data will offer an improvement in proper motion precision by a factor of 3, enabling the measurement of velocities to ~1 km/s. Using this information, we will map the velocities as a function of mass to test star formation models. These data will provide new insight into the origin and universality of the IMF. Our program to measure the internal kinematics of the massive young cluster, Westerlund 1, requires precise astrometric observations. Archival HST data sets of Wd 1 include three epochs multi-band WFC3-IR imaging of the full extent of the cluster, which we will use as our initial epochs. New observations in cycle 30 will provide a critical fourth near-infrared astrometric epochs, providing membership confirmation and precise velocities down to the substellar limit. A 2x2 (4'x4') mosaic is needed to cover the full cluster extent. Our target goal is to identify and measure cluster members down to the limits of the existing WFC3-IR data at 0.1 solar masses, which corresponds to H=20.5. In order to effectively select the field stars, we require a 1 sigma proper motion precision of <0.3 mas/yr. We will use existing data from 2010, 2013, and 2015 with a total time baseline of 12 years to achieve our desired proper motion errors. We will measure the astrometry with WFC3's longest-wavelength filter (F160W) to minimize the impact of extinction. Therefore, we need a total SNR=160 on the stars of interest to achieve an astrometric precision of 1 mas and a final velocity precision of 0.1 mas/yr. Additionally, to minimize the impact of geometric distortions, we request that the astrometric observations have the SAME ORIENT with small POSTARG offsets as the 2013 and 2015 observations. Our observations require a high dynamic range as we are interested in both the higher mass, brighter stars (typically H=0) and the lower mass, fainter stars (typically H=20.5) in the cluster. As a result we must limit our integration time per exposure so as to avoid saturating too many stars, such that the resulting persistence images would not impact the astrometric measurements. We also adopt a minimum integration time that still allows us to dump the WFC3 buffer in parallel (249 s for a STEP50 readout pattern with 10 MULTIACCUM reads). Integration times for observations of Wd 1 in the F160W filter were calculated with the WFC3 exposure time calculator to achieve SNR=160 for an H=20.5 star with a late M dwarf spectral type and an E(B-V) = 3.5. For each position in our proposed 2x2 mosaic of Wd 1, we require 13-14 exposures for a total of 3240-3490 s of integration time per pointing. We also require additional short exposures in sub-arrayed mode to capture the most massive stars that were saturated in the longer exposures. This amounts to 7 orbits to complete the entire mosaic in cycle 30. --------- Additional Comments ---------- The archival observations have the PID 11708 from 2010 and PID 13809 from 2013/2015. We request that our new observations have the same orientation and detector position as the F160W images from the archived data set. Our team has extensive experience in works involving kinematics in star forming regions. PI Konopacky (UC San Diego) uses both ground and space-based, high resolution imaging and spectroscopy to study star and planet formation. Co-I Wei is a graduate student at UC San Diego who is leading analysis on the 3-D kinematics of the Orion Nebula Cluster. He will lead the analysis of the dataset gathered here to search for trends in the kinematics with mass. Co-I Lu is a world-expert on astrometry in young clusters, and will assist with the data analysis and modeling. Co-I Theissen is an expert on studies of low mass stars and large data sets, and will assist with cluster modeling. Co-I Hosek has worked extensively on astrometry of massive clusters with HST, with a focus on the massive clusters near the Galactic Center. He will assist with the derivation of precise astrometry and proper motions, as well as vetting of the membership catalog. 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