normal submission 1707380773 Assigned ID: 5417 ----- Attempting Submission 1 (Tue Mar 26 14:10:32 GMT 2024) ----- 0 ----- Attempting Submission 1 (Tue Aug 13 08:26:53 GMT 2024) ----- HST Phase II Proposal 17792 successfully submitted. Receipt: # 17792-1 ----- Attempting Submission 2 (Tue Mar 11 09:02:48 GMT 2025) ----- I corrected the mistake in the visit 05 that was using E230M/2415 before and now it uses E230M/2707, the correct one. I also change the ETC IDs for the target acquisition that was using the wrong filter, 50CCD. The currect version has the ETC IDs with the proper filter, F28X50LP. STIS Analysis of the metal-poor r-element-rich star TYC 3814-1598-1 The formation site of rapid neutron-capture ('r-process') elements is still uncertain. The two most accepted mechanisms are magneto-rotational MHD-jet supernovae and neutron-star mergers, with the latter channel confirmed by observations of the kilonova counterpart of the gravitational-wave event GW170817. However, predictions from the latest nucleosynthesis models argue that neutron-star mergers cannot be the main contributor to r-process enrichment, and we require further empirical constraints on the r-process abundance pattern from early nucleosynthesis in the Galaxy. Here we propose STIS E230M echelle spectroscopy of TYC~3814-1598-1, a metal-poor ([Fe/H]~-3.0), actinide-enriched ([Eu/Fe] > 1.3) star that will provide new observational constraints on r-process enrichment. The STIS observations will provide the first abundance determinations for at least seven elements for this star, as well as much improved abundances for more than ten other heavy elements that have better diagnostics in the space ultraviolet than from optical spectroscopy. As the brightest known star of this rare class, the proposed analysis of TYC~3814-1598-1 will be a benchmark case for the abundance pattern of the so-called 'actinide boost' stars and provide much needed constraints on galactic chemical-evolution models. The spectra should be acquired with the E230M grating of the STIS echelle spectrograph and the 0.2" 0.2" slit for a resolving power R = 30,000. The E230M setting c2707 spectra provide complete high-resolution coverage of the stellar spectrum in the interval 2300 - 3111 \AA. The observation was organized into groups of 3-orbits visits to minimize overheads allowing some scheduling flexibility. Each group is divited into 4 exposure: Orbit 1 ACQ and SCIENCE, Orbists 2 and 3, SCIENCE. To acount for the 13 orbits we also included the 5th visit that has a single orbit, Orbit 1 ACQ and SCIENCE. The coordenates and propermotion are taken from Gaia DR3. H. Ernandes is expert on spectroscopy in the near-UV and nucleosynthesis. B. Barbuy is expert on spectrocopy, nucleosynthesis and stellar populations. C. Evans has pioneered large-scale spectroscopic surveys of massive stars in the SMC, and has led a number of key UV and optical studies of OB stars in low-metallicity galaxies in the Local Group. Until 2022 he was the Project Scientist for the design of the VLT-CUBES near-UV spectrograph and, together with Ernandes and Barbuy, helped develop the case for heavy-element studies of metal-poor stars with CUBES. Stellar Physics and Stellar Types Stellar Populations and the Interstellar Medium 6 false false false false false false false false SUPPORTED STAR K III-I POPULATION II This object was generated by the targetselector and retrieved from the SIMBAD database. SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM. GAIADR3828438619475671936 2MASSJ09544277+5246414 J2000 J2000 STIS/NUV-MAMA Spectroscopic No No E230M 2707 /Users/heitor/Desktop/Astronomy/HST-proposal/HST-phase2-apt/OP-cache/phase2-v1-v01.xml The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. Each visit should contain three orbits. 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CASM was run in Phase II mode. Each visit should contain three orbits. 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