All That Glitters Isn't Gold (But It Could Be!): Constraining 3rd-Peak R-Process Abundances in Hyades

0 Assigned ID: 7725 ----- Attempting Submission 1 (Thu Apr 16 22:22:58 GMT 2026) ----- This target is not used in this proposal. This target is not used in this proposal. I have removed the E270H/1830 cenwave from the previous version! And I have updated the exposure times to (the best of my understanding) fulfill the targets set out in the Phase I proposal using synthetic spectra for all the stars. These spectra should be more reflective of the observed values than the preloaded Castelli-Kurucz models. A justification for the removal of HD-28462 and HD-27771 will be sent over email. 1409255603 ----- Attempting Submission 1 (Fri Aug 07 19:16:38 GMT 2026) ----- HST Phase II Proposal 18371 successfully submitted. Receipt: # 18371-1 ----- Attempting Submission 2 (Wed Aug 19 08:59:08 GMT 2026) ----- Warning (Form): The list of Investigators does not match the STScI records for this program. Answer: I will be starting as a postdoc at STScI and as a result I cannot be the finanical PI of this project. I have added Rachael Beaton as she will fill that role. Warning (Form): This target is not used in this proposal. Occurrence: #5 HD-28462 #6 HD-27771 Answer: These two stars were not observable in the alloted number of orbits and were removed from the sample. My PC has been notified already. All That Glitters Isn't Gold (But It Could Be!): Constraining 3rd-Peak R-Process Abundances in Hyades The nucleosynthetic origins and abundance patterns of 3rd-peak rapid-neutron-capture-process elements, particularly lanthanides and actinides, in metal-rich stars remain an ongoing mystery in galactic archaeology, as most 3rd-peak elements are only detectable in the ultraviolet. These elements are hypothesized to be forged in highly energetic events (e.g., electron-capture supernovae and neutron-star mergers); therefore, knowledge of their Galactic abundance patterns is crucial for developing a self-consistent understanding of galactic chemical evolution. We will provide this knowledge by observing seven stars (four K-giants and three K-dwarfs) in the Hyades (Melotte 25), a 600 Myr-old, solar-metallicity open cluster, with the Hubble Space Telescope Imaging Spectrograph. Using high-resolution STIS E230M/E230H spectra, we will place the first-ever constraints in metal-rich stars for the following elements: Ga, Ge, As, Se, Cd, In, Sn, Sb, Te, Ta, W, Re, Pt, Au, Hg, Tl, Pb, and Bi. By jointly analyzing our targets with optical Magellan/MIKE and near-infrared McDonald/IGRINS spectra, we will measure chemical abundances and constrain cluster homogeneity to within 0.1 dex for over sixty elements. Our analysis will provide a key age-resolved anchor for understanding 3rd-peak element enrichment and establish Hyades as one of the best chemically characterized objects in the Galaxy. The goal of this observing program is to collect E230H R=114,000 and E230M R=30,000 spectra of seven stars in the open star cluster Hyades (Melotte 25). All targets are non-variable stars, meaning spectra can be obtained at any point in time. Observations for all targets have been distributed across 1-3 orbit visits to maximize scheduling flexibility. ICRS coordinates and proper motions were taken from Gaia DR3 I have checked the target confirmation chart, and the crosshairs line up to within 1 DSS pixel for all targets. Giant Star Sample: The four giant stars each have observations grouped into 2 and 3 orbit visits respectively. Visit 1 contains: ACQ, ACQ/PEAK, and 5 science exposures on the E230H/2063 central wavelength. The only exception to this is TET-TAU, which includes 1 orbit for: ACQ, ACQ/PEAK, and 3 exposures on E230H/2063. This choice was due to TET-TAU's low luminosity in at 2000 angstroms, and our requirement of fitting our observations into 28 orbits. Visit 2 contains: ACQ, ACQ/PEAK, and SCIENCE exposures. Our target SNR for the giant same is SNR > 50 across the spectrum redward of 2200. Between 2000-2200 we aim for SNR between 10-30. We test this by providing the ETC with synthetic spectra at each star's effective temperature, surface gravity, metallicity, and apparent magnitude. For the 2063 and 3012 we get the warning "WARNING MESSAGE: Partial overlap between instrument throughput band and target spectrum. Please doublecheck the wavelength range covered by the selected spectrum, and the instrument documentation for the selected filter." This is bcause our spectra only cover the range of 2000-3000 angstroms, and show not affect science observations. The BOT gives unsafe warning for the four giant stars; however, it assumes an O5V type star. All giant stars in this sample are K0III stars, and their target information includes their B, Gaia, and 2MASS magnitudes. When tested on the STIS-ETC calculator we do not exceed the maximum count rate. Dwarf Star Sample: The three dwarf stars in the sample have observations grouped into 1-2 visits. HD-28258 has individual visits for the E230M/2269 and E230M/2707 gratings that follow the format: :ACQ, ACQ/PEAK, and SCIENCE exposures. V-V997-TAU and HD-28099 have both gratings grouped in the same visits. These three stars were classified as safe using the BOT. We remove HD-28462 and HD-27771 from our sample as their observations caused our orbit allocation to be exceeded, and individually we could not reasonably group their observations without overrun orbits. There are four key areas of expertise required for this programme of study: 1) Expertise with deriving neutron-capture elements, 2) Experience in open cluster analysis and chemistry, 3) Skill in observing and reducing high-resolution spectra, and 4) Familiarity connecting star cluster chemistry and stellar abundances to the broader galactic context. We have assembled a team of experts that spans these required areas. Zoe Hackshaw is an expert in deriving heavy neutron-capture abundances from high precision spectroscopy in metal-poor stars (Hackshaw et al., 2025) and will contribute to the connection between the r-process abundance pattern and their nucleosynthetic origins in the context of the Hyades. She also has institutional access to McDonald Observatory/IGRINS. Dr. Natalie Myers has extensive experience working with open clusters and deriving neutron-capture abundances for those groups, particularly with optical MIKE and HIRES spectra (Myers et al., 2025). She will aid in reducing Magellan/MIKE spectra and in analyzing and interpreting the abundances derived from the STIS data. Drs. Catherine Manea and Madeline McKenzie are experts in the development of our linelist and in the determination and interpretation of high-precision neutron-capture element abundances from high-resolution near-ultraviolet, optical, and infrared data (McKenzie et al., 2024; Manea et al., 2023). Dr. McKenzie also has institutional access to the Magellan Telescope. Dr. Carrie Filion is an expert in Local Group archaeology and the Korg stellar spectral synthesis code. She will contribute to fitting and analyzing the spectra, as well as interpreting the results in the Galactic context (Filion et al., 2025). Dr. Aida Behmard is an expert in exoplanet formation and connecting host surface abundances to exoplanet composition using high-resolution spectra (Behmard et al., 2025). She will contribute to our focused analysis of Epsilon Tauri and its exoplanet companion. Dr. Gail Zasowski is an expert in galactic archaeology and in using the chemistry of mono-age populations within the Milky Way to study galaxy evolution (Zasowski et al., 2025). She will provide key guidance on connecting bulk abundance to broader GCE trends. Amaya Sinha is an expert in deriving neutron-capture abundances within open clusters, and has plentiful experience constraining chemical homogeneity and chemical variations due to pollution (Sinha et al., 2024, 2026). She developed and tested the analysis plan outlined in this proposal, and will lead this project. Stellar Populations and the Interstellar Medium Galaxies 0 false true false false false false true SUPPORTED STAR K III-I NO 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. J2000 J2000 B: 4.54 (Johnson) G: 3.28 BP: 3.90 RP: 2.66 (Gaia DR3) J: 1.90 H: 1.31 K: 1.31 (2MASS) STAR K III-I NO 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. J2000 J2000 B: 4.64 (Johnson) G: 3.40 BP: 3.97 RP: 2.77 (Gaia DR3) J: 2.02 H: 1.50 K: 1.49 (2MASS) STAR K III-I NO 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. J2000 J2000 B: 4.78 (Johnson) G: 3.58 BP: 4.13 RP: 2.97 (Gaia DR3) J: 2.29 H: 1.75 K: 1.73 (2MASS) STAR K III-I NO This object was generated by the target selector 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. J2000 J2000 B: 4.74 (Johnson) G: 3.52 BP: 4.06 RP: 2.88 (Gaia DR3) J: 2.15 H: 1.58 K: 1.59 (2MASS) STAR K V-IV NO 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. Target removed from sample due to SNR requirements and orbit limitations. J2000 J2000 STAR K V-IV NO 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. Target removed from sample due to SNR requirements and orbit limitations. J2000 J2000 STAR K V-IV NO 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. J2000 J2000 B: 9.86 (Johnson) G: 8.84 BP: 9.25 RP: 8.26 (Gaia DR3) J: 7.51 H: 7.14 K: 7.00 (2MASS) STAR K V-IV NO 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. J2000 J2000 B: 9.40 (Johnson) G: 8.48 BP: 8.84 RP: 7.94 (Gaia DR3) J: 7.32 H: 7.02 K: 6.94 (2MASS) STAR K V-IV NO 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. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 18371 :visit-id "14" :proposal-version -1 :trans-version "20260618" :date "19-Aug-2026 01:33:08.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 313680 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18371 :visit-id "14" :obset-id "14" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18371 :visit-id "14" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2594 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2974 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18371 :visit-id "14" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2593 :al-overhead-at-end 0 :internal-dur-at-end 375 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2974 :pcs-gap 0 ) true 2 0 1787128392058 /Users/amayasinha/Documents/OP-cache/hst_hyades_phaseII-v16.xml The scheduling data was generated by CASM 34.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 18371 :visit-id "16" :proposal-version -1 :trans-version "20260618" :date "19-Aug-2026 01:33:11.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 626848 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18371 :visit-id "16" :obset-id "16" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18371 :visit-id "16" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2596 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2976 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18371 :visit-id "16" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2595 :al-overhead-at-end 0 :internal-dur-at-end 113 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2976 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18371 :visit-id "16" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2594 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2976 :pcs-gap 0 ) true 3 0 1787128394439 /Users/amayasinha/Documents/OP-cache/hst_hyades_phaseII-v17.xml The scheduling data was generated by CASM 34.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 18371 :visit-id "17" :proposal-version -1 :trans-version "20260618" :date "19-Aug-2026 01:33:14.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 400672 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18371 :visit-id "17" :obset-id "17" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18371 :visit-id "17" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2595 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2976 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18371 :visit-id "17" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2594 :al-overhead-at-end 0 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2976 :pcs-gap 0 ) true 2 0