For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.Added V-mag for GALEX-J001235.6-422011.-769708585Assigned ID: 7409
----- Attempting Submission 1 (Thu Apr 16 14:55:02 GMT 2026) -----
HST Phase I Proposal 7409 successfully submitted.
Receipt: # 7409-1
----- Attempting Submission 2 (Thu Apr 16 19:47:16 GMT 2026) -----
HST Phase I Proposal 7409 successfully submitted.
Receipt: # 7409-2Warnings are only related to G160M.Move Visit 04 to ACCUM, as requested by the contact scientist (Matthew R. Siebert)-323084489----- Attempting Submission 1 (Mon Aug 17 17:04:14 GMT 2026) -----
HST Phase II Proposal 18334 successfully submitted.
Receipt: # 18334-1
----- Attempting Submission 2 (Fri Aug 28 01:43:31 GMT 2026) -----Constraining the i-process with heavy-metal subdwarfsThe origin of heavy elements remains a fundamental problem in astrophysics, with growing evidence for an intermediate neutron-capture (i-)process beyond the classical s- and r-process framework. However, its astrophysical sites and yields remain poorly constrained due to degeneracies in evolved stars, where mixing, binary mass transfer, and ongoing nucleosynthesis obscure clear interpretation.
Heavy-metal hot subdwarfs provide a uniquely clean environment to isolate the i-process. These core helium-burning stars bypass the asymptotic giant branch, excluding s-process enrichment on evolutionary grounds, and possess stable, radiative atmospheres free of deep convection. A subset of hot subdwarfs stars exhibits extreme overabundances of trans-iron elements, consistent with i-process nucleosynthesis triggered by proton ingestion during the helium core flash. Crucially, HST ultraviolet spectroscopy of the benchmark system EC22536-5304 enabled the first complete abundance pattern across the trans-iron regime, which is successfully reproduced by i-process models.
We propose HST ultraviolet spectroscopy of 13 heavy-metal subdwarfs to obtain the first representative sample of complete trans-iron abundance patterns. The ultraviolet domain contains diagnostic lines of ~25 heavy elements inaccessible from the ground, enabling robust, quantitative comparisons with nucleosynthesis models. Our goals are (1) to definitively establish the i-process origin of the observed heavy-element enhancements through population-level abundance patterns, and (2) to constrain i-process yields as a function of metallicity and formation channel through direct comparison with state-of-the-art models.Nine bright hot subdwarf stars (sdO/sdB) are observed with STIS/E140M (m_FUV < 13.2mag). Two of these stars can achieve SNR > 25 in a single orbit, seven require two orbits.
The four fainter (14.6 < m_FUV < 15.4mag) stars are observed with COS/G130M-1291 and COS/G160M-1600 at one orbit per grating per target (two orbits each). Because the position of these stars is well known from Gaia DR3 and the COS aperature is large, we do not require a specific target acquisition for stars observed with COS.
Three stars are binaries (sdOB + F5V main sequence star: PB-6355, PG1459-048, GALEX_J202216.8+015225). In each system, the sdOB completly dominates in the UV and the F-type takes over at wavlengths > 5000 Angstrom. Models used for the ETC consider both stars. The binaries are not resolved by HST.Our team has leading expertise in the spectral analysis of hot subdwarf stars, including heavy-metal stars. We have published several papers on the analysis these stars. We have published several papers on the spectral analysis of hot subdwarf stars, which include the most detailed abundance analyses performed for these stars. In our analyses we have made extensive use of HST spectra, including STIS and COS.
The PI, M. Dorsch, is a post-Doc with Prof. S. Geier and has extensively worked with FUV spectra of hot subdwarfs using non-LTE model atmospheres, including He-sdOs and heavy metal enhanced stars.
Prof. U. Heber, Prof. S. Geier, and Prof. C. S. Jeffery are experts on sdB stars, their evolution, and spectral modelling, including binaries, and so is Prof. M. Vuckovic.
Prof. C. S. Jeffery is the leading expert on helium-rich subdwarf stars, and first discovered heavy-metal hot subdwarfs.
Dr. T. Battich and Dr. E. Bauer are experts on stellar evolution theory, including the formation of hot subdwarf stars through all channels described in the proposal. The i-process models of hot subdwarf stars were created by Dr. T. Battich.
The remaining CO-Is are PhD students that may help analysing the spectra; they already have experience in spectral analysis of various kinds of hot subdwarf stars.Stellar Physics and Stellar Types6falsetruefalsefalsefalsefalsefalseSUPPORTEDSTARSDBNOThis 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.J2000J2000STARSDBNOThis 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.J2000J2000STARSDBNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
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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.J2000J2000STARSDBNOJ2000J2000STARSDBNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
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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.J2000J2000STARSDBNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
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