0
Assigned ID: 3364
----- Attempting Submission 1 (Fri Mar 25 17:40:46 GMT 2022) -----
This is hopefully the final (re)submission of all targets and visits
2107459728
----- Attempting Submission 1 (Sat Jul 02 16:27:11 GMT 2022) -----
HST Phase II Proposal 17184 successfully submitted.
Receipt: # 17184-1
----- Attempting Submission 2 (Tue Jul 12 12:41:05 GMT 2022) -----
Signatures of neutron star mergers hidden in Gaia Enceladus?
The production sites of heavy elements such as Eu and Au are hotly debated. Observational evidence strongly indicates two main sites for the r-process: Neutron star mergers (NSM), and a subset of core-collapse supernovae (r-ccSN). The key question is: What is the difference between the heavy elemental abundance pattern produced by NSM and r-ccSN? This can be answered by looking at stars that have been independently enriched by each source. This is possible by comparing the properties of stars born in the r-process rich accreted galaxy Gaia Enceladus, which is believed to be primarily enriched with NSM, with those stars born in the Milky Way, predominantly enrichment by r-ccSN. For this purpose, a sample of stars with both these origins has been awarded time for high-quality VLT/UVES observations to characterise their chemical signatures. However, many of the key r-process elements are inaccessible from the ground, making HST fundamental for a comprehensive comparison between the two r-process sites. Thus we ask for STIS MAMA HR spectra to measure the detailed r-process abundance pattern for 4 bright stars from the UVES sample: 2 that have primarily been enriched by NSM (Gaia Enceladus), and 2 that are dominated by r-ccSN (the Milky Way). This will be the first time several third peak elements (e.g. Pt, Au) are measured in stars formed outside of the Milky Way, and the combined HST+VLT spectra will provide the most complete abundance pattern that has ever been obtained in an external galaxy. Most importantly, this programme is a unique and innovative way of observationally probing whether r-ccSN provide a different r-process abundance pattern to NSM.
Spectra of stars. S/N important to maximise.
All Co-Is have extensive experience of stellar spectroscopy and stellar abundance analysis and Galactic Archaeology. One of our team (Francesca Primas) also has specific and extensive experince with HST UV stellar spectroscopy abundance analysis.
Stellar Populations and the Interstellar Medium
Stellar Physics and Stellar Types
6
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false
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SUPPORTED
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F3-F9
This object was generated by the targetselector and retrieved from the SIMBAD database.
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This object was generated by the targetselector and retrieved from the SIMBAD database.
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F3-F9
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
F0-F2
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
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STIS/NUV-MAMA
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E230H
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(Tic-Orbit
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(Tic-Orbit
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true
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The scheduling data was generated by CASM 30.3.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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(Tic-Orbit
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true
4
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/Users/et/work/prop/HST/hst22/OP-cache/17184-v12.xml
The scheduling data was generated by CASM 30.3.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 17184
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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true
3
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/Users/et/work/prop/HST/hst22/OP-cache/17184-v13.xml
The scheduling data was generated by CASM 30.3.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Obset
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)
(Tic-Orbit
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)
(Tic-Orbit
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(Tic-Orbit
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true
3
0