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Assigned ID: 146
----- Attempting Submission 1 (Wed Apr 03 19:21:17 GMT 2019) -----
HST Phase I Proposal 146 (metalz.apt) successfully submitted.
Receipt: # 146-1
----- Attempting Submission 2 (Thu Apr 04 01:40:39 GMT 2019) -----
HST Phase I Proposal 146 (metalz.apt) successfully submitted.
Receipt: # 146-2
----- Attempting Submission 3 (Thu Apr 04 21:26:07 GMT 2019) -----
HST Phase I Proposal 146 (metalz.apt) successfully submitted.
Receipt: # 146-3
----- Attempting Submission 4 (Fri Apr 05 20:07:06 GMT 2019) -----
HST Phase I Proposal 146 (metalz.apt) successfully submitted.
Receipt: # 146-4
----- Attempting Submission 5 (Fri Apr 05 20:30:24 GMT 2019) -----
HST Phase I Proposal 146 (metalz.apt) successfully submitted.
Receipt: # 146-5
This new submission includes HOPR 91793 for failed visit 11 (target IC1613-67559), partially repeated in visit 25 (only the G130M/1309 exposures at LP3 with FPPOS = 1,2,3,4 are repeated). Adjustement in exposure times were required to accomodate changes in visibility windows.
1676798672
----- Attempting Submission 1 (Thu Jul 25 19:55:13 GMT 2019) -----
----- Attempting Submission 2 (Tue Sep 17 17:25:40 GMT 2019) -----
----- Attempting Submission 3 (Mon Oct 07 19:37:56 GMT 2019) -----
----- Attempting Submission 4 (Thu Mar 05 21:46:55 GMT 2020) -----
----- Attempting Submission 5 (Wed Jul 01 01:48:53 GMT 2020) -----
----- Attempting Submission 6 (Tue Jul 14 15:25:05 GMT 2020) -----
Visit planner was run for the visit being resubmitted
METAL-Z: Metal Evolution, Transport, and Abundance at Low Metallicity (Z)
A key component of the baryon cycle is the depletion of metals between the gas and dust phases in the neutral ISM. Our understanding of the dust and gas contents of galaxies via dust emission-based gas mass estimates and of the chemical enrichment of the Universe via spectroscopy of damped lyman-alpha systems (DLAs) critically relies on the characterization of the variations of the dust-to-metal mass ratio (D/M) with environment (metallicity, density, morphology). This understanding must be built in the nearby universe, where both gas-phase abundances and photospheric abundances of young stars recently formed out of the ISM can be measured. We propose to obtain COS G130M spectra toward 14 massive stars in IC 1613 (Z=0.15 Z_sun) and Sextans-A (Z=0.08 Z_sun), lower than the critical metallicity at which chemical evolution models predict D/M decreases steeply with metallicity. The COS spectra will be used to derive interstellar depletions of iron and sulfur, from which D/M and the dust-to-gas mass ratio (D/G) will be inferred. Combined with depletion measurements available in the Milky Way, LMC (0.5 Z_sun), and SMC (0.2 Z_sun), we will be able for the first time to measure depletions, D/G, and D/M as a function of metallicity down to 0.08 Z_sun, and enable a comprehensive characterization of the lifecycle of metals in neutral gas and dust in galaxies, thereby observationally addressing important questions about chemical enrichment and galaxy evolution. In particular, this program will provide the depletion calibrations required to interpret DLA metallicity measurements, and substantially improve the accuracy of dust-based gas-mass estimates at low and high redshift.
We will observe 7 massive stars in IC 1613 (Z = 0.15 Z_sun) and 4 massive stars in Sextans A (Z = 0.087 Z_sun) with COS/G130M/1291 (LP4) and 1309 (LP3). The LP4 observations will allow us to derive gas phase column densities of iron (using the 1142-1144 A lines) and sulfur (1250, 1253 A lines). The LP3 observations will allow us to measure the column density of HI along the same lines of sight using lorentzian profile fitting of the 1216 A line. Lyman-alpha based HI column densities cannot be obtained at LP4 as the 1216 A line falls in the gap of the 1222 and the gain-sag gap of the 1291. Using the 1309 at LP3 will give us the most margin on either side of the lines to measure how the absorption trough recovers to the continuum in damped wings of the line.
The COS/FUV modal gain at LP3 will be declining with usage. We will work with the COS team to ensure that, by the time these observations are taken, the modal gain at LP3 is still sufficiently above 3 to enable observations of Lyman-alpha absorption with the 1309.
The PI, Dr. Julia Roman-Duval, is an expert in COS data reduction and interstellar medium research, particularly dust properties and interstellar depletions (Roman-Duval+2010, 2014, 2017). She is the PI of the METAL (GO-14675) large HST program (Roman-Duval+2019) to obtain depletions, extinction curves, and extinction maps in the LMC. She will oversee the progress of the proposed program, participate in the abundance and depletion derivation, and address the science questions listed in the proposal.
Dr. Edward Jenkins is a world-renowned expert in deriving ISM properties from UV spectroscopy. He is the PI of HST program GO-13778 to obtain depletions in the SMC (Jenkins & Wallerstein 2017). Dr. Jenkins will play an important role in the abundance determinations from the spectra.
Mr. Kirill Tchernyshyov is an expert in line profile fitting and UV spectroscopy (Tchernyshyov+2015). He will participate in the line profile fitting for abundance determination using the proposed COS spectra.
Dr. Marc Rafelski is an expert in chemical abundance and star-formation studies of damped Lyman-alpha systems.
Dr. Karl Gordon, Dr. Lea Hagen, Dr. Christopher Clark,and Dr. Monica Relano are experts in dust and SED modeling, IR and UV observations of nearby galaxies, dust properties, and dust attenuation (Gordon+2003, 2009, Hagen+2017, Clark et al. 2018, 2019, Relano et al. 2018).
Dr. Yong Zheng is an expert in the CGM and galaxy-scale inflows and outflows (Zheng et al. 2017). She is the is the PI of GO-15156 to perform an accounting of metals in the halos of local group low metallicity dwarf galaxies.
Dr. Alex Fullerton is an expert in stellar astrophysics, particularly in studies of the winds of massive stars.
Galaxies and the IGM
Stellar Populations
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AVAILABLE
EXT-STAR
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