0 Assigned ID: 2175 ----- Attempting Submission 1 (Fri Apr 09 19:57:42 GMT 2021) ----- HD206267: - added ORIENT parameters (225 - 245 and 45 - 65) 1201642367 ----- Attempting Submission 1 (Thu Jul 22 12:27:58 GMT 2021) ----- HST Phase II Proposal 16750 successfully submitted. Receipt: # 16750-1 ----- Attempting Submission 2 (Thu Jul 29 14:11:31 GMT 2021) ----- HST Phase II Proposal 16750 successfully submitted. Receipt: # 16750-2 ----- Attempting Submission 3 (Fri Oct 08 09:50:46 GMT 2021) ----- ----- Attempting Submission 5 (Fri Mar 25 14:41:35 GMT 2022) ----- ----- Attempting Submission 6 (Wed Jun 08 13:06:50 GMT 2022) ----- HST Phase II Proposal 16750 successfully submitted. Receipt: # 16750-6 ----- Attempting Submission 7 (Wed Jun 29 12:22:57 GMT 2022) ----- HST Phase II Proposal 16750 successfully submitted. Receipt: # 16750-7 ----- Attempting Submission 8 (Thu Jul 14 11:22:32 GMT 2022) ----- HST Phase II Proposal 16750 successfully submitted. Receipt: # 16750-8 ----- Attempting Submission 9 (Wed Sep 07 09:49:43 GMT 2022) ----- HST Phase II Proposal 16750 successfully submitted. Receipt: # 16750-9 ----- Attempting Submission 10 (Fri Sep 09 13:39:13 GMT 2022) ----- HST Phase II Proposal 16750 successfully submitted. Receipt: # 16750-10 ----- Attempting Submission 11 (Sun Oct 09 13:06:10 GMT 2022) ----- Inhomogeneities and pristine gas infall in the ISM Is the neutral ISM in the Galaxy clumpy? Does pristine gas infalling on the disk immediately mix with the metal-enriched gas? Recent medium-resolution STIS studies found frequent sub-solar metallicities in the neutral ISM, integrated along the line of sight, suggesting the contribution of low-metallicity gas. Intriguingly, in some cases deviations from the expected depletion patterns were observed for volatile elements. One possible explanation for both effects is a mix between metal/dust-rich and pristine gas (low metallicity and zero depletion) in the ISM. Indeed, an inhomogeneous ISM mix has been recently observed in high-resolution STIS observations of HD 62542. Here we propose to target 8 lines of sight that show potential contribution of pristine gas in the following ways: 1) low metallicity integrated along the line of sight, 2) deviations in the depletion of the volatile elements, and 3) complex/asymmetric kinematics, as measured from lower-resolution studies. The STIS high-resolution will enable a component-by-component analysis to characterize the depletion properties of individual clumps. Our primary goal is to constrain dust-rich and dust-free ISM clumps towards our targets. In addition, we aim at roughly constraining the metallicity of these ISM clumps by exploring the parameter space that can reproduce the observed deviations of the volatile elements. This way we will characterize the inhomogeneities in the ISM and unveil the potential presence of clumps of pristine gas. While chemical evolution models show that infalling pristine gas is necessary to sustain star formation and reproduce the observed abundances, its presence in the ISM is yet to be confirmed. We aim at characterising the ISM chemical and kinematical properties by studying narrow metal lines in the far and near UV associated with the ISM toward Galactic stars. We target 8 hot bright stars that have previous STIS E230M observations. Here we use STIS high resolution spectroscopy (R~114,000) to characterise the individual components of the line profiles in individual gas clouds along lines of sight. We deploy the E140H and E230H settings in order to detect a wide range of ions. The E140H setting at a central wavelength of 1271 A will cover transitions from SiII, MnII, MgII, PII, OI, SII, NiII, CII, and CuII. The E230H setting at a central wavelength of 2113 A will cover transitions of ZnII, CoII, CrII, and FeII lines. The minimum set of ions that we need to characterise to fulfil our scientific goals are: ZnII, CrII, OI. Five out of eight targets will be observed with both the E140H and E230H settings. The other three targets (Rho-Oph-A, HD 206267 and HD 207198) will be observed only with the E230H setting in a single orbit per target, because E140H archival data exists already. For all except for one target, one orbit per setting will ensure the minimum required S/N of 50. For our faintest target HD 154368 two orbits per setting will be necessary to reach a S/N of ~50, for a total of four orbits for this target. The structure of each visit is structured as follows: first we acquire the target with a normal acquisition and an additional peakup target acquisition in case of slits narrower than 0.1", then we plan the science exposures, each with an attached wavelength calibration (in occultation). For the visits including both settings, the science exposure and wavelength calibration for the E140H setting will be done in the second orbit to maximise the S/N for the weakest lines. We increased the science exposure time to fill unused time in each the orbit. We deploy a range of slit apertures for the science exposures, which were chosen to both ensure the safety of the MAMA detectors and maximise the photon collection. We note that in several cases the expected count rate is above 40% of the nominal bright limit. We investigate the variability range of these targets from the General Catalog of Variable Stars (http://www.sai.msu.su/gcvs/) and ensure that the expected count-rate with the selected aperture will not exceed the MAMA bright limit in case the star is at its brightest state. Overall, we expect S/N values between ~50 and ~100. The aperture of the peak acquisition was set to match the aperture of the first science exposure. The orientation of the long slit (31") is specified for Theta Ori-C to avoid neighbouring sources that could contaminate the spectrum. For the other stars with a long slit (Chi-Oph, HD 206267 and Kap-Aql) no preferred orientation is needed. Dr. Annalisa De Cia (Co-PI) has expertise in absorption-line spectroscopy and dust depletion in the neutral ISM in the Galaxy and distant galaxies. She has developed some of the techniques that will be used for the analysis of the observations proposed here, published 2 of the key papers, and is the PI of the complementary Programs HST 15335 and VLT/ESPRESSO 0102.C-0699. She is currently publishing a paper reporting the discovery of low metallicities in the neutral ISM towards the targets proposed here. Dr. Andrew Fox is an expert in the analysis and interpretation of HST/COS and HST/STIS spectra of diffuse gas in the Universe. He has led seven HST GO proposals in this science area. Dr. Edward Jenkins has had well over 4 decades of experience in working with UV spectroscopicdata gathered from Copernicus, IUE, FUSE, IMAPS, and HST. His principal interest is in studies of the composition and physical state of the interstellar and intergalactic medium. His landmark paper published in 2009 formed the basis of unifying the trends in gas-phase element depletions in the Milky Way ISM, and this paper forms the basis of the research program proposed here. He has also recently published a paper on the abundances of elements and depletion trends for the ISM inside the Small Magellanic Cloud, based on HST observations. Christina Konstantopoulou is a PhD student working with Dr. Annalisa De Cia. The main focus of her research is to study the properties of cosmic dust, and in particular dust depletion, through the investigation of the gas-phase abundances in the ISM in the Galaxy as well as in distant galaxies. Dr. Jens-Kristian Krogager (Co-PI) is an expert on absorption line analysis and spectral modelling. Dr. Cedric Ledoux has expertise in absorption-line spectroscopy and dust depletion in the neutral ISM in the Galaxy and distant galaxies. He is an expert in ground-based high-resolution spectroscopy. Tanita Ramburuth-Hurt (Co-PI) is a PhD student working with Dr. Annalisa De Cia. The main focus her research is to study the properties of the neutral ISM using absorption-line spectroscopy, in our own Galaxy as well as in high-z galaxies, with particular emphasis on the local variations inside and around galaxies. Dr. Daniel Welty is currently a support scientist and member of the STIS instrument team at STScI, after many years on the research staff at the University of Chicago. His research has focused on characterizing the abundances and physical conditions in diffuse and translucent interstellar clouds in the Milky Way and Magellanic Clouds, generally via detailed analyses of the atomic and molecular absorption lines seen in high-resolution optical and UV spectra. He is author or co-author of 85 refereed publications (mostly on various aspects of interstellar material); he has been PI for 9 previous HST GO or archival programs (using data from GHRS, FOS, COS, and STIS) and a co-I for several other programs. Stellar Populations and the Interstellar Medium 6 false false true false false false false AVAILABLE STAR B0-B2 V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B0-B2 III-I This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR GIANT O This object was generated by the targetselector and retrieved from the SIMBAD database. 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