0Assigned ID: 1466
----- Attempting Submission 1 (Mon Apr 05 09:40:14 GMT 2021) -----
HST Phase I Proposal 1466 successfully submitted.
Receipt: # 1466-1
----- Attempting Submission 2 (Fri Apr 09 12:57:02 GMT 2021) -----The Ly-alpha line in visits 8 and 9 can be affected by the OI airglow emission line.
Therefore, the observations should preferentially be taken in orbital shadow to minimize this
contamination. We used a table with the orbital visibility to select optimal observing periods with
a shadow visibility of more than 25 minutes. These have been implemented with BETWEEN constraints
for visits 08 and 09.1500271099----- Attempting Submission 1 (Fri Jul 09 09:57:01 GMT 2021) -----
HST Phase II Proposal 16672 successfully submitted.
Receipt: # 16672-1
----- Attempting Submission 2 (Sun Jul 18 16:43:18 GMT 2021) -----
HST Phase II Proposal 16672 successfully submitted.
Receipt: # 16672-2
----- Attempting Submission 3 (Tue Jul 20 09:12:01 GMT 2021) -----Ly-alpha emission from the low-z most metal-deficient star-forming galaxiesExtremely metal-deficient (XMD), compact and low-mass star-forming galaxies (SFGs) at low redshifts are considered to be the likely nearby counterparts of the high-z star-forming dwarf galaxies thought to be responsible for the reionization of the Universe. We propose to observe with the HST/COS a complete sample of the nine most metal-deficient (12+logO/H<7.25) compact SFGs known in the local universe, to obtain medium-resolution spectra of the Ly-alpha emission line. Only one galaxy with such a low metallicity, I Zw 18, has been studied previously with the HST/COS. These SFGs were selected from the Data Release 16 and earlier releases of the Sloan Digital Sky Survey to be not only XMD, but also to be very compact and to have very young starbursts (EW(Hbeta)>100A). Among them one galaxy, J0811+4730 with 12+logO/H = 6.98, is one of the lowest-metallicity low-z SFG known to date. The Ly-alpha profiles in those medium resolution spectra will be used to indirectly estimate the escape fraction of the Lyman continuum and will provide important insight on the ISM and radiation field of the star-forming regions. Obtaining the rest-UV spectra of these nine XMD SFGs which will serve as templates for the analysis of spectra of high-z dwarf galaxies with active star formation, is thus both urgent and crucial for upcoming studies with the JWST and the largest ground-based facilities.The galaxies are faint and satisfy safety conditions for observing with the COS. Furthermore, there are no sources brighter than the COS safety limits in circular regions with the diameter of 43 arcsec centered on the selected galaxies. NUV acquisition images of the targets will be obtained with the standard Mirror A and the ACQ/IMAGE mode to reach a S/N20 inside a 9x9 pixel box centered on the brightest part of the galaxy. The adopted GALEX NUV magnitudes were used to estimate exposure times. The angular galaxy radius is chosen to be 0.2", inside which most of the galaxy light is concentrated. The total time for acquisition is up to 120s+2x700s=1520s per object (HST Primer manual), or half of orbit. As a bonus, the UV morphology of the selected objects will be studied with these images. For medium-resolution spectroscopy, the COS in combination with the G130M grating will be used to observe the Ly-alpha line. This resolution is required to resolve the Ly-alpha line profile and to measure features such as the velocity separations between different emission peaks which give the best estimate of the LyC escape fraction. The Ly-alpha emission-line profiles in the spectra of the proposed galaxies will be compared to those in LyC leaking galaxies and in Green Pea galaxies. The GALEX FUV magnitude is used to calculate for each object the required number of orbits to obtain a S/N > 5 for the continuum near Ly-alpha line, in the case of a 100-pixel binned spectrum. This S/N would be enough to obtain the Ly-alpha profile with a sufficient accuracy for radiative transfer modeling and for deriving velocity separations between the peaks. For each target, 0.5 orbit for acquisition, and 2.5 or 3.5 orbits for the spectrum with the medium-resolution G130M grating are needed, totalling 3 or 4 orbits per object. A total of 34 orbits for 9 objects is requested.Data reduction, analysis, and interpretation will be done as in our previous GO 13744, GO 14635, GO 15136 and GO 15639 projects and documented in Izotov et al. (2016a,b, 2018b,c, 2020a, 2021b). Our team includes experts on all relevant aspects and disposes of all necessary tools, including a custom pipeline for faint COS spectra (Worseck et al. 2011, Syphers et al. 2012), SED fitting tools, Ly-alpha radiation transfer models and others. Our team has also extensive experience in Ly-alpha observations of both low and high redshift star-forming galaxies (Thuan & Izotov 1997, Thuan et al. 1997, Hayes et al. 2010, Oti-Floranes et al. 2012, Hayes et al. 2013, Izotov et al. 2016a,b, 2018b,c, 2020a, 2021b), as well as modeling and interpretation of Ly-alpha data (e.g., Verhamme et al. 2015, 2017, Schaerer et al. 2011, Duval et al. 2014, Kimm et al. 2019). All galaxies possess SDSS spectra with which Izotov and Guseva derived data such as nebular line ratios, Hbeta and HeII emission-line luminosities, starburst ages and masses, limits on photoionization by WR stars and shocks, element abundances, specific star formation rates, etc. necessary for interpreting the LyC, and Ly-alpha data. We will empirically derive LyC escape fractions from the observed Ly-alpha profiles using the methods described by Izotov et al. (2018b,c). The Ly-alpha line profiles will be analyzed empirically similarly to Izotov et al. (2016a,b, 2018b,c, 2020a, 2021b). We thus expect to produce scientific results promptly after the data are obtained, as already demonstrated for our successful GO programs 13744, 14635, 15136, 15433 and 15639 in papers by Izotov et al. 2016a,b, 2018b,c, 2020a, 2021b; Schaerer et al 2017, 2018; Verhamme et al. 2017.GalaxiesIntergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.51+/-0.09, NUV=21.46+/-0.10GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000NUV=22.17+/-0.15GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.00+/-0.40, NUV=21.90+/-0.40GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.25+/-0.33, NUV=21.53+/-0.49GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000NUV=22.35+/-0.18GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=22.28+/-0.14, NUV=22.25+/-0.12GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.24+/-0.38, NUV=22.17+/-0.57GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.54+/-0.32, NUV=21.29+/-0.18GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.45+/-0.28, NUV=21.88+/-0.37COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291/home/izotov/out/Proposals/HST/HST_2021_Cycle29/POOR/OP-cache/16672-v01.xmlThe scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.(Tic-Visit
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)true30/home/izotov/out/Proposals/HST/HST_2021_Cycle29/POOR/OP-cache/16672-v09.xmlThe scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.The Ly-alpha line can be affected by the OI airglow emission line. Therefore, the observations should preferentially be taken in orbital shadow to minimize this contamination. We used a table with the orbital visibility to select optimal observing periods with a shadow visibility of more than 25 minutes. These have been implemented with BETWEEN constraints.(Tic-Visit
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