0Assigned ID: 2805
----- Attempting Submission 1 (Mon Mar 21 16:02:24 GMT 2022) -----
HST Phase I Proposal 2805 successfully submitted.
Receipt: # 2805-1
----- Attempting Submission 2 (Thu Mar 24 09:29:38 GMT 2022) -----
HST Phase I Proposal 2805 successfully submitted.
Receipt: # 2805-2
----- Attempting Submission 3 (Thu Mar 24 16:52:37 GMT 2022) -----
HST Phase I Proposal 2805 successfully submitted.
Receipt: # 2805-3
----- Attempting Submission 4 (Fri Mar 25 13:24:32 GMT 2022) -----0----- Attempting Submission 1 (Fri Jul 01 03:13:30 GMT 2022) -----UV spectra of the most metal-deficient 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 sample of the six most metal-deficient (12+logO/H=6.98-7.23) compact SFGs known in the local universe, to obtain low-resolution spectra from Lyman-alpha to ~1700 Ang (covering e.g. the Lya, CIV 1550, HeII 1640, OIII]1661,1666 emission lines) of all XMDs. 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)=159-177A). 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 spectra will be used to constrain the properties of extremely metal-deficient massive stars, the ISM, and the radiation field of these objects, which are extremely rare in the local Universe, but were common at high redshift. Obtaining the rest-UV spectra of these six 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 relatively 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. All objects are planned for observing with the COS (Program GO 16672) but only with the G130M grating. No dublications exist for G140L grating. NUV acquisition images of the targets will be obtained with the standard Mirror A and the ACQ/IMAGE mode to reach a S/N~20 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+2x500s=1120s per object. The UV lines of interest here (primarily C IV 1550, He II 1640, O III] 1661,1666) can be observed with the FUV channel of COS with the low-resolution G140L grating with a single setting for all the targets. Due to rapid decrease of the sensitivity at long wavelengths, C III] 1907,1909 cannot be detected with reasonable exposure times. The prime goal is to obtain spatially integrated flux measurements for the C IV 1550 and He II 1640 emission lines. The targets are very compact (by selection) from ground-based imaging (SDSS). Observations with the 2.5 arcsec aperture will thus capture most of the emission line flux, even if it was somewhat more extended than the UV continuum. We use the GALEX FUV magnitude and the spectroscopic COS ETC to estimate the exposure time needed to obtain SNR = 4 in the continuum at 1540A. The ETC run numbers of these calculations are given in the proposal for each exposure. We also computed detailed mock spectra of our faint targets to assess the detectability of the C IV 1550 doublet at the Poisson limit. We assumed an f(lambda) = const galaxy continuum normalized to the (relatively uncertain) GALEX FUV magnitude and a standard 2:1 CIV doublet ratio. [Note: For two targets, J0811+4730 and J1004+3256, the FUV and NUV magnitudes are derived from extrapolation of the SED in the optical range to the UV range.] Based on observations at higher metallicity and to constrain photoionization models we must conservatively detect EW(C IV)> 2 A. Mock spectra were simulated by adopting the G140L dispersion and line spread function, converting to predicted counts for a given exposure time with the G140L sensitivity and COS detector dark rate predicted from the COS ETC, and adding Poisson noise. We then computed the probability that the spectrum across the C IV doublet is consistent with Poisson noise of the galaxy continuum. For each of the five z < 0.08 galaxies we will be able to detect EW(C IV)= 2 A at 4-5sigma significance in 13, 200 s, i.e. 5 orbits including acquisition. Due to the decreasing G140L sensitivity the higher-redshift galaxy J1234+3901 will require a spectroscopic exposure of 20, 800 s, i.e. two visits with four orbits each. The sources are sufficiently bright and compact for standard target acquisition with short overheads. Our total request sums to 33 orbits.Data reduction, analysis, and interpretation will be done as in our previous GO 13744, GO 14635, GO 15136, GO 15639, GO 15941 and GO 16271 projects and documented in Izotov et al. (2016a,b, 2018b,c, 2020, 2021b). Our team includes experts on all relevant aspects and disposes of all necessary tools, including a custom pipeline for faint COS spectra (Makan et al. 2021, http://adsabs.net/abs/2021ApJ...912...38M), SED fitting tools, Ly-alpha radiation transfer models and others. 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 thus expect to produce scientific results promptly after the data are obtained, as already demonstrated for our successful GO programs 13744, 14635, 15136, 15433, 15639, GO 15941 and GO 16271 in papers by Izotov et al. 2016a,b, 2018b,c, 2020a, 2021b; Schaerer et al 2016, 2018, 2022.Stellar Populations and the Interstellar Medium6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.00+/-0.40, NUV=21.90+/-0.40GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.25+/-0.33, NUV=21.53+/-0.49GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.55+/-0.40, NUV=21.77+/-0.40GALAXYDWARF 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/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.1697648329000283.8509403094258(Tic-Visit
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