Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. 0 Assigned ID: 2963 ----- Attempting Submission 1 (Thu Mar 24 11:31:31 GMT 2022) ----- HST Phase I Proposal 2963 successfully submitted. Receipt: # 2963-1 ----- Attempting Submission 2 (Fri Mar 25 06:16:15 GMT 2022) ----- <Our exposures are long enough (~1.5 orbits) with G160M grating for all targets, therefore we plan to use the default lifetime position LP6 with 4 FP-POS for all targets.>Warning (Form): Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Occurrence: 1 2 3 4 5 6 7 8 Explanation: Please consult the instrument handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position for your G160M observation. 0 ----- Attempting Submission 1 (Fri Jul 01 03:29:25 GMT 2022) ----- One of the key questions in observational cosmology is the identification of the sources responsible for cosmic reionization. The general consensus is that a population of faint low-mass and low-metallicity galaxies must be responsible for the bulk of the ionizing photons at high redshifts. However, for a long time, attempts at identifying individual galaxies showing Lyman continuum (LyC) leakage have only found very few such galaxies, both at high and low redshifts. A breakthrough was achieved in the last few years by Izotov et al. (2016ab,2018ab,2021), who detected LyC emission in 15 out of 20 low-z (z~0.3) compact star-forming galaxies (SFG) with LyC escape fractions of 2-72%, using HST/COS observations. Furthermore, a Large Program of COS observations of 66 z~0.3-0.4 SFGs with the LyC detections in ~50 SFGs has been completed. However, almost all these SFGs have 12+logO/H>7.7, while it is expected that lower-metallicity galaxies were the main sources of the reionization of the Universe. It is proposed here to extend the previous studies to a sample of eight compact SFGs at z~0.3-0.4 at lower metallicities 12+logO/H~7.45-7.70 derived by a direct method, a range almost not explored before by HST/COS. This will allow us to study how LyC escape varies with metallicity in a larger range. The observations will also allow for the determination of the Ly-alpha line profile, providing an empirical probe of this robust indirect LyC leakage indicator for a wide range of metallicities. Since these low- metallicity compact SFGs share many properties with typical SFGs at high redshift, this study will provide important insight on the sources of reionization of the early Universe. The selected galaxies are sufficiently faint to 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'' centered on the selected galaxies. NUV acquisition images of the targets will be obtained with the standard Mirror A and the ACQ/IMAGE mode, with exposures of 300 seconds to reach a S/N~20 inside a 9x9 pixel box centered on the brightest part of the galaxy. The GALEX NUV magnitudes were adopted to estimate the S/N. 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+2x300s=720s per object. As a bonus, it will be possible to study the UV morphology of the selected objects with these images. The COS will be used in combination with the following 2 gratings: 1) the low-resolution G140L grating centered at 800A to measure the LyC. The required number of orbits for each object is calculated so as to detect the LyC at the level above 1sigma with a 100-pixel binning of the data at the observed wavelength near 912x(1+z) Angstrom. For the LyC, an escape fraction of 5% and the intrinsic LyC flux density obtained from the relation I(Hbeta)/I(912)~10A are adopted, where I(Hbeta) is the extinction-corrected flux of the Hbeta emission line; 2) the medium-resolution G160M grating to observe the Ly-alpha line with an observed resolution better than 50 km/s, sufficient to separate blue and red peaks. The required number of orbits to obtain a S/N > 1 in the continuum near Ly-alpha line for a 10-pixel binned spectrum is derived adopting a flux density at the wavelength 1216x(1+z) Angstrom obtained from the SED fit of the optical spectrum. This S/N would be enough to obtain the Ly-alpha profile with a sufficient accuracy for measurements of peak separation and radiative transfer modeling. Each target needs 0.3 orbit for acquisition, 1.5 orbits for the spectrum with the medium-resolution G160M grating, and 2 orbits per object (for the six brightest galaxies with FUV < 21.5 mag) or 3 orbits per object (for the remaining two galaxies) for the spectrum with the low-resolution G140L grating, totalling 4 or 5 orbits per object. We request a total of 34 orbits for 8 objects. Our present proposal is the fifth (following the succesful proposals GO13744 and GO14635, GO15639, GO15845 with a LyC detection in 18 out of 27 proposed galaxies, and the proposal GO16271 with ongoing observations to target directly the LyC of high-excitation compact dwarf galaxies and simultaneously provide other independent tests of LyC leakage which can be applied to high-z galaxies. These observations would increase the number of low-z LyC leakers and extend to lower values the range of metallicities probed to study escaping LyC radiation from star-forming galaxies. Data reduction, analysis, and interpretation will be done as in our previous GO 13744, GO 14635 and GO 15639 projects and documented in Izotov et al. (2016ab, 2018ab, 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 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. 2016ab, 2018ab, 2020, 2021b), as well as modeling and interpretation of Ly-alpha data and absorption lines in the UV range (e.g., Verhamme et al. 2012, 2015, 2017, Schaerer et al. 2011, Duval et al. 2014, Chisholm et al. 2018, Gazagnes et al. 2018, 2020). All galaxies possess SDSS spectra with which Izotov and Guseva will be deriving data such as nebular line ratios, H and He II 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 derive LyC escape fractions from the observed LyC using the methods described by Izotov et al. (2018ab). We thus expect to produce scientific results promptly after the data are obtained, as already demonstrated for our successful GO programs 13744, 14635, 15639 and 15845. The Ly-alpha line profiles will be analyzed empirically and using state-of-the art 3D Monte Carlo radiation transfer models (Verhamme et al. 2006, Schaerer et al. 2011). These models have been used to study the relation between the Ly-alpha line profile and LyC leakage, and were applied to the interpretation of the COS Ly-alpha line profiles of the objects from our sample of leakers (Verhamme et al. 2015, 2017). Galaxies Intergalactic Medium and the Circumgalactic Medium 6 false false true false false false false false SUPPORTED GALAXY DWARF COMPACT STARBURST NO J2000 J2000 FUV=21.47+/-0.20, NUV=21.63+/-0.43, F(1216*(1+z)=1608A)=4.7e-17 erg/s/cm2/A, intrinsic F(912*(1+z)=1206A)=8.7e-17 erg/s/cm2/A GALAXY DWARF COMPACT STARBURST NO J2000 J2000 FUV=21.64+/-0.20, NUV=22.02+/-0.32, F(1216*(1+z)=1600A)=7.3e-17 erg/s/cm2/A, intrinsic F(912*(1+z)=1200A)=5.6e-17 erg/s/cm2/A GALAXY DWARF COMPACT STARBURST NO J2000 J2000 FUV=21.20+/-0.20, NUV=21.71+/-0.23, F(1216*(1+z)=1671A)=1.3e-16 erg/s/cm2/A, intrinsic F(912*(1+z)=1254)=9.7e-17 erg/s/cm2/A GALAXY DWARF COMPACT STARBURST NO J2000 J2000 FUV=20.83+/-0.20, NUV=20.98+/-0.20, F(1216*(1+z)=1649A)=1.8e-16 erg/s/cm2/A, intrinsic F(912*(1+z)=1238)=9.0e-17 erg/s/cm2/A GALAXY DWARF COMPACT STARBURST NO J2000 J2000 FUV=22.07+/-0.20, NUV=22.08+/-0.20, F(1216*(1+z)=1675A)=5.7e-17 erg/s/cm2/A, intrinsic F(912*(1+z)=1257)=3.3e-17 erg/s/cm2/A GALAXY DWARF COMPACT STARBURST NO J2000 J2000 FUV=20.33+/-0.20, NUV=20.36+/-0.20, F(1216*(1+z)=1582A)=3.3e-16 erg/s/cm2/A, intrinsic F(912*(1+z)=1187)=2.4e-16 erg/s/cm2/A GALAXY DWARF COMPACT STARBURST NO J2000 J2000 FUV=21.93+/-0.35, NUV=21.59+/-0.20, F(1216*(1+z)=1592A)=1.1e-16 erg/s/cm2/A, intrinsic F(912*(1+z)=1194)=8.7e-17 erg/s/cm2/A GALAXY DWARF COMPACT STARBURST NO J2000 J2000 FUV=21.48+/-0.20, NUV=21.51+/-0.20, F(1216*(1+z)=1591A)=1.2e-16 erg/s/cm2/A, intrinsic F(912*(1+z)=1193)=8.9e-17 erg/s/cm2/A COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G160M 1589 1656388166854 The scheduling data was generated by CASM 30.3. 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CASM was run in Phase II mode. 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The central wavelength 1589 (Phase I proposal) of the G160M grating is replaced with 1533 in order to place the redshifted Ly-alpha line within segment A. The central wavelength 1589 (Phase I proposal) of the G160M grating is replaced with 1533 in order to place the redshifted Ly-alpha line within segment A. The central wavelength 1589 (Phase I proposal) of the G160M grating is replaced with 1533 in order to place the redshifted Ly-alpha line within segment A. 1656388177504 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1696042729000 72.47520758195111 (Tic-Visit :proposal-id 17109 :visit-id "07" :proposal-version -1 :trans-version "20220516" :date "28-Jun-2022 06:49:37.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 209376 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17109 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17109 :visit-id "07" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2787 :al-overhead-at-end 0 :internal-dur-at-end 2230 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17109 :visit-id "07" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 458 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17109 :visit-id "07" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17109 :visit-id "07" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17109 :visit-id "07" :orbit-number 5 :pcs-time 392 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 5 0 1656388179202 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1693527702000 99.82722873020538 (Tic-Visit :proposal-id 17109 :visit-id "08" :proposal-version -1 :trans-version "20220516" :date "28-Jun-2022 06:49:39.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 192000 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17109 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17109 :visit-id "08" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2807 :al-overhead-at-end 0 :internal-dur-at-end 2210 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17109 :visit-id "08" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2808 :al-overhead-at-end 0 :internal-dur-at-end 458 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17109 :visit-id "08" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2808 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17109 :visit-id "08" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2808 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) true 4 0 The central wavelength 1589 (Phase I proposal) of the G160M grating is replaced with 1533 in order to place the redshifted Ly-alpha line within segment A. The central wavelength 1589 (Phase I proposal) of the G160M grating is replaced with 1533 in order to place the redshifted Ly-alpha line within segment A. The central wavelength 1589 (Phase I proposal) of the G160M grating is replaced with 1533 in order to place the redshifted Ly-alpha line within segment A. The central wavelength 1589 (Phase I proposal) of the G160M grating is replaced with 1533 in order to place the redshifted Ly-alpha line within segment A.