0 Assigned ID: 3022 ----- Attempting Submission 1 (Thu Mar 24 17:42:31 GMT 2022) ----- HST Phase I Proposal 3022 successfully submitted. Receipt: # 3022-1 ----- Attempting Submission 2 (Fri Mar 25 10:10:00 GMT 2022) ----- ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN This is a submission to compensate for the failed visit 05. As requested it has been shortened by 1 orbit. No link to the original visit is necessary. (I made a mistake, deleted something, and hence had to redo. Hence also the "REPEAT" object.) -775793 ----- Attempting Submission 2 (Fri Jul 01 03:35:22 GMT 2022) ----- ----- Attempting Submission 3 (Sat Apr 27 19:43:45 GMT 2024) ----- I hope this is ok. Please check. Thanks Uncovering the Lyman continuum SED of star-forming galaxies from ~550 to 912 Angstroem The Lyman continuum (LyC = hydrogen-ionizing radiation at wavelengths < 912 Ang) of galaxies plays a fundamental role in determining the physical and observational properties of the ISM and IGM, including cosmic reionization. Yet it is basically inaccessible to direct observations, and one therefore heavily relies on theoretical, yet untested predictions from synthesis models. Furthermore the ionizing spectra differ significantly between different models, with important implications on widely used emission line diagnostics and other observables. We here propose to observe for the first time the shape of the ionizing continuum of star-forming galaxies over a wide spectral range, from ~550 to 912 Angstroem. This can be achieved with COS by targeting LyC emitters at z~0.8-1. The observations will measure stellar and nebular features in the LyC, and thus provide direct constraints for stellar population models in this generally inaccessible part of the spectrum. The proposed observations will provide unique insight on the hardness of the ionizing spectra of star-forming galaxies, with numerous possible implications on our understanding of the emission line properties of distant galaxies, sources of cosmic reionization, emission line diagnostics, and related topics. We have verified that our targets are sufficiently faint to satisfy safety conditions for observing with the COS and that there are no sources brighter than the COS safety limits in proximity within circle of 43'' diameter) of our targets. We will obtain NUV acquisition images of the targets with the standard Mirror A and the ACQ/IMAGE mode, with exposures of ~ 300 seconds to reach a S/N~20 within a 9x9 pixel box centered on the brightest part of the galaxy. We have used the GALEX NUV magnitudes 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 0.3 orbit. The acquisition image will allow us to analyse the UV morphology of the sources. The COS will be used in combination with 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 ~ 900x(1+z)A. For the LyC flux we have assumed the mimimum value corresponding to an escape fraction of 5 %, and the intrinsic LyC flux density that is obtained from the relation I(Hbeta)/I(912) ~ 9A, where I(Hbeta) is the extinction-corrected flux of the Hbeta emission line. For intrinsic fluxes at shorter wavelengths we have taken a range of predictions from Starburst99 and BPASS models. We have also done simulations of the expected observations using synthetic spectra obtained from SED fits to the available photometry and SDSS spectra and using Starburst99 and BPASS models. These confirm that a sufficient S/N can be obtained over the wavelength range of interest. The extinction of the targets, measured from the Balmer decrement is very low (E(B-V) ~ 0 - 0.07). All the available data (including combination of COS + SDSS spectra, GALEX photometry and SED) will be used to model and correct for selective extinction. It is difficult to foresee the selective extinction in this spectral range. For each target 0.3 orbit is needed for acquisition, and 4.7 orbits for the spectrum with the low-resolution G140L grating, i.e. 5 orbits in total. All four FP-POS are used in consecutive orbits of a visit. We therefore request a total of 25 orbits for 5 objects. The team has all the expertise, tools, and background to successfully carry out the proposed project and to exploit the data in a timely manner. We have recently obtained the first measurement of the SED in the Lyman continuum from ~700-912 Ang in a star-forming galaxy at z~0.6 with COS/HST (GO 16271, PI Schaerer), which motivates and demonstrates the feasibility of the present proposal. Our team has also been responsible for the recent discovery of the low-z strong LyC leakers/emitters with HST/COS observations (Izotov et al.\ 2016ab, 2018ab, 2021). These COS observations of 21 z~0.3-0.4 compact star-forming galaxies have led to a series of numerous interesting publications on LyC, Lyman-alpha, UV absorption lines, outflows, ISM etc. and to significant new insight onto analogs of the sources of cosmic reionization. Data reduction, analysis, and interpretation will be done as in our previous projects and documented in Izotov et al. (2016ab, 2018ab, 2021). 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), which has also been used for simulations of the observations. The team also includes experts of stellar synthesis models and their applications to UV spectra (Schaerer and Chisholm). We can also rely on a large grid of CLOUDY photoionization models, which has recently been computed to examine the behavior of the main emission lines in presence of different ionizing spectra (low metallicities, very hot stars, PopIII, and AGN), and which have been confronted to UV line measurements from the VUDS survey and to most HST observations of low-z galaxies (Nakajima et al. 2018). The model calculations have also been extended to treat the case of density-bounded, i.e. LyC emitting regions (see Schaerer et al. 2018). Finally, we have recently constructed tailored CLOUDY photoionization models of LyC emitters, using one- and two-zone models of the sources, to reproduce/study the observed emission line properties of the LyC emitters (Ramambason, Schaerer et al. 2020). These model suites will be used to analyse the z~0.8-1.0 galaxies of this proposal, taking also into account the direct constraints which will be obtained from the first LyC SED measurements. The available rich ancillary data of the targets including existing imaging (GALEX, SDSS, WISE etc.) and spectroscopic data (SDSS) has already partly been analyzed using methods described in Izotov et al. (2016ab, 2018b, 2021). The analysis will be completed once the HST data will be obtained. Galaxies Intergalactic Medium and the Circumgalactic Medium 6 false false true false false false false false SUPPORTED GALAXY DWARF COMPACT STARBURST NO J2000 J2000 NUV=21.57+/-0.07, f(912*1.81474=1717A)=3.70e-18 erg s-1 cm-2 A-1 - 5% of the intrinsic LyC flux GALAXY DWARF COMPACT STARBURST NO J2000 J2000 NUV=21.33+/-0.12, f(912*1.91414=1746A)=3.2e-18 erg s-1 cm-2 A-1- 5% of the intrinsic LyC flux GALAXY DWARF COMPACT STARBURST NO J2000 J2000 NUV=21.61+-0.11, f(912*1.81474=1655A)=3.10e-18 erg s-1 cm-2 A-1 - 5% of the intrinsic LyC flux GALAXY DWARF COMPACT STARBURST NO J2000 J2000 NUV=21.11+/-0.31, f(912*1.82936=1668A)=4.5e-18 erg s-1 cm-2 A-1 - 5% of the intrinsic LyC flux GALAXY DWARF COMPACT STARBURST NO J2000 J2000 NUV=20.75+/-0.05, f(912*2.00509=1828A)=6.6e-18 erg s-1 cm-2 A-1 - 5% of the intrinsic LyC flux GALAXY DWARF COMPACT STARBURST NO J2000 J2000 NUV=20.75+/-0.05, f(912*2.00509=1828A)=6.6e-18 erg s-1 cm-2 A-1 - 5% of the intrinsic LyC flux COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 The scheduling data was generated by CASM 32.0. CASM was run in Phase II mode. 1690895145000 249.0 (Tic-Visit :proposal-id 17171 :visit-id "01" :proposal-version -1 :trans-version "20230626" :date "27-Apr-2024 20:36:51.0" :trans-errors '(:WARNINGS 5 :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 139344 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17171 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17171 :visit-id "01" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2749 :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 3136 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17171 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2750 :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 3136 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17171 :visit-id "01" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2750 :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 3136 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17171 :visit-id "01" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2750 :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 3136 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17171 :visit-id "01" :orbit-number 5 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 369 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3136 :pcs-gap 0 ) true 5 5 The scheduling data was generated by CASM 32.0. 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