0Assigned ID: 2775
----- Attempting Submission 1 (Sat Mar 19 17:00:05 GMT 2022) -----
HST Phase I Proposal 2775 successfully submitted.
Receipt: # 2775-1
----- Attempting Submission 2 (Fri Mar 25 14:35:54 GMT 2022) -----
HST Phase I Proposal 2775 successfully submitted.
Receipt: # 2775-2
----- Attempting Submission 3 (Fri Mar 25 14:42:03 GMT 2022) -----0----- Attempting Submission 1 (Mon Jul 04 15:56:40 GMT 2022) -----Revealing the link between strong LyC emitters and enigmatic CIV emittersCIV 1550 emission is exceedingly rare in low-redshift star-forming galaxies but has been detected in increasing numbers at high-redshift (in lensed galaxies at z~2-3 and up to z~6-7). The nature of this emission, which requires relatively hard ionizing spectra, is currently unknown and highly debated.
STIS observations of Lyman continuum (LyC) emitters at low-redshift have just revealed intense nebular CIV1550 emission and high ratios of CIV 1550/ CIII]1908 in all galaxies with cosmologically-important escape fractions fesc>0.1. This suggests empirically a link between LyC escape and carbon emission lines, which - if confirmed - would both have important applications for searches of the sources of cosmic reionization (with JWST and from the ground), and could explain the enigmatic CIV emitters.
The discovery of new strong LyC emitters from the Low-redshift Lyman Continuum Survey provides a unique chance to place these exciting results on a more firm base. To do so, we propose STIS observations of ten newly discovered strong leakers to obtain their UV spectra covering all major emission lines between 1200 and 2000 Ang (i.e. Lyman-alpha, HeII, CIV, CIII], OIII], and others). The observations will increase by a factor of ~3 the number of spectra of strong leakers and be compared to a control sample of the same size. Together with existing+scheduled observations, we will thus obtain a sample of 26 star-forming galaxies with full spectral coverage from the Lyman Continuum to ~2000 Ang restframe. This will represent an important HST legacy for studies of the sources of cosmic reionization, with numerous applications and potentially far-reaching implications.The proposed observations will follow the same strategy as earlier, successful STIS observations of LyC emitters, which obtained the first complete UV spectra of strong LyC leakers and confirm the feasibility of the proposed observations. At z ~0.3 the UV lines of interest here (primarily CIV 1550, HeII 1640, OIII] 1661,1666, CIII] 1907,1909) are at 2000-2800A, a range in principle observable with the NUV channel of COS or with STIS. However, STIS is preferred for this spectral range, since STIS is more sensitive in the 1700-3200A domain and the NUV channel of COS is not well calibrated. Also, STIS provides spatially resolved spectroscopy and sky background subtraction, whereas for COS this is not possible due to the circular aperture. The goal is to obtain spatially integrated flux measurements for the emission lines. A low spectral resolution (R~750) is thus sufficient. The G230L (MAMA) has a higher throughput than the G230LB (CCD) at < 2800A, where our lines of interest are. The targets are compact (primarily by selection), both from ground-based imaging (SDSS) and from the COS NUV acquisition images, where the UV half-light radii are < 250 pc for all sources. Observations with the 0.5 arcsec slit will thus capture most of the emission line flux, even if it was somewhat more extended than the UV continuum. The wider slit (2 arcsec) is not optimal because it would degrade the spectral resolution and reduce the contrast of narrow nebular lines against the continuum, making them harder to detect.
The exposure time was determined to reach a S/N=6-7 per STIS G230L pixel in the central 500A of the spectrum, where the S/N is flat. This is the same S/N as obtained in the earlier, public STIS observations of LyC emitters. It will thus provide significant detections for weak lines of EWrest~1-1.5A, and also place strong constraints on the emission lines in case of non-detection. We used the STIS ETC with as input the known continuum flux (determined from the observed UV-optical SEDs based on COS, SDSS spectra, and/or GALEX photometry) at 2000A rest-frame. We adopted the extended object option with 0.5 arcsec in diameter to estimate exposure for acquisition and point-like source option and GALEX NUV magnitude to estimate science exposure with G230L grating. Given the UV magnitudes of the targets, the required time varies from 1-5 orbits typically. All sources are sufficiently bright/compact for standard target acquisition with short overheads, as demonstrated by the earlier COS observations. In total 34 orbits are needed to observe the 10 requested targets.
Buffer times have been adjusted to guarantee regular buffer dumps (often APT makes the last buffer interval in an orbit too long). Visits 09 and 10 are on the same target and should be taken at the same orientation.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.
Our team has been responsible for the recent discovery of the low-z strong LyC leakers/emitters with HST/COS observations (Izotov et al. 2016ab, 2018ab, 2021) and for the recently completed Low-$z$ Lyman Continuum Survey (LzLCS) with HST (PI A Jaskot) which has allowed us to discover several strong leakers (Flury et al. 2022, Saldana-Lopez et al. 2022), which are the targets of this proposals (cf. Figure 2).
The team has also led the first STIS observations of strong LyC emitters, first using mid-cycle 25 observations published in Schaerer et al. (2018), and a nearly completed Cycle 27 program (GO 15941, PI Schaerer), which has led to the discovery of strong CIV emission in strong LyC emitters (Schaerer et al. 2022).
In short, we have thus ample experience with HST and STIS spectroscopy in particular, and we have demonstrated an efficient and rapid exploitation of the data.
The team has already analyzed the available rich ancillary data of our targets (including all HST observations, ground-based and UV photometry, optical SDSS spectroscopy), which have just been discovered, and which represent some of the most interesting and peculiar sources from the LzLCS. The derived data includes all the major observations and numerous physical properties as described in Flury et al. (2022) and Saldana-Lopez et al. (2022).
Members of the team (Schaerer, Nakajima, Jaskot, Ravindranath, Berg and others) have also experience with photoionization models which will be also used to analyse and interpret the UV emission lines. We can, e.g., rely on a large grids of CLOUDY photoionization models, which have recently been computed to examine the behavior of the main UV 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 (see Nakajima et al. 2018). The model calculations have also recently been extended to treat the case of density-bounded, i.e. LyC emitting regions (see Schaerer et al. 2018).
Finally, members of the team (Berg, Chisholm, Jaskot, Ravindranath) have ample experience with low-z galaxy UV spectroscopic observations and are PI and Co-PI of the HST Large Program "COS Legacy Archive Spectroscopic SurveY: A Treasury of Star-Forming Galaxies" (CLASSY).GalaxiesStellar Populations and the Interstellar Medium6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.31+/-0.35, NUV=21.83+/-0.25GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=19.89+/-0.05, NUV=19.88+/-0.03GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.13+/-0.22, NUV=19.78+/-0.10GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=19.31+/-0.14, NUV=19.58+/-0.10GALAXYDWARF COMPACTSTARBURSTJ2000J2000FUV=22.40+/-0.14, NUV=20.94+/-0.05GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.44+/-0.04, NUV=20.63+/-0.04GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.5+/-0.23, NUV=20.78+/-0.13GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.44+/-0.15, NUV=20.97+/-0.14GALAXYDWARF COMPACTSTARBURSTJ2000J2000FUV=22.21+/-0.16, NUV=22.52+/-0.23GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.34+/-0.36, NUV=22.24+/-0.42STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.(Tic-Visit
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