0Assigned ID: 177
----- Attempting Submission 1 (Thu Apr 04 11:16:57 GMT 2019) -----
HST Phase I Proposal 177 (STIS_unsubmitted.apt) successfully submitted.
Receipt: # 177-1
----- Attempting Submission 2 (Fri Apr 05 10:57:55 GMT 2019) -----This is the revised phase 2 material, adding visit 11 with 2 orbits, which was granted after failed observations during visit 11.
See HOPR 92230 for HST program 15941.
**please ignore my previous submission (8 june 2022).
We have deliberately reduced the time for acquisition, as the object is sufficiently bright to be acquired with a shorter exposure.
The expected number of counts in the brightest pixel should be ~100.-1207392483----- Attempting Submission 1 (Fri Jul 19 12:53:03 GMT 2019) -----
----- Attempting Submission 3 (Thu Jun 09 07:01:41 GMT 2022) -----TBD by the PCUV emission line spectra of z~0.3-0.4 Lyman continuum emitters a key reference to uncover the sources of cosmic reionizationFew UV templates of low-z star-forming galaxies covering all major UV emission lines between 1200 and 2000 Ang (i.e. Lyman-alpha, HeII, CIV, CIII], OIII], and others) exist and most importantly only one for galaxies with known Lyman continuum (LyC) leakage. Selecting for high [OIII]/[OII] optical line ratios and compactness, a breakthrough in the identification of Lyman continuum emitting galaxies has recently been achieved with COS/HST. Indeed, Izotov et al. (2016ab, 2018ab) have found eleven strongly star-forming galaxies at z~0.3-0.4 with escape fractions fesc=2-72 %, which currently represent the best analogs of the sources of cosmic reionization. It is proposed to obtain full UV spectra of all the known z~0.3-0.4 LyC emitters with STIS/HST. The emission line measurements will allow to address a variety of important questions regarding the consistency between UV and optical diagnostic diagrams, the behavior of CIII] emission in low metallicity galaxies, the hardness of the ionizing spectrum of the LyC emitters, their ionizing photon production, the use of UV emission lines as an indirect indication for LyC escape, and others. The proposed observations will provide for the first time empirical UV emission line spectra of a sample of confirmed Lyman continuum emitters, which are rare at low redshift but whose properties are very similar to those of common high-z star-forming galaxies. Obtaining rest-UV spectra of known Lyman continuum emitters is both crucial and urgent in the quest for the understanding of cosmic reionization and its sources, and for upcoming studies with the JWST and the largest ground-based facilities.We aim at observing all the confirmed z ~0.3 - 0.4 LyC emitters discovered recently with the HST. This amounts to 11 sources, out of which one was already recently observed with STIS. The galaxies were selected for their high ratio O32 > 5, compactness, and strong emission lines. Their measured LyC escape fractions vary between 1.4 and 72 %, stellar masses between 1e8 and 3x10e9 Msun. The physical properties of the rare low-z sources selected here are very similar to those of typical star-forming galaxies observed at z > 6. They are thus the best known low-z analogs of the sources of cosmic reionization. At z ~0.3 - 0.4 the UV lines of interest here (primarily C iv 1550, He ii 1640, O iii] 1661,1666, C iii] 1907,1909) are at 2000 - 2800 A, a range which is in principle observable with the NUV channel of COS or with STIS. STIS observations are preferred for this spectral range, since the NUV channel of COS is not well calibrated, STIS is more sensitive in the 1700 - 3200 A domain, and has no spectral gaps. 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 < 2800 A. Since most lines (C iv 1550, He ii 1640, O iii] 1661,1666) are at observed wavelengths 2000 - 2160 A and C iii] 1907,1909 is likely the strongest, we prefer G230L (MAMA), even for the highest-z sources. The targets are very compact (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. The UV surface brightness profiles have exponential scale heights of 0.6 - 1.75 kpc, corresponding to 0.13 - 0.40 arcsec. 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=3 for weak lines of EWrest = 1 - 1.5 A, which will also place strong constraints on the emission lines in case of non-detection. C iii] 1908 equivalent widths of 5 - 15 A are not uncommon in normal star-forming galaxies with low metallicities. The other targetted lines (C iv 1550, He ii 1640, and O iii] 1666) are normally weaker.
We used the STIS ETC with as input the known continuum flux (determined from the observed UVoptical SEDs based on COS, SDSS spectra, and/or GALEX photometry at 2000 A rest-frame. We adopted the extended object option with 0.4 arcsec in diameter. The acquisition time is calculated to obtain SNR=40 and adopting the surface brightness g/0.4**2, where g is the SDSS g apparent magnitude. The science exposure is calculated to obtain SNR=5 for C iii] 1907,1909 line adopting its extent along the spectral and spatial axes of 15 pix and 20 pix, respectively. Then SNR=5 in the line would correspond to SNR in the continuum of 5/sqrt(15x20)~0.2. The total required time corresponds to 3-5 orbits per source. The sources are sufficiently bright and compact for standard target acquisition with short overheads. The total request amounts to 42 orbits for 10 targets. The recent STIS observations of one of the faintest z ~ 0.3 - 0.4 LyC emitters, J1154+2443, using the same settings as the proposed ones and with a similar exposure time (4 orbits), confirms the feasibility of the present observation.
Our observations do not require repeated visits to the same galaxy and do not require constraints on the HST orientation. Therefore, operating HST in reduced gyro mode would likely affect our program a little, slightly increasing the time for acquisition and slightly reducing the time for science observations.The team has all the expertise, tools, and background to successfully carry out the proposed project.
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). These COS observations of 11 z ~ 0.3 - 0.4 compact star-forming galaxies have led to a series of numerous interesting publications on LyC, Ly-alpha, UV absorption lines, outflows, ISM etc. and to significant new insight onto analogs of the sources of cosmic reionization. In late april 2018 we have obtained the first UV (STIS) spectrum covering ~ 1200 - 2000 A (rest-frame) of a confirmed LyC leaker, the source J1154+2443 with an escape fraction fesc=46%. These mid-cycle 25 observations and results have been published in Schaerer et al. (2018).
We can also rely on a large grid of CLOUDY photoionization models, which has 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 (cf. Fig. 2, and Nakajima et al. 2018ab). 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). Our team also includes Swara Ravindranath and Anne Jaskot, who have studied in depth C III] 1908 emission in ''green pea''-like galaxies and who have conducted recent HST observations of a small sample of such galaxies (Jaskot & Ravindranath 2016, Ravindranath et al. 2019).
The team also includes Danielle Berg, an expert on Carbon abundances in nearby galaxies, who will conduct the detailed analysis of the C/O abundances and related topics using the proposed observations.
The available rich ancillary data of our targets (including all HST observations, ground-based and UV photometry, optical SDSS spectroscopy) has already been analyzed, and the basic physical properties derived as documented in Izotov et al. (2016ab, 2018b). We have also recently obtained deep high-resolution optical spectra with the ESO Very Large Telescope (VLT) and the Gran Telescopio Canarias (GTC), which allows us to search for fainter emission lines and address other questions.Galaxies and the IGMCosmology6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=20.71+/-0.05, NUV=20.75+/-0.04, frest(1909)=0.8e-16 erg s-1 cm-2 A-1 in the continuumGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=20.66+/-0.30, NUV=20.38+/-0.17, frest(1909)=0.8e-16 erg s-1 cm-2 A-1 in the continuumGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=20.72+/-0.17, NUV=20.97+/-0.17, frest(1909)=0.6e-16 erg s-1 cm-2 A-1 in the continuumGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=20.16+/-0.17, NUV=20.31+/-0.05, frest(1909)=1.0e-16 erg s-1 cm-2 A-1 in the continuumGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=21.02+/-0.31, NUV=20.76+/-0.18, frest(1909)=0.6e-16 erg s-1 cm-2 A-1 in the continuumGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=22.06+/-0.12, NUV=22.17+/-0.14, frest(1909)=0.3e-16 erg s-1 cm-2 A-1 in the continuumGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=22.08+/-0.50, NUV=21.31+/-0.27, frest(1909)=0.4e-16 erg s-1 cm-2 A-1 in the continuumGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=21.31+/-0.24, NUV=21.61+/-0.24, frest(1909)=0.4e-16 erg s-1 cm-2 A-1 in the continuumGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=21.42+/-0.38, NUV=21.16+/-0.28, frest(1909)=(0.3-0.4)e-16 erg s-1 cm-2 A-1 in the continuumGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=21.66+/-0.30, NUV=21.85+/-0.27, frest(1909)=0.3e-16 erg s-1 cm-2 A-1 in the continuumSTIS/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 27.2.CASM was run in Phase II mode.1616324395000115.0(Tic-Visit
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