0 Assigned ID: 1525 ----- Attempting Submission 1 (Fri Sep 29 09:55:44 GMT 2017) ----- HST Phase I Proposal 1525 (UVlines.apt) successfully submitted. Receipt: # 1525-1 ----- Attempting Submission 2 (Sat Sep 30 14:41:27 GMT 2017) ----- 6/18/2018 - ROYLE - Added visit 52 as repeat of failed visit 02 - correcting previous visit confusion. -996112680 ----- Attempting Submission 1 (Fri Dec 01 17:30:30 GMT 2017) ----- ----- Attempting Submission 2 (Wed Jun 13 22:04:52 GMT 2018) ----- ----- Attempting Submission 3 (Tue Jun 19 12:47:04 GMT 2018) ----- Duplicate of visit 02 Few 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 none for galaxies with known Lyman continuum (LyC) leakage. Selecting for high [OIII]/[OII]>4 optical line ratios and compactness, our team has recently achieved a breakthrough in the identification of Lyman continuum leaking galaxies with high escape fraction (fesc=6-13%), which currently represent the best analogs of the sources of cosmic reionization. In recent (20-21 july 2017) COS/HST observations we discovered a new LyC leaker showing very strong Lyman continuum flux, with an escape fraction fesc=46+-3%, the highest LyC escape fractions observed so far in low-z galaxies. We here request STIS spectroscopy of this unique source to measure the complete UV spectrum, including all of the above UV lines. The proposed observations will provide for the first time an empirical UV emission line spectrum of Lyman continuum leakers, 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 Lyman continuum leakers, currently the best analogs of the sources of cosmic reionization, is both crucial and urgent for upcoming studies with the JWST and the largest ground-based facilities. So far, we have observed the Lyman continuum and the Ly-alpha line with COS, using the G140L and G160M grisms in the FUV channel, which is in practice limited to wavelengths shorter than 2000 A. At z > 0.3 the UV lines of interest here (primarily C iv 1550, He ii 1640, O iii] 1661,1666, C iii] 1907,1909) are at 2000-2600 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. Our goal is to obtain spatially integrated flux measurements for the emission lines. A low spectral resolution is thus sufficient. The G230L (MAMA) has a higher throughput than the G230LB (CCD) at < 2250. 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). Our objects are very compact (by selection), both from ground-based imaging (SDSS) and from the COS FUV acquisition images, where the objects show UV surface brightness profiles with exponential scale heights of 0.6-1.4 kpc, corresponding to 0.13-0.32 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 A to place also 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 considerably weaker. We used the STIS ETC using the known continuum flux (from COS spectra and/or GALEX photometry) at 2000 A rest-frame. We adopted the extended object option with 0.5 arcsec in diameter. The required time corresponds to 8 orbits. The observations will be split into two visits, 4 orbits each. Our object is sufficiently bright and compact for standard target acquisition with short overheads. Cosmology Galaxies and the IGM 6 false false true false false false false SUPPORTED GALAXY DWARF COMPACT EMISSION LINE NEBULA STARBURST NO J2000 J2000 FUV=22.10+/-0.26, NUV=21.57+/-0.24, acq=870s, spectrum=23000s, http://etc.stsci.edu/etc/results/STIS.sp.1026387 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/NUV-MAMA Spectroscopic No No G230L 2376 1512124422370 Hst Same orient constraint links visits (01 02 51) The scheduling data was generated by CASM 26.0. 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