We present the first measurements of the Lyman-continuum photon production efficiency xi(ion.0) at z similar to 4-5 for galaxies fainter than 0.2 L* (-19 mag). xi(ion.0) quantifies the production... Show moreWe present the first measurements of the Lyman-continuum photon production efficiency xi(ion.0) at z similar to 4-5 for galaxies fainter than 0.2 L* (-19 mag). xi(ion.0) quantifies the production rate of ionizing photons with respect to the UV luminosity density assuming a fiducial escape fraction of zero. Extending previous measurements of xi(ion.0) to the faint population is important, as ultra-faint galaxies are expected to contribute the bulk of the ionizing emissivity. We probe xi(ion.0) to such faint magnitudes by taking advantage of 200-h depth Spitzer/IRAC observations from the GREATS program and approximate to 300 3 < z < 6 galaxies with spectroscopic redshifts from the MUSE GTO Deep + Wide programs. Stacked IRAC [3.6] [4.5] colors are derived and used to infer the H alpha rest-frame equivalent widths, which range from 403 angstrom to 2818 angstrom. The derived xi(ion.0) is log(10)(xi(ion.0)/Hz erg(-1)) = 25.36 0.08 over-20.5 < Muv <-17.5, similar to those derived for brighter galaxy samples at the same redshift and therefore suggesting that 6011 shows no strong dependence on M-UV. The xi(ion.0) values found in our sample imply that the Lyman-continuum escape fraction for M-UV approximate to-19 star-forming galaxies cannot exceed approximate to 8-20% in the reionization era. Show less
Deep optical spectroscopic surveys of galaxies provide a unique opportunity to investigate rest-frame ultra-violet (UV) emission line properties of galaxies at z similar to 2-4.5. Here we combine... Show moreDeep optical spectroscopic surveys of galaxies provide a unique opportunity to investigate rest-frame ultra-violet (UV) emission line properties of galaxies at z similar to 2-4.5. Here we combine VLT /MUSE Guaranteed Time Observations of the Hubble Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other publicly available data from VLT /VIMOS and VLT /FORS2 to construct a catalogue of He II lambda 1640 emitters at z greater than or similar to 2. The deepest areas of our MUSE pointings reach a 3 sigma line flux limit of 3.1 x 10(19) erg s(-1) cm(-2). After discarding broad-line active galactic nuclei, we find 13 He II lambda 1640 detections from MUSE with a median M-UV = -20.1 and 21 tentative He II lambda 1640 detections from other public surveys. Excluding Ly alpha, all except two galaxies in our sample show at least one other rest-UV emission line, with C III] lambda 1907, lambda 1909 being the most prominent. We use multi-wavelength data available in the Hubble legacy fields to derive basic galaxy properties of our sample through spectral energy distribution fitting techniques. Taking advantage of the high-quality spectra obtained by MUSE (similar to 10-30 h of exposure time per pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics of the He II lambda 1640 emitters. Line ratios of our sample can be reproduced by moderately sub-solar photo-ionisation models, however, we find that including effects of binary stars lead to degeneracies in most free parameters. Even after considering extra ionising photons produced by extreme sub-solar metallicity binary stellar models, photo-ionisation models are unable to reproduce rest-frame He II lambda 1640 equivalent widths (similar to 0.2-10 angstrom), thus additional mechanisms are necessary in models to match the observed He II lambda 1640 properties. Show less
Paalvast, M.; Verhamme, A.; Straka, L.A.; Brinchmann, J.; Herenz, E.C.; Carton, D.; ... ; Wisotzki, L. 2018
