The properties of He II 1640 emitters at z ~ 2.5 - 5 from the VANDELS survey

A. Saxena, L. Pentericci, M. Mirabelli, D. Schaerer, R. Schneider, F. Cullen, et al.
2020 Astronomy and Astrophysics  
Aims. Strong He ii emission is produced by low-metallicity stellar populations. Here, we aim to identify and study a sample of He ii λ1640-emitting galaxies at redshifts of z ∼ 2.5−5 in the deep VANDELS spectroscopic survey. Methods. We identified a total of 33 Bright He ii emitters (S /N > 2.5) and 17 Faint emitters (S /N < 2.5) in the VANDELS survey and used the available deep multi-wavelength data to study their physical properties. After identifying seven potential AGNs in our sample and
more » ... carding them from further analysis, we divided the sample of Bright emitters into 20 Narrow (FWHM < 1000 km s −1 ) and 6 Broad (FWHM > 1000 km s −1 ) He ii emitters. We created stacks of Faint, Narrow, and Broad emitters and measured other rest-frame UV lines such as O iii] and C iii] in both individual galaxies and stacks. We then compared the UV line ratios with the output of stellar population-synthesis models to study the ionising properties of He ii emitters. Results. We do not see a significant difference between the stellar masses, star-formation rates, and rest-frame UV magnitudes of galaxies with He ii and no He ii emission. The stellar population models reproduce the observed UV line ratios from metals in a consistent manner, however they under-predict the total number of He ii ionising photons, confirming earlier studies and suggesting that additional mechanisms capable of producing He ii are needed, such as X-ray binaries or stripped stars. The models favour subsolar metallicities (∼0.1 Z ) and young stellar ages (10 6 −10 7 years) for the He ii emitters. However, the metallicity measured for He ii emitters is comparable to that of non-He ii emitters at similar redshifts. We argue that galaxies with He ii emission may have undergone a recent star-formation event, or may be powered by additional sources of He ii ionisation.
doi:10.1051/0004-6361/201937170 fatcat:4hmdfuei3zas7psmql2i24efte