Deep, high resolution spectroscopic observations have been obtained for six compact, strongly star-forming galaxies at redshift z ∼ 0.1 − 0.3, most of them also known as green peas. Remarkably, these galaxies show complex emission-line profiles in the spectral region including Hα, [N II]λλ6548, 6584Å and [S II]λλ6717, 6731Å, consisting of the superposition of different kinematical components on a spatial extent of few kpc: a very broad line emission underlying more than one narrower component. For at least two of the observed galaxies some of these multiple components are resolved spatially in their 2D-spectra, whereas for another one a faint detached Hα blob lacking stellar continuum is detected at the same recessional velocity ∼7 kpc away from the galaxy. The individual narrower Hα components show high intrinsic velocity dispersion (σ ∼ 30-80 km s −1), suggesting together with unsharped masking HST images that star formation proceeds in an ensemble of several compact and turbulent clumps, with relative velocities of up to ∼ 500 km s −1. The broad underlying Hα components indicate in all cases large expansion velocities (full width zero intensity FWZI ≥ 1000 km s −1) and very high luminosities (up to ∼ 10 42 erg s −1), probably showing the imprint of energetic outflows from SNe. These intriguing results underline the importance of green peas for studying the assembly of low-mass galaxies near and far.

X-shooter and ISIS WHT spectra of the starforming galaxy PHL 293B also known as A2228-00 and SDSS J223036.79-000636.9 are presented in this paper.We find broad (FWHM = 1000km/s) and very broad (FWZI = 4000km/s) components in the Balmer lines, narrow absorption components in the Balmer series blueshifted by 800km/s, previously undetected FeII multiplet (42) absorptions also blueshifted by 800km/s, IR CaII triplet stellar absorptions consistent with [Fe/H] < −2.0 and no broad components or blushifted absorptions in the HeI lines. Based on historical records, we found no optical variability at the 5 σ level of 0.02 mag between 2005 and 2013 and no optical variability at the level of 0.1mag for the past 24 years.The lack of variability rules out transient phenomena like luminous blue variables or SN IIn as the origin of the blue shifted absorptions of HI and FeII. The evidence points to either a young and dense expanding supershell or a stationary cooling wind, in both cases driven by the young cluster wind.

We present new results from our search for giant H ii regions in galaxies visible from the Southern hemisphere. In this work we study two galaxies: NGC 7479 and NGC 6070. Using high‐resolution spectra, obtained with different instruments at Las Campanas Observatory, we are able to resolve the emission‐line profile widths and determine the intrinsic velocity dispersion of the ionized gas. We detect profile widths corresponding to supersonic velocity dispersions in the six observed H ii regions. We find that all of them show at least two distinct kinematical components: a relatively narrow feature (between 11 and 22 km s−1) and a broader (between 31 and 77 km s−1) component. Two of the regions show a complex narrow profile in all ion lines, which can be further split into two components with different radial velocities. Whereas the wing broadening of the overall profile can be fitted with a low‐intensity broad component for almost all profiles, in one region it was better reproduced by two separate shell‐like wings. We have analysed the impact that the presence of multiple components has on the location of the H ii regions in the log (L)–log (σ) plane. Although the overall distribution confirms the presence of a regression, the precise location of the regions in the plane is strongly dependent on the components derived from the profile fitting.