English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

NGC 3311 is the central galaxy of the Hydra I galaxy cluster. It has a hotinterstellar medium and hosts a central dust lane with emission lines. Thesedust lanes are frequent in elliptical galaxies, but the case of NGC 3311 mightbe particularly interesting for problems of dust lifetime and the role of coolgas in the central parts. We aim to use archival HST images and MUSE data toinvestigate the central dust structure of NGC 3311. We used the tool PyParadiseto model the stellar population and extract the emission lines. The HST/ACScolour map reveals the known dust structures, but also blue spots, which areplaces of strong line emission. A dusty 'mini-jet' emanates from the centre.The distribution of the emission line gas matches the dust silhouette almostexactly. Close to the brightest Halpha emission, the ratio [NII]/Halpharesembles that of HII-regions; in the outer parts, [NII] gets stronger and issimilar to LINER-like spectra. The gas kinematics is consistent with that of arotating disc. The Doppler shifts of the strongest line emissions, whichindicate the areas of highest star formation activity, smoothly fit into thedisc symmetry. The metallicity is supersolar. The presence of neutral gas isindicated by the fit residuals of the stellar NaI D absorption line, which weinterpret as interstellar absorption. We estimate the mass of the neutral gasto be of the order of the X-ray mass. The dynamical mass infers a stellarpopulation of intermediate age, whose globular clusters have already beenidentified. Our findings can be harmonised in a scenario in which the starformation is triggered by the accretion of cold gas onto a pre-existinggas/dust disc or ring. Newly produced dust then contributes to the longevity ofthe dust.

Dust and star formation in the centre of NGC 3311