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/

Zendy Plus

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

Zendy Tools

Zendy Open

A fundamental role is attributed to supermassive black holes (SMBH), and thefeedback they generate, in the evolution of galaxies. But theoretical modelstrying to reproduce the relation between the SMBH mass and stellar velocitydispersion of the galaxy bulge make broad assumptions about the physicalprocesses involved. These assumptions are needed due to the scarcity ofobservational constraints on the relevant physical processes which occur whenthe SMBH is being fed via mass accretion in Active Galactic Nuclei (AGN). Insearch for these constraints, our group -- AGN Integral Field Spectroscopy(AGNIFS) -- has been mapping the gas kinematics as well as the stellarpopulation properties of the inner few hundred parsecs of a sample of nearbyAGN hosts. In this contribution, I report results obtained so far which showgas inflows along nuclear spirals and compact disks in the inner tens tohundreds of pc in nearby AGN hosts which seem to be the sources of fuel to theAGN. As the inflow rates are much larger than the AGN accretion rate, theexcess gas must be depleted via formation of new stars in the bulge. Indeed, inmany cases, we find ~100 pc circumnuclear rings of recent star formation (ages~ 10 - 500 Myr) that can be interpreted as a signature of co-evolution of thehost galaxy and its AGN.

The co-evolution of galaxies and supermassive black holes in the near Universe