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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We have used optical Integral Field Spectroscopy in order to map the starformation history of the inner kiloparsec of the Post-Starburst Quasar (PSQ)J0330--0532 and to map its gas and stellar kinematics as well as the gasexcitation. PSQs are hypothesized to represent a stage in the evolution ofgalaxies in which the star formation has been recently quenched due to thefeedback of the nuclear activity, as suggested by the presence of thepost-starburst population at the nucleus. We have found that the old stellarpopulation (age $\ge$ 2.5 Gyr) dominates the flux at 5100 \AA\ in the inner0.26 kpc, while both the post-starburst (100 Myr $\le$ age $<$ 2.5 Gyr) andstarburst (age $<$ 100 Myr) components dominate the flux in a circumnuclearring at $\approx$0.5 kpc from the nucleus. With our spatially resolved study wedo not have found any post-starburst stellar population in the inner 0.26\,kpc.On the other hand, we do see the signature of AGN feedback in this region,which does not reach the circumnuclear ring where the post-starburst populationis observed. We thus do not support the quenching scenario for the J0330-0532.In addition, we have concluded that the strong signature of the post-starburstpopulation in larger aperture spectra (e.g. from Sloan Digital Sky Survey) ispartially due to the combination of the young and old age components. Based onthe M$_{\rm BH}-\sigma_{\rm star}$ relationship and the stellar kinematics wehave estimated a mass for the supermassive black hole of 1.48 $\pm$ 0.66$\times$10$^7$ M$_\odot$.

2D stellar population and gas kinematics of the inner kiloparsec of the post-starburst quasar SDSS J0330-0532