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

Black hole driven outflows in galaxies hosting active galactic nuclei (AGN)may interact with their interstellar medium (ISM) affecting star formation.Such feedback processes, reminiscent of those seen in massive galaxies, havebeen reported recently in some dwarf galaxies. However, such studies haveusually been on kiloparsec and larger scales and our knowledge on the smallestspatial scales to which these feedback processes can operate is unclear. Herewe demonstrate radio jet$-$ISM interaction on the scale of an asymmetric tripleradio structure of $\sim$ 10 parsec size in NGC 4395. This triple radiostructure is seen in the 15 GHz continuum image and the two asymmetric jet-likestructures are situated on either side of the radio core that coincides withthe optical {\it Gaia} position. The high resolution radio image and theextended [OIII]$\lambda$5007 emission, indicative of an outflow, are spatiallycoincident and are consistent with the interpretation of a low power radio jetinteracting with the ISM. Modelling of the spectral lines using {\tt MAPPINGS},and estimation of temperature using optical integral field spectroscopic datasuggest shock ionization of the gas. The continuum emission at 237 GHz, thoughweak, was found to spatially coincide with the AGN. However, the CO(2$-$1) lineemission was found to be displaced by around 20 parsec northward of the AGNcore. The spatial coincidence of molecular H$_2$$\lambda$2.4085 along the jetdirection, the morphology of ionised [OIII]$\lambda$5007 and displacement ofthe CO(2$-$1) emission argues for conditions less favourable for star formationin the central $\sim$ 10 parsec region.

Evidence for low power radio jet-ISM interaction at 10 parsec in the dwarf AGN host NGC 4395