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

Intermediate mass black holes (10$^3$-10$^5$ M$_\odot$) in the center ofdwarf galaxies are believed to be analogous to growing Active Galactic Nuclei(AGN) in the early Universe. Their characterization can provide insight aboutthe early galaxies. We present optical and near-infrared integral fieldspectroscopy of the inner $\sim$50 pc of the dwarf galaxy NGC4395, known toharbor an AGN. NGC 4395 is an ideal candidate to investigate the nature ofdwarf AGN, as it is nearby ($d\approx4.4$ Mpc) enough to allow a close look atits nucleus. The optical data were obtained with the Gemini GMOS-IFU coveringthe 4500 A to 7300 A spectral range at a spatial resolution of 10 pc. The J andK-band spectra were obtained with the Gemini NIFS at spatial resolutions of$\sim$5 pc. The gas kinematics show a compact, rotation disk component with aprojected velocity amplitude of 25 km s$^{-1}$. We estimate a mass of$7.7\times10^5$ M$_\odot$ inside a radius of 10 pc. From the H$\alpha$ broadline component, we estimate the AGN bolometric luminosity as $L_{bol}=(9.9\pm1.4)\times10^{40}$ erg s$^{-1}$ and a mass $M_{BH}=(2.5^{+1.0}_{-0.8})\times10^5$ M$_\odot$ for the central black hole. Themean surface mass densities for the ionized and molecular gas are in the ranges(1-2) M$_{\odot} $pc$^{-2}$ and (1-4)$\times10^{-3}$ M${_\odot}$ pc$^{-2}$ andthe average ratio between ionized and hot molecular gas masses is $\sim$500.The emission-line flux distributions reveal an elongated structure at 24 pcwest of the nucleus, which is blueshifted relative to the systemic velocity ofthe galaxy by $\approx$30 km s$^{-1}$. We speculate that this structure isoriginated by the accretion of a gas-rich small satellite or by a lowmetallicity cosmic cloud.

A close look at the dwarf AGN of NGC 4395: optical and near-IR integral field spectroscopy