Luminosity-variation independent location of the circum-nuclear, hot dust in NGC 4151

TL;DR

This study uses interferometric data to analyze the hot dust distribution in NGC 4151, revealing that dust size scales are independent of nuclear luminosity variations and are consistent with radiative transfer models.

Contribution

It provides the first interferometric size measurement of the circum-nuclear dust in NGC 4151 that does not depend on nuclear luminosity variations, challenging previous scaling assumptions.

Findings

Dust emission size is roughly 55±5 milliparsecs.

Size scales are insensitive to nuclear luminosity changes.

Data do not support a simple R_dust ∝ L_nuc^0.5 scaling relation.

Abstract

After recent sensitivity upgrades at the Keck Interferometer (KI), systematic interferometric 2um studies of the innermost dust in nearby Seyfert nuclei are within observational reach. Here, we present the analysis of new interferometric data of NGC 4151, discussed in context of the results from recent dust reverberation, spectro-photometric and interferometric campaigns. The complete data set gives a complex picture, in particular the measured visibilities from now three different nights appear to be rather insensitive to the variation of the nuclear luminosity. KI data alone indicate two scenarios: the K-band emission is either dominated to ~90% by size scales smaller than 30mpc, which falls short of any dust reverberation measurement in NGC 4151 and of theoretical models of circum-nuclear dust distributions. Or contrary, and more likely, the K-band continuum emission is dominated by hot dust (>= 1300K) at linear scales of about 50mpc. The linear size estimate varies by a few tens of percent depending on the exact morphology observed. Our interferometric, deprojected centro-nuclear dust radius estimate of 55+-5mpc is roughly consistent with the earlier published expectations from circum-nuclear, dusty radiative transfer models, and spectro-photometric modeling. However, our data do not support the notion that the dust emission size scale follows the nuclear variability of NGC 4151 as a R_dust \propto L_nuc^0.5 scaling relation. Instead variable nuclear activity, lagging, and variable dust response to illumination changes need to be combined to explain the observations.