AGN STORM 2. XI. Spectroscopic reverberation mapping of the hot dust in Mrk 817

TL;DR

This study uses spectroscopic reverberation mapping to measure the hot dust radius in Mrk 817, revealing a luminosity-invariant dusty wall and extended dust structures linked to the host galaxy's starburst activity.

Contribution

It provides the first spectroscopic reverberation mapping of hot dust in Mrk 817, demonstrating a stable dusty wall and connecting dust structures to host galaxy features.

Findings

Dust reverberation radius of ~90 light-days consistent with previous results.

Inner dusty wall is luminosity-invariant and likely composed of carbonaceous material.

Extended hot dust on scales > 140-350 pc associated with the galaxy's bulge and starburst.

Abstract

The AGN Space Telescope and Optical Reverberation Mapping 2 (STORM 2) campaign targeted Mrk 817 with intensive multi-wavelength monitoring and found its soft X-ray emission to be strongly absorbed. We present results from 157 near-IR spectra with an average cadence of a few days. Whereas the hot dust reverberation signal as tracked by the continuum flux does not have a clear response, we recover a dust reverberation radius of $\sim 90$ light-days from the blackbody dust temperature light-curve. This radius is consistent with previous photometric reverberation mapping results when Mrk 817 was in an unobscured state. The heating/cooling process we observe indicates that the inner limit of the dusty torus is set by a process other than sublimation, rendering it a luminosity-invariant `dusty wall' of a carbonaceous composition. Assuming thermal equilibrium for dust optically thick to the incident radiation, we derive a luminosity of $\sim 6 \times 10^{44}$ erg s$^{-1}$ for the source heating it. This luminosity is similar to that of the obscured spectral energy distribution, assuming a disk with an Eddington accretion rate of $\dot{m} \sim 0.2$. Alternatively, the dust is illuminated by an unobscured lower luminosity disk with $\dot{m} \sim 0.1$, which permits the UV/optical continuum lags in the high-obscuration state to be dominated by diffuse emission from the broad-line region. Finally, we find hot dust extended on scales $> 140-350$ pc, associated with the rotating disk of ionised gas we observe in spatially-resolved [SIII] $\lambda 9531$ images. Its likely origin is in the compact bulge of the barred spiral host galaxy, where it is heated by a nuclear starburst.