# Constraining AGN Torus Sizes with Optical and Mid-Infrared Ensemble Structure Functions

## TL;DR

This paper introduces a novel ensemble structure function method to measure the size of AGN dusty tori using optical and MIR variability data, providing a less demanding alternative to reverberation mapping.

## Contribution

The paper develops and validates a new SF-based approach to constrain AGN torus sizes from optical and MIR light curves, demonstrating its effectiveness with SDSS quasar data.

## Key findings

- Torus size correlates with luminosity as log R_eff (pc) = 0.51 * log(L_bol/10^46 erg/s) - 0.38.
- The MIR torus sizes are approximately 1.4 times larger in W2 band than in W1 band.
- The SF method agrees well with dust reverberation mapping results.

## Abstract

We propose a new method to constrain the size of the dusty torus in broad-line active galactic nuclei (AGNs) using optical and mid-infrared (MIR) ensemble structure functions (SFs). Because of the geometric dilution of the torus, the MIR response to optical continuum variations has suppressed variability with respect to the optical that depends on the geometry (e.g., size, orientation, opening angle) of the torus. More extended tori have steeper MIR SFs with respect to the optical SFs. We demonstrate the feasibility of this SF approach using simulated AGN light curves and a geometric torus model. While it is difficult to use SFs to constrain the orientation and opening angle due to insensitivity of the SF on these parameters, the size of the torus can be well determined. Applying this method to the ensemble SFs measured for 587 SDSS quasars, we measure a torus $R-L$ relation of ${\rm log}\,R_{\rm eff}\, {(\rm pc)} = 0.51_{-0.04}^{+0.04} \times {\rm log}\,(L_{\rm bol}/10^{46}\,\rm erg\,s^{-1}) -0.38_{-0.01}^{+0.01}$ in the WISE $W1$ band, and sizes $\sim1.4$ times larger in the $W2$ band, which are in good agreement with dust reverberation mapping measurements. Compared with the reverberation mapping technique, the SF method is much less demanding in data quality and can be applied to any optical+MIR light curves for which a lag measurement may not be possible, as long as the variability process and torus structure are stationary. While this SF method does not extract all information contained in the light curves (i.e., the transfer function), it provides an intuitive interpretation for the observed trends of AGN MIR SFs compared with optical SFs.