# Observability of Forming Planets and their Circumplanetary Disks II. -- SEDs and Near-Infrared Fluxes

## TL;DR

This study combines 3D radiative hydrodynamic simulations with radiative transfer modeling to analyze the observability of forming planets and their circumplanetary disks in various wavelengths, highlighting optimal detection strategies.

## Contribution

It provides the first comprehensive near-infrared modeling of circumplanetary disks, showing their brightness dependence on disk parameters and identifying optimal wavelengths for detection.

## Key findings

- CPDs are 20-100 times brighter than embedded planets in near-IR.
- Best contrast for detecting CPDs is in sub-mm/radio and 8-33 micron wavelengths.
- Near-IR contrast is poor, emphasizing the importance of longer wavelengths.

## Abstract

Detection of forming planets means detection of the circumplanetary disk (CPD) in reality, since the planet is still surrounded by a disk at this evolutionary stage. Yet, no comprehensive CPD modeling was done in near-infrared wavelengths, where high contrast imaging is a powerful tool to detect these objects. We combined 3D radiative hydrodynamic simulations of various embedded planets with RADMC-3D radiative transfer post-processing that includes scattering of photons on dust particles. We made synthetic images for VLT NaCo/ERIS in the Ks, L', M' bands as well as examined the spectral energy distributions (SEDs) of disks between 1 $\mu m$ and 10 cm. We found that the observed magnitudes from the planet's vicinity will mostly depend on the CPD parameters, not on the planet's. The CPD is 20-100x brighter than the embedded planet in near-IR. We also show how the CPD parameters, e.g. the dust-to-gas ratio will affect the resulting CPD magnitudes. According to the SEDs, the best contrast ratio between the CPD and circumstellar disks is in sub-mm/radio wavelengths and between 8-33 microns in case if the planet opened a resolvable, deep gap ($\ge 5 \rm{M_{Jup}}$), while the contrast is particularly poor in the near-IR. Hence, to detect the forming planet and its CPD, the best chance today is targeting the sub-mm/radio wavelengths and the 10-micron silicate feature vicinity. In order to estimate the forming planet's mass from the observed brightness, it is necessary to run system specific disk modeling.