Simulating Reflected Light Exoplanet Spectra of the Promising Direct Imaging Target, $\upsilon$ Andromedae d, with a New, Fast Sampling Method Using the Planetary Spectrum Generator

TL;DR

This paper introduces a fast, accurate sampling method for simulating reflected light spectra of exoplanets, applied to $$ Andromedae d, demonstrating its potential as a target for future space telescope observations.

Contribution

The paper presents a novel, efficient subsampling technique for exoplanet spectrum simulations and applies it to model $$ Andromedae d, aiding future direct imaging efforts.

Findings

$$ Andromedae d is a promising target for Roman Space Telescope imaging.

The new sampling method is ten times faster than traditional techniques.

Simulated spectra suggest feasible observation times for signal detection.

Abstract

Simulations of exoplanet albedo profiles are key to planning and interpreting future direct imaging observations. In this paper we demonstrate the use of the Planetary Spectrum Generator to produce simulations of reflected light exoplanet spectra. We use PSG to examine multiple issues relevant to all models of directly imaged exoplanet spectra and to produce sample spectra of the bright, nearby exoplanet $\upsilon$ Andromedae d, a potential direct imaging target for next-generation facilities. We introduce a new, fast, and accurate subsampling technique that enables calculations of disk-integrated spectra one order of magnitude faster than Chebyshev-Gauss sampling for moderate- to high-resolution sampling. Using this method and a first-principles-derived atmosphere for $\upsilon$ And d, we simulate phase-dependent spectra for a variety of different potential atmospheric configurations. The simulated spectra for $\upsilon$ And d include versions with different haze and cloud properties. Based on our combined analysis of this planet's orbital parameters, phase-and illumination-appropriate model spectra, and realistic instrument noise parameters, we find that $\upsilon$ And d is a potentially favorable direct imaging and spectroscopy target for the Coronagraph Instrument (CGI) on the Nancy Grace Roman Space Telescope. When a noise model corresponding to the Roman CGI SPC spectroscopy mode is included, PSG predicts the time required to reach a signal-to-noise ratio of 10 of the simulated spectra in both the central wavelength bin of the Roman CGI SPC spectroscopy mode (R=50 spectrum) and of the Band 1 HLC imaging mode is approximately 400 and less than 40 hr, respectively. We also discuss potential pathways to extricating information about the planet and its atmosphere with future observations and find that Roman observations may be able to bound the interior temperature of the planet.