Exoplanetology: Exoplanets & Exomoons

Joint Analysis of Multicolor Photometry: A New Approach to Constrain the Nature of Multiple-Star Systems Hosting Exoplanet Candidates

By Keith Cowing

astro-ph.EP

May 19, 2021

Filed under exoplanet

Joint Analysis of Multicolor Photometry: A New Approach to Constrain the Nature of Multiple-Star Systems Hosting Exoplanet Candidates — The first result of SED term derived in Section 4. Top panel for each target : Horizontal axis represents the median wavelength of each passband and vertical axis represents apparent magnitude. The star points are observed values listed in Table 2. The width of the red blurred line represents the Gaussian uncertainties of the Gaia parallax, E(B − V), and the extinction vector. The black dashed lines represent the models that do not include reddening and have widths corresponding to the ±1σ uncertainty of the parallaxes. We list the extinction module in V band, Av and the E(B − V) for each target. Bottom panel for each target : Residual plots from the mean of the models.

We present a new method to assess the properties of transiting planet candidates by multicolor photometry.

By analyzing multicolor transit/eclipse light curves and apparent magnitudes of the target in parallel, this method attempts to identify the nature of the system and provide a quantitative constraint on the properties of unresolved companion(s). We demonstrate our method by observing the six systems hosting candidate transiting planets, identified by the K2 mission (EPIC 206036749, EPIC 206500801, EPIC 210513446, EPIC 211800191, EPIC 220621087, and EPIC 220696233). Applying our analysis code to the six targets, we find that EPIC 206036749, EPIC 210513446, and EPIC 211800191 are likely to be triple-star systems including eclipsing binaries, and EPIC 220696233 is likely a planetary system, albeit further observations are required to confirm the nature.

Additionally, we confirm that the systematic errors in the derived system parameters arising from adopting specific isochrone models and observing instruments (passbands) are relatively small. While this approach alone is not powerful enough to validate or refute planet candidates, the technique allows us to constrain the properties of resolved/unresolved companions, and prioritize the planet candidates for further follow-up observations (e.g., radial-velocity measurements).

Kohei Miyakawa, Teruyuki Hirano, Bun’ei Sato, Akihiko Fukui, Norio Narita

Comments: 17 pages, 5 figures, 6 tables; submitted to AJ
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR)
Cite as: arXiv:2105.08223 [astro-ph.EP] (or arXiv:2105.08223v1 [astro-ph.EP] for this version)
Submission history
From: Kohei Miyakawa
[v1] Tue, 18 May 2021 01:37:14 UTC (5,195 KB)
https://arxiv.org/abs/2105.08223
Astrobiology,

Keith Cowing

Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻

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