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From Pixels to Population: New tools to understand M dwarf exoplanets
Add to Calendar 2021-09-20T16:10:00 2021-09-20T17:00:00 UTC From Pixels to Population: New tools to understand M dwarf exoplanets
Start DateMon, Sep 20, 2021
12:10 PM
End DateMon, Sep 20, 2021
1:00 PM
Presented By
Shubham Kanodia (PSU)
Event Series: CEHW Seminar

Abstract:  In this talk I will start off by discussing my contribution in the development of the two new radial velocity spectrographs - the Habitable zone Planet Finder (HPF) and NEID. HPF is a near infrared spectrograph that specializes in the search for planets around mid-to-late M dwarfs, while NEID is an optical spectrograph achieving sub m/s precision around G,K, and early M dwarfs. I will discuss how we use these two instruments to follow up on TESS planet candidates around M dwarf hosts. In addition, I've helped develop novel nonparametric tools to model the mass-radius plane for exoplanets. 
Finally, I will briefly discuss plans for future characterization of the M dwarf planetary population using a combination of precise RVs, high dimensional nonparametric techniques, and estimates of TESS occurrence rates for planets orbiting M dwarfs. By simultaneously fitting 4-5 dimensions (planetary mass, radius, period, stellar mass, stellar metallicity, etc.) using these flexible nonparametric methods, we hope to search for trends in the sample that can give clues about the validity of different formation mechanisms. For example: i) simultaneously probing the changes in the radius valley as a function of stellar mass, metallicity, insolation flux, etc., to help distinguish between core powered mass loss and photoevaporation ii) Giant planets orbiting M dwarfs - bridging the gap between the long period RV planets and the short period transiting planets. The former shows a weaker correlation with metallicity that hints at disk instability as a potential formation mechanism. On the contrary, the sample of transiting giant planets around M dwarfs strongly favors the core accretion theory of planet formation.

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