GUIbrush®: Characterizing the atmospheres of the new worlds with Python

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GUIbrush® i.e. Characterizing the atmospheres of new worlds with Python Paolo Giacobbe1 & Francesco Amadori1 (1INAF-Osservatorio Astrofisico di Torino, Pino Torinese, Italy.)

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When it all began (?) On 6 October 1995, Michel Mayor and Didier Queloz announced the discovery of a planetary mass object (0.5 times Jupiter) orbiting the solar-type star 51 Peg.

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Indirect detection methods: Radial Velocities

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Indirect detection methods: transits Credits: NASA

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Why study exoplanetary atmospheres? The Holy Grall of an exoplanetologist Biosignatures “..object, substance, and/or pattern whose origin specifically requires a biological agent” (Des Marais and Walter, 1999; Des Marais et al., 2008; Schwieterman et al. 2017)

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Why study exoplanetary atmospheres? ▪We are in the era of comparative exoplanetology ▪Already now we reveal a rich diversity of chemical compositions and atmospheric processes hitherto unseen in the Solar System. ▪The spectrum of an exoplanet reveals the physical, chemical, and biological processes that have shaped its history and govern its future.

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A graphical representation of the Trappist-1 system Credit: NASA/JPL-Caltech/Robert Hurt (IPAC) A C/O > 1 suggest that the planet formed beyond the water snowline and later migrated towards its star at the we observe it today

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Variation of the C/O ratio of the gas in a disc due to freeze-out (Madhusudan 2019, Booth+2017).

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Transmission Spectroscopy for Exoplanet Atmospheres

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Credits: NASA

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Transmission Spectroscopy for Exoplanet Atmospheres Sedaghati et al 2017 Low resolution spectroscopy R < 1000

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Low resolution spectroscopy and hot jupiters Figure from Sing+2016

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Telescopio Nazionale Galileo @ La Palma

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GIANO-B @ TNG - La Palma (Spain) NIR spectrograph mounted at the 3.6-metre Telescopio Nazionale Galileo (TNG). Simultaneous coverage in the 0.92-2.45 µm range (fifty orders ) Spectral resolving power of R = 50,000. Oliva et al. 2006

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At high spectral resolution, molecular features are resolved into a dense forest of of tens of thousands of individual lines in a pattern that it is unique for a given molecule -> a kind of ﬁngerprint High Resolution ( R = 25,000 - 100,000) Transmission Spectroscopy

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The high resolution spectroscopy helps to disentangle and isolate the exoplanet’s spectrum. Disentangle moving planet lines from stationary telluric & stellar lines High Resolution ( R = 25,000 - 100,000) Transmission Spectroscopy Snellen et al. (2010) C - HD209458b

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GUIbrush® Graphic User Interface for Bayesian Retrieval Using Spectroscopy at High Resolution

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Guibrush® is coded in Python > 3.8 THE DEMCMC is parallelized with the Multiprocessing Python library DEMCMC PetitRadTrans: Radiative Transfer Code ~10 sec for one model in the 0.9-2.5 micron range GPU? The goal is a 100x faster code for ANDES/JWST range, 3D models, etc etc

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Bottleneck #1 The Bayesian estimator

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Bottleneck #1 The Bayesian estimator

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Bottleneck #2 The radiative transfer code

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Bottleneck #2 The radiative transfer code

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Radiative equilibrium calculations for HD209458b

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C/O =1

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Are there clouds?

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The “final” matrix for Giano is 102’400 x 60 = 6’144’000 Bottleneck #3 The model reprocessing

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