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

Video: https://video.linux.it/w/igKJp9HopEWjsA69zsQTkd?start=57m12s&stop=2h9m45s

Vediamo un progetto basato su Python per il recupero delle proprietà atmosferiche dei pianeti extrasolari, concentrandoci sulle sfide astrofisiche e computazionali.

Dott. Paolo Giacobbe — Ricercatore presso l'Osservatorio Astrofisico di Torino

Transcript

1. GUIbrush® i.e. Characterizing the atmospheres of new worlds with Python Paolo Giacobbe1 & Francesco Amadori1 (1INAF-Osservatorio Astrofisico di Torino, Pino Torinese, Italy.)
2. 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.
3. Indirect detection methods: Radial Velocities
4. Indirect detection methods: transits Credits: NASA
5. 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)
6. 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.
9. 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
10. Variation of the C/O ratio of the gas in a disc due to freeze-out (Madhusudan 2019, Booth+2017).
11. Transmission Spectroscopy for Exoplanet Atmospheres
12. Credits: NASA
13. Transmission Spectroscopy for Exoplanet Atmospheres Sedaghati et al 2017 Low resolution spectroscopy R < 1000
14. Low resolution spectroscopy and hot jupiters Figure from Sing+2016
19. Telescopio Nazionale Galileo @ La Palma
20. 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
22. 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
24. 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
27. GUIbrush® Graphic User Interface for Bayesian Retrieval Using Spectroscopy at High Resolution
28. VS
29. 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
30. Bottleneck #1 The Bayesian estimator
31. Bottleneck #1 The Bayesian estimator
32. Bottleneck #2 The radiative transfer code
33. Bottleneck #2 The radiative transfer code
34. Radiative equilibrium calculations for HD209458b
35. C/O =1
36. Are there clouds?
37. The “final” matrix for Giano is 102’400 x 60 = 6’144’000 Bottleneck #3 The model reprocessing
40. When will the first 'good' news about biosignatures be released?