Haze in Exoplanets Atmospheres with BlueMUSE

Valentin D. Ivanov (ESO)

What is an exoplanet?

Exoplanet - planet around another star.

2M1207b (Chauvin et al. 2004)

Direct imaging method: - delivarables: emission spectrum of the planet - exoplanet.eu: 142 planets in 105 systems (5 multi- planet systems) as of Nov 8, 2020

Early „discoveries“ of exoplanets

1952, Obs, 72, 199:

Attn: Selection biases

Batalha (2014)

RV: delivers Mplanet*sin(i); 909 planets in 668 systems (164 multi- planet systems)

Transits: delivers Rplanet, density, transmission spectrum; 3107 planets in 2335 systems (502 multi-planet systems) Photometric transits

First exoplanet transit: d HD209458b – 0.7 MJup, P~3.5 , V=7.65m Charbonneau et al. (2000, ApJ, 529, L45), Henri et al. (2000, ApJ, 529, L41)

Secondary transit (occultation)

Caceres et al. (2011)

Transits

Ortiz et al. (2015) Zheng et al. (2016, 2017) Spectroscopic transits

- WASP-31b - Gibson et al. (2017, MNRAS, 467, 4591) Spectroscopic transits

Spectroscopic transits

Zak et al. (2019) Clouds!

Transits

Target Reference (Telluric standard)

- WASP-31b - Gibson et al. (2017, MNRAS, 467, 4591) Transits

- WASP-31b - Gibson et al. (2017, MNRAS, 467, 4591) WASP-31b - Gibson et al. Transits (2017, MNRAS, 467, 4591)

WASP-39b – an exosaturn with a clear atmosphere; Fischer et al. (2016)

WASP-31b - Gibson et al. Transits (2017, MNRAS, 467, 4591)

ution istrib ize d e ~ s icles l slop part ptica /haze UV-o rosol of ae

WASP-39b – an exosaturn with a clear atmosphere; Fischer et al. (2016)

Transits

- Chemistry of exo-atmospheres („... planets around metal-rich hosts are more likely to have thick refractory clouds...“ - Wakeford et al. 2017): -- left: WASP-39b – an exosaturn with a clear atmosphere; Fischer et al. (2016); WASP- 19b with VLT - Sedaghati, Boffin et al. (2017, Nat, 549, 238),

-- right: GJ436b with HST – Knutson et al. (2013, Nat, 505, 66); WASP_101b (Wakeford et al. 2017) Transits

- Mass-metallicity relation for exoplanets (Wakeford et al. 2017)

IFU – no slit losses

IFU – no slit losses

IFU – no slit losses

eecc ccss aarr ..88 × 22 cc × ssee rrcc 8 aa 22..8

Why BlueMUSE/MUSE? Pros: - UV turns the clouds/haze from foe to friend (together with the much harder mid-IR), we can learn somehting about the exoatmosphere - no slit losses - more efficient than FORS2 - no LADC – the number of moving elements in the light path is smaller than for FORS2

Cons: - limited field of view of 1×1/2x2 arcmin, 6.8×6.8 for FORS2), e.g. only ~10 of the transiting planets have nearby references - multiple spectrographs, so extra systematics - still have a moving path – the derotator - known temperature dependent changes of the MUSE flat field properties, unknwon for BlueMUSE Resources

Catalogs exoplanet.eu; 4374 planets / 3234 planetary systems / 715 multiple planet systems , as of Nov 8, 2020 Database http://nexsci.caltech.edu/ Community analisys and tools: https://exoplanets.nasa.gov/exep/exopag/overview/ - The Exoplanet Exploration Program Analysis Group (ExoPAG) ETD - Exoplanet Transit Database: http://var2.astro.cz/ETD/predictions.php Extrasolar Planet Transit Finder: https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TransitView/nph -visibletbls?dataset=transits K2 photometry, detrended by Andrew Vandenburg, at MAST: https://www.cfa.harvard.edu/~avanderb/k2.html The Exoplanet Handbook, by Michael Perryman: http://hrsbstaff.ednet.ns.ca/jenninj2/Astronomy %2012/Miscellaneous/Projects/Habitability/Perryman,%20Michael %20-%20The%20Exoplanet%20Handbook.pdf Paid addvertisment: ESO pipelines and advanced data products

https://www.eso.org/sci/software/pipelines/

http://archive.eso.org/scienceportal/home