39 Topic 3: A roadmap towards detecting biomarkers: Earth analogs Earth biomarkers: detecting towards roadmap A 3: Topic system the contextualize and noise spurious avoid to star the understanding and modeling characterization: exoplanet in sources background as spectra Stellar 2: Topic spectroscopy resolution low- with synergy its and resolution spectral high at exoplanets of characterization Atmospheric 1: Topic 17:50 17:20 17:00 16:40 16:20 16:00 15:30 15:10 14:50 14:30 14:00 12:20 11:50 11:30 11:00 10:40 10:20 09:50 09:30 End of day of End Discussion Bourrier Yan Keles Pino Coffee Bean Jenkins Mcintyre (invited) Meadows hall the in Lunch Discussion Schwarz Coffee Hoeijmakers Rauscher (invited) Snellen Intro Monday 17:50 17:20 17:00 16:40 16:20 15:50 15:20 15:00 14:40 14:20 14:00 12:20 11:50 11:30 11:00 10:40 10:20 10:00 09:30 End of day of End Discussion Rugheimer Desert Zhao (invited) Lovis Coffee Desiderà Burt Malavolta Nortmann hall the in Lunch Discussion Wilson Coffee Brogi & Chiavassa Dravins Fortney (invited) Collet Tuesday 12:20 12:00 11:40 11:20 11:00 10:30 10:10 09:50 09:30 09:00 Lunch pack Lunch Discussion Casasayas-Barris Chen Machado (invited) Line Coffee Poretti Dumusque (invited) Haywood Wednesday 19:30 17:50 17:20 17:00 16:40 16:20 16:00 15:30 15:10 14:50 14:30 14:00 12:40 12:10 11:50 11:30 11:00 10:30 10:10 09:50 09:30 Social dinner Social day of End Discussion Komacek Gonçalves Wang Gopinathan Coffee Birkby Palle confirmed) be (to Santos (invited) Sousa-Silva hall the in Lunch Discussion Guilluy Allart (invited) Kempton Coffee Espinoza Molaverdikhani Alonso-Floriano Thursday 12:00 11:40 11:20 11:00 10:40 10:20 10:00 09:30 Discussion Molliere Garcia-Mejia Vigan Coffee Wyttenbach Crossfield (invited) Donati Friday Monday Speaker Title 09:30 Introduction 09:50 Ignas Snellen (invited) Techniques of high-dispersion spectroscopy for exoplanet characterization 10:20 Emily Rauscher Detecting Doppler signatures of winds and rotation in high-resolution spectra using direct predictions from 3D circulation models 10:40 Jens Hoeijmakers Discovery of iron and titanium in the atmosphere of an ultra-hot Jupiter 11:00 Coffee 11:30 Henriette Schwarz Spinning Worlds - The rotation of young gas giants and brown dwarf companions 11:50 Discussion

12:20 Lunch in the hall

14:00 Victoria Meadows (invited) The Search for Life Beyond the Solar System: Prospects for High-Resolution Spectroscopy 14:30 Sarah Mcintyre Multi-Parameter Approach to Habitability (M-PAtH) 14:50 James Jenkins Searching for the atmosphere of the habitable zone rocky planet LHS1140b 15:10 Jacob Bean Comparative exoplanetology in era of the Great Observatories, JWST, and beyond 15:30 Coffee 16:00 Lorenzo Pino A global view of the atmosphere of hot Jupiters: combining low- to high-resolution transmission spectroscopy 16:20 Engin Keles Detection of Potassium in the exoplanet atmosphere of HD189733b using high resolution spectroscopy 16:40 Fei Yan An extended hydrogen envelope of the hottest exoplanet KELT-9b 17:00 Vincent Bourrier Warm Neptunes : a sweet spot for atmospheric characterization 17:20 Discussion

Tuesday Speaker Title 09:30 Remo Collet (invited) Three-dimensional model stellar atmospheres and spectra of solar- and late-type stars 10:00 Jonathan Fortney Constraints on Giant Planet Atmospheres and Formation From Structure Models and Stellar Abundances 10:20 Dainis Dravins Stellar atmospheres behind transiting exoplanets 10:40 A. Chiavassa & M. Brogi Synergy between stellar physics and planetology, a pathway for high-resolution spectroscopy of exoplanet atmospher 11:00 Coffee 11:30 Paul Wilson Signs of the Beta Pictoris b Hill Sphere Transit? 11:50 Discussion

12:20 Lunch in the hall

14:00 Lisa Nortmann High-resolution studies of the He I absorption feature in multiple planets 14:20 Luca Malavolta GAPS2: the origin of planetary systems diversity 14:40 Jennifer Burt RVxK2: Simultaneous PRV Program with Kepler/K2 Campaign 16 15:00 Daria Desidera' Exploiting the potential of Low-Resolution spectrophotometry to characterize exoplanetary atmospheres 15:20 Coffee 15:50 Christophe Lovis (invited) Towards the characterization of Earth analogs with high-resolution spectroscopy 16:20 Lily Zhao EXPRES, the Extreme Precision Spectrograph 16:40 Jean-Michel Desert Combining low and high resolution spectroscopy to retrieve atmospheric metallicities of giant exoplanets 17:00 Sarah Rugheimer Detecting Biosignatures and Pre-Biosignatures in the Atmospheres of Earth-like Planets Around Other Stars 17:20 Discussion

Wednesday Speaker Title 09:00 Raphaelle Haywood (invited) Identifying and modelling the signatures of magnetic activity from Sun-like stars in exoplanet observations 09:30 Xavier Dumusque Boosting or mitigating the stellar activity signal in high-resolution spectroscopy 09:50 Ennio Poretti The use of TNG facilities in the study of exoplanetary atmospheres 10:10 Coffee 10:30 Michael Line (invited) Retrieving Exoplanet Atmosphere Properties from High Dispersion Cross-Correlation Spectroscopy 11:00 Pedro Machado Comparative study of circulation regimes of terrestrial planets’ atmospheres 11:20 Guo Chen Characterization of multiple alkali metals in the atmosphere of the super-Neptune WASP-127b 11:40 Nuria Casasayas-Barris Na I and Ha absorption features in the atmosphere of MASCARA-2b/KELT-20b 12:00 Discussion

12:20 Lunch pack

Thursday Speaker Title 09:30 Francisco Javier Alonso-Floriano Simultaneous detection of the water bands at 1.14 and 1.40 microns on the transmission spectrum of HD 189733 b using CARMENES 09:50 Karan Molaverdikhani A new classification scheme based on water/methane dominancy in the atmospheric spectra of irradiated planets 10:10 Nestor Espinoza Unveiling exoplanet atmospheres with the ACCESS survey 10:30 Coffee Synergy between stellar physics and planetology, a pathway for high-resolution spectroscopy of exoplanet atmospher 11:00 Eliza Kempton (invited) Modeling Exoplanet Atmospheres at High Spectral Resolution 11:30 Romain Allart Resolved helium absorption signature from the extended atmosphere of the warm Neptune HAT-P-11b 11:50 Gloria Guilluy Detection of water vapor in the dayside spectrum of the non-transiting gas giant HD102195b with GIANO 12:10 Discussion

12:40 Lunch in the hall

14:00 Clara Sousa-Silva (invited) Molecular Simulations for the Spectroscopic Detection of Atmospheric Gases 14:30 Nuno Santos (to be confirmed) Reflections from other worlds 14:50 Enric Palle HIRES: A planet-characterizer high-resolution spectrograph for the ELT 15:10 Jayne Birkby Enabling precise C/O ratios from high resolution spectroscopy: the MMT Exoplanet Atmosphere SURvEy (MEASURE) 15:30 Coffee 16:00 Sreejith Aickara Gopinathan CUTE CubeSat Mission 16:20 Ji Wang Detecting water in HR 8799 c with L band high dispersion spectroscopy 16:40 Ruben Goncalves Venus’ cloud top wind measurements with TNG/HARPS-N and coordinated Akatsuki observations 17:00 Thaddeus Komacek Constraining the drag mechanism in hot Jupiter atmospheres using a heat engine approach 17:30 Discussion

19:30 Social event

Friday Speaker Title 09:30 Jean-Francois Donati (invited) Filtering stellar activity with Doppler tomography and spectropolarimetry 10:00 Ian Crossfield Isotopes in M dwarfs: 13CO 10:20 Aurelien Wyttenbach Observations of sodium in exoplanet atmospheres 10:40 Coffee 11:00 Arthur Vigan HiRISE: Bringing high-spectral resolution to VLT/SPHERE 11:20 Juliana Garcia-Mejia A Fabry Perot Based Instrument for Biomarker detection 11:40 Paul Molliere Detecting Isotopologues in Exoplanet Atmospheres 12:00 Discussion 39 Techniques of high-dispersion spectroscopy for exoplanet characterization

1 Ignas Snellen⇤†

1Leiden University – Netherlands

Abstract

In this talk I will review the di↵erent techniques and methods for exoplanet characteriza- tion, show some of the highlights and early attempts. I will also try to pose some questions about possible avenues to improve the methods in the next years/decades.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:222731 Detecting Doppler signatures of winds and rotation in high-resolution spectra using direct predictions from 3D circulation models

1 2 3 4 Emily Rauscher⇤ , Erin Flowers , Matteo Brogi , Andrea Chiavassa , and Eliza Kempton5

1University of Michigan [Ann Arbor] – 500 Church Street Ann Arbor, MI 48109-1090, United States 2Princeton University – Princeton, NJ 08544 USA, United States 3University of Warwick [Coventry] – Coventry CV4 7AL, United Kingdom 4Observatoire de la Cˆote dAzur´ (OCA) – Centre National de la Recherche Scientifique : UMS2202 – B.P. 4229 06304 Nice Cedex 4, France 5University of Maryland [College Park] – College Park, MD 20742, United States

Abstract

The atmospheres of hot Jupiters move very quickly; both the wind speeds and the ro- tational velocities are on the order of kilometers per second. This means that Doppler signatures of these atmospheric motions appear in high-resolution spectra. Previous work has been able to constrain wind speeds and rotation rates from high-resolution measurements of exoplanets, by applying ad hoc Doppler shifts and/or broadening to the template spectra used to fit the data. However, the rotation rate of a planet strongly influences its atmospheric circulation pattern, meaning that the winds and rotation are not independent of each other. We present a more consistent analysis of Doppler signatures in high-resolution transmission spectra of HD 189733b by directly using spectra predicted from three-dimensional circulation models as the template spectra for extracting the planet’s signal. We test models of this planet with a range of rotation rates, as well as di↵erent assumptions about its atmospheric abundances. In the first analysis of its kind, where the atmospheric velocities are completely determined by the circulation model, we are able to significantly detect the planet’s spectrum and also consistently constrain its rotation rate and wind speeds.

⇤Speaker

sciencesconf.org:horse:222155 Discovery of iron and titanium in the atmosphere of an ultra-hot Jupiter

1,2 Jens Hoeijmakers⇤

1Center for Space and Habitability (CSH) – University of Bern, Hochschulstrasse 4, 3012 Bern, Switzerland 2Observatoire Astronomique de lUniversit´ede´ Gen`eve (ObsGE) – chemin des Maillettes CH-1290 Sauverny, Switzerland

Abstract

Kelt-9 b orbits its hot A-type host star at a distance of only three stellar radii. In this environment, it is the hottest exoplanet known to date; with an equilibrium temper- ature around 4,000K. In Kitzmann et al. 2018 we predicted that under such conditions, most species in the atmo- sphere of Kelt-9 b should be atomic, and that there should be no more than trace amounts of molecules and no aerosols. In this sense, the atmosphere may resemble that of a K-dwarf stellar photosphere, and this motivated our search for the presence of iron and titanium - the strongest line absorbers in the photospheres of cool dwarf stars. With this talk I will present our discovery of ionized and neutral iron, and ionized titanium in the atmosphere of Kelt-9 b at high confidence, using the high resolution cross-correlation technique applied to transit transmission spectra by the HARPS-North spectrograph. Excitingly, because these detections are so strong and free from masking by clouds/aerosols, through the line ratio’s they will enable us to determine the chemical abundance ratio’s and metallicity, while the high spectral resolution delivers a precise absolute measurement of the planet’s orbital velocity. In addition we are exploring the possibility of using these detections for constraining the atmospheric ionization structure and velocity profile; and I will provide an update on this exciting analysis.

⇤Speaker

sciencesconf.org:horse:222067 Spinning Worlds - The rotation of young gas giants and brown dwarf companions

1 Henriette Schwarz⇤†

1University of California, Santa Cruz (UCSC) – UC SANTA CRUZ, 1156 HIGH STREET, SANTA CRUZ, CA 95064, United States

Abstract

I present rotation measurements of directly imaged planets and brown dwarf companions, measured from the Doppler broadening of the spectral lines. The rotation influences weather and climate, temperature distribution, chemical mixing, and the magnetic field. More than that, the planetary spin is the result of accretion of angular momentum during the formation, and observing planetary spin rates may promote our understanding of the accretion process or even help di↵erentiate between opposing formation scenarios. The observed targets span a range of masses, ages and orbital distances, providing the first opportunity to compare the spin parameters of young exoplanets and brown dwarf companions. Although the observed sample is small, we do see a correlation of spin velocity with age, which we interpret as due to the youngest objects still accreting angular momentum and spinning up through subsequent cooling and contraction.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:222043 The Search for Life Beyond the Solar System: Prospects for High-Resolution Spectroscopy

1,2,3 Victoria Meadows⇤

1University of Washington – University of Washington SEATTLE, United States 2Astrobiology Center, The National Institutes of Natural Sciences (ABC-NINS) – AstroBiology Center, NINS. 181 - 8588 2-21-1 Osawa Mitaka-shi, Tokyo, within the National Astronomical Observatory, Japan 3NASA Nexus for Exoplanet System Science (NExSS) – United States

Abstract

Recently discovered exoplanets, especially those orbiting nearby M dwarfs, will provide intriguing near-term targets for JWST and ground-based telescopes to engage in the search for habitable environments and life beyond our Solar System. Although plentiful, M dwarf planets experience star-planet interactions that likely drive planetary evolutionary processes di↵erent to those experienced by Earth, which could complicate the search for life on these planets. This review will describe new, comprehensive frameworks that are being developed for planetary target selection and biosignature assessment. Components of these frameworks include identification of potential false negatives – planetary or stellar phenomena that sup- press life’s impact on an environment and make it harder to detect, and false positives – planetary or stellar phenomena that mimic the signs of life. These comprehensive frame- works for biosignature assessment in the context of the planetary environment will increase the probability that we will be able to detect, and more confidently identify, those planetary environmental characteristics that are due to life. Specific applications for upcoming high- resolution spectroscopy capabilities will be discussed, including key desired measurements for habitability and biosignature searches for both transmission and reflected light spectra.

⇤Speaker

sciencesconf.org:horse:222099 Multi-Parameter Approach to Habitability (M-PAtH)

1 Sarah Mcintyre⇤

1Australian National University (ANU) – The Australian National University Canberra ACT 0200 Australia, Australia

Abstract

We are standing on the cusp of a major discovery in planetary sciences. For the first time in human history, upcoming surveys and telescopes working together will be able to remotely detect potential biosignatures in exo-Earth atmospheres and discover signs of life beyond our Solar System. The conviction that biosignatures will be detected by remote sensing from space telescopes is moderated by current time limitations and observational opportunities. Unfortunately, none of the new space- and ground-telescopes will be solely dedicated to the characterization of exoplanet atmospheres. In order to make the most of the limited ob- servational resources available, optimal target selection will be of the utmost importance. Selection of targets for this characterisation relies on ambiguously defined concepts of hab- itability, which are currently constrained by only the density of the planet and the distance from its host star. With the expected increase in the number of detected exoplanets from TESS, we might end up with hundreds of planets that suit these criteria and are accordingly all equally likely to host life. Therefore, it is imperative that we rethink our classification of what makes a planet habitable. Until recently, we have defined a ‘habitable world’ as a rocky body with enough surface gravity to sustain an atmosphere, which orbits its host star at a distance where the stellar radiation is suitable for the presence of surface liquid water. However, there are numerous planetary and astronomical factors that could influence an exoplanets ability to maintain liquid water. The majority of our assessments on habitability stems from what we have observed in our own solar system. One of the di↵erences amongst the terrestrial planets in our solar system is the presence of a strong magnetic dipole moment on Earth that protects the surface and shields liquid water from solar winds and flares. It is postulated that plan- etary magnetism has a significant e↵ect on the long-term maintenance of atmosphere, and subsequently liquid water, on an exoplanet. To determine which of the currently detected exoplanets would have a magnetosphere that could provide protection from cosmic and stel- lar irradiation, we used Olsen & Christiensen’s (2006) model to determine the maximum magnetic dipole moment of terrestrial exoplanets, further analysing those located in the Cir- cumstellar Habitable Zone (CHZ). Our results indicate that 17% of potentially habitable exoplanets (subterran/terran planets located in the CHZ) from our sample, even when mod- elled based on the best-case scenario - modelling the maximum dipole moment and taking the upper uncertainty limit - would not have a magnetic moment that would prevent loss of atmosphere, and subsequent loss of liquid water, due to stellar and cosmic irradiation. This evidence would suggest that the CHZ might not be the ”liquid water zone” that we have thought so far.

⇤Speaker

sciencesconf.org:horse:221235 Continuing to expand to a multi-parameter approach to habitability (M-PAtH) by including factors such as magnetic field, albedo, stellar type, orbit characteristics, tidal locking, impact events, and plate tectonics, will enable us to prioritize planets most likely to maintain liquid water. By analysing, modelling and constraining how these factors interact on any given planetary body, we can generate a flexible framework for prioritisation that involves multi- ple observable characteristics and features that influence continuous planetary habitability. Based on the results, we will be able to provide a revised model of planetary habitability and suggest a suitable strategy for future astrobiological and biosignature observations of life in the universe. In conjunction with the rapidly increasing information from exoplanet databases expected within the next 2 years, this research will help determine optimal targets for near-future ground- and space-based spectroscopic observations of planetary atmospheres and the potential detection of life in space. Olson, P., & Christensen, U. R. (2006). Dipole moment scaling for convection-driven plane- tary dynamos. Earth and Planetary Science Letters, 250(3-4), 561-571. Searching for the atmosphere of the habitable zone rocky planet LHS1140b

1 James Jenkins⇤

1Universidad de Chile – Av. Libertador Bernardo O’Higgins 1058, Santiago de Chile, Chile

Abstract

Understanding the atmospheric physical processes and chemistries of rocky planets orbit- ing distant stars can reveal the true nature of the population of planets in the galaxy, from their formation mechanisms to their subsequent evolution. Such research is at the fore-front of modern astrophysics. In particular, the so called super-Earth planets are as yet not well understood. On one hand they could be gas dominated (mini-Neptunes) or on the other hand they can be core dominated, rocky planets like the Earth. When that planet turns out to be an exo-Earth orbiting in the Habitable Zone (HZ) of a nearby star, the study of its atmosphere takes on even greater importance, since these worlds may be the nearest hosts to exolife that we can study in the foreseeable future. I will present a search for the atmosphere of the newly discovered habitable zone planet LHS1140b. I will discuss our observations of the transit from the optical to the near-infrared (GROND, SOFI, and HAWK-I), with the overall aim of searching for evidence of the planet’s atmosphere. I will introduce our new observational methods and Gaussian Process modeling techniques that we have been apply- ing in this work. Finally, I will conclude with the optical and near-infrared transmission spectrum for the planet and discuss the impact of these results in relation to the current ensemble of small planet atmospheric studies that have been performed.

⇤Speaker

sciencesconf.org:horse:210731 Comparative exoplanetology in era of the Great Observatories, JWST, and beyond

1 Jacob Bean⇤

1University of Chicago – United States

Abstract

Transiting exoplanet spectroscopy from space is highly complementary to ground-based, high-resolution observations because the former uniquely retains information about the planet’s broadband continuum. I will present a summary of new results from large surveys of exoplanet atmospheres using the Hubble and Spitzer Space Telescopes, with an empha- sis on results that are the most relevant for exploring the connection between ground- and space-based data. Building on these results, and anticipating discoveries from TESS and other transit detection experiments, I will discuss the likely exoplanet atmosphere science objectives in the JWST era. I will conclude with a look ahead at the potential synergies between ground-based observations and the ARIEL mission.

⇤Speaker

sciencesconf.org:horse:221469 A global view of the atmosphere of hot Jupiters: combining low- to high-resolution transmission spectroscopy

1 2 3 4 Lorenzo Pino⇤† , David Ehrenreich , Aur´elien Wyttenbach , Vincent Bourrier , Valerio Nascimbeni5, Kevin Heng6, Simon Grimm6, Christophe Lovis7, Matej Malik6, Francesco Pepe4, Giampaolo Piotto5, and Matteo Brogi8

1Astronomical Institute Anton Pannekoek (AI PANNEKOEK) – PO Box 94249, 1090 GE Amsterdam, Netherlands 2University of Geneva – 51, chemin des Maillettes 1290 Sauverny, Switzerland 3Leiden Observatory, Leiden University – P.O. Box 9513 2300 RA Leiden, Netherlands 4Observatoire de Geneve – Switzerland 5Universit`adi Padova - DFA – Italy 6University of Bern, Center for Space and Habitability (CSH) – Sidlerstrasse 5, CH-3012, Bern, Switzerland, Switzerland 7Observatoire de l’Universit´ede Gen`eve – Chemin des Maillettes 51, Sauverny, CH-1290 Versoix, Switzerland 8University of Warwick [Coventry] – Coventry CV4 7AL, United Kingdom

Abstract

Combining all transit spectroscopy data sets available from the optical to the near-infrared (NIR) for one of the most iconic exoplanets, the hot Jupiter HD189733b, reveals the domi- nance of scattering by aerosols layers, above which a damped water band arises in the NIR and the sodium doublet reaches high altitudes in the thermosphere, as seen in the optical. Only high thermospheric temperatures (up to 10,000 K) or supersolar sodium abundance can explain the deep absorption in the cores of the sodium lines in the presence of aerosols. I will present the PyETA code for comparing synthetic transmission spectra to observa- tions from di↵erent instruments (ground-based or space-borne, resolving powers from 10ˆ2 to 10ˆ5), which I employed to obtain these results. By using PyETA models, I will also illustrate a novel technique to characterize aerosols with simultaneous the optical to near- infrared coverage of new generation, high-resolution spectrographs (GIARPS: HARPS-N + GIANO, CARMENES, ESPRESSO, CRIRES+,...), which opens new perspectives for the characterization of exoplanetary atmospheres.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:221117 Detection of Potassium in the exoplanet atmosphere of HD189733b using high resolution spectroscopy

1 1 1 1 Engin Keles⇤ , Matthias Mallonn† , Thorsten Carroll‡ , Klaus Strassmeier§ , Ilya 1 1 Ilyin¶ , and Xanthippi Alexoudik

1Leibniz-Institut f¨ur Astrophysik Potsdam (AIP) – An der Sternwarte 16, 14482 Potsdam, Germany

Abstract

To characterize exoplanetary atmospheres, transmission spectroscopy is one of the most successfully used techniques. This technique provides the possibility of investigating the presence of constituents within the atmospheres of hot Jupiters. Several works presented the detection of specific alkali atoms in exoplanetary atmospheres creating excess absorption curves i.e. where in- and out- of- transit data are used to show an increased absorption in the line during transit. In this work we present high resolution transit observations of the exoplanet HD189733b, using the 2 x 8.4m Large Binocular Telescope and the Potsdam Echelle´ Polarimetric and Spectroscopic Instrument (PEPSI). We investigate the potassium excess absorption at 7698.98A˚ after correcting for telluric line contamination and center-to- limb variation and show the first high-resolution potassium detection in the atmosphere of HD189733b.

⇤Speaker †Corresponding author: [email protected] ‡Corresponding author: [email protected] §Corresponding author: [email protected] ¶Corresponding author: [email protected] kCorresponding author: [email protected]

sciencesconf.org:horse:220523 An extended hydrogen envelope of the hottest exoplanet KELT-9b

1 1 Fei Yan⇤† and Thomas Henning

1MPIA – K¨onigstuhl 17, Heidelberg, Germany

Abstract

With a dayside temperature of ˜ 4600 K, KELT-9b is the hottest exoplanet known so far. It is particularly interesting to study its atmosphere as the planet receives immense stellar irradiation from its host A0-type star. We have detected an extended hot hydrogen atmosphere around KELT-9b. The detection was achieved by measuring the atomic hydrogen absorption during transit with the Balmer H↵ line using the CARMENES spectrograph. The obtained H↵ transmission spectrum has a strong extra absorption of 1.15% at the line centre. The observation implies that the e↵ective radius at the line centre is 1.64 times the size of the planetary radius, indicating the planet has a largely extended hydrogen⇠ envelope close to the size of the Roche lobe and is probably undergoing dramatic atmosphere escape. We also detected a significant wavelength shift of the H↵ absorption which is mostly attributed to the planetary orbital motion.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:219956 Warm Neptunes : a sweet spot for atmospheric characterization

1 Vincent Bourrier⇤

1Observatoire de Geneve – Switzerland

Abstract

Observations of exoplanets during the transit of their host star allow us to probe the structure and composition of their atmospheres. The intense stellar energy input into ex- oplanets on short orbits can lead to a dramatic expansion of their upper atmosphere, and the loss of massive amounts of gas escaping into space. Recently, spectrally-resolved UV observations of the warm Neptune GJ436b with the Hubble Space Telescope revealed the largest atmospheric structure ever detected, a tail of hydrogen extending over more than 10 millions of km. This discovery raised questions as to the origin and continued existence of low-mass planets like GJ436b at the fringes of the Neptunian desert of close-in planets. I will shed new light on these questions thanks to the discovery of a giant hydrogen exosphere around another warm Neptune bordering the desert, GJ3470b. Its atmosphere occults up to 35% of the star at Lyman-alpha wavelengths. Analyzing the Doppler shift of the atmo- spheric absorption signature, temporally and spectrally resolved over the transit, allows us to determine the spatial and dynamical structure of the hydrogen gas escaping the planet. GJ436b and GJ3470b display striking di↵erences, and I will show how the high-energy envi- ronment of their M dwarf host stars shapes their upper atmosphere and a↵ect the planets’ evolution. These detections show that much larger atmospheric signals can be retrieved from the upper atmosphere of moderately irradiated, low-mass planets. Many such systems will be discovered in the coming years by transit (TESS, CHEOPS, PLATO) and velocimetry (CARMENES, ESPRESSO, SPIRou, NIRPS) surveys, and the development of new tracers of atmospheric escape like helium at infrared wavelengths o↵ers thrilling perspectives for their characterization with high-resolution ground-based spectrographs.

⇤Speaker

sciencesconf.org:horse:218948 Three-dimensional model stellar atmospheres and spectra of solar- and late-type stars

1 Remo Collet⇤†

1Stellar Astrophysics Centre, Aarhus University – Denmark

Abstract

I will review the results from recent realistic, time-dependent, three-dimensional radiation- hydrodynamics simulations of convection at the surface of solar- and late-type stars with applications to the modelling of stellar atmospheres and spectra. I will highlight the main structural properties of such simulations and their most important di↵erences with respect to classical stationary, one-dimensional hydrostatic model stellar atmospheres. I will discuss the impact of three-dimensional simulations on the modelling of the emergent spectral en- ergy distributions. I will focus in particular on the simulations’ predictions of the spatial and temporal properties of stellar granulation, of the strengths, asymmetries and wavelength shifts of spectral lines, and of the centre-to-limb intensity variations at the stellar surface. Finally, I will discuss applications of three-dimensional model stellar atmospheres to the de- termination of stellar parameters and compositions as well as to the analysis of exoplanet transits and exoplanet characterisation.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:223002 Constraints on Giant Planet Atmospheres and Formation From Structure Models and Stellar Abundances

1 2 3 Jonathan Fortney⇤ , Johanna Teske , and Daniel Thorngren

1University of California [Santa Cruz] (UCSC) – 1156 High Street, Santa Cruz, Ca 95064, United States 2Cargenie Institution for Science – United States 3UC-Santa Cruz – United States

Abstract

Since giant planets are thought to be fully convective, the abundances and metal enrich- ment of their entire H/He envelope can be observed in their visible atmospheres. We can observe these abundances via spectroscopy, but we can also constrain the overall enrichment by comparing a planet’s bulk density to those from a range of structure models. In this contribution I will show recent work on the transiting planet mass-metallicity relation for giant planets, which is a key prediction of core-accretion planet formation. We find that this relation depends strongly on planet mass but, curiously, does not appear to depend on parent star metallicity - metal rich stars do not seem to make metal-rich planets. To further pursue and quantify this e↵ect we have obtained new high-precision spectra and derived stel- lar abundances for ”planet-forming elements” like, O, C, Fe, Mg, and Si for ˜25 transiting giant planet host stars. When combining these stellar abundances with planetary structure models, we see tentative evidence that the most metal-rich planets are actually around stars that have a high ratio of volatiles (C and O) to refractories, independent of total stellar metallicity. Finally we show how structure models can be used to place firm upper limits at planetary atmospheric metallicity, which can guide current and future atmospheric retrieval studies of these atmospheres.

⇤Speaker

sciencesconf.org:horse:221476 Stellar atmospheres behind transiting exoplanets

1 2 Dainis Dravins⇤† and Hans-G¨unter Ludwig

1Lund Observatory – Box 43, SE-221 00 Lund, Sweden, Sweden 2Zentrum f¨ur Astronomie der Universit¨atHeidelberg (ZAH) – Germany

Abstract

Atmospheric studies of transiting exoplanets require stellar background spectra to be known along the transit path while detection of ”true” Earth analogs require stellar mi- crovariability to be well understood. Hydrodynamic modeling of stellar atmospheres is feasi- ble for various stars but such models and their ensuing spectra could in the past be tested in detail only for the Sun with its resolved surface features. Using exoplanet transits, such spa- tially resolved spectroscopy can be extended to also other stars. During a transit, successive stellar surface portions become hidden and di↵erential spectroscopy between various transit phases provide spectra of small surface segments temporarily hidden behind the planet [1]. Such retrievals of spatially resolved high-resolution photospheric line profiles have now been achieved along the exoplanet transit chords across HD209458 (G0 V) and HD189733A (K1 V), using data from the ESO UVES and HARPS spectrometers [2,3]. A challenge in finding ”truly” Earth-like planets lies in understanding stellar microvariabil- ity in radial velocity and photometric irradiance. Some calibration should be possible by correlating fluctuations in irradiance with simultaneous changes in radial velocity. This may become feasible from hydrodynamic models, which may be verified from observed center-to- limb changes in stellar photospheric line profiles.

Since even giant planets cover only a tiny fraction of any solar-type star, the directly ob- servable signal is small and extremely precise observations are required. To reach adequate signal-to-noise ratios, further requires averaging over numerous lines with similar parame- ters. However, the method will likely be applicable to several more stars in the near future, as new targets are being found by ongoing searches for bright host stars with transiting large planets.

Dravins, D., Ludwig, H.-G., Dahl´en, E., & Pazira, H. 2017a, A&A, 605, A90

Dravins, D., Ludwig, H.-G., Dahl´en, E., & Pazira, H. 2017b, A&A, 605, A91 Dravins, D., Gustavsson, M. & Ludwig, H.-G. 2018, A&A, submitted

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:200147 Synergy between stellar physics and planetology, a pathway for high-resolution spectroscopy of exoplanet atmosphere

1 2 Andrea Chiavassa⇤† and Matteo Brogi

1lagrange – Observatoire de la Cote d’Azur – France 2Univerisity of Warwick – United Kingdom

Abstract

Progress with high-resolution spectroscopy with ground-based instruments has led to de- tections of atomic and molecular species in the atmospheres of hot giant exoplanets. The advent of high-resolution spectrographs at large and medium-size facilities will extend the sample of exoplanet atmospheres that can be targeted with this technique towards cooler and smaller planets.

However, stars are not smooth and have a convective envelope. Their photospheres are covered with a pattern associated with convective heat transport (i.e., granulation). The convection-related structures have di↵erent sizes, depth and temporal variations compared to the stellar type concerned. Convection is a dicult process to understand because it is nonlocal, and three-dimensional, and it involves nonlinear interactions over many disparate length scales. To account for the complex physics behind, nowadays we compute numerical 3D radiative hydrodynamical simulations of stellar convection that cover a substantial por- tion of the Hertzsprung-Russell diagram. With this tool at hand, we aim to quantify and eliminate stellar noise in high resolution spectra coming from both convective motion and from the transit geometry of exoplanets, i.e. the occultation of a portion of a rotating stellar surface leading to Rossiter-McLaughlin e↵ect and center-to-limb variations. Accounting for these sources of noise will allow us to secure unambiguous detections of chemical species in exoplanet atmospheres, while at the same time deriving fundamental property about the mutual planet/star spins, planetary winds, and the dynamics at the surface of the host stars.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:221185 Signs of the Pictoris b Hill Sphere Transit?

1 Paul Wilson⇤

1WARWICK UNIVERSITY – United Kingdom

Abstract

The Hill sphere of the directly-imaged planet beta Pictoris b recently transited its host star resulting in the first opportunity for astronomers to study the circumplanetary environ- ment of a young ( ˜23 Myr) exoplanet. The rarity of such a unique event combined with the knowledge that the next transit will not happen for another ˜23 years spurred the astron- omy community to obtain a cascade of new beta Pic observations using some of the worlds largest telescopes (e.g. HST, VLT and SALT) and lead to the creation of dedicated beta Pic telescopes (e.g. bRING, PICSAT). In this talk I will introduce the beta Pic system and report on our observational e↵orts aimed at observing the Hill sphere transit. The talk will focus on the results of a 27 orbit HST observing campaign of beta Pic in the far-UV. I will present the variable emission and absorption signatures seen in the data and discuss their potential relationship with the Hill sphere transit.

⇤Speaker

sciencesconf.org:horse:221220 High-resolution studies of the He I absorption feature in multiple planets

1 2 Lisa Nortmann⇤ and Carmenes Exoplanet Atmospheres Working Group

1Instituto de Astrof´ısica de Canarias (IAC) – Calle V´ıa L´actea, s/n, 38205 San Crist´obal de La Laguna, Santa Cruz de Tenerife, Spain 2Instituto de Astrofisica de Canarias (IAC) – Calle V´ıa L´actea, s/n, 38205 San Crist´obal de La Laguna, Santa Cruz de Tenerife, Spain

Abstract

We discuss the study of the He I feature obtained for several exoplanets observed at high resolution with CARMENES (Calar Alto high-Resolution search for M dwarfs with Exoearths with Nearinfrared and optical Echelle Spectrographs).

⇤Speaker

sciencesconf.org:horse:222064 GAPS2: the origin of planetary systems diversity

1,2 Luca Malavolta⇤

1Dipartimento di Fisica e Astronomia, Universit`adi Padova (DFA - UniPD) – Vicolo dell’Osservatorio 3 35121 - Padova (PD), Italy 2INAF - Osservatorio Astronomico di Padova (OAPD) – Vicolo dellOsservatorio,´ 5, 35122 Padova, Italy

Abstract

After the successful Global Architecture of Planetary Systems (GAPS) project, the Ital- ian exoplanet community has gathered together again to exploit the unique capabilities of GIARPS (GIANO+HARPS-N) at the Telescopio Nazionale Galileo (La Palma), with a par- ticular focus on the training of young researchers. In GAPS2 we shift our focus from the detection and characterization of planets to the study of the origin of planetary systems.

We will investigate migration mechanisms by looking for planets around young (< 0.1 Gyr) and intermediate-age (< 0.7 Gyr) stars, thanks to the improved characterization of stellar activity and planetary signals provided by simultaneous GIANO (NIR) and HARPS- N (VIS) observations in GIARPS mode. We will trace the original formation site and path to migration of planets by looking for sodium (VIS), water, titanium monoxide (VIS/NIR), and other molecules (NIR) in the atmospheres of the largest sample of hot transiting planets to date. In this talk I will focus on the exoplanet atmosphere characterization within the GAPS2 project. I will describe the target selection, observational strategy, and data analysis tools that will allow us to reach the ambitious goals of GAPS2. I will dedicate the last part of the talk to introduce the Spectral Lines Of Planets with python (SLOPpy) pipeline for automatic, homogeneous, and reproducible extraction of transmission spectra at high-resolution.

⇤Speaker

sciencesconf.org:horse:221751 RVxK2: Simultaneous PRV Program with Kepler/K2 Campaign 16

1 2 3 Jennifer Burt⇤† ,SharonWang, and Johanna Teske

1MIT Kavli Institute for Astrophysics and Space Research – 70 Vassar Street, Cambridge, MA 02139, USA, United States 2Department of Terrestrial Magnetism [Carnegie Institution] – Washington, DC, United States 3Observatories [Carnegie Institution] – Pasadena, California, United States

Abstract

We present the RVxK2 program which combines K2 Campaign 16 photometry with simul- taneous precise radial velocity (PRV) observations from instruments such as Keck/HIRES, APF, and IRTF/iSHELL on five carefully selected stars. Our primary science goal is to char- acterize and understand stellar jitter, and this program will provide the community with a dataset of RV spectra and precise photometry to study jitter on a broad range of time scales ranging from minutes to months. We have collected high cadence ( ˜minutes) RV data on a subgiant an M dwarf, as well as near nightly cadence data on M/K dwarfs with APF. We will continue RVxK2 with RVxTESS in the near future, targeting a sample of subgiants and active M dwarfs.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:221296 Exploiting the potential of Low-Resolution spectrophotometry to characterize exoplanetary atmospheres

1 1 Daria Desider`a⇤ and Valerio Nascimbeni⇤

1Universit`adi Padova - DFA – Italy

Abstract

Transmission spectroscopy is one of the most fruitful techniques exploited to characterize exoplanetary atmospheres. During a transit, light coming from the host star is selectively absorbed or scattered by the planetary limb depending on the atmosphere chemical composition, physical state and verti- cal structure. Therefore the wavelength dependence of the apparent transit depth or plane- tary radius, the so-called ”transmission spectrum”, probes the chemical composition and the physical state of the planetary atmosphere at the terminator. On typical Hot Jupiters, the most spectroscopically active species in the optical range are neutral alkali metals (sodium, NaI; potassium, KI) and aerosols, that a↵ect the slope of the continuum by Rayleigh or Mie scattering. In the near-infrared range, the signal is dominated by molecular bands such as water and CO. Each of these components give us important and complementary clues on the physical processes that are going on. The optical slope of the transmission spectrum cannot be investigated through high-resolution spectroscopy, since its observables are normalized w. r. t. the continuum. Low- to mid-resolution di↵erential measurements with spectrophoto- metric slits, achievable with MOS spectrographs such as MODS@LBT, are able to deliver accurate chromatic light curves over a wide spectral range, without losing any information on the continuum, therefore this approach is complementary with high-resolution spectroscopy. Here we present some results obtained using SCOLOPENDRA, our publicly-available soft- ware pipeline specifically developed to perform high-accuracy di↵erential spectrophotometry. We show the first results of SCOLOPENDRA on both unpublished and archival data, sug- gesting how it could be exploited as a flexible and accurate tool to homogeneously analyze and merge data sets from di↵erent instruments and setups.

⇤Speaker

sciencesconf.org:horse:221142 Towards the characterization of Earth analogs with high-resolution spectroscopy

1 Christophe Lovis⇤†

1University of Geneva – Switzerland

Abstract

Among the realistic, near-future prospects of characterizing temperate rocky exoplanets, ground-based high-resolution spectroscopy has a prominent role to play. In this talk I will review its application to observations of transiting and non-transiting Earth analogs, and will present the current and future instrumental landscape in this field. I will also advocate for a stronger involvement of the exoplanet community in the development of the future high-resolution spectrographs, in particular for the ELTs.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:222736 EXPRES, the Extreme Precision Spectrograph

1 Lily Zhao⇤†

1Yale University – United States

Abstract

The EXtreme PREcision Spectrograph (EXPRES) was commissioned at the Lowell Ob- servatory 4.3-m Discovery Channel Telescope (DCT), Flagsta↵, Arizona in February 2018. EXPRES is environmentally stabilized in a vacuum enclosure. This R=135,000, fiber-fed, optical spectrograph spans a wavelength range from 390-700 nm. Wavelength calibration is carried out with a Menlo Systems Laser Frequency Comb. The multi-instrument port configuration of the DCT allows for high-cadence, flexible scheduling of stars (up to 280 partial nights per year). The RV precision goal with EXPRES is 10 cm/s; reaching this goal requires successful modeling of the photospheric velocities and microtelluric contamination in our spectra. EXPRES is capable of conducting ground-based transit spectroscopy and characterizing reflected light curves to probe exoplanet atmospheres.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:222743 Combining low and high resolution spectroscopy to retrieve atmospheric metallicities of giant exoplanets

1 Jean-Michel Desert⇤†

1University of Amsterdam (UvA) – Amsterdam, Netherlands

Abstract

A central prediction made by the core accretion model of planetary formation is that atmospheric metallicity should increase with decreasing planet mass. This prediction is born out in the Solar System, where a clear anti-correlation between planet mass and atmospheric metallicity is observed. Exoplanets can thus be used to determine whether this trend is a universal outcome of the planet formation process. I present a portfolio of observational projects for which we have recently succeeded in mea- suring the atmospheric metallicities of gas giant exoplanets. These projects use diverse and complementary approaches to retrieve the metallicity, such as measuring the molecular abun- dances and using novel tracers (e.g. alkali metals and hydrides). I focus this talk on the strength of combining both low- and high-resolution spectroscopy to retrieve the metallicity of gas giants planets. I present the breakthroughs but also the main challenges to overcome while making these measurements.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:221960 Detecting Biosignatures and Pre-Biosignatures in the Atmospheres of Earth-like Planets Around Other Stars

1,2 3,4 Sarah Rugheimer⇤ and Paul Rimmer

1University of St. Andrews – United Kingdom 2Oxford University – United Kingdom 3SUPA, School of Physics and Astronomy, University of St. Andrews – United Kingdom 4Cambridge University – United Kingdom

Abstract

When we observe the first terrestrial exoplanet atmospheres, we expect to find planets at a wide range of geological conditions and evolution. In our own Solar System we already have three very di↵erent terrestrial exoplanets in Earth, Mars, and Venus. Additionally the atmospheres of these planets have not been fixed in time. Earth itself o↵ers many possible atmospheric states of a planet. We set out to examine how an Earth-like planet at di↵erent geological epochs might look around other star types (F, G, K and M dwarf stars). Additionally, we examine the plausibility of detecting prebiotically interesting molecules, such as HCN, NH3, CH4, and C2H6 in an early-Earth type atmosphere. We find that some of these molecules could be produced abiotically in a CO2/CH4/H2 rich atmosphere with lighting and photochemistry. These molecules would be interesting to detect in an exoplanet atmosphere since they are known to be useful for key prebiotic chemical pathways. HCN, for example, is present at each of the initial photochemical reactions that produce lipids, amino acids and nucleosides, the three building blocks of life (Patel et al. 2015). We also look at the rise of oxygen and the detectability of combinations of biosignature gases throughout Earth history, modeling the great oxygenation event and Neoproterozoic oxygenation event event around other star types. We show the VIS - IR spectral features, with a focus on biosignatures observable through geological time for FGKM stars and the e↵ect of clouds on the signal.

⇤Speaker

sciencesconf.org:horse:218878 Identifying and modelling the signatures of magnetic activity from Sun-like stars in exoplanet observations

1 Rapha¨elle Haywood⇤†

1Harvard College Observatory – United States

Abstract

Magnetic activity features, such as faculae, spots and granulation leave an imprint in the optical spectrum of a star. Their spectroscopic signatures are the main obstacle to detecting and characterising Neptune- to Earth-size planets and their atmospheres. I will describe the stellar magnetic activity features and processes that preclude us from determining precise and accurate planet masses via radial-velocity monitoring. I will show how magnetic activity can also a↵ect our interpretation of atmosphere measurements obtained through transmission spectroscopy. I will present what we are learning about the magnetic behaviour of Sun- like stars through the study of our own Sun. The Sun is the only star whose surface can be imaged directly and at high spatial resolution, allowing us to identify the spectroscopic signatures of individual features directly. Studying the Sun as a planet-hosting star enables us to quantify activity-induced ”noise” in exoplanet observations, which is key to estimate uncertainities and to optimise our use of telescope time. Building on our knowledge of the Sun and Sun-like stars, we are developing physically motivated models for magnetic activity. This is a necessary step to examining small planets and their atmospheres in detail, and to ultimately assess their potential for hosting life.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:222732 Boosting or mitigating the stellar activity signal in high-resolution spectroscopy

1 Xavier Dumusque⇤

1Observatory of Geneva – 51 Chemin des Maillettes, 1290 Sauverny, Switzerland

Abstract

Stellar activity is the main limitation to the detection of Earth-twins orbiting cool stars using the radial-velocity (RV) technique, and it is not well understood yet how it impacts atmospheric characterisation of exoplanets. In any case, it is crucial of finding a way to mitigate eciently stellar activity for a successful RV follow-up of TESS candidates but also improving our precision in atmospheric characterisation. Stellar activity of quiet cool stars can be probed by looking at spectral lines presenting a chromospheric emission, like the Ca II H and K lines, H-alpha or the Ca triplet. However, spectral lines formed in the photosphere should also be a↵ected by activity. Photospheric lines have di↵erent sensitivities to temperature, they are formed at di↵erent depth, therefore stellar activity that create spots much cooler than the photosphere and that modifies the convection as a function of depth should a↵ect every spectral line in a di↵erent way.

By deriving the RV of each individual spectral line in HARPS high-resolution spectra, we found that the RV of some spectral lines are much more sensitive to activity than others. By looking at the radial-velocity data of Alpha Centauri B in 2010 and the Sun, where clear activity signals are observed, we can either boost by three the activity signal seen in RV, or mitigate it by a factor of 2.5, depending on the choice of lines used to measure the stellar radial velocity.

By looking at the physical properties of the spectral lines used to increase or decrease the activity signal seen in RV, we are able, using machine learning algorithms, to understand what are the main physical properties of lines that make them sensitive or not to stellar activity. In conclusion, this new way of deriving RVs can be either used to probe better stellar activity, as the related signal in RV can be increased by a factor of three, or to mitigate its e↵ects by a factor of 2.5, to detect tiny planetary signal in RV measurements.

⇤Speaker

sciencesconf.org:horse:217013 The use of TNG facilities in the study of exoplanetary atmospheres

1 Ennio Poretti⇤†

1National Institute for Astrophysics (INAF) – Italy

Abstract

The high-resolution spectrographs available at the Telescopio Nazionale Galileo (Roque de Los Muchachos Observatory, La Palma) are currently used to study exoplanetary atmo- spheres. They are HARPS-N and GIANO-B, also combined in the new GIARPS configu- ration, simultaneously covering visible and near-infrared domains. I present the scientific highlights obtained since 2012 by di↵erent teams with these instruments and discuss future improvements. Inputs are welcome. I remind that the access to the TNG is open to the international community through distinct calls.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:200050 Retrieving Exoplanet Atmosphere Properties from High Dispersion Cross-Correlation Spectroscopy

1 2 3 4 Michael Line⇤† , Matteo Brogi , Jacob Bean , Jean-Michel Desert , and Jonathan Fortney5

1Arizona State University – United States 2University of Warwick – United Kingdom 3University of Chicago – United States 4University of Amsterdam – Netherlands 5University of California, Santa Cruz – United States

Abstract

A powerful emerging approach for characterizing exoplanet atmospheres is high disper- sion cross-correlation spectroscopy (HDCCS). HDCCS leverages the planetary Doppler shift of the large number of molecular lines attainable at high resolutions (R> ˜30000) com- bined with large ground-based apertures to robustly detect molecules. This is the best technique to unambiguously identify molecules, and it is the only technique to have reli- ably detected carbon-based molecules in exoplanet atmospheres. However, little work has focused on constraining the abundances of molecules, vertical temperature structures, and other fundamental atmospheric properties from HDCCS data in a rigorous way. One of the primary challenges in doing so is placing the HDCCS within a robust atmospheric retrieval framework, a widely applied and key tool in LDS data interpretation. Here I will present a novel atmospheric retrieval framework recently developed by our team that combines power- ful Bayesian methods with HDCCS observations with applications to current state-of-the-art HDCCS observations, the prospects for rigorously combining low resolution HST or JWST- like observations with HDCCS observations, and prospects for future HDCCS observations to characterize potentially habitable worlds.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:222741 Comparative study of circulation regimes of terrestrial planets’ atmospheres

1 1 2 1 Pedro Machado⇤ , Ruben Gon¸calves⇤ , Thomas Widemann⇤ , and Gabriella Gilli⇤

1INSTITUTE OF ASTROPHYSICS AND SPACE SCIENCES (IA) – Tapada da Ajuda - Edif´ıcio Leste -2o Piso 1349-018 Lisboa, Portugal, Portugal 2Observatoire de Paris – LESIA, Observatoire de Paris – France

Abstract

Understanding our Solar System Planetary Atmospheres is a significant step forward for paving the way for future studies of Extrasolar Planets’ atmospheres. Notably, Venus and Mars are natural comparative laboratories to investigate diversity of circulation regimes of terrestrial planets’ atmospheres. In this context, comparative studies are essentials to un- derstand the evolution of climate on Earth, both in the past and in the future. Notably, Venus and Mars are natural comparative laboratories to investigate diversity of circulation regimes of terrestrial planets’ atmosphere. Venus for example, is Earth’s closest sibling but it has ended up with a radically di↵erent climate. Venus atmospheric science is thus increasingly important in an era in which we are trying to understand the divergent evolutionary outcomes for terrestrial planets, whether we are considering the future of our Earth or the habitability in other planetary systems.

We will present a study based on large scale and small scale processes going on the mid- dle/upper atmosphere of Venus and Mars combining wind measurements and 3D model simulations.

Venus is a slowly rotating planet with a dense atmosphere. The mechanisms for the gen- eration and maintenance of superrotation are still unclear and no model has been able to successfully reproduce its circulation in decades (Lebonnois 2013). A proper monitoring of Venus winds is crucial towards a full understanding of this phenomena. With this aim, we intend to conduct a synthesis e↵ort that could provide important constraints on atmo- spheric models. In Venus’s mesosphere (65-85 km), visible observations of Doppler shifts in solar Fraunhofer lines, based on high-resolution spectra, have provided the only Doppler wind measurements near the cloud tops in recent years (Machado et al. 2014, 2017). We will present wind measurements based on VLT/UVES and CFHT/ESPaDOnS observations (around 70 km), wind measurements based on Akatsuki space probe data (and ESA’s Venus Express archive data) with cloud tracking methods (from 48 km till 70 km), using an im- proved version of a cloud tracking tool based on phase-correlation between images. The objective of this work is to help constrain the planetary atmospheric characterization, and to take a step forward in the comparative studies of terrestrial planets.

⇤Speaker

sciencesconf.org:horse:199925 Characterization of multiple alkali metals in the atmosphere of the super-Neptune WASP-127b

1 Guo Chen⇤

1Instituto de Astrofisica de Canarias (IAC) – Calle V´ıa L´actea, s/n, 38205 San Crist´obal de La Laguna, Santa Cruz de Tenerife, Spain

Abstract

Absorption lines of alkali metals carry crucial information to understand the pressure- temperature profile of the atmosphere at high altitude. The pressure-broadened line wing of alkali metals is an important characteristic of clear skies and could help mitigate the de- generacy between pressure and abundance, while the fully resolved line cores could provide insight into thermosphere. We observed a transit of the super-Neptune WASP-127b simul- taneously using the optical low-resolution spectrograph OSIRIS at the 10.4 m GTC and the optical+NIR high-resolution spectrographs HARPS-N + GIANO-B at the 3.6 m TNG. The low-resolution transmission spectrum has a uniform spectral bin width of 5 nm, and exhibits spectrally-resolved pressure-broadened line wings of Na and K. This results in the first-ever multiple robust detectections of alkali metals (Na, K, and Li) in an exoplanet. We performed spectral retrieval modeling with a patchy cloudy model, derived the abundances of alkali metals, and constrained the presence of haze coverage. The high-resolution data are limited by S/N owing to single-transit observation, faintness of the star, and small number of out-of-transit measurements, but the derived trasmission spectrum clearly resolves the line cores of Na. We will discuss the prospects of combining high- and low-resolution transmission spectra to interpret exoplanet atmospheres.

⇤Speaker

sciencesconf.org:horse:221366 Na I and Ha absorption features in the atmosphere of MASCARA-2b/KELT-20b

1 1 Nuria Casasayas-Barris⇤ and Enric Palle

1Instituto de Astrofisica de Canarias (IAC) – Calle V´ıa L´actea, s/n, 38205 San Crist´obal de La Laguna, Santa Cruz de Tenerife, Spain

Abstract

We have used the HARPS-North high resolution spectrograph (R=115 000) at TNG to observe one transit of the highly irradiated planet MASCARA-2b/KELT-20b. Using only one transit observation, we are able to clearly resolve the spectral features of the atomic sodium (Na I) doublet and the Ha line in its atmosphere, which are corroborated with the transmission calculated from their respective transmission light curves. In particular, we observe two spectral features centred on the atomic sodium (Na I) doublet position with an averaged absorption depth of 0.17+/-0.03 % for a 0.75A bandwidth. The Na I transmission light curves have been also computed, showing a large Rossiter-McLaughlin (RM) e↵ect, with a 0.20+/-0.05% Na I transit absorption for a 0.75A passband, consistent with the absorption depth value measured from the final transmission spectrum. We observe a second feature centred on the Ha line with an absorption depth of 0.59+/-0.08% for a 0.75A passband, which corresponds to an e↵ective radius of Rp’/Rp=1.20+/-0.04, and with consistent absorptions in its transmission light curves. While S/N of the final transmission spectrum is not sucient to adjust di↵erent temperature profiles to the lines, we find that higher temperatures than the equilibrium (Teq=2260+/-50K) are needed to explain the lines contrast. Particularly, we find that the Na I lines core require a temperature of T=4210+/- 180K and that Ha requires a temperature of T=4330+/-520K.

⇤Speaker

sciencesconf.org:horse:220978 Simultaneous detection of the water bands at 1.14 and 1.40 microns on the transmission spectrum of HD 189733 b using CARMENES

1 2 3 Francisco Javier Alonso-Floriano⇤† , Ignas Snellen , Alejandro S´achez-L´opez ,and Manuel Lopez-Puertas3

1Leiden Observatory, Leiden University – P.O. Box 9513 2300 RA Leiden, Netherlands 2Leiden Observatory, Leiden University – Netherlands 3Instituto de Astrofisica de Andalucia (IAA) – Spain

Abstract

Most ground-based detections of molecular species in exoplanet atmospheres have been obtained using high-resolution spectrographs mounted on the largest telescopes which tar- geted a specific narrow wavelength range. However, even when mounted in smaller telescopes, the new highly-stabilized spectrographs can be used for detecting molecular species on exo- planet atmospheres due to their wider instantaneous wavelength coverage. Thus, we have used the high-resolution spectrograph CARMENES on the 3.5m Calar Alto Telescope, to observe HD 189733 b during transit. After e↵ectively removing the stellar and telluric signal using Sysrem (a Principal Component Analysis like technique), we have detected the planet water signal by cross-correlating the residuals with physically accurate water transmission models. Besides, we have divided the wide near-infrared wavelength cov- erage of CARMENES (0.96 - 1.7 microns) in smaller wavelength regions, and applying the same technique, we were able to detect the water signal caused by the 1.14 and 1.40 microns water bands individually and simultaneously.

These results probe the capabilities of CARMENES for studying exoplanet atmospheres and can be a promising new way of constraining the presence of hazes in planetary atmospheres from ground facilities.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:220675 A new classification scheme based on water/methane dominancy in the atmospheric spectra of irradiated planets

1 2 1 Karan Molaverdikhani⇤ , Paul Molliere , and Thomas Henning

1Max-Planck-Institut f¨ur Astronomie (MPIA) – K¨onigstuhl 17, 69117 Heidelberg, Germany 2Sterrewacht Leiden, Huygens Laboratory – Niels Bohrweg 2, 2333 CA Leiden, Netherlands

Abstract

We introduce a simple but powerful technique to estimate the contribution of each atmo- spheric constituent in its spectrum, averaged over all pressures. Estimating these contribution coecients provides us with a tool to quantitatively study relative importance of individual species in both emission and transmission spectra. We employ this spectral contrast between molecular features, namely water and methane, to explore the parameter spaces where either methane or water is the dominant spectral feature. We propose a classification scheme, with four classes, for irradiated planets based on the dominancy of water and methane features in their atmospheric spectra and the asso- ciation of their boundary with planetary e↵ective temperature, surface gravity, metallicity and their host star’s spectral type. We find C/O< 1 is not a global indicator for a water-dominated atmosphere and neither C/O> ˜1 is a ubiquitous indication of methane-dominancy. We report, the best tempera- ture range to look for CH4 features is somewhat not very cold as one might expect, ranging from 800k to 1500k and requiring carbon to oxygen ratio to be about 0.7 or higher. This temperature range is also in favor of less cloudy atmosphere in contrast to colder planets, however the presence of clouds is not unlikely and consequently the TP structure as well as species abundances might alter, and similarly non-equilibrium chemistry could also change the spectral appearance of these planets. We present the e↵ect of non-equilibrium chemistry on these regions and show how non-equilibrium chemistry modifies the classification and the regions where it can be neglected.

⇤Speaker

sciencesconf.org:horse:210655 Unveiling exoplanet atmospheres with the ACCESS survey

1 2,3,4 5 6 N´estor Espinoza⇤ , Daniel Apai , Andr´es Jord´an , Mercedes Lopez-Morales , Benjamin Rackham4, Alex Bixel4, Dave Osip7, Ian Weaver6, Chima Mcgruder6, Jonathan Fortney8, Nikole Lewis9, and Florian Rodler10

1Max-Planck-Institut f¨ur Astronomie (MPIA) – K¨onigstuhl 17, D-69117 Heidelberg, Germany 2Earths in Other Solar Systems Team (EOS) – 933 N Cherry Avenues Tucson, AZ 85721, United States 3Lunar and Planetary Laboratory, University of Arizona – United States 4Steward Observatory, University of Arizona – 933 N Cherry Avenue University of Arizona Tucson AZ 85721 USA, United States 5Pontificia Universidad Cat´olica de Chile (PUC) – Casilla 306, Santiago 22, Chile 6Harvard-Smithsonian Center for Astrophysics (CFA) – 60 Garden Street, Cambridge, MA 02138, United States 7Observatories [Carnegie Institution] – Pasadena, California, United States 8University of California [Santa Cruz] (UCSC) – 1156 High Street, Santa Cruz, Ca 95064, United States 9Space Telescope Science Institute (STSci) – 3700 San Martin Drive, Baltimore, MD 21218, USA, United States 10European Southern Observatory [Santiago] (ESO) – Casilla 19001, Santiago 19, Chile

Abstract

One of the most exciting possibilities enabled by transiting exoplanets is to measure their atmospheric properties through the technique of transmission spectroscopy. The optical win- dow, in particular, is rich in atmospheric information which is capable of disentangling several degeneracies in atmospheric modelling. In this context, ACCESS is a multi-institutional col- laboration aimed at responding to this opportunity by generating a uniform observational set of ˜ 0.35 – 1.0 µm low-resolution transmission spectra of a sample of ˜20 exoplanet atmospheres, spanning those from hot Jupiters to super-Earths, which might be either used to screen good targets for further high-resolution transmission spectroscopy or to combine analyses with both high and low resolution data (a-la Brogi et al., 2017, ApJ, 839, 2). In this talk, we present the survey methodology and lessons learned to date following over 40 transits observed using the IMACS multi-object spectrograph on the 6.5-m Magellan Baade Telescope at Las Campanas Observatory. We will present a brief overview of the survey and highlight results on multiple targets, including hot Jupiters and the sub-Neptune GJ 1214b. Of particular interest are recent results obtained from a series of 6 observed transits of WASP-19b which show transmission spectra that are in striking contrast with published VLT/FORS2 results for which claims of TiO and a strong blue-optical slope were postu- lated. Finally, we will elucidate where we see the brightest future prospects in the era of space missions such as TESS and JWST, and future high and low-resolution instruments in the era of the ELTs.

⇤Speaker

sciencesconf.org:horse:209404 Modeling Exoplanet Atmospheres at High Spectral Resolution

1 Eliza Kempton⇤†

1University of Maryland – United States

Abstract

In this talk I will focus on the modeling of exoplanet spectra at high resolution with an eye toward how the high dispersion spectroscopy (HDS) technique can be used to place unique constraints on the properties of exoplanet atmospheres. Observations using current facilities have already been used to measure atmospheric abundance patterns and planetary rotation rates, and to suggest the presence of high-speed day-to-night winds. Interpreting these observations requires cross correlation against model template spectra. Because individual spectral lines are resolved at high resolution, the template models should accurately account for line broadening and line shifting mechanisms. I will describe e↵orts to couple together 3- D general circulation models (GCMs) with 1-D radiative transfer to properly account for the e↵ects of atmospheric dynamics, planetary rotation, and 3-D atmospheric structure at high spectral resolution. I will conclude with a forward looking view of the types of atmospheric characterization studies that could be undertaken with 30-meter class telescopes equipped with high resolution spectrographs, and a description of the atmospheric modeling e↵orts that would be required to accompany such observations.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:222730 Resolved helium absorption signature from the extended atmosphere of the warm Neptune HAT-P-11b

1 Romain Allart⇤†

1University of Geneva – Switzerland

Abstract

Stellar irradiation causes the atmospheres of close-in exoplanets to expand and escape to space. In addition to the neutral hydrogen at ultraviolet wavelengths that probes the exosphere and the gas escaping from the atmosphere, the near infrared triplet transition of helium (at 10833 A)˚ probe extended thermosphere. Previous studies have shown that warm Neptunes are more likely, than Hot Jupiters, to see their hydrogen atmosphere extended and escaping into space. In this talk, I will present a helium detection in the transiting warm Neptune HAT-P-11b using ground-based, high-resolution CARMENES observations. The helium feature is repeatable over two independent transits, with an average absorption of 1.08 0.05% (21). The spectral and spatial resolution of our data allow for a detailed characterisation± of the processes shaping its extended thermosphere. To conclude, these results show that spectral identification of helium will greatly enhance atmospheric studies of low-mass exoplanets from Neptunes to Super-Earths, and probe their evolution.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:221764 Detection of water vapor in the dayside spectrum of the non-transiting gas giant HD102195b with GIANO

1,2 2 3 2 Gloria Guilluy⇤ , Alessandro Sozzetti , Matteo Brogi , Aldo Bonomo ,andPaolo Giacobbe2

1Universit`adegli Studi di Torino – Italy 2Osservatorio astrofisico di Torino – Italy 3The University of Warwick – United Kingdom

Abstract

Recent observations of the transiting hot Jupiter HD189733b with the GIANO infrared (0.9-2.45) µm spectrograph at the Telescopio Nazionale Galileo have successfully proven that a 4-m class telescope with a performing high-resolution spectrograph can successfully study the atmospheres of exoplanets at high spectral resolution (R ˜50,000). Here we report on dayside spectroscopy observations with GIANO of the non-transiting hot giant planet HD 102195b, aimed at detecting water vapour in its atmosphere. We employ a technique to disentangle the Doppler-shifted planet spectrum (whose individual lines are resolved at high spectral resolution) from the stationary telluric/stellar components. We then extract the planetary signal by cross-correlating the residual spectra with template models of the planet atmosphere computed through line-by-line radiative transfer calculations, and containing molecular absorption lines from water. We detect molecular absorption from water vapor with a SN of 6.92, at a projected planet orbital velocity of Kp= 140 -8 ˆ +12 km/s. We derive a first estimate of the planet true mass, Mp=0.44 -0.03 ˆ +0.04{ } { Mjup} , and 1, 2 lower limits on orbital inclination of 73.09 ,63.47 . By{ the non-detection} { } of the planet in previous photometric monitoring, conducted with the T10 0.8 m automatic photometric telescope (APT) at Fairborn Observatory, we set an upper limit on the system inclination imax= (84.79 0.09) . ±

⇤Speaker

sciencesconf.org:horse:221653 Molecular Simulations for the Spectroscopic Detection of Atmospheric Gases

1 1 1 Clara Sousa-Silva⇤ , Sara Seager , and Janusz Petkowski

1Massachusets Institute of Technology (MIT) – United States

Abstract

Unambiguously identifying molecules in spectra is of fundamental importance for a vari- ety of scientific and industrial uses; a compelling modern focus is the spectroscopic detection of volatiles in exoplanet atmospheres, and the assessment of habitability in these planets. Analyses of observational spectra require information about the spectrum of each of its pu- tative components. However, spectral data currently only exist for a few hundred molecules and only of fraction of those have complete spectra (e.g. water, ammonia). Consequently, molecular detections in exoplanet atmospheres are vulnerable to false positives, false neg- atives and miss-assignments. There is a key need for spectral data for a broad range of molecules. Here we present ATMOS : Approximate Theoretical MOlecular Spectra. Using a combina- tion of experimental measurements, organic chemistry, and quantum mechanics, ATMOS is a programme that: a) Provides approximate spectral data (band centres and relative intensities) for thousands of molecules in seconds. b) Assesses hundreds of molecules simultaneously, highlighting patterns and any distinguish- ing features. Traditional methods for obtaining spectra are extremely costly and time- consuming (i.e. months/years per molecule); ATMOS will inform prioritization protocols for future high accuracy studies. c) Demonstrates that, at low resolution, individual spectral features could belong to a large number of molecules. Molecular detections in spectra are often made by assigning one, or a few, spectral features to a given molecule. ATMOS can highlight ambiguities in such molecular detections and also direct observations towards spectral regions that reduce the degeneracy in molecular identification.

⇤Speaker

sciencesconf.org:horse:218684 Reflections from other worlds

1,2 1,2 1 Nuno Santos⇤ , Martins Jorge , and Olivier Demangeon

1Instituto de Astrof´ısica e Ciˆencias do Espa¸co (IA/U. Porto) – CAUP, Rua das Estrelas, 4150-762 Porto, Portugal 2Departamento de F´ısica e Astronomia, FCUP, Portugal (DFA-FCUP) – Departamento de F´ısica e Astronomia, Faculdade de Ciˆencias, Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal, Portugal

Abstract

The detection and study of exoplanet atmospheres using high resolution spectroscopy has been achieved both in the optical and near-IRregimes. In the optical, most of the success in this domain made use of transmission spectroscopy measurements.

An alternative (and complementary) avenue to explore the atmospheres of exoplanets is to detect their reflected light. So far, these measurements were possible for a handful of cases thanks to high precision photometry from space missions such as CoRoT and the Kepler. However, both CoRoT and Kepler observed in a unique and broad wavelength band, limiting the physical information that is gathered. Ground based high resolution spectroscopy has, in this context, an important role to play to push the physical interpretation further. The proof of concept has been made with the detection of the reflected light spectrum of 51 Peg-b with HARPS.

In this talk we will present the method used to detect reflected light spectra using high resolution spectroscopy as well as its prospects. We will show that with new and future high resolution spectrographs working in the optical regime, namely ESPRESSO@VLT and HIRES@ELT, this method can be applied to a handful of planets. In particular, we will show that these instruments will allow to recover the wavelength albedo function, even in cases of non-transiting planets. The potential to obtain a longitudinal map of the albedo spectrum will also be discussed.

⇤Speaker

sciencesconf.org:horse:205938 HIRES: A planet-characterizer high-resolution spectrograph for the ELT

1 2 Enric Palle⇤ and Consortium Hires

1Instituto de Astrofisica de Canarias (IAC) – Calle V´ıa L´actea, s/n, 38205 San Crist´obal de La Laguna, Santa Cruz de Tenerife, Spain 2Instituto de Astrof´ısica de Canarias (IAC) – Spain

Abstract

Ongoing searches for exoplanetary systems have revealed a wealth of planetary systems with extremely diverse physical properties. Earth-size planets have already been detected around many stellar types, including some interesting planets within the habitable zone of cool M-type stars. Over the coming decades, the e↵orts of future space missions and large telescope facilities will be aimed at the discovery of small rocky exoplanets within the habitable zones of the brighter stars in the sky providing key targets for further followup. Once these prime targets are found, e↵orts will shift toward the characterization of their atmospheres, and the search for possible bio-signatures. This is a daunting task that will require bringing to the limit the capabilities of the largest telescopes in search for faint signatures, that once detected will quite likely become a subject of controversy for several years. In this talk I will review the capabilities of the HIRES instrument at the European 39-m ELT, for the confirmation a characterization of planetary atmospheres.

⇤Speaker

sciencesconf.org:horse:221249 Enabling precise C/O ratios from high resolution spectroscopy: the MMT Exoplanet Atmosphere SURvEy (MEASURE)

1 Jayne Birkby⇤

1University of Amsterdam (UvA) – Science Park 904, Amsterdam, 1098XH, Netherlands

Abstract

The sensitivity of high-resolution spectroscopy to the shape and Doppler shift of exoplanet spectral lines makes it a robust and powerful tool in exoplanet characterization. However, most analysis techniques so far require a normalisation of the high resolution spectra and thus loses information about the planet’s continuum level. This results in degeneracies between abundances and temperature-pressure atmospheric profiles, inhibiting precise measurements of C/O ratios that may inform us about the formation and birth location of the planet in its protoplanetary disk. This can be alleviated by i) observing multiple molecular features over a wide instantaneous wavelength range, which makes it harder for degenerate models to match all the spectral features, and ii) by combining high resolution data with lower resolution data where the continuum information is preserved. I will present the first results from MEASURE: the MMT Exoplanet Atmosphere SURvEy. It is a large, homogenous survey of exoplanet atmospheres at R ˜30,000 from 1.5-2.5 microns simultaneously, coupled with Spitzer phase curves and complementary CRIRES spectroscopy. Its goal is to provide precise atmospheric C/O ratios and thus stringent constraints on the planets’ formation mechanisms and natal environments.

⇤Speaker

sciencesconf.org:horse:222090 CUTE CubeSat Mission

1 2 3 4 Sreejith Aickara Gopinathan⇤ , Kevin France , Brian Fleming , Jean-Michel Desert , Arika Egan3, Luca Fossati1, Tommi Koskinen5, Pascal Petit6, and Aline Vidotto7

1Space Research Institute, Austrian Academy of Sciences (IWF/OeAW) – Austria 2University of Colorado – United States 3LASP, University of Colorado – United States 4University of Amsterdam – Netherlands 5University of Arizona, Lunar and Planetary Laboratory – United States 6Observatoire Midi-Pyr´en´ees (OMP) – CNRS : UMR5277, univ – 14 avenue Edouard Belin, 31400 Toulouse, France 7Trinity College Dublin, School of Physics, University of Dublin – Ireland

Abstract

Short-period exoplanets provide the unique opportunity to observe phenomena critical to the development and evolution of our own solar system, including atmospheric escape and star-planet interactions. Owing to their large sizes and short-periods, atmospheric escape can be studied with a dedicated small instrument operating in the near-ultraviolet. We present the Colorado Ultraviolet Transit Experiment (CUTE), a 6U CubeSat mission that will spectrally isolate diagnostic atomic and molecular transitions arising within the upper planetary atmospheres to study the physics of atmospheric escape in near ultraviolet regime. CUTE is planned for launch in 2020, with a nominal baseline survey program designed to observe 10 transits of approximately 12 bright exoplanetary systems. CUTE’s flexible observing⇡ plan also allows for coordinated observations of particularly interesting targets with a number of facilities. We will discuss the details of CUTE data simulator and show how it CUTE matches our science case.

⇤Speaker

sciencesconf.org:horse:221244 Detecting water in HR 8799 c with L band high dispersion spectroscopy

1 Ji Wang⇤

1Caltech – United States

Abstract

High dispersion spectroscopy of brown dwarfs and exoplanets enables exciting science cases, e.g., mapping surface inhomogeneity and measuring spin rate. Here, we present $L$ band observations of HR 8799 c using Keck NIRSPEC in adaptive optics (AO) mode (NIRSPAO). We search for molecular species (H$ 2$O, CO and CH$ 4$) in the atmosphere of HR 8799 c with a template matching method, which involves cross correlation between reduced spectrum and a template spectrum. We detect water in $L$ band data but do not detect methane or CO. We conduct planet signal injection simulation to estimate the sensitivity of our AO-aided high dispersion spectroscopy observations. We conclude that $10ˆ -4 $ contrast can be reached. { }

⇤Speaker

sciencesconf.org:horse:214724 Venus’ cloud top wind measurements with TNG/HARPS-N and coordinated Akatsuki observations

1,2 1 3 4,5 Ruben Gon¸calves⇤† , Pedro Machado , Thomas Widemann , Javier Peralta , Shigueto Watanabe6, Atsushi Yamazaki4,5, Takehiko Satoh4,5, Masahiro Takagi7, Kazunori Ogohara8, Yeon Joo Lee4,5, Harutyunyan Avet9, and Jos´eSilva1,2

1INSTITUTE OF ASTROPHYSICS AND SPACE SCIENCES (IA) – Tapada da Ajuda - Edif´ıcio Leste -2o Piso 1349-018 Lisboa, Portugal, Portugal 2Faculdade de Ciˆencias [Lisboa] (FCUL) – Universidade de Lisboa, Campo Grande, Edificio CS, 7749-076 Lisboa, Portugal 3Observatoire de Paris – LESIA, Observatoire de Paris – France 4Institute of Space and Astronautical Science (ISAS) – Sagamihara City, Kanagawa Prefecture 252-5210, Japan 5Japan Aerospace Exploration Agency [Sagamihara] (JAXA) – Chuo Ku, Sagamihara, Kanagawa 2525210, Japan, Japan 6Hokkaido University – 5 Chome Kita 8 J¯onishi, Kita Ward, Sapporo, Hokkaido Prefecture 060-0808, Japon, Japan 7Kyoto Sangyo University – Motoyama, Kamigamo, Kita-ku Kyoto-City 603-8555 Japan, Japan 8School of Engineering, University of Shiga Prefecture – Japan 9Istituto Nazionale di Astrofisica (INAF) – Viale del Parco Mellini 84, 00136 Roma, Italy

Abstract

Introduction We present wind velocity results based in the measurements of the horizontal wind field at the cloud top level of the atmosphere of Venus, near 70 km altitude, in the visible range on the dayside. At this altitude the wind circulation is dominated by the retrograde zonal superrotation.

The ground observations were carried out, on the 28 and 29 of January 2017, at the 3.58-meter ”Telescopio Nazionale Galileo” (TNG) using the ”High Accuracy Radial velocity Planet Searcher” spectrograph (HARPS-N) in the visible range (0.38-6.9 µm). It was the first use of this high-resolution (R 115000) spectrograph to study the dynamics of a solar system atmosphere. The sequential⇡ technique of visible Doppler velocimetry is based on solar light scattered by cloud top particles in motion. This technique was developed over the last decade (Widemann et al. 2008, Machado et al. 2012, 2014) and has proven to be a reference in the retrieval of instantaneous zonal and meridional winds - it has provided successful results using two high resolution spectrographs: (1) slit spectrograph UVES at VLT (Machado et a.l

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:201464 2012) and (2) fiber-fed spectrograph ESPaDOnS at CFHT (Machado et al. 2014, 2017). In this work we successfully adapt this technique to the HARPS-N fiber-fed spectrograph with consistent results. HARPS-N is the most stable and precise high-resolution spectrograph observing the northern skies in the world, and it was especially made for extrasolar planet searches. However, the stability of the HARPS-N spectrograph provided unprecedented high-quality spectra at Venus atmosphere, which allow us to retrieve wind velocities with an unmatched precision and spatial and temporal accuracy. With the data obtained now, we would contribute to better constrain the zonal wind, the meridional wind flow and detect and characterize mesoscale atmospheric waves on Venus’ atmosphere. With this project, TNG and HARPS-N opened a new window for Planetary Systems atmospheric characterization.

The cloud-tracking space observations were carried out, between 26-31 January 2017, by the ”Ultra Violet Imager” (UVI) onboard Akatsuki’s Venus Climate Orbiter (VCO), using the 365 nm filter. The cloud-tracking technique we used was evolved from a phase correlation method between images developed by Peralta et al. 2007.

The HARPS-N ground observations focused on the meridional wind field between 60 S and 55 N latitude and zonal wind field near equator (latitudes between 10 S and 10 N). HARPS-N results present an unprecedented high-precision meridional wind latitudinal pro- file, which is essential for the understanding of the super-rotation atmosphere mechanisms.

The Akatsuki/UVI observations provided 3 high-quality images per observation day, sep- arated by ˜2h interval. Due to its low inclination orbit (< 10o), Akatsuki’s images o↵er a great range in Venus’ dayside, allowing us to track cloud features from 60o N to 70o S latitude and from 7:30 to 17:00 local time. This has enable a study of spatial and time variability of both zonal and meridional wind.

This work intends to contribute to the characterization of Venus’ cloud top zonal and merid- ional wind by studying latitudinal behavior on hour and day timescales as well as wind temporal and spatial variability. Similar studies have proven the relevance of both space- based cloud tracking observations (S´anchez-Lavega et al. 2008, Hueso et al. 2012, 2015, Hourinouchi et al. 2018) and ground-based doppler velocimetry (Machado et al. 2014, 2107), as well as the usefulness of coordinated observations in the cross validation of both technique results.

Method With HARPS-N, the complete optical spectrum, from 383 to 690 nm, is collected over 40 spectral orders in a single exposure at a resolution of about 115,000. In the single scattering approximation, the Doppler shift measured in solar light scattered on Venus dayside is the result of two instantaneous motions: (1) a motion between the Sun and Venus upper clouds particles, which scatter incoming radiation in all directions including the observer’s; this Doppler velocity is minimal near Venus sub-solar point; (2) a motion between the observer and Venus clouds, resulting from the topocentric velocity of Venus cloud particles in the ob- server’s frame; this e↵ect is minimal near Venus sub-terrestrial point. The measured Doppler shift is the sum of those two terms. It therefore varies with planetocentric longitude. The Doppler shift vanishes at the half phase angle meridian, where both terms cancel each other, and we use this meridian as ”zero-Doppler-reference” to check for instrumental or calibration drifts. In this work we adapted the method used by Machado et al. 2017. Constraining the drag mechanism in hot Jupiter atmospheres using a heat engine approach

1 2 Thaddeus Komacek⇤ and Daniel Koll

1University of Chicago – United States 2Massachusetts Institute of Technology – United States

Abstract

Hot Jupiters are likely tidally locked and receive copious amounts of incident stellar flux, causing extremely fast wind speeds in their atmospheres that can approach or exceed the speed of sound. Using a heat engine framework, we have developed a theory to estimate the bulk wind speeds in hot Jupiter atmospheres. This theory predicts the wind speed as a function of relevant planetary parameters: incident stellar flux, pressure level, planetary gravity, and atmospheric drag strength. This drag strength may be due to Lorentz forces (i.e., magnetic e↵ects) and/or shear instabilities and shocks in these hot, partially ionized, and dynamic atmospheres. We find that our theory matches well the wind speeds calculated from numerical simulations of the atmospheric circulation of hot Jupiters. As a result, one can apply this theory to observations of Doppler blue-shifts in high resolution spectral lines, which constrain wind speeds, to then constrain the drag mechanism in hot Jupiter atmospheres. We find that given the Doppler observations for HD 189733b and HD 209458b, we expect that magnetic drag is too weak to match the wind speed for HD 189733b but is consistent with the wind speed for HD 209458b. However, shear instabilities and/or shocks can match the wind speeds observed for both planets. As a result, we hope that a larger sample of observed Doppler wind speeds can place constraints on how the atmospheric drag mechanisms in hot Jupiters vary with planetary parameters.

⇤Speaker

sciencesconf.org:horse:194443 Filtering stellar activity with Doppler tomography and spectropolarimetry

1 Jean-Francois Donati⇤†

1Institut de Recherche en Astrophysique et Plan´etologie – Institut de Recherche en Astrophysique et Plan´etologie (IRAP) – France

Abstract

Cool stars hosting outer convective zones are known to trigger magnetic fields and re- lated activity phenomena a↵ecting their photospheres and inducing temporal variability of their spectra on a wide range of timescales. As a result, activity impacts radial velocity (RV) measurements of low-mass stars, thus hampering our ability to detect and characterize planets orbiting these stars. This is especially critical when studying low-mass planets in the habitable zones of moderately-active Sun-like stars, or even hot Jupiters orbiting young pre-main-sequence stars, whose reflex motions is often much smaller than the RV jitter that activity generates. Diagnosing, modeling and filtering the activity jitter is thus essential to ensure reliable planet detections and derive accurate orbital properties and (minimum) mass measurements of the detected planets. I will outline in my talk the various steps that this process requires, focusing on promising methods based on Doppler tomography and spec- tropolarimetry, along with the specific observational strategies and instrumentation that they require.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:222734 Isotopes in M dwarfs: 13CO

1 Ian Crossfield⇤

1MIT – United States

Abstract

Mid-type M dwarfs represent the single most common outcome of star formation and so these objects are popular in studies of stellar and planetary properties. However, the derivation of precise ages and elemental abundances for these stars remains a challenge. A new generation of high-dispersion, infrared echelle spectrographs sheds new light on these dim stars. In particular, these instruments enable new, precise studies of isotopic, not just elemental, abundances. The Galactic 13C/12C ratio in particular is predicted to evolve with time and Galactocentric radius, so measuring this ratio may enable an ”isotopic clock” that measures the ages of individual stars. I will report on our first measurements with IRTF/iSHELL at R ˜70,000 to measure 13C/12C in the first overtone bands (2.3 micron) and in the fundamental band at 5 micron. Such data will also enable a broad diversity of ancillary stellar science and prepare the way for future, similar studies of brown dwarfs and [eventually] giant extrasolar planets.

⇤Speaker

sciencesconf.org:horse:220361 Observations of sodium in exoplanet atmospheres

1 Aur´elien Wyttenbach⇤

1Universiteit Leiden [Leiden] – P.O. Box 9500 2300 RA Leiden, Netherlands

Abstract

Exoplanet atmospheres are studied with the transmission spectroscopy method since the early 2000s, especially with the sodium D doublet on which we focused here. Later, the use of high-resolution spectrographs installed on giant and medium size telescopes allowed to resolved the lines and to infer new physical properties of exoplanet atmospheres. Up to now, sodium has been detected in the atmosphere of about 18 exoplanets, from which six were observed (several times) at high spectral resolution. Some observations led to the measures of absolute abundances, winds or temperature gradients in upper atmospheres. it is important to realize, that if we want to infer accurate physical parameters on exoplanet atmospheres, our measurement must be free of any biases or systematic errors. After having clarified the observational and instrumental setup, the treatment and correction of telluric lines pollution, one is now facing the problem to understand properly the impact of the stellar host itself on transmission spectra. E↵ects such as stellar activity, center-to-limb variation across the stellar lines or changes in line shape due to the Rossiter-McLaughlin e↵ect can cause spurious residuals in transmission spectra. All these e↵ects have been also observed through the sodium lines. We want to correct from them to avoid biases in physical retrivials. All these works made on the sodium have to be put into perspectives with the recent results obtained with new probes such as helium or iron, which bring new hopes for the characterization of upper atmospheres.

⇤Speaker

sciencesconf.org:horse:221732 HiRISE: Bringing high-spectral resolution to VLT/SPHERE

1 Arthur Vigan⇤

1Laboratoire d’Astrophysique de Marseille / CNRS (LAM / CNRS) – INSU, CNRS : UMR7326, Aix Marseille Universit´e, Centre National des Etudes Spatiales - CNES – 38, rue Fr´ed´eric Joliot-Curie 13388 Marseille cedex 13, France

Abstract

New-generation exoplanet imagers, like VLT/SPHERE or Gemini/GPI, have been de- signed to achieve very high contrast (> 15 mag) at small angular separations (< 0.5”) for the detection of young giant planets in the near-infrared, but they only provide very low spectral resolutions (R< 100) for their characterization. High-dispersion spectroscopy at resolutions up to 10ˆ5 is one of the most promising pathways for the detailed characteri- zation of exoplanets, but it is currently out of reach for most directly imaged exoplanets because high-dispersion spectrographs in the near-infrared lack coronagraphs to attenuate the stellar signal and the spatial resolution necessary to resolve the planet. Project HiRISE (High-Resolution Imaging and Spectroscopy of Exoplanets) ambitions to develop a demon- strator that will combine the capabilities of two flagship instruments installed on the ESO Very Large Telescope, the high-contrast exoplanet imager SPHERE and the high-resolution spectrograph CRIRES+. I will first present a status of the project with simulations, prelim- inary design, expected performance, and I then will present the astrophysical perspectives for the project.

⇤Speaker

sciencesconf.org:horse:206427 A Fabry Perot Based Instrument for Biomarker detection

1 1 1 Sagi Ben-Ami⇤ , Mercedes Lopez-Morales , Andrew Szentgyorgyi , and Gonzalo Gonzalez Abad1

1Harvard-Smithsonian Center for Astrophysics (CfA) – Cambridge, MA 02138, United States

Abstract

With new missions and surveys such as TESS and SPECULOUS, the discovery of the first transiting, potentially earth-like planets is just around the corner. Once discovered, those planets will immediately become the focus of observations in search of atmospheric biomarkers such as H2O, CH4, O3, and O2. Recent studies suggest the latter will be best detected from the ground. Here we present a study of technical and observational parameters which will produce the most sensitive observations of O2 using instrumentation on the next generation of extremely large telescopes (ELTs). Our study suggests spectral resolution well in excess of R ˜100,000 is optimal for O2 detection. Therefore, we have developed a concept instrument based on an array of Fabry Perot Interferometers capable of achieving spectral resolutions in excess of R ˜300,000 on ELTs. Despite its high spectral resolution, the concept instrument has modest dimensions, and allows high throughput. We discuss simulations re- sults, suggesting that such an instrument can reduce the number of observed transits needed for molecular oxygen detection by ˜30% and more. Finally, we discuss design parameters and the unique aspects that need to be taken into account in the design of such an instru- ment, and present initial data from a lab pathfinder demonstrating its capabilities.

⇤Speaker

sciencesconf.org:horse:221400 Detecting Isotopologues in Exoplanet Atmospheres

1 Paul Molliere⇤

1Sterrewacht Leiden, Huygens Laboratory – Niels Bohrweg 2, 2333 CA Leiden, Netherlands

Abstract

The cross-correlation technique is a well-tested method for exoplanet characterization, having lead to the detection of various molecules, and to constraints on atmospheric temper- ature profiles, wind speeds, and planetary spin rates. A new, potentially powerful application of this technique is the measurement of atmospheric isotope ratios. In particular HDO/H2O ratios can give unique insights in the formation and evolution of planets and their atmo- spheres. In this talk I will report on the detectability of molecular isotopologues in the high-dispersion spectra of exoplanet atmospheres. I will show why we expect to see 13CO already with the class of current telescopes, once instruments such as CRIRES+ become available. The more exciting detection of HDO will be more challenging, but it could become a prime science case for the first-light instrument METIS on the European ELT: for Proxima Cen b, a single night of observation may be enough to detect HDO if the planet is water-rich. For more mas- sive self-luminous planets the HDO detection may help to constrain the planets’ accretion history.

⇤Speaker

sciencesconf.org:horse:220366 39 Characterisation of Atmosphere Dynamics and Structure with Doppler Velocimetry and High-Resolution Spectroscopy High-Resolution and Velocimetry Doppler with Structure and Dynamics Atmosphere of Characterisation N'Diaye Mamadou spectroscopy integral-field and imaging high-contrast with GTC/FRIDA on capabilities observation exoplanet Exploring Lothringer Joshua Birkby, Jayne Crossfield, Ian Mehrle, Nicholas (MEASURE) SURvEY Exoplanet MMT the from results Preliminary Johnson John Charbonneau, David Fortney, Jonathan Montet, Ben Birkby, Jayne Schwarz, Henriette Hood, Callie Spectroscopy High-Resolution with LHS6343C Dwarf Brown Transiting Benchmark the Studying Goulinski Nadav planets free-floating of rate capture The Santos dos A. Leonardo planets small of atmospheres upper the observing in opportunities and Challenges Boucher Anne SPIRou with Spectroscopy Transit Resolution High of Simulations Halverson Sam Blake, Cullen Baker, Ashley Atmospheres Exoplantary of Characterization the for Instrument New A Oxyometer: The Antoniciello Giuliano removal feature spectral stellar and telluric for procedure independent Model contributions Poster of List Eleanor Spring Eleanor Spectroscopy Resolution High Using b Pegasi 51 of Signal Light Reflected Elusive the Detecting Mirror: Black Silva Miguel Gonçalves, Ruben Machado, Pedro Silva, José Model independent procedure for telluric and stellar spectral feature removal

1 Giuliano Antoniciello⇤

1Dipartimento di Fisica e Astronomia - Universit`adi Padova (DFA) – Vicolo Osservatorio, 3 35122 Padova, Italy

Abstract

The accuracy of ground-based high resolution spectroscopy of transiting exoplanets is limited by the presence of telluric lines, arising from atomic and molecular transitions in chemical species of Earth atmosphere. We can discriminate between stellar features, telluric lines and spectral signatures of planetary atmospheres by exploiting the rest frame di↵er- ences between the planetary signal, the host star and the Earth atmosphere. During the time of observations, telluric lines and stellar features can be considered almost constant in wavelength in the reference frame of the observer, while telluric absorption varies with airmass and water vapour content. However, during the transit, the planet’s radial veloc- ity varies on the scale of tenths of km/s, and such velocity variation results in a Doppler shift with the order of magnitude of 1 Angstrom. Here we propose to remove the telluric lines and the stellar features from high-resolution spectra with a model independent pro- cedure based on Principal Component Analysis. Our spectra have been obtained with the CARMENES spectrograph at Calar Alto Observatory and the PEPSI spectrograph at LBT. Our aim is to detect the spectral signatures of Na and TiO in hot Jupiters’ atmospheres, and to characterize the atmospheric vertical profile.

⇤Speaker

sciencesconf.org:horse:222027 The Oxyometer: A New Instrument for the Characterization of Exoplantary Atmospheres

1 1 2,3 Ashley Baker⇤ , Cullen Blake , and Sam Halverson

1Department of Physics Astronomy [University of Pennsylvania] (UPenn) – 209 S 33rd St Philadelphia, PA 19104, United States 2MIT Kavli Institute for Astrophysics Space Research – 77 Massachusetts Ave, 37-241, Cambridge, MA 02139, United States 3NASA Sagan Fellow – United States

Abstract

With TESS and other ground-based surveys searching for rocky exoplanets around cooler, nearby stars, the number of Earth-size exoplanets well-suited for atmospheric follow-up stud- ies will increase significantly, enabling the study of the planets’ compositions and their for- mation mechanisms. For atmospheric characterization, these systems will each still require a significant amount of observing time. As a result, JWST will only be able to target a small fraction of the most interesting targets, and the usefulness of ground based observato- ries will remain limited by telluric atmospheric absorption. Here we explore a new method for ground-based exoplanet atmospheric characterization that relies on simultaneous, di↵er- ential, ultra-narrow-band photometry. The instrument uses custom-cut wedge prisms and a narrow-band interference filter that enables simultaneous observing over two 0.3nm full width at half maximum bands spaced 1nm apart. This design enables one band to overlap the 760nm oxygen band head, which can be accessible in systems with high line-of-sight velocities, while the other imaging band is centered on an oxygen-free continuum region. Given the expected planet output from TESS, we estimate that multiple systems discovered by next generation of exoplanet surveys will be amenable to ground-based characterization by our instrument, which we call an oxyometer. We show that observations of an Earth- like planet orbiting an 8 magnitude M4 dwarf using an oxyometer on a 10m telescope can achieve a signal-to-noise ratio of 3 in eleven transits. We describe the design of our oxyometer and present a test detection of a 50ppm faux-transit signal in lab in addition to an on-sky photometry sequence to demonstrate the ease of use of the compact instrument design.

⇤Speaker

sciencesconf.org:horse:221836 Simulations of High Resolution Transit Spectroscopy with SPIRou

1 Anne Boucher⇤†

1University of Montreal – Canada

Abstract

SPIRou, the new infrared spectro-polarimeter at the CFHT, will soon provide us with near-infrared spectroscopy at high resolution (R ˜73500) over an unprecedented large simul- taneous spectral range (0.98–2.35 um). This will greatly enhance our ability to characterize the atmosphere of exoplanets from the ground via the transit spectroscopy method. Here, we present the SPIRou simulations that were developed to show its capabilities for exo- planet characterization, how it should perform relative to the previous instruments, such as CRIRES, and how it will contribute to advance this field. Namely, SPIRou will be able to detect and constrain the abundance of the main atmospheric constituents of giant planets, as well as measure the speed of their upper-atmosphere winds.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:226771 Challenges and opportunities in observing the upper atmospheres of small planets

1 Leonardo A. Dos Santos⇤

1Observatoire Astronomique de lUniversit´ede´ Gen`eve (ObsGE) – chemin des Maillettes CH-1290 Sauverny, Switzerland

Abstract

Characterizing the atmospheres of small planets has been extremely challenging with the current instruments, and even with the operation of JWST, many questions will still remain. The observation of the upper atmospheres of sub-Neptune sized planets using ground- and space-based high-resolution spectroscopy present an important opportunity to study plane- tary evolution in the context of comparative exoplanetology. In this contribution, I will show how we can use FUV transit spectroscopy from space to infer about the presence of water in the lower atmospheres of nearby rocky planets and to probe the composition of clouds in Neptune-sized planets. In addition, I will briefly discuss the opportunity to study planetary evolution by observing atmospheric escape in planets of varying ages.

⇤Speaker

sciencesconf.org:horse:221192 The capture rate of free-floating planets

1 Nadav Goulinski⇤†

1Technion - Israel Institute of Technology – Israel

Abstract

Evidence of exoplanets with orbits that are misaligned with the spin of the host star may suggest that not all bound planets were born in the protoplanetary disc of their cur- rent planetary system. Observations have shown that free-floating Jupiter-mass objects can exceed the number of stars in our Galaxy, implying that capture scenarios may not be so rare. To address this issue, we construct a three-dimensional simulation of a three-body scattering between a free-floating planet and a star accompanied by a Jupiter-mass bound planet. We distinguish between three di↵erent possible scattering outcomes, where the free- floating planet may get weakly captured after the brief interaction with the binary, remain unbound or ‘kick out’ the bound planet and replace it. The simulation was performed for di↵erent masses of the free-floating planets and stars, as well as di↵erent impact parameters, inclination angles and approach velocities. The outcome statistics are used to construct an analytical approximation of the cross-section for capturing a free-floating planet by fitting their dependence on the tested variables. The analytically approximated cross-section is used to predict the capture rate for these kinds of objects, and to estimate that about 1percent of all stars are expected to experience a temporary capture of a free-floating planet during their lifetime. Finally, we propose additional physical processes that may increase the cap- ture statistics and whose contribution should be considered in future simulations in order to determine the fate of the temporarily captured planets.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:222934 Studying the Benchmark Transiting Brown Dwarf LHS6343C with High-Resolution Spectroscopy

1 1 2,3 4 5 Callie Hood⇤ , Henriette Schwarz , Jayne Birkby , Ben Montet , Jonathan Fortney , David Charbonneau3, and John Johnson3

1University of California at Santa Cruz (UCSC) – 1156 High St, Santa Cruz, CA 95064, United States 2University of Amsterdam – Netherlands 3Harvard University – Massachusetts Hall, Cambridge, MA 02138, United States 4University of Chicago – United States 5University of California at Santa Cruz (UCSC) – 1156 High Street, Santa Cruz, Ca 95064, United States

Abstract

The techniques developed for high-resolution spectroscopic characterization of exoplanets can also be applied to a brown dwarf/M-dwarf system, allowing us to measure a model- independent mass and radius for the brown dwarf while also measuring its atmospheric abundances. Robust tests of brown dwarf formation and evolution models require bench- mark objects that can be precisely characterized. However, there are currently no cool, old, field brown dwarfs with model-independent measurements of their masses and radii. LHS 6343C, a brown dwarf transiting one member of a wide M+M binary system, provides a unique opportunity to make such mass and radius measurements. Furthermore, this data set approaches the type of data we might expect from a planet in the habitable zone of an M-dwarf star, allowing us to identify and address some of the associated challenges, such as strong stellar lines and only a small change in the companion’s velocity over the course of one night. I will present preliminary results from applying this technique to K-band spectra of LHS 6343 observed with NIRSPAO on Keck II.

⇤Speaker

sciencesconf.org:horse:222018 Preliminary results from the MMT Exoplanet SURvEY (MEASURE)

1 1 2 3 Nicholas Mehrle⇤ , Ian Crossfield , Jayne Birkby , and Joshua Lothringer

1Massachusetts Institute of Technology (MIT) – 77 Massachusetts Ave, Cambridge, MA 02139, United States 2Leiden Observatory, Leiden University – P.O. Box 9513 2300 RA Leiden, Netherlands 3University of Arizona (Lunar and Planetary Laboratory) – Tucson, AZ, United States

Abstract

We report on results from the MMT Exoplanet SURvEy (MEASURE), a survey of 11 hot Jupiter/sub Saturn planets across a range of masses and temperatures. Its goal is to characterize the atmospheres of these planets in terms of composition and atmospheric structure, and ultimately determine the transition region where a hot Jupiter’s atmosphere inverts. MEASURE is a 40 night program observing in the near infrared H/K bands on MMT/ARIES at R=30,000. Observing at high spectral resoltion allows for the detection of individual molecular species in a planet’s atmosphere and also for a model-dependent detection of the p-T profile. Because the planet undergoes a radial velocity change of several to several 10’s of km/s over the course of observations, spectral features in its atmosphere will exhibit a characteristic doppler shift, while features from the star or the Earth remain stationary. This allows features from the planet to be identified, even at the 10ˆ-4 level. We will report on the progress of the MEASURE survey, and our analysis of its target planets.

⇤Speaker

sciencesconf.org:horse:221763 Exploring exoplanet observation capabilities on GTC/FRIDA with high-contrast imaging and integral-field spectroscopy

1 Mamadou N’diaye⇤

1Observatoire de la Cote d’Azur (OCA) – Observatoire de la Cote d’Azur – France

Abstract

Over the past few years, several large ground-based facilities have enhanced their exo- planet direct imaging capabilities to observe planetary companions and debris disks around nearby stars. By early 2020s, the Gran Telescopio Canarias (GTC) will have its first high- contrast capabilities with FRIDA. This near-infrared imager and integral field spectrograph will operate with GTCAO, the adaptive optics system of the telescope that will feed the instrument with a corrected beam achieving a 60% Strehl ratio in K-band. While cover- ing a broad range of astrophysical topics, FRIDA will enable the study of circumstellar environments with its high-resolution spectroscopy capabilities and coronagraph modes. In this communication, we discuss possible combinations of high-dispersion spectroscopy and high-contrast imaging for advanced exoplanet observations with this instrument.

⇤Speaker

sciencesconf.org:horse:221520 Characterisation of Atmosphere Dynamics and Structure with Doppler Velocimetry and High-Resolution Spectroscopy

1,2 1 1,2 1,2 Jos´eSilva⇤ , Pedro Machado , Ruben Gon¸calves , and Miguel Silva

1INSTITUTE OF ASTROPHYSICS AND SPACE SCIENCES (IA) – Tapada da Ajuda - Edif´ıcio Leste -2o Piso 1349-018 Lisboa, Portugal, Portugal 2Faculdade de Ciˆencias [Lisboa] (FCUL) – Universidade de Lisboa, Campo Grande, Edificio CS, 7749-076 Lisboa, Portugal

Abstract

High-resolution visible and infrared spectroscopic capabilities applied to the Solar Sys- tem planets opens a new window by accessing atmospheric composition, mixing ratios and isotopic ratios. In particular, the measurement of spectral lines’ Doppler shifts allow the retrieval of wind velocities and this technique has a strong potential to be used to constrain planetary circulation dynamics also on exoplanets. The Doppler velocimetry method has already been proved successful in measuring winds on Venus’ cloud top with VLT/UVES (Machado et al. 2012) and CFHT/ESPaDOnS (Machado et al. 2017) and adaptation to the gas giants Jupiter and Saturn is an ongoing work with promissing preliminary results.

The Doppler shift used to compute the velocity of a weather layer, measured in solar light scattered on the planet’s dayside is the result of two instantaneous motions: a motion be- tween the Sun and the planet upper cloud particles, which scatter incoming radiation in all directions; a motion between the observer and the planet clouds, resulting from tropocentric velocity of the planet cloud particles in the observer’s frame. The measured Doppler shift is the combined e↵ect of these instantaneous motions (Machado et al.2017).

With the addition of the new instrument ESPRESSO to VLT, we also believe that our Doppler method can be adapted to perform seismology on the planets of the solar system, detecting and characterising infrasound waves on Jupiter and Saturn, using the high fre- quency capabilities of this instrument. This will be a starting point for the development of versatile atmosphere characterization tools, provided that with the future E-ELT we are likely to be able to detect the reflected light spectrum on Neptunes and Super-Earths (Martins2015), and in selected cases to constrain atmosphere composition and to derive wind velocities (Kawahara2012).

⇤Speaker

sciencesconf.org:horse:204109 Black Mirror: Detecting the Elusive Reflected Light Signal of 51 Pegasi b Using High Resolution Spectroscopy

1 Eleanor Spring⇤†

1University of Amsterdam – Netherlands

Abstract

The detection of the stellar light reflected by an exoplanet can provide a wealth of insight into that planet’s atmosphere, internal heat and fundamental structure. Unfortunately such a signal is challenging to isolate, and the detection of reflected light in the optical regime has rarely been presented. Highly-resolved spectral data, however, reveal a finely spaced forest of molecular lines. The reflected spectrum from an orbiting exoplanet is significantly Doppler shifted in comparison to its parent star. Therefore at high resolution, the Doppler shifted spectrum reflected from an exoplanet can be disentangled from the stellar spectrum. Thus high resolution spectroscopy o↵ers the possibility of extracting the elusive stellar reflection - and insights into the composition and structure of the exoplanet itself. As the wealth of data from the observations of planetary systems grows, and we enter the age of extremely large telescopes, there is a necessity to perfect robust methods for characterising planetary atmo- spheres, including composition, structure and dynamics. When a star’s light is reflected by a planet, that planet’s signature will be hidden within that light. I am using high-resolution data from HARPS-N of 51 Pegasi b - the first exoplanet and hot Jupiter ever discovered orbiting a Sun-like star. 51 Peg does not transit, and thus transmission spectroscopy is not a feasible method for investigating this star. Therefore this high resolution method o↵ers a new means of detecting the planet’s signal and learning about its atmosphere, by detecting the 51 Peg’s Doppler shifted reflected light signal, and ultimately analysing how interaction with 51 Peg’s atmosphere has altered the stellar light. I present a reduced data set, alongside a model planetary signal which I will use to isolate the true planetary signal.

⇤Speaker †Corresponding author: [email protected]

sciencesconf.org:horse:226196 39 List of participants

Aickara Gopinathan Sreejith Austrian Academy of Sciences Austria Allart Romain Geneva Observatory Switzerland Alonso-Floriano F. Javier Leiden Observatory The Netherlands Antoniciello Giuliano Univerity of Padova Italy Baker Ashley University of Pennsylvania USA Bean Jacob University of Chicago USA Bigot Lionel Observatoire de la Cote d'Azur France Birkby Jayne University of Amsterdam The Netherlands Bonomo Aldo University of Turin Italy Boucher Anne University of Montréal Canada Bourrier Vincent Geneva Observatory Switzerland Brogi Matteo University of Warwick UK Burt Jennifer MIT USA Casasayas-Barris Nuria Instituto de Astrofísica de Canarias Spain Chen Guo Instituto de Astrofísica de Canarias Spain Chiavassa Andrea Observatoire de la Cote d'Azur France Collet Remo Stellar Astrophysics Centre Aarhus University Danemark Crossfield Ian MIT USA Desert Jean-Michel University of Amsterdam The Netherlands Desiderà Daria Univerity of Padova Italy Dittmann Jason MIT USA Donati Jean-Francois Institut de Recherche en Astrophysique et Planétologie France dos Santos Leonardo University of Geneva Switzerland Dravins Dainis Lund Observatory Sweden Dumusque Xavier University of Geneva Switzerland Espinoza Nestor Max Planck Institute for Astronomy Heidelberg Germany Fortney Jonathan University of California Santa Cruz USA Garcia-Mejia Juliana Harvard College Observatory USA Gilli Gabriella Institute of Astrophysics and Space Science Portugal Gonçalves Ruben Institute of Astrophysics and Space Science Portugal Goulinski Nadav Technion – Israel Institute of Technology Israel Guilluy Gloria University of Turin Italy Halverson Samuel University of Pennsylvania USA Haywood Raphaëlle Harvard College Observatory USA Hoeijmakers Jens Geneva Observatory Switzerland Hood Callie University of California at Santa Cruz USA Jenkins James Universidad de Chile Chile Jordan Andres Pontificia Universidad Católica de Chile Chile Kempton Eliza University of Maryland USA Keles Engin Leibniz Institute for Astrophysics Potsdam Germany Komacek Thaddeus University of Chicago USA Line Michael Arizona State University USA Louie Dana University of Maryland USA Lovis Christophe University of Geneva Switzerland McIntyre Sarah Australian National University Australia Malavolta Luca University of Padova Italy Machado Pedro Institute of Astrophysics and Space Sciences Portugal Meadows Victoria University of Washington USA Mehrle Nicholas MIT USA Molaverdikhani Karan Max Planck Institute for Astronomy Heidelberg Germany Mollière Paul Leiden Observatory The Netherlands Nardetto Nicolas Observatoire de la Cote d'Azur France Nortmann Lisa Instituto de Astrofísica de Canarias Spain Palle Enric Instituto de Astrofísica de Canarias Spain Pearse David James Cook University Australia Petrus Simon Institut de Planétologie et d'Astrophysique de Grenoble France Poretti Ennio INAF - Telescopio Nazionale Galileo Italy Pino Lorenzo Anton Pannekoek Institut for Astronomy The Netherlands Quirrenbach Andreas University of Heidelberg Germany Rauscher Emily University of Michigan USA Rugheimer Sarah University of St. Andrews UK Schwarz Henriette UC Santa Cruz USA Silva José Institute of Astrophysics and Space Science Portugal Singh Vikash Observatory of Catania Italy Snellen Ignas Leiden University The Netherlands Sousa-Silva Clara MIT USA Thorsbro Brian Lund Observatory Sweden Vigan Arthur Laboratoire d'Astrophysique de Marseille France Wang Ji California Institute of Technology USA Wilson Paul Anthony Leiden Observatory The Netherlands Wyttenbach Aurélien Leiden Observatory The Netherlands Yan Fei Max Planck Institute for Astronomy Heidelberg Germany Yoffe Gideon Weizmann Institute of Science Israel Zhao Lily Yale University USA 39