CERN - Data Acces, Visualisation & Analysis CERN | July 2017

CERN - Data acces, Visualisation & Analysis CERN | July 2017

Damien Ségransan, University of Geneva and Geneva planet Search team

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation 55 Cnc DACE aims at federating the European expertise in exoplanets’ research by providing an open access to all type of published (exo)planets data with dedicated visualisation, exchange and analysis tools.

(Exo)planets related Data Access

- Wide range of published Observational Data such as Radial Velocities and Transit Light Curves - Exoplanets Tables : exoplanets.org & exoplanet.eu - Theoretical data such as planet synthesis populations

Visualisation & Statistical Online tools to compare, correlate and combine (Exo)planets data - Javascript visualisation library - Time series, images, correlation plots - Histograms, distribution parameters

Direct access to state of the art data analysis tools

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Principe: mesure du décalage Doppler - Jupiter-Soleil : 12 m/s - Saturne-Soleil: 3 m/s - Terre-Soleil : 8 cm/s

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Observatoire de La 1ère planète extrasolaire : Haute-Provence 51 Pegase Tel. de 193 cm

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Comment découvrir une nouvelle planète...

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Quelques années plus tard...

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Fantastique!

Mais que se passe-t-il?

Période : 44 jours Période : 1000 jours Orbite excentrique Orbite circulaire masse minimum : 2 Mjup masse minimum : 7 Mjup

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation

HARPS: précision < 1 m/s - Observatoire de Genève - Physikalisches Institut, Bern - Observatoire Haute-Provence ΔRV =1 m/s - Service d’Aéronomie, Paris - ESO

ΔRV =1 m/s Δλ=0.00001 A

ΔT =0.01 K 15 nm

Δp=0.01 mBar 1/1000 pixel

Pression contrôlée Température contrôlée

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation . .

HD10180 - a 7 planet low mass planetary system 6 Lovis et al., A&A 528, A112, 2011 4 ] s / m

[ 2

V RV [m/s] R P = 1.17 .. 2248 days 0 K=0.85 .. 4.5 m/s msin(i)=1.4 .. 65 M 2

213 meas. O-C rms =1.40 m/s 0 50 100 150 200 250 300 350 True Longitude [deg] ...... 10 5 ] s / m [ 0 C 5 C [m/s] 5 5 O O ] ] 5 ] s s s / / / m m m

[ 0 50 100 150 200 250 300 350 [ [

V V 0 V 0 True Longitude [deg] RV [m/s] R R RV [m/s] 0 RV [m/s] R

5 5 5

0 50 100 150 200 250 300 350 0 50 100 150 200 250 300 350 0 50 100 150 200 250 300 350 True Longitude [deg] . . . True Longitude [deg] . . True Longitude [deg] . 8 5 5

] 8

] 5 ] s s / s /

6 / m m 6 m [ [

[

0 0 60 C [m/s] C C C [m/s] C [m/s] C 4 4 O O O O O 4 ] ] 5 ] 5 s s 5 s / / / m

m 2 0 50 100 150 200 250 300 350 m [ [ 2 [ 0 50 100 150 200 250 300 350

2 0 50 100 150 200 250 300 350

V V True Longitude [deg] V True Longitude [deg] True Longitude [deg] RV [m/s] R RV [m/s] R RV [m/s] R 0 0 0 2 2 2 4 4

0 50 100 150 200 250 300 350 0 50 100 150 200 250 300 350 0 50 100 150 200 250 300 350 True Longitude [deg] True Longitude [deg] True Longitude [deg]

5 The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Transit photometry Flux δ R =( p Time R p R / R s s ) 2 =( F out - F in )/ F transit le Flux dans F transit du Flux hors F in out out

HD 209458b

Période : 3.524 jours Orbite circulaire Charbonneau et al. 2000 (ApJ 529, L45) demi-grand axe : 0.045Jupiter UA masse minimum : 0.7 Mjup HD 209458b Précision photométrique 0.2–0.4% Petit télescope de 10cm!!

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation ~3h

Jupiter ~1.7% HD 209458b

110 ppm/min

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation ρ = 1.3 g cm-3 ρ = 0.4 g cm-3

Jupiter HD 209458b

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation HR8799

Image dans prisent dans l’infrarouge proche - 1-2.5 microns Rapport de flux entre les planète et l’étoile : 10 000

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation HR8799 - découverte 2008, Marois. Distance : 129 AL Age : 30 million d’années (Soleil 5 Milliard d’années) Masse : 1.5 Msol Luminosité : 4.9 Lsol Température effective : 7300K (Soleil ~5800K)

4 planètes massives Température : 900-1100 K <=> 630 - 830 ° C Présence de Méthane et CO dans l’atmosphère

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation 1.593 microns) and H3 (1.667

Toute nouvelle Découverte Cheetham, Ségransan et al., Décembre 2016 Distance : 136 AL Age : 5 milliard d’années (comme le Soleil) Masse : 1.0 Msol Luminosité : ~1 Lsol Température effective : 5700 K

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Détection avec SPHERE/VLT 1.593 µm 1.667 µm

1 objet massif et très froid! Température : 400-500 K <=> 130 - 230 ° C Présence de Méthane et CO dans l’atmosphère Séparation 0.53’’ => ~23 UA

1.0-1.3 µm

Rapport de flux entre le companion et son étoile : 160 000 - 250 000

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Les chasseurs de planètes de l’Université de Genève

Les académiques (7) : F. Bouchy, D. Ehrenreich, C. Lovis, F. Pepe, D.Queloz, D. Ségransan, S. Udry, M. Mayor (retraite)

Les Post-Docs et collaborateurs scientifiques (~10) : S. Saesen, D. Bayliss, N. Blind, M. Marmier, N. Astudillo, V. Bourrier, H. Cegla, A. Cheetham, J-B. Delisle, X. Dumusque, …

Les Doctorants (~15) : E. Cersullo, A. Coffinet, U. Conod, A. Deline, H. Giles, B. Lavie, D. Martin, F. Motalebi, E. Obrzud, S. Peretti, M. Raimbault, J. Rey Cerda, E. Rickmann, T. Roger, A. Wyttenbach

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation 358 F. Mignard / Advances in Space Research 47 (2011) 356–364 to compute the location of the images during the CCD the relationship between the G magnitude and the more crossing. usual V magnitude as a function of the colour index While the above estimate of astrometric performances V I. One has with a sufficient accuracy for this purpose includes the CCD charge loss resulting from the energetic (JordiÀ and Carrasco, 2007), particles bombardment during the Gaia lifetime, it does G V 0:0107 0:0879 V I 0:1630 V I 2 not take into account other consequences of this bombard- ¼ À À ð À ÞÀ ð À Þ ment like the PSF distortion and the still poorly modelled 0:0086 V I 3 1 effects observed during CCD readouts at high frequency. þ ð À Þ ð Þ These sources of degradation in the CCD performances, meaning that a red star of visual magnitude 15, looks and susceptible of generating bias in image locations and brighter for Gaia than a hotter star of similar visual mag- are being closely investigated by the prime contractor nitude. The standard deviations in Table 2 are averaged (EADS Astrium), ESA and the Data Processing Consor- out over the sky and the actual accuracy in a particular tium. This issue remains today the main instrumental chal- direction on the sky varies slightly with the ecliptic latitude, lenge for Gaia and a serious source of complication for the by a factor of ±20% about the average for the parallax, data processing. In the performances indicated here, a mar- right ascension and proper motion in right ascension, while gin of 20% has already been applied to allow for unmod- the factor is less than 5% for the corresponding quantities elled effects, but in some range of magnitude or colours, in declination. This pattern is entirely determined by the the astrometric degradation could be larger, let alone the scanning law and fully understood. consequences for the calibration of the photometric and The sky-averaged performances are relevant for single spectroscopic data, which are not discussed in this paper. stars or quasars, for which one can fit a simple model with In summary the expected performances in Table 2 and a very small number of parameters to the individual obser- Fig. 1 are based on the best current knowledge of the vations to describe the slow displacement on the sky. Basi- instrument,GAIA as it is : designed, lancement combined withDec. the known2013. callyFin five de parameters mission do the 2018-2023 job, with two for the position capabilities of the data processing. at a reference epoch, two for the components of the proper FAQThe photon: arrival fluctuation is the main source of ran- motion and one for the parallax. For multiple stars, this dom noise for magnitudes between 12 and 20, while CCD becomes quickly more complex if the orbital period is com- saturationMission European and calibration Space eff ectsAgency bring a limitation to the parable to the mission length, in which case a full orbital astrometricDurée de precisionla mission of : the5-10 brightest ans stars. The model model must be considered. Long period binaries whose rel- allows2 miroirs for all 1,5x0.5 types of stars,m early or late types, giants or ative motion between the components is not noticeable dwarfsmasse: and 2030 includes km the reddening of the light during its over the mission length, only need a separation and a posi- journey through the interstellar matter. The sky-averaged tion angle as additional astrometric parameters and do not resultsorbite are :L2 summarised (0.01 AU/ in Table1.5 megakm) 2 for a nearly solar-like make the general model much more complex. Intermediate star. The magnitude scale used is defined by the optics cases with orbital periods between 20 and 100 years, transmission and detector quantum efficiency over the vis- can be handled by taking a time-variable proper motion, ible wavelengthsMesure (k précise350–1000 nm), de meaning la position that the val- deor >10 equivalently6 étoiles by adding two acceleration components ues in the table should’ not change very much with star and possibly, a derivative of higher order. colours.=> Dé Whattection is relevant herede forplanètes comparison purposesgéantes is parBut thereastrométrie are instances where the single observation precision is more meaningful, specifically for solar system objects. The corresponding expected positional accuracy over one field transit, amounting to a total of 40 s of inte- gration on the CCDs, is shown in Fig. 1 as a function of the Gaia magnitude. There are clearly two regimes, according to the star brightness, with a nearly constant accuracy for the bright end and a standard degradation due to photon noise for sources fainter than G = 12 with also a contribu- tion of the CCD readout noise at the faint end. The saw- tooth wiggles at the bright end are of instrumental origin and result from the particular mode of CCD operation to deal with saturation. This diagram indicates that for bright asteroids Gaia has the potential of improving the astrometry by a factor of a 100 compared to the current ground-based capabilities. However, a bright asteroid means in general a significant Fig. 1. Astrometric precision expected with Gaia for a single observation angular size and a shift between barycentre and photocen- corresponding to a 40 s transit on the Gaia astrometric CCDs. For faint stars, this is primarily determined by the photon noise, while at the bright tre, which will degrade the nominal precision of point like end, the CCD operations close to saturation, calibration and attitude sources. But for fainter sources, the angular dimension will determination take over. decrease quickly below the width of the optical response of Les prochaines missions spatiales

TESS — Transiting Exoplanet Survey Satellite - USA - 2018 https://www.youtube.com/watch?v=mpViVEO-ymc

CHEOPS — ESA Small mission - Swiss Space Office - 2018 http://www.cosmos.esa.int/web/cheops

JWST — NASA/ESA - 6.5 m Launch 2018 with Ariane 5 https://www.youtube.com/watch?v=v6ihVeEoUdo

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation

European-Extremely Large Telescope

European Southern Observatory Miroir segmenté : 39 m (798 miroirs de 1.4m) Miroir secondaire : 4m Mise en service :2024

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation

A Roadmap to Interstellar Flight P. Lubin, UC Santa Barbara, 2016

Dans une génération, faire une image des systèmes planétaires autour des 3 étoiles les plus proches du Soleil, Proxima Cen, Alpha Cen A, B Distance : 4.2 AL Durée du voyage : 20 ans

The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation