Atmospheric Study of Exoplanets by Transmission Spectroscopy (keynote talk)

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1 Atmospheric Study of Exoplanets by Transmission Spectroscopy (keynote talk) Akihiko Fukui Okayama Astrophysical Observatory (OAO), NAOJ Main collaborators: ObservaDon: N. Narita, T. Hirano, N. Kusakabe, M. Onitsuka, T. Ryu Theory: M. Ikoma, Y. Hori, K.Krosaki, Y. Kawashima 2015 June 4 3 rd DTA

2 Studying Exoplanetary Atmospheres Expansion of Planetary Atmospheric Sciences Exoplanets have diverse atmospheric environments: temperature, composidon, stellar irradiadon, etc. Trace of Planetary FormaDon History Atmospheric composidon can vary depending on where and how the planet has formed Tool to Search for Biomarkers Future ground- based huge telescopes and space- based dedicated ones can probe biomarkers in possible habitable worlds

3 RelaDon with Planetary FormaDon/MigraDon Öberg et al Madhusudhan et al C/O rado can be a good tracer of formadon and migradon C/O rado in disk gas varies along with the orbital distance Water abundance ( metallicity) is also important (Madhusudhan et al. 2014)

4 Transmission Spectroscopy Atmosphere Star Observer Stellar Relative brightness flux Planet Transit Light Curves redder wavelength bluer wavelength Time When a planet transits, a part of the stellar light passes through the planetary atmosphere Atmospheric opacity changes with wavelength depending on the atmospheric composidon Atmosphere can be observed as a wavelength dependence of transit depth (=(R p /R s ) 2 )

5 Three ObservaDonal Techniques High- resolu,on Spectroscopy SensiDve to specific atomic and molecular lines e.g., Na, K, CO Low- resolu,on Spectroscopy Broad spectral features can be probed Rayleigh slope in opdcal and molecular features in NIR Mul,- band Photometry Overall spectral features can be studied Scale height, cloudy/hazy atmosphere Even small- to- mid class telescopes can be used Planet- to- star radius rado TheoreDcal transmission spectrum H 2 O Na K CH 4 1 Wavelength [μm] CH 4 CO

6 Hot- Jupiter Atmosphere: Alkali Metals (Na, K) In opdcal region, spectral features of Na (λ~589 nm) and K (λ~768nm) can be observed in hot Jupiter atmospheres can be probed by low- or high- resoludon spectroscopy The first atmospheric detecdon was achieved by Charbonneau et al. (2002), who detected Na in HD209458b by HST The first detecdon of exoplanet atmosphere (Na) in HD209458b Na and K have been detected in a number of hot Jupiters using HST and ground- based large telescopes HD189733b, WASP- 17b, HAT- P- 1b, XO- 2b, WASP- 31b, etc. Wavelength [nm] Charbonneau et al. 2002

7 Hot- Jupiter Atmosphere: Water In NIR region, molecular features can be observed by low- resoludon spectroscopy (or Spitzer photometry) Water (H 2 O) is predicted to be one of the most abundant molecules aker hydrogen in hot Jupiters The first detecdons of water in hot Jupiters HST/STIS transmission spectrum for HD209458b Spitzer spectrum for HD189733b Barman 2007 Tinel et al. 2007, Nature

8 Hot- Jupiter Atmosphere: Other Molecules DetecDons of other molecules, e.g., CH 4, CO 2, and CO, in addidon to H 2 O were reported based on the observadons by HST/NICMOS HD189733b XO- 1b Swain et al. 2008, Nature Tinel et al. 2010

9 Instrumental SystemaDcs HST/NICMOS spectra of HD189733b with different systemadc correcdons HST/NICMOS spectrum of HD189733b Swain et al. 2008, Nature The results from HST/NICMOS data are controversial due to instrumental systemadcs Researchers have learned that understanding the nature of instrumental systemadcs is very important Gibson et al. 2011

10 HST/WFC3 A new instrument, Wide Field Camera 3 (WFC3), was installed in HST in 2009 WFC3 offers smaller instrumental systemadcs and a new observadonal mode (spadal scan mode), which significantly reduce uncertaindes Water have been convincingly detected in a number of hot Jupiters by using HST/WFC3 Benneke 2015, submioed

11 Water Abundance Solar value Solar value Madhusudhan et al Benneke 2015, submioed Possible sub- Solar water abundance for three hot Jupiters (Madhusudhan et al. 2014) Water abundance could be underesdmated due to the presence of cloud or haze

12 C/O rado Posterior probability of C/O rado for HD209458b with different cloud models Benneke 2015, submioed C/O rado is also affected by the presence of cloud/haze C/O < 0.9 for many hot- Jupiter atmospheres (Benneke 2015)

13 Cloudy/Hazy Atmosphere Spectrum of WASP- 12b by HST, Gemini, and Spitzer Spectrum of WASP- 29b by Gemini Sing et al Gibson et al In some hot Jupiters, flat or feature- less spectra have been observed, indicadng cloudy or hazy atmospheres Understanding the nature of cloud/haze is important to extract the informadon of molecular abundances

14 Haze ProducDon in Low- temperature Atmosphere CH 4 can exist in low- temperature (T eq <1,000K) atmosphere Hydrocarbon haze (tholin) can be produced via photo- chemical processes e.g., Titan Liole has been studied for low- temperature atmospheres of exoplanets CH 4 C 2 H 2, C 2 H 4, C 6 H 6, hydrocarbon polymer (tholin) planet UV photo- dissociadon

15 Warm Jupiter WASP- 80b A Jovian planet transidng a bright late- K/early- M dwarf Discovered in 2013 (Triaud+ 2013) TheoreDcally and observadonally rare The planet is warm The equilibrium temperature is only 800K Tholin haze might exist Host star is acdve Strong UV flux Transit depth is large ~2.9% Suitable for tesdng existence condidons of tholin DistribuDon of TransiDng Jovian Planets around Bright Stars

16 MulD- band Photometry with Three Telescopes 1.88m & 1.4m 1.4m NIR three bands (J, H, and Ks) simultaneously We observed three transits NIR one band (J, H, or Ks) We observed two transits 0.5m OpDcal three bands (g, Rc, and Ic) simultaneously We observed two transits simultaneously with 188cm/ISLE

17 Example Light Curves 2013 Aug. 13 OAO 1.88m & 0.5m tel Oct m IRSF 0.5m 0.5m 0.5m 1.88m In total, we obtained 17 transit light curves in six bands.

18 Observed Transit Spectrum of WASP- 80b Fukui et al OpDcal spectrum (λ<1μm) is averagely ~1% higher than NIR at 2.9σ, possibly indicadng the existence of haze If true, this is consistent with the theoredcal predicdon

19 Atmospheres of super- Earths and Neptunes Lissauer et al. (2013) GJ3470b Hot super- Earths & Neptunes R Jup R Earth GJ1214b 55 Cnc e CoRoT- 7b Mass and Radius alone cannot uniquely determine the interior structure Rocky core + H/He gas Icy core + steam (H 2 O) Atmospheric composidon can provide important clue to speculate the formadon histories of super- Earths/Neptunes

20 ObservaDonal Requirements for Small Planets Transit depth = (R p /R s ) 2 Small planet around a sun- like star shows only a Dny transit Need small host star (M dwarf) Need nearby (bright) star Currently, only three transidng super- Earths/Neptunes are known around nearby M dwarfs GJ436b, GJ1214b, GJ3470b Planetary radius(r Earth ) Bright (Near) GJ436b GJ3470b circle s area transit depth GJ1214b R magnitude FGK dwarfs M dwarfs Faint (Far)

21 Super- Earth GJ1214b The most famous super- Earth - Discovered in 2009 as the first transidng super- Earth around nearby M dwarf (Charbonneau+ 2009, Nature) Early observadons showed a flat spectrum R p /R s - - Steam dominant or Cloudy? The NIR K s and op,cal B bands were in debate H 2 - rich + Solar- Metallicity H 2 - rich + sub- Solar + cloud H 2 O- rich B band K s band M p R p Period R s Clear hydrogen Steam Hydrogen + cloud 6.6 M Earth 2.6 R Earth 1.6 days 0.2 R sun Wavelength [μm] 2 de Mooij et al. (2011)

22 Our observadons with 1.4m IRSF and 8.2m Subaru NIR J,H,Ks band photometry with 1.4m IRSF OpDcal B- band photometry with 8.2m Subaru 2012 June August 12 J B H 2012 October 8 K s B

23 Observed Spectrum of GJ1214b Narita et al. 2013a,b We confirm that the spectrum is flat over from opdcal to NIR

24 Intensive NIR ObservaDons of GJ1214b by HST/WFC3 Kreidberg+ 2014, Nature 15 transits were obtained by HST/WFC3 SDll flat even with the marvelous precision Possibly covered by a thick cloud layer

25 Hot Uranus GJ3470b The third low- mass transidng planet around an M dwarf Discovered in 2012, originally by RV survey (Bonfils et al. 2012) The mass is similar to Uranus M p R p Period R s 14 M Earth 4.3 R Earth 3.3 days 0.5 R sun A rare sample to invesdgate low- mass planet atmosphere Bonfils et al. 2012

26 Time MulD- band Photometry by Two Telescopes at OAO OAO 1.88m/ISLE RelaDve stellar flux OAO 0.5m MITSuME

27 Observed Spectrum of GJ3470b Planet- to- star radius rado by Spitzer (Demory et al. 2013) Wavelength [nm] Fukui et al A sign of R p /R s variadon is observed The planet is not be covered by thick cloud GJ1214b

28 Follow- up ObservaDons by Other Teams Observed transmission spectrum of GJ3470b Fukui et al. (2013) Nascimbeni et al. (2013) by BLT (8.2m x 2) Ehrenreich et al. (2014) by HST/WFC3 NIR spectrum seems to be consistent with a flat line OpDcal spectrum has a slope, possibly indicadng the existence of haze Crossfield et al. (2013) by Keck (10m) Demory et al. (2013) by Spitzer Ehrenreich et al. (2014)

29 ObservaDons for Other Neptunes GJ436b hot Neptune around M dwarf HAT- P- 11b hot Neptune around K dwarf H 2 O Knutson et al. 2014, Nature Fraine et al. 2014, Nature A flat spectrum was observed in GJ436b, indicadng a cloudy or high- metallicity atmosphere A detecdon of H 2 O was reported in HAT- P- 11b

30 Future Prospects for super- Earths/Neptunes The current problem is the lack of good targets The next- generadon transit survey satellite TESS will find hundreds of transidng super- Earths around nearby M dwarfs Narita- san s talk TESS will be launched in 2017 OAO 1.88m telescope + a new muld- band camera MuSCAT (PI: N.Narita) Subaru TMT Search for sunny super- Earths In- depth observadons for selected super- Earths Toward atmospheres of Earth- size planets

31 Summary Transmission spectroscopy can probe exoplanetary atmospheres, which can provide informadon about the planetary formadon histories A lot of efforts have been made for hot Jupiters, detecdng water in many hot Jpiters mainly by HST/WFC3 Treatment of cloud/haze is important We conducted muld- band photometry for three transidng planets: WASP- 80b: detected a sign of haze GJ1214b: confirmed a flat spectrum GJ3470b: detected a non- flat spectrum We need more targets for super- Earths and Neptunes

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