Observations of proto-planetary disks and exo- planets with the JWST E. Pantin, P.O. Lagage and the...

Observations of proto-planetary disks and exo-planets with the JWST

E. Pantin, P.O. Lagageand the MIRI science team

28-30/05/2010 KielDisks and exoplanets : sciences cases for interferometry

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SPITZER (IRAC, 8 m) JWST (MIRI, 7.7 m)


Thermal Background






+ FGS: Tunable Filter Instrument 1.5-5 um, R= 100, NRM (21 baselines)


NIRCAM coronagraphic occulters



3 apodized SPOTS 2 apodized WEDGES


MIRI Fields of View, Coronagraphs

F1550C or (F1550C+ F1140C) => Teff , CO2, cloudsF1065C + F1140C => Ammonia, clouds, T° probeF0560W => waterF0770W => methaneAll + modeling => some atmospheric parameters

Some degeneracies exist => combination with NIR is crucial

4QPM Coronagraphs

15.5µm 11.4µm10.65µm

24 x 24 arcsec.

Low Resolution Spectrometer5 x 0.6 arcsec

Imager75 x 113 arcsec

Medium Resolution Spectrometer

> 3.5 x 3.5 arcsec

Lyot Mask 23m30” x 30”


Principle of 4QPMPrinciple of 4QPM

IWA /D 0.35"



(n-1)e =(n-1)e =/2/2


NIRCAM MIRI TFI-NRM

Central wavelength

2.5 m 15 m 4 m

Median angular resolution

0.1 " 0.6 " 0.07 "

Coronagraphic mode

Yes Yes NA

Field ~ 20x20 " ~ 20x20 " ~ 0.6 "


Sensitivity




Major points:

• extreme sensitivity combined fairly good angular resolution ("a VISIR in space")

• stability

• JWST is not meant to discover new exoplanets but characterize already known ones

Exo-planets

Exo-planets imaging science case


Simulated coronagraphic images



NIRCAM:M0 star4 pc2 Mj

7 AU

1 M1 MJupJup 5 M5 MJupJup 10 M10 MJupJup

500 K500 K 10 Myr10 Myr 165 Myr165 Myr 670 Myr670 Myr

300 K300 K 80 Myr80 Myr 1 Gyr1 Gyr 3.5 Gyr3.5 Gyr

MIRI:M2V star10 pc5, 10, 15 AU1h integration

= 11.4 m


Rejection performance





Beichman, 2010


Parameters space





NIRCAM/TFI/MIRI

M stars

Bright early-type stars

GROUND-BASED IMAGING

JWST exoplanets imaging science case

A simulated targets sample for exoplanets detection


Simulated performances



Sample program Monte-Carlo ~700 stars)1000 runsd< ~150age : 1 Myr- 1 Gyr

1 dispersion, all stars

25 best (highest detection success rate)

symbol sizes fractional detection rate

Beichman et al., 2010


Full sample




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NIRCAM MIRI TFI-NRM


M stars only





NIRCAM MIRI

young planets < Mj

old planets > Mj

Giant planets formation mechanism around low-mass stars:

The M stars niche for MIRI imager


The ("adolescent") M stars opportunity




The M stars opportunity



12 M0-M5 stars

d=10-40 pc

ages < 200 Myr

•TW Hya (10 Myr) Pic mg (12 Myr)•Tucana-Horologium (30 Myr)•AB doradus (80 Myr)•Castor mg (200 Myr)

complementary NIRCAM and TFI observations are compulsory to assess the planetary nature of sources found !!

Exoplanets characterization using mid-IR spectroscopy


Exoplanets mid-IR spectra




Hot Jupiter primary and secondary transits (NIRCAM, NIRspec)



courtesy of J. Valenti

HD209459 b

secondary transit primary transit

t=6h

hot neptunes spectra (4 transits) are accessible using NIRCAM-NIRspec instruments


Exo-Earths transit spectra (NIRspec, MR)



NIRspec simulated spectrum of a (H2 rich) super-Earth exoplanet (GL581-like, M3, 6 pc, 20 transits)

Clampin, 2009


MIRI

• transit spectroscopy (probably not as performant as NIRCAM/NIRspec, TBC)

• imaging (++)

• spectral deconvolution using the MRS

A couple of (non exhaustive) niches concerning telluric planets !


The molten exo-Earths opportunity







Miller-ricci et al., 2009

•No atmosphere 100 000 yr cooling time

•Atmosphere 1-10 Myr cooling time


Exo-rings

SECP rings can survive on Gyr-timescales !

Pantin et al., in prep


Exo-rings

Detection limit

"Fomalhaut b-like" ring

Circumstellar disks

Spectroscopy of PP disks


Spectroscopy of PP disks : a key program for MIRI GTO observations









Full inventory of organic (pre-biotic) species :

o NH3

o C6H6

o CH4

o HCO+

o HCN

Full inventory of organic (pre-biotic) species :

o NH3

o C6H6

o CH4

o HCO+

o HCN

THE MIRI GTO imaging proposal on proto-planeteary disks


Goals

study:

large-scale geometry of the disks: MIRI tremendous sensitivity allows to observe the disks up to very large distances from the star

for the first time, a large sample of T-Tauri disks are observable/resolvable in the mid-IR

disks (dust) vertical structure dust settling dust coagulation disks stratification

search for forming/formed planets signature: direct detection of forming protoplanet is highly unlikely (brightness peak@accreting phase ?)

embedded massive bodies produce structures in disks:o gapso bright rimso asymmetries

MIRI study of Large Scale Structure of

Protoplanetary Disks


What do we observe in the mid-IR range ?

• Mainly the thermal emission from heated dust grains

• Mainly the inner rim (1500 K) that produces >90% of the total 10 m flux (continuum)

coronagraphic mode is compulsory to avoid detector saturation (Fmax=20 mJy) and decrease photon noise

• Once, the inner rim masked/subtracted, the thermal emission produced at the disks' surface (=1), on intermediate distance scales (3-100 AU)

• PAH emission (7.7, 8.6, 11.3 m) on larger scales ( Rout)





~1 AU,10 mas

~100 AU


Large Scale Parameters



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measure: scale height at a given distanceflaring parameterdust sizes vs distancedust composition vs distance

indirect indications/constraints on:

gas contentturbulence (small grains)surface density



HD97048 8.6 m VLT/VISIR(Lagage et al. 2006)


Disks in "transition" phase



HD 95881 model sketch


Continuum profiles

In the case of Herbig disks, the PAH emission (8.6, 11.3 m) is brighter and more extended than continuum emission

MIRI MIRI


Scattered mid-IR emission

MIRI study of Disks Vertical Structure


Disks appareance


PAH dominated spectrum

Disks appareance as a probe of dust settling

Signatures of giant planets formation in PP disks


Simulated observations of a PP disk with a giant exoplanet

ELT/METIS (2018 + ?)1 Mj@20 AU

d = 100 pc

Herbig Ae-type disk


Why "long-wavelength" data (>20 m) are also very important ?

HD142527 Q2 PSF subtracted

PSF subtraction

Verhoeff et al., 2010, submitted

11.8 m

19 m19 m

11.8 m

1"

HD142527 Herbig starVISIR image SiC (10.8 um)

= 18.7 m


The MIRI disks imaging GTO sample

• 10.6, 11.4, 15.5, 23 m coronagraphic imaging

• 10 Herbig / 14 T-Tauri / 2 brown dwarves

• A large sample of moderately inclined disks

• A handful of almost edge-on disks ("disk tomography", direct imaging)

• a selection of "transition disks" (last stages of planet formation ???)

• Several star forming regions/evolutionary stages represented (Chameleon, Taurus-Aurigae, Scorpus, Ophiuchi

• Good overlap/complementarity with the spectroscopic program

Imaging of debris disks


NIRCAM imaging



Pic-like disk @ 100 pc

residual wavefront error

(~ 200 "zodis")


MIRI imaging




Complementary with existing/future facilities




Conclusions

no major step in angular resolution capabilities (~ground)

not an exoplanets "hunter"

but

amazing sensitivity (extended sources !) and stability: 103 gain factor

full set of space-born coronagraphic capabilities 2-25 m

JWST will characterize wide separation (5-100 AU) giant exoplanets (M>Ms) and discover new ones around faint (M) stars

spectroscopy of giant exoplanets R=10 R=3000

unique to detect/characterize thermal emission ( scattered emission) of disks


Things the JWST cannot (or badly) do

• faint stars (M!), no AO limitation

• PSF subtraction• very long integrations• follow-ups


Compared performances

ELT/METIS(see M.Kissler-Patig presentation, B.Brandl poster)

good sensitivity to point sources and peaky structures (~25 Jy at 10 m)

excellent angular resolution (0.05"/10 m), direct imaging of planetary regions (r<30 AU) in closest disks (d<150 pc) will be achievable

very limited sensitivity (~10 mJy/"2, nul in some cases !) to extended emission

JWST/MIRI(see A.Glasse presentation)

very good sensitivity to point sources (~1 Jy at 10 m)

angular resolution (0.3" at 10 m) comparable to that of current 8m-class telescopes instruments (e.g. VISIR)

awesome sensitivity to extended emission (~1 Jy/"2 at 10 m)

Same wavelength coverage, high level of complementary Same wavelength coverage, high level of complementary between extended source sensitivity/angular resolutionbetween extended source sensitivity/angular resolution Same wavelength coverage, high level of complementary Same wavelength coverage, high level of complementary between extended source sensitivity/angular resolutionbetween extended source sensitivity/angular resolution

Observations of proto-planetary disks and exo- planets with the JWST E. Pantin, P.O. Lagage and the...

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