FORMATION AND EVOLUTION OF PLANETARY SYSTEMS:
PROBING INITIAL CONDITIONS AND OUTCOMES WITH E-ELT
Michael R. Meyer
Institute for Astronomy
Department of Physics
(and many, many, others)
HARMONI Early Science, Oxford, 2 July, 2015
What we need to explain…
Pepe, Ehrenreich, & Meyer, 2014, Nature, V513, 358
Collapsing Cores & Specific Angular Momentum
Time
Williams & Cieza (2011) ARAA; see also Belloche (2013)
Structure of Protostellar Disks
1 AU
From M. Meyer, Physics World, November, 2009
Based on Dullemond et al. (2001) with artwork from R. Hurt (NASA)
100 AU
JWST/ELT Complementary Capabilities
Physical Resolution:
JWST
ELT
1.65 mm
10 mm
1.65 mm
10 mm
Spectral Resolution :
Field of View:
15 pc
1 AU
7 AU
.2 AU
1 AU
50 pc
3 AU
20 AU
.5 AU
3 AU
150 pc
10 AU
60 AU
1.5 AU
10 AU
450 pc
30 AU
180 AU
5 AU
30 AU
R = 100 (molecular features)
R = 1000 (atomic features)
R = 10,000 (30 km/sec)
R = 100,000 (3 km/sec)
JWST
JWST
ELT
ELT
2’ (star clusters within 1 kpc)
JWST
1.5” (circumstellar disk at 150 pc) ELT
METIS Instrument Baseline

Imaging at 3 – 19 μm. with low/medium
resolution slit spectroscopy as well as
coronagraphy for high contrast imaging.
 High
resolution (R ~ 100,000) IFU spectroscopy
at 3 – 5 μm, including extended instantaneous
wavelength coverage.
 Work
at the diffraction limit with single conjugate
(SC) and eventually assisted by a laser
tomography adaptive optics (LTAO) system.
Instrument Concept
Common Fore-Optics
AO Wavefront Sensor
Imager
IFU Spectrograph
Warm Calibration Unit
as well as Q!
(SC)AO Performance
H band
D=39m, V=6 guide star, 100 Hz closed loop
N band
LM band
Probing Planet-Forming Disks from 1-1000 mm
Follette et al. (2015), van der Marel et al. (2013); METIS/MICADO/ALMA Science
Inner CO Gas vs. Outer Dust Continuum:
CO gas with METIS
Dust continuum with ALMA
Transitional disk SR 21
Pinella et al. (2015); Pontoppidan et al. (2008); METIS/HARMONI Science
(Multiple) Planet Forming Disks: HD 100546
L-band Scattered Light
Avenhaus et al. (2014)
Spectro-astrometry with CRIRES
Brittain et al. (2014)
(Multiple) Planet Forming Disks: HD 100546
Not yet detected in K-band (Quanz et al. 2013; 2015b)
and there are other examples…
Direct Detection (and Characterization)
of Circumplanetary Disks
Quanz et al. (2015b); METIS/HARMONI/MICADO Science
Direct Detection of Thermal Emission for Planets
of Known Mass with E-ELT: Calibrating the Models
RV+Gaia follow-up requires imaging photometry and IFU spectroscopy!
Quanz et al. (2015a); METIS/MICADO/HARMONI Science
Phenomenological Planet Populations:
RV Data
GI
CA
Benz et al. (2014); Galvagni & Mayer (2014); Forgan & Rice
(2013)
Direct (Non-)
Detections of Gas
Giant Planets
Few massive planets
at large orbital radii.
NACO-LP: Chauvin et al. (2014)
Not good for GI
[>3 Mjup @ > 50 AU]
dN/da ~ ab
Lafrenerie et al. (2007);
Nielssen & Close (2009);
Heinze et al. (2010);
Chauvin et al. (2010);
Delorme et al. (2011);
Vigan et al. (2012);
Reggiani et al. (submitted); SPHERE+ERIS
DIRECT IMAGING: DISRUPTING PLANET
FORMATION THEORY WITH THE E-ELT
a. Start with a fit to RV distributions (Cumming et al. 2008)
with brown dwarf companions (Reggiani et al. submitted)
b. Evidence for dependence of Co, planet frequency over
range of mass and orbital radius, on stellar mass
(Johnson et al. 2010; Clanton et al. 2014).
c. Initial conditions (and theory) suggest dependence on
ratio of planet mass to star mass.
d. RV/micro-lensing/Imaging consistent with log-normal
surface density peaking at 10 AU (Meyer et al. in prep).
METIS
The Survey:
75 G stars
< 50 pc
< 300 Myr
-0.5
-0.5
Log(Jupiter Mass)
1.0
0.5
0.0
Log(Jupiter Mass)
1.0
0.5
0.0
1.5
1.5
HARMONI
Follow-up
Required!
10
20
30
Separation (AU)
40
50
10
20
30
Separation (AU)
40
50
High Resolution Spectra of Brown Dwarfs and Planets:
METIS/HARMONI Characterization Science
Brown dwarf doppler imaging with CRIRES
Crossfield et al. (2014)
Wind speeds on planets with CRIRES
Snellen et al. (2014)
Star Clusters, Disks, & Planets: E-ELT Opportunities
SYNERGIES
=> Building on legacy of VLT: E-ELT, JWST, and ALMA.
=> METIS and first-light instruments HARMONI & MICADO.
STAR CLUSTERS => Resolved IMFs within 10 Mpc.
DISKS
=> E-ELT will resolve planet-forming disks (gas and dust) inside 10 AU.
=> Spectro-astrometry: of what are forming planets in disks made?
=> E-ELT will detect planets in formation (and circumplanetary disks).
PLANETS
=> Direct detection of planets with known mass (constrain models).
=> Collide planet formation theory with planet populations vs. stellar mass.
=> Characterize gas giant planets, including phase maps, and weather!
=> Possible to image (and characterize) a handful of super-earths.
BACKUP SLIDES
Resolved Stellar Pops: HARMONI/MICADO @ Confusion Limit
PSF
MMT-AO 6.5m PSF
from Close et al. 2003.
0.5 kpc
5 kpc
Simulated Trapezium Observations
R(Sky Noise) = 1 Rc = 0.2 pc
using Hillenbrand & Carpenter (2000). Hcomp(at Rc) < 24 mag
25 kpc
R(sky noise) = 2.5 Rc = 0.5 pc
Hcomp(at Rc) < 17.8 mag.
50 kpc
R(Sky Noise) = 4 Rc = 0.8 pc
Hcomp(at Rc) < 15.3 mags.
0.5 Mpc
R(Sky Noise) > 20 Rc = 4-5 pc
Core Radius not resolved.
Primordial Disk Evolution: A Scenario…
Volatiles
(Ciesla et al; Banzatti et al.)
Few AU
Williams & Cieza ARAA (2011); Effects of Photoevaporation? Ercolano et al. (2015)
Typical Disk Parameters
Parameter
Median
~1σ Range
Log(M(disk)/M(star))[all ~1 Myr]
[detected disks
only]
-3.0 dex
-2.3 dex
±1.3 dex
±0.5 dex
Disk lifetime
-q]
Temperature
power
law
[T(r)~r
Parameter
2-3 Myr
0.6
Median
1-6 Myr
0.4-0.7
~1σ Range
R(inner)
0.1 AU
~0.08-0.4 AU
R(outer)
Surface density power [Σ(r) ~ r-p]
[Hayashi min. mass nebula]
[steady state viscous α disk]
200 AU
0.6
1.5
1.0
~90-480 AU
0.2-1.0
(predicted)
(predicted)
Surface density norm. Σo (5AU)
14 g cm-2
±1 dex
Taken from (or interpolated/extrapolated from):
Muzerolle et al. (2003), Andrews & Williams (2007), Hernandez et al. (2008), Isella et al. (2009)
Circumplanetary Disk Detection with ALMA (mm grains)
From Pineda et al. Cycle 3 Proposal (submitted)
CA Phenomenology: Planet Masses and Orbits
Solid growth time: tp ~ Rp rp / [ Sd x
with
Sd ~ M*/a and
d]
3)
~
sqrt(M
/a
d
*
tp ~ a5/2/ [M*3/2] cf. gas disk lifetime td ~ 1/M*
Given aouter, there is a timescale td ~ 1/M* giving Rp.
aouter ~ [td M*3/2]2/5 ~ M*1/5
Very hard to form critical mass core beyond 10s of AU (all stars).
If Mp set by disk accretion: Mp ~ [dMacc/dt ] td ~ M*2 x (1/M*) ~ M*
Planet Mass linearly related to star mass.
GI Phenomenology: Planet Masses and Orbits
Toomre Parameter: Q ~ cs(a) W/ GS(a)
with
Sd ~ M*/a,
3), and c ~ sqrt(T) ~ (M /a)1/4
~
sqrt(M
/a
s
*
d
*
Q ~ 1/ [M*1/4 a3/4]
Depends “weakly” on stellar mass, more strongly on radius.
For typical disk parameters, should operate > 50 AU.
Typical fragment mass would be ~ cs4/S(a) ~ 5 Mjupiter.
Massive planets, beyond 50 AU, independent of stellar mass.
Companions to Stars: Brown Dwarfs and Planets
Reggiani et al. (2011; 2013; 2015); Sahlman et al. (2011)
Planet Populations versus Stellar Mass:
Co ~ M*
Mp/M*
Meyer, Reggiani, & Quanz (in preparation)
Can ELTs Directly Image Super-Earths?
Hinz et al. (2010), Quanz et al. (2015) and the METIS Science Team