Water and Organic Molecules in

Protoplanetary Disks- High-R Spectroscopy -

TMT science & instrument workshop 　

Oct. 16-17, 2013 @ Tokyo

Hideko Nomura (Tokyo Tech.)Matthew J. Richter (UC Davis)

§1 Introduction

From protoplanetary disk to planets

Planetisimal formation

Collisional growth

of planetisimals

Planet formation

Dispersal of gas

Dust growth& settling

(e.g., Hayashi et al. 1985)

Observationally diagnose planet formation theory and

origin of materials in our Solar System

(C) Newton Press

Obs. of Gas in Protoplanetary Disks

12CO 6-5, 3-2, 2-1, 1-0,13CO 3-2, 2-1, 1-0,

C18O 2-1, 1-0,HCN, HNC, DCN, CN, CS, C34S, C2H, H2CO,HCO+, H13CO+, DCO+,

N2H+, HC3N, c-C3H2, etc.

(sub)mm

H2 v=1-0 S(1), S(0),CO Dv=2, Dv=1, etc.

H2 Lyman-Werner band transitions

Optical[OI] 6300A

[OI] 63um, 145um, CO, H2O, CH+, HD, etc.

(Herschel Space Observatory)

H2O, OH, HCN, C2H2, CO2, NH3

(Ground & Spitzer Space Telescope)FIR

H2 v=0-0 S(1), S(2), S(4)

NIR

MIR

UV

HCO+(4-3)

ALMA SVTW Hya100AU

TMT will be able to observe IR lines with high-R & high

sensitivity

Need for High-R SpectroscopyTypical width of IR lines from PPDs ~ 10-20km/s→need high-R spectroscopy (R~15,000) for detection need very high-R (R~100,000) for analysing profiles

Kepler rotation

S(1)@17mm

S(2)@12mm

H2 S(4)@8mmAB Aur Gemini/TEXES (R>80,000)

(Bitner et al. 2007, 2008)F~10-14erg/s/cm2, Dv~10-20km/s

Need for High-R SpectroscopyTypical width of IR lines from PPDs ~ 10-20km/s→need high-R spectroscopy (R~15,000) for detection need very high-R (R~100,000) for analysing profiles

Kepler rotation

→ See also Matt Richter’s poster

4.7mm CO line profiles → Line emitting regions

HD141569Subaru/IRCS (R=20,000)

(Goto et al. 2006)

(Pontoppidan+ 2008)

VLT/CRIRES (R=100,000) SR21

Inner hole @ 11AU

Inner hole @ 7AU

High-R spectroscopy@TMT will enable us to detect fainter

lines & analyse profiles of weaker

lines

(Y.K. Okamoto)

MICHI

a

Water & Organic Mol. in PPDs

ESA

Halley

H2O, CO2, CH4, CH3OH, H2CO, NH3,

etc.

§3 H2O snow line

§2 formation of organic mol.

Detect H2O snow lines Detect complex organic moleculeswith high-R spectroscopy @ TMT

§2 Formation of

Organic Moleclues in

PPDs

H2COH+HOCO+HCS+

CH4C2H2HOC+

HCNH+

HNCCCCH3HCO+ OHCH2CH2OH

HCCNCC3SC2S CH3COCH3

C8H-

CH2CNC3OC2O

C2H5OHCH2CHOHHC3NH+H2C3C3NCO2CF+

CH3OCH3c-C2H4OH2C4c-C3H2c-C3HC3CO+

CH3C5NC6HC5HC4HC3HC2HCH

CH3C4H

H2C6

CH2CHCNNH2CHONH2CNHNCSCH2C2

C2H5CNCH2CHCHOCH3CHOCH3SHCH2COHNCOOCSCN

HC11NCH3COOHCH3NH2CH3NCCH2NHH2CNHCOCO

HC9NCH3C3NCH3CCHCH3CNHCOOHH2CSHNCCS

HC7NHCOOCH3HC5NCH3OHHC3NH2COHCNCH+

C6H-

C2H5OCHO

by ~1975

C4H-

CH2OHCHO

CH3CONH2CN- C5N-

C3N-NH2CH2COOH?→ amino acids ?

Observed Interstellar Molecules

Amino acids in comet @ STARDUST

Amino acids in meteorites⇔ relation with

interstellar molecules ?

(Elsila et al. 2009)

after ~1997

Complex Molecule Fomration on Grain Surface

grain surface

C, O, N, S, CO, …H

\

desorption UV, CR,X-rays

themal

cold: < 20K warm: 30-50K

Unsaturated mol.HCOOCH3, NH2CHO, …

NH2, HCO, … CH3O

grain surface

(e.g., Garrod+ 2006, 2008)

UV

migrate

CH4, H2O, NH3, H2S, CH3OH, …

Saturated mol.

Complex molecules are formed on grainsMore complex molecules on warm grains

Complex Molecules on Warm Grains

Complex mol. are formed on warm grains at T~30-35K(~50A) = cometary region

Z/R

R [AU]

Z/R

R [AU]

CH3OH

C2H5OH

CH3COCH3

aceton

Tdust

30-50K

(Wals

h,

Mill

ar,

HN

et

al. 2

01

3,

sub

mit

ted

)

OSU chemical network (Harada et al. 2010, Garrod et al. 2008) 　

Frequency [GHz]

CH3OH line spectra3 4 6 7 8 9 10

Flux D

en

sity

[Jy

]

ALMA band

Strong methanol lines will be observable

Methanol will be observable only at outer disk even with ALMA…

↓Detect complex molecules &

understand grain surface reactions at planet forming region with TMT!

ALMA

TMT!

Line flux [erg/s/cm2] 5e-17Line width [km/s] 20R 15,000NELF [erg/s/cm2] 5e-16S/N 3Integration time [min] 15

MIR HCOOH Lines @ TMT!

Try first detection of MIR formic acid lines from protoplanetary disks with

TMT!

Z/R

R [AU]

HCOOH

telluric

§3 H2O Snow Line

CO Snow Lines in DisksSMA

CO6-5@691GHzCO3-2@346GHzCO2-1@231GHz

13CO2-1@220GHzC18O2-1@220GHzC17O3-2@337GHz

HD163296

dust settling

(Qi et al. 2011)CO snow line @

R~155AU

(Mathews et al. 2013)

[DCO+]/[HCO+]

=0.3

ALMA SV@band7, DCO+ 5-4

ALMA cycle 0

N2H+ 5-4

(Qi et al. 2013c)

CO snow line @

R~30AU

TW Hya

H2O snow lines around low mass stars will be difficult to access even

with ALMA…↓

Detect H2O snow lines by obs. with high-spectral res. @ TMT!

Obs. of water lines from PPDs

hot MIR lines

warm FIR lines

cold FIR lines

AA TauSpitzer/IRS

(Carr & Najita 2008)

H2O, OH, HCN, C2H2

TW Hya

(Hogerheijde+ 2011)

Herschel/HIFI(Riviere-Marichalar+

2012)

AA TauHerschel/PACS

[OI] H2O

Herschel cold H2O @267mm, 539mm, TW Hya, HD100546

Spitzer hot H2O@10-35mm, TTSs: detect, HAEBEs: upper limitsHerschel warm H2O TTSs, HAEBEs: @55-180mm

　H2O snow lines in PPDs

(Zhang+ 2013)

TW Hya Spitzer/IRS

Herschel

Inner hole

Spitzer/IRS

H2O Snow line @ ~4AUH2O Snow line @ ~1AU(Meijerink+ 2009)

model

model with snow line

AA Tau

DR Tau

AS 205

H2O line ratios + disk model→ predict H2O snow lines

The results are model dependent…

PACS HIFI

H2O Snow Line by High-R Obs.Line width ~ 10-20km/s

→need high-R spectroscopy (R~100,000) for analysis

Kepler rotation

Line flux [erg/s/cm2] 1e-15Line width [km/s] 20R 120,000NELF [erg/s/cm2] 2e-16S/N 25Integration time [min] 20

Line fluxes @ Spitzer > 1e-14 erg/s/cm2

(Carr & Najita 2011)TMT/MICHI

TMT will be able to analyze statistical properties of H2O snow

lines!

Summary

High-R spectroscopy of transition lines of water & organic molecules in PPDs

Detect H2O snow line by very high (R~100,000) spectroscopy for

understanding rocky/gaseous planet forming regions

Detect complex organic molecules and understand grain surface reactions in planet forming regions by high

(R~15,000) spectroscopy for predicting formation of more complex molecules