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 transitionsOptical

[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

HalleyH2O, 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

migrateCH4, 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

CH3COCH3aceton

Tdust

30-50K

(Wal

sh, M

illar,

HN e

t al.

2013

, su

bmitt

ed)

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

Frequency [GHz]

CH3OH line spectra3 4 6 7 8 9 10

Flux

Den

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, C2H2TW 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!

SummaryHigh-R spectroscopy of transition lines of

water & organic molecules in PPDsDetect H2O snow line by very high

(R~100,000) spectroscopy for understanding

rocky/gaseous planet forming regionsDetect 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