Water and Organic Molecules in Protoplanetary Disks - High-R Spectroscopy -

1. TMT science & instrument workshop Oct. 16-17, 2013 @ Tokyo Water and Organic Molecules in Protoplanetary Disks- High-R Spectroscopy - Hideko Nomura(Tokyo Tech.) Matthew J. Richter (UC Davis)

2. §1 Introduction

3. From protoplanetary disk to planets Dust growth & settling Planetisimal formation Collisional growth of planetisimals Planet formation Dispersal of gas (e.g., Hayashi et al. 1985) Observationally diagnose planet formation theory and origin of materials in our Solar System (C) Newton Press

4. Obs. of Gas in Protoplanetary Disks UV (sub)mm H2Lyman-Werner band transitions TMT will be able to observe IR lines with high-R & high sensitivity 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. Optical [OI] 6300A NIR H2 v=1-0 S(1), S(0), CO Dv=2, Dv=1, etc. MIR H2 v=0-0 S(1), S(2), S(4) H2O, OH, HCN, C2H2, CO2, NH3 (Ground & Spitzer Space Telescope) ALMASV 100AU TW Hya FIR [OI] 63um, 145um, CO, H2O, CH+, HD, etc. (Herschel Space Observatory) HCO+(4-3)

5. Need for High-R Spectroscopy Typical 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 H2 S(4)@8mm AB Aur Gemini/TEXES (R>80,000) S(2)@12mm S(1)@17mm Kepler rotation F~10-14erg/s/cm2, Dv~10-20km/s (Bitner et al. 2007, 2008)

6. Need for High-R Spectroscopy Typical 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 High-R spectroscopy@TMT will enable us to detect fainter lines & analyse profiles of weaker lines VLT/CRIRES (R=100,000) Subaru/IRCS (R=20,000) HD141569 SR21 Inner hole @ 7AU (Goto et al. 2006) 4.7mm CO line profiles → Line emitting regions MICHI (Y.K. Okamoto) Kepler rotation Inner hole @ 11AU (Pontoppidan+ 2008) → See also Matt Richter’s poster

7. Water & Organic Mol. in PPDs ESA Detect H2O snow lines Detect complex organic molecules with high-R spectroscopy @ TMT Halley a §2 formation of organic mol. H2O, CO2, CH4, CH3OH, H2CO, NH3, etc. §3 H2O snow line

8. §2 Formation of Organic Moleclues in PPDs

9. Observed Interstellar Molecules CH+ HCN H2CO HC3N CH3OH HC5N HCOOCH3 HC7N CS HNC H2CS HCOOH CH3CN CH3CCH CH3C3N HC9N CO HCO H2CN CH2NH CH3NC CH3NH2 CH3COOH HC11N CN OCS HNCO CH2CO CH3SH CH3CHO CH2CHCHO C2H5CN C2 CH2 HNCS NH2CN NH2CHO CH2CHCN CH3C4H CH C2H C3H C4H C5H C6H CH3C5N H2C6 CO+ C3 c-C3H c-C3H2 H2C4 c-C2H4O CH3OCH3 CF+ CO2 C3N H2C3 HC3NH+ CH2CHOH C2H5OH C2O C3O CH2CN C6H- C2S C3S HCCNC CH3COCH3 HCO+ CH3 HNCCC OHCH2CH2OH C2H5OCHO HOC+ C2H2 CH4 HCS+ HOCO+ H2COH+ C8H- HCNH+ CH2OHCHO CN- C5N- CH3CONH2 Amino acids in comet @ STARDUST Amino acids in meteorites ⇔ relation with interstellar molecules ? →amino acids ? (Elsila et al. 2009) C4H- NH2CH2COOH? C3N- by ~1975 after ~1997

10. Complex Molecule Fomration on Grain Surface cold: < 20K C, O, N, S, CO, … warm: 30-50K H desorption NH2, HCO, … CH3O grain surface grain surface \ Saturated mol. Unsaturated mol. HCOOCH3, NH2CHO, … migrate UV, CR, X-rays UV CH4, H2O, NH3, H2S, CH3OH, … themal (e.g., Garrod+ 2006, 2008) Complex molecules are formed on grains More complex molecules on warm grains

11. Complex Molecules on Warm Grains OSU chemical network (Harada et al. 2010, Garrod et al. 2008) CH3OH line spectra CH3OH Tdust 3 4 6 7 8 9 10 ALMA band Methanol will be observable only at outer disk even with ALMA… ↓ Detect complex molecules & understand grain surface reactions at planet forming region with TMT! Z/R 30-50K (Walsh, Millar, HN et al. 2013, submitted) Flux Density [Jy] C2H5OH CH3COCH3 aceton Z/R Frequency [GHz] Strong methanol lines will be observable R [AU] R [AU] Complex mol. are formed on warm grains at T~30-35K(~50A) = cometary region

12. MIR HCOOH Lines @ TMT! telluric ALMA HCOOH TMT! Try first detection of MIR formic acid lines from protoplanetary disks with TMT! Z/R R [AU]

13. §3 H2O Snow Line

14. CO Snow Lines in Disks HD163296 SMA CO6-5@691GHz 13CO2-1@220GHz C18O2-1@220GHz CO3-2@346GHz C17O3-2@337GHz CO2-1@231GHz dust settling 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! CO snow line @ R~155AU (Qi et al. 2011) TW Hya ALMA SV @band7, DCO+ 5-4 ALMA cycle 0 N2H+ 5-4 [DCO+] /[HCO+] =0.3 CO snow line @ R~30AU (Qi et al. 2013c) (Mathews et al. 2013)

15. Obs. of water lines from PPDs cold FIR lines warm FIR lines hot MIR lines Spitzer hot H2O@10-35mm, TTSs: detect, HAEBEs: upper limits Herschel warm H2O TTSs, HAEBEs: @55-180mm Herschel cold H2O @267mm, 539mm, TW Hya, HD100546 Herschel/HIFI TW Hya H2O, OH, HCN, C2H2 AA Tau Spitzer/IRS (Hogerheijde+ 2011) (Carr & Najita 2008) (Riviere-Marichalar+ 2012) [OI] H2O Herschel/PACS AA Tau

16. H2O snow lines in PPDs TW Hya Spitzer/IRS Spitzer/IRS model Inner hole AA Tau H2O line ratios + disk model → predict H2O snow lines The results are model dependent… DR Tau Herschel PACS HIFI AS 205 model with snow line H2O Snow line @ ~1AU H2O Snow line @ ~4AU (Meijerink+ 2009) (Zhang+ 2013)

17. H2O Snow Line by High-R Obs. Line width ~ 10-20km/s →need high-R spectroscopy (R~100,000) for analysis Line fluxes @ Spitzer > 1e-14 erg/s/cm2 TMT will be able to analyze statistical properties of H2O snow lines! (Carr & Najita 2011) TMT/MICHI Kepler rotation

18. 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