1. 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)

2. §1 Introduction

3. 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

4. Obs. of Gas in Protoplanetary Disks 12 CO 6-5, 3-2, 2-1, 1-0, 13 CO 3-2, 2-1, 1-0, C 18 O 2-1, 1-0, HCN, HNC, DCN, CN, CS, C 34 S, C 2 H, H 2 CO, HCO +, H 13 CO +, DCO +, N 2 H +, HC 3 N, c-C 3 H 2, etc. (sub)mm H 2 v=1-0 S(1), S(0), CO v=2, v=1, etc. H 2 Lyman-Werner band transitions Optical [OI] 6300A [OI] 63um, 145um, CO, H 2 O, CH +, HD, etc. (Herschel Space Observatory) H 2 O, OH, HCN, C 2 H 2, CO 2, NH 3 (Ground & Spitzer Space Telescope) FIR H 2 v=0-0 S(1), S(2), S(4) NIR MIR UV HCO + (4-3) ALMA SV TW Hya 100AU TMT will be able to observe IR lines with high-R & high sensitivity

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 Kepler rotation S(1)@17 m S(2)@12 m H 2 S(4)@8 m AB Aur Gemini/TEXES (R>80,000) (Bitner et al. 2007, 2008) F~10 -14 erg/s/cm 2, v~10-20km/s

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 Kepler rotation See also Matt Richters poster 4.7 m CO line profiles Line emitting regions HD141569 Subaru/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

7. a Water & Organic Mol. in PPDs ESA Halley H 2 O, CO 2, CH 4, CH 3 OH, H 2 CO, NH 3, etc. §3 H2O snow line §2 formation of organic mol. Detect H2O snow lines Detect complex organic molecules with high-R spectroscopy @ TMT

8. §2 Formation of Organic Moleclues in PPDs

9. by ~ 1975 C4H- CH2OHCHO CH3CONH2 CN-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

10. 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. HCOOCH 3, NH 2 CHO, … NH 2, HCO, … CH 3 O grain surface (e.g., Garrod+ 2006, 2008) UV migrate CH 4, H 2 O, NH 3, H 2 S, CH 3 OH, … Saturated mol. Complex molecules are formed on grains More complex molecules on warm grains

11. 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] CH 3 OH C 2 H 5 OH CH 3 COCH 3 aceton T dust 30-50K (Walsh, Millar, HN et al. 2013, submitted) OSU chemical network (Harada et al. 2010, Garrod et al. 2008) Frequency [GHz] CH 3 OH line spectra 3 4 6 7 8 9 10 Flux Density [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!

12. ALMA TMT! Line flux [erg/s/cm 2 ]5e-17 Line width [km/s]20 R15,000 NELF [erg/s/cm 2 ]5e-16 S/N3 Integration 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

13. §3 H2O Snow Line

14. CO Snow Lines in Disks SMA CO6-5@691GHz CO3-2@346GHz CO2-1@231GHz 13 CO2-1@220GHz C 18 O2-1@220GHz C 17 O3-2@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 N 2 H + 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!

15. Obs. of water lines from PPDs hot MIR lines warm FIR lines cold FIR lines AA Tau Spitzer/IRS (Carr & Najita 2008) H 2 O, OH, HCN, C 2 H 2 TW Hya (Hogerheijde+ 2011) Herschel/HIFI (Riviere-Marichalar+ 2012) AA Tau Herschel/PACS [OI] H2OH2O Herschel cold H2O @267 m, 539 m, TW Hya, HD100546 Spitzer hot H2O @10-35 m, TTSs: detect, HAEBEs: upper limits Herschel warm H2O TTSs, HAEBEs: @55-180 m

16. H2O snow lines in PPDs (Zhang+ 2013) TW Hya Spitzer/IRS Herschel Inner hole Spitzer/IRS H 2 O Snow line @ ~4AU H 2 O 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… PACSHIFI

17. 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/cm 2 ]1e-15 Line width [km/s]20 R120,000 NELF [erg/s/cm 2 ]2e-16 S/N25 Integration time [min]20 Line fluxes @ Spitzer > 1e-14 erg/s/cm 2 (Carr & Najita 2011) TMT/MICHI TMT will be able to analyze statistical properties of H2O snow lines!

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