Jonathan Tennyson Physics and Astronomy, University College London Emory October 2012 Molecular line lists for exoplanets and other atmospheres Artist’s impression of HD189733b C. Carreau, ESA

Spectrum of a hot star: black body-like

Infra red spectrum of an M-dwarf star

Cool atmospheres : dominated by molecular absorption Brown Dwarfs M-dwarf The molecular opacity problem Exoplanets? M Dwarf Planet Marley & Leggett (2008)

Cool stars: T = 2000 – 4000 K Thermodynamics equilibrium, 3-body chemistry C and O combine rapidly to form CO. M-Dwarfs: Oxygen rich, n(O) > n(C)‏ H 2, H 2 O, TiO, ZrO, etc also grains at lower T C-stars: Carbon rich, n(C) > n(O) H 2, CH 4, HCN, C 3, HCCH, CS, C 2, CN, etc S-Dwarfs: n(O) = n(C) Rare. H 2, FeH, MgH, no polyatomics Also (primordeal) ‘metal-free’ stars H, H 2, He, H , H 3 + only at low T

Sub-stellar objects: CO less important L-Dwarfs: T ~ 1500 K H 2, H 2 O, CH 4 T-Dwarfs: T ~ 1000 K ‘methane stars’ Y-Dwarfs: T ~ 500 K ammonia signature Exoplanets: hot Jupiters super-Earths How common are these objects? Deuterium burning test using HDO? Burn D only No nuclear synthesis

7 Taken from Bill Borucki’s presentation 2012: (nearly) every star has planets

Transit of Venus June 8 th 2004 June 5 th /6 th 2012

Radial velocity / Occultation Period = 3.52 days Mass = 0.69 ±0.05 M Jupiter Radius = 1.35 ±0.04 R Jupiter Density = 0.35 ±0.05 g/cm 3 HD b

Beaulieu et al., 2007 Knutson et al., 2007 HD189733b: Primary transit with Spitzer

Tinetti et al., Nature, 448, 163 (2007) ‏ Water, different T-P Water line list: BT2 Barber et al., 2006

Confirmation of Water,methane and hazes! Beaulieu et al., 2007 Knutson et al., 2007 Swain et al., 2008 Pont et al., 2007 G. Tinetti (private communication, 2008)‏

Giovanna Tinetti, UCL So far discovered: Water H 2 O Methane CH 4 Carbon dioxide CO 2 Carbon monoxide CO On HD189733b with more to come HD189733b too hot for life HCCH / HCN degeneracy

 m R ~ 300 ESA M3 candidate mission PI Giovanna Tinetti (UCL) launch 2024? Exoplanet Characterisation Observatory Telescope Baffle V-groove Side Sunshield GaAs Solar Cells Detectors Service Module 1.5m Silicon Carbide Mirror

Primordial (Metal-poor) Terrestrial Planets (Oxidising) Giant-Planets & Cool Stars (Reducing atmospheres) Already available H 2, LiH HeH +, H 3 + H 2 D + OH, CO 2, O 3, NO H 2 O, HDO, NH 3 H 2, CN, CH, CO, CO 2, TiO HCN/HNC, H 2 O, NH 3, ExoMolO 2, CH 4, SO 2, SO 3 HOOH, H 2 CO, HNO 3 CH 4, PH 3, C 2, C 3, HCCH, H 2 S, C 2 H 6, C 3 H 8, VO, O 2, AlO, MgO, CrH, MgH, FeH, CaH, AlH, SiH, TiH, NiH, BeH, YO Molecular line lists for exoplanet & other atmospheres Available from elsewhere Already calculated at UCL Will be calculated during the ExoMol project list of molecules Full details: J. Tennyson and S.N. Yurchenko, MNRAS, 425, 21 (2012) NaH, HF, HCl

Why theory, not experiment?

Exoplanets

Absorption ( T =300K) spectrum of NH 3 : Accuracy Experiment Theory

Absorption ( T =300K) spectrum of NH 3 : Accuracy Experiment Theory

Absorption ( T =300K) spectrum of NH 3 : Accuracy

Theory

Completeness: Absorption of ammonia (T=300 K) Less than 30,000 NH 3 lines known experimentally: BYTe contains 1.1 billion lines, about 40,000 times as many! BYTe

Absorption spectra of 14 NH 3 : Temperature effect

Ab initio calculations DMSPES Variational calculations Rovibrational wavefunctions Rovibrational energies Intensities (Einstein A if ) Line list Refinement Method: Spectrum from the “first-principles”

Shayesteh et al 2007 MOLPRO Line list: MgH Potential energy curve Dipole moment curve Line list: 6690 lines, N max =60 Solve for the motion of the nuclei MOLPRO REFINED Ab initio: solve for motion of electrons B Yadin et al, MNRAS 425, 34 (2012) LEVEL 8.0 R. Le Roy, Waterloo, Canada

Line list (in progress): C 2 Solve for the motion of the nuclei New program duo Sergei Yurchenko Line list: being computed … Potential energyDipole moment MOLPRO T. W. Schmidt et al 2011 Istvan Szabo REFINED

Dipole moment LEVEL 8.0 DVR3D C3C3 Potential energy Ab initio 18 electrons Ground electronic state Solve for the motion of the nuclei Line list: Ab initio: solve for motion of electrons to be computed … CASSCF P. Jensen, C. McMichael Rohlfing, and J. Almlöf, 1992, J. Chem. Phys. 97, 3399.

Dipole moment TROVE: Yurchenko, Thiel, Jensen 300 K line list, Clara Sousa-Silva PH 3 Potential energy Tunneling motion neglected Solve for the motion of the nuclei Line list: T=300 K ~ 14 M transitons Hot: will be > billion TROVE HITRAN JPL Ab initio PES [CCSD(T)/aug-cc-pV(Q+d)Z] Refined using lab spectra R. I. Ovsyannikov et al. J. Chem. Phys 129, (2008). Ab initio: CCSD(T)/aug-cc-pVTZ S.N. Yurchenko et al. J. Mol. Spectrosc 239, 71 (2006). TROVE JPL HITRAN First principles Predictions of tunnelling being investigated

Dipole moment TROVE Yurchenko, Thiel, Jensen CH 4 9D surface geometries Potential energy Ab initio 10 electrons Ground electronic state Three 9D surfaces geometries Solve for the motion of the nuclei Line list: Billions of transitions MOLPRO CCSD(T)-f12/QZ MOLPRO CCSD(T)-f12/QZ Ab initio: solve for motion of electrons Sergei Yurchenko

Line list for warm Methane (T>600 K, J34 ) : line positions, Einstein coefficients, lower state energies, quantum numbers T=300K 212,000 lines 323,720,766 lines

A1A1 A2A2 E F1F1 F2F2 F1F1 F2F2 1,000,000 elements E F1F1 F2F2 … 0 … T d (M) CH 4 : Matrix diagonalization (Symmetry representation)

T d (M) CH 4 : Matrix diagonalization (Symmetry representation) A1A1 A2A2 E F1F1 F2F2 F1F1 F2F2 1,000,000 elements E F1F1 F2F2 … 0 … g ns = 5 g ns = 2 g ns = 3 g ns = 5

Structure of the sub-matrix:  K=±2 factorization (J =8) K=0 K=1 K=2 K=3 K=4 K=5 K=6 K=7 K=8 C s C 2v C 3v D 3h C 2h … Td (M) … 0 …

NH 3 diagonalization: Size of the matrix LAPACK: DSYEV PARPACK E ’’ E’E’ A ’’ A’A’

Absorption of Methane (T=300 K)

Albert et al., JCP 2008

Absorption of Methane (T=300 K) n Albert et al., JCP

THz absorption of Methane (T=300 K)

Absorption spectra of CH 4 : Temperature effect

50,000 processor hours. Wavefunctions > 0.8 terabites 221,100 energy levels (all to J=50, E = 30,000 cm  )‏ 14,889 experimentally known 506 Million transitions (PS list has 308M) >100,000 experimentally known with intensities  Partition function % of Vidler & Tennyson’s value at 3,000K BT2 linelist Barber et al, MNRAS 368, 1087 (2006).

Obs: A. Coppalle & P. Vervisch, JQSRT, 35, 121 (1986)‏ New edition of HITEMP: LS Rothman, IE Gordon, RJ Barber, H Dothe, RR Gamache, A Goldman, VI Perevalov, SA Tashkun + J Tennyson, JQSRT, 111, 2139 (2010).

BT2 linelist used to to detect/model water Nova-like V838 MonCometary coma Atmosphere of Venus Exoplanets (4 so far!) Brown and M-dwarfs

As well as..... Water concentrations in explosions Design of high-T gas sensors Remote detection of forest fires Imaging gas turbine engines Temperature profile in flames Atmospheric models

Primordial (Metal-poor) Terrestrial Planets (Oxidising) Giant-Planets & Cool Stars (Reducing atmospheres) Already available H 2, LiH HeH +, H 3 + H 2 D + OH, CO 2, O 3, NO H 2 O, HDO, NH 3 H 2, CN, CH, CO, CO 2, TiO HCN/HNC, H 2 O, NH 3, ExoMolO 2, CH 4, SO 2, SO 3 HOOH, H 2 CO, HNO 3 CH 4, PH 3, C 2, C 3, HCCH, H 2 S, C 2 H 6, C 3 H 8, VO, O 2, AlO, MgO, CrH, MgH, FeH, CaH, AlH, SiH, TiH, NiH, BeH, YO Molecular line lists for exoplanet & other atmospheres list of molecules Full details: J. Tennyson and S.N. Yurchenko, MNRAS, 425, 21 (2012) NaH, HF, HCl

Primordial (Metal-poor) Terrestrial Planets (Oxidising) Giant-Planets & Cool Stars (Reducing atmospheres) Already available H 2, LiH HeH +, H 3 + H 2 D + OH, CO 2, O 3, NO H 2 O, HDO, NH 3 H 2, CN, CH, CO, CO 2, TiO HCN/HNC, H 2 O, NH 3, ExoMol In progress O 2, CH 4, SO 2, SO 3 HOOH, H 2 CO, HNO 3 CH 4, PH 3, C 2, C 3, HCCH, H 2 S, C 2 H 6, C 3 H 8, VO, O 2, AlO, MgO, CrH, MgH, FeH, CaH, AlH, SiH, TiH, NiH, BeH, YO Molecular line lists for exoplanet & other atmospheres list of molecules Full details: J. Tennyson and S.N. Yurchenko, MNRAS, 425, 21 (2012) NaH, HF, HCl SiO, CS, NaCl, KCl

H2SH2S HCN CH 4 C3C3 SO 3 PH 3 CrH NiH VO HOOH AlO YO cross sections MSc students SiO, CS, NaCl, KCl + one Citizen scientist: AlH

H2SH2S HCN CH 4 C3C3 SO 3 PH 3 CrH NiH VO HOOH AlO YO cross sections MSc students SiO, CS, NaCl, KCl + one Citizen scientist: AlH Ala’a Azzam Bob Barber Sergei Yurchenko Dan Underwood Oleg Polyansky Clara Sousa-Silva Lorenzo Lodi Renia Diamantopoulou Maire Gorman Christian Hill Andrei Patrascu

About the first edition “The best book for anyone who is embarking on research in astronomical spectroscopy” Contemporary Physics (2006) Published 2011

Primordial (Metal-poor) Terrestrial Planets (Oxidising) Giant-Planets & Cool Stars (Reducing atmospheres) Already available H 2, LiH HeH +, H 3 + H 2 D + OH, CO 2, O 3, NO H 2 O, HDO, NH 3 H 2, CN, CH, CO, CO 2, TiO HCN/HNC, H 2 O, NH 3, ExoMolO 2, CH 4, SO 2 HOOH, H 2 CO, HNO 3 CH 4, PH 3, C 2, C 3, HCCH, H 2 S, C 2 H 6, C 3 H 8, VO, O 2, AlO, MgO, CrH, MgH, FeH, CaH, AlH, SiH, TiH, NiH, BeH, YO, NaH, HF, HCl Molecular line lists for exoplanet & other atmospheres Pierandrea Conti Thomas Veness Benjamin Yadin Istvan Szabo Ala’a Azzam Clara Sousa Silva Andrei atrascu Sergei Yurchenko Jonathan Tennyson Lorenzo Lodi SO 3