Submillimeter-wave lines ofSubmillimeter-wave lines ofHH22DD++ and D and D22HH++ as probes into as probes into
chemistry in cold dark cloudschemistry in cold dark clouds
T. Amano
Institute for Astrophysics and Planetary Sciences
Ibaraki University
In this talkIn this talk
Overview of spectroscopy of D2H+ and H2D+
TuFIR lines of H2D+
H5+ and its deuterated species
Spectroscopy of HSpectroscopy of H22DD++ and D and D22HH++
Shy, Farley, Wing (1981): Ion beam Shy, Farley, Wing (1981): Ion beam Amano & Watson (1984), Amano (1985): Amano & Watson (1984), Amano (1985): 11 band (H band (H22DD++))
Lubic & Amano (1984): Lubic & Amano (1984): 11 band (D band (D22HH++) )
Foster et al. (1986): Foster et al. (1986): 2 2 / /3 3 bands (Hbands (H22DD++))
Foster, McKellar, Watson. (1986): Foster, McKellar, Watson. (1986): 2 2 / /3 3 bands (Dbands (D22HH++ ) )
Polyansky & McKellar (1990): All available data were fitted togetPolyansky & McKellar (1990): All available data were fitted together to improve molecular constants. (Dher to improve molecular constants. (D22HH++) )
Amano & Hirao, J. Mol. Spectrosc. 233, 7 (2005)
IR
Bogey et al. (1984): 1Bogey et al. (1984): 11010-1-11111 H H22DD++ (372.4 GHz) (372.4 GHz)
Warner et al.(1984): Warner et al.(1984): Saito, Kawaguchi, Hirota (1985): 2Saito, Kawaguchi, Hirota (1985): 22020-2-22121 H H22DD++ (156.0 GHz) (156.0 GHz)
Jennings, Demuynck, Banek, Evenson (unpublished): Jennings, Demuynck, Banek, Evenson (unpublished):
110101-0-00000 H H22DD+ + (1370.1 GHz) (1370.1 GHz)
111111-0-00000 D D22HH++ (1476.6 GHz) (1476.6 GHz)
222020-2-21111 D D22HH++ (1370.1 GHz) (1370.1 GHz)
Hirao & Amano (2003): 1Hirao & Amano (2003): 11010-1-10101 D D22HH++ (691.7 GHz) (691.7 GHz)
Amano & Hirao (2005): 3Amano & Hirao (2005): 32121-3-32222 H H22DD++ (646.4 GHz) (646.4 GHz)
mm-, sub-mm, FIR
Theoretical workTheoretical work
Carney and Porter(1977)Carney and Porter(1977)
Tennyson, Polyansky and coworkers carried Tennyson, Polyansky and coworkers carried out very high level out very high level ab initioab initio calculations, an calculations, and interactions between theory and experimed interactions between theory and experiments were often very crucial in assigning the nts were often very crucial in assigning the spectra and in deriving the accurate spectrosspectra and in deriving the accurate spectroscopic constants .copic constants .
See for example, Polyansky and Tennyson, See for example, Polyansky and Tennyson, JCPJCP,,110110, 50, 5056(1999)56(1999)
Ibaraki sub-mm systemIbaraki sub-mm system
Russian BWO(Backward-wave oscillator)
270-860 GHz ~1 mW
stabilized, using double phase-lock loop
Double modulation technique frequency-discharge
frequency-magnetic field
extended negative glow discharge
Double modulation sub-mm system at Ibaraki(University of Waterloo)
Submillimeter-wave system in Ibaraki
Extended negative glow discharge source.Extended negative glow discharge source. (Magnetic field: 200G).(Magnetic field: 200G).
Double modulation.Double modulation. HH22/D/D22/Ar = 4 /2 /17 mTorr/Ar = 4 /2 /17 mTorr for Hfor H22DD++
=3 /2 /17 mTorr for D=3 /2 /17 mTorr for D22HH++
I = 8 mA, T ~ 77 KI = 8 mA, T ~ 77 K
Experimental DetailsExperimental Details
Ap.J. Lett. 597, L85-L87(2003). 691660.440(20) MHz
TuFIR Spectrometer ( Toyama University )
Energy Level Diagram of HEnergy Level Diagram of H22DD++
Energy Level Diagram of HEnergy Level Diagram of H22DD++
Hyperfine structure of H2D+ and D2H+
Jensen et al. Mol. Phys. 91, 319(1997)H2D+
D2H+
H2D+
Yamaguchi, Gaw, Remington, Schaefer.J. Chem. Phys. 80, 5072(1987)
H5+
Xie, Braams, Bowman. J. Chem. Phys.122,224307(2005)
1-C2v
2-D2d
3-C2v
4-D2h
4 low energy conformers of H5+
Financial support
•Ministry of Education, Science, and Culture of Japan•Japan Society for Promotion of Science(JSPS)•Japan Space Forum(JSF)•JEM/SMILES Project