Odin observations of H<sub>2</sub>O in the Galactic Centre

Sandqvist, Aa.; Bergman, P.; Black, J. H.; Booth, R. S.; Buat, V.; Curry, Charles L.; Encrenaz, P.; Falgarone, É.; Feldman, P. A.; Fich, M.; Florén, Hans-Gustav; Frisk, U.; Gérin, M.; Gregersen, E. M.; Harju, J.; Hasegawa, T.; Hjalmarson, Å.; Johansson, Lars; Kwok, Sun; Larsson, Bengt; Lecacheux, A.; Liljeström, T.; Lindqvist, Michael; Liseau, R.; Mattila, K.; Mitchell, G. F.; Nordh, L.; Olberg, M.; Olofsson, A. O. H.; Olofsson, G.; Pagani, L.; Plume, R.; Ristorcelli, I.; Schéele, F. von; Serra, G.; Tothill, N.; Volk, Kevin; Wilson, C. D.; Winnberg, A.

doi:10.1051/0004-6361:20030341

Cited by 26 publications

(20 citation statements)

References 23 publications

(24 reference statements)

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“…• is −30 km s −1 (Menon & Ciotti 1970;Liszt et al 1977;Linke et al 1981;Greaves & Williams 1994;Sandqvist et al 2003). This feature was originally detected in 1967 (Kerr & Vallak 1967), but we would like to point that no molecular counterpart has been associated with it.…”

Section: Extinction and Distancementioning

confidence: 69%

The connection between W31, SGR 1806–20, and LBV 1806–20: Distance, extinction, and structure

Corbel

Eikenberry

2004

A&A

109

130

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Abstract. We present new millimeter and infrared spectroscopic observations towards the radio nebula G10.0−0.3, which is powered by the wind of the Luminous Blue Variable star LBV 1806−20 also closely associated with the soft gamma-ray repeater SGR 1806−20, and believed to be located in the giant Galactic H  complex W31. Based on observations of CO emission lines and NH 3 absorption features from molecular clouds along the line of sight to G10.0−0.3, as well as the radial velocity and optical extinction of the star powering the nebula, we determine its distance to be 15.1 +1.8 −1.3 kpc in agreement with Corbel et al. (1997). In addition, this strengthens the association of SGR 1806−20 with a massive molecular cloud at the same distance. All soft gamma-ray repeaters with precise location are now found to be associated with a site of massive star formation or molecular cloud. We also show that W31 consists of at least two distinct components along the line of sight. We suggest that G10.2−0.3 and G10.6−0.4 are located on the −30 km s −1 spiral arm at a distance from the Sun of 4.5 ± 0.6 kpc and that G10.3−0.1 may be associated with a massive molecular cloud at the same distance as the LBV star, i.e. 15.1 +1.8 −1.3 kpc, implying that W31 could be decomposed into two components along the line of sight.

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Section: Extinction and Distancementioning

confidence: 69%

The connection between W31, SGR 1806–20, and LBV 1806–20: Distance, extinction, and structure

Corbel

Eikenberry

2004

A&A

109

130

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“…Water is a key molecule for the chemistry and the energy balance of the gas in cold clouds and star forming regions, thanks to its relatively large abundance and large dipole moment. A wealth of observational data has been obtained by the Infrared Space Observatory (see for example: Cernicharo & Crovisier 2005;Spinoglio et al 2001;Tsuji 2001;Wright et al 2000), the Submillimeter Wave Astronomy Satellite (Melnick et al 2000) and the ODIN satellite (Sandqvist et al 2003;Wilson et al 2003). In the near future the Heterodyne Instrument for the Far-Infrared (HIFI) will be launched on board the Herschel Space Observatory.…”

Section: Introductionmentioning

confidence: 99%

Rotational excitation of ortho-H₂O by para-H₂ (j₂ = 0, 2, 4, 6, 8) at high temperature

Dubernet

Daniel

Grosjean

et al. 2009

A&A

102

163

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Aims. Our objective is to obtain the best possible set of rotational (de)-excitation state-to-state and effective rate coefficients for temperatures up to 1500 K. We present state-to-state rate coefficients among the 45 lowest levels of o-H 2 O with H 2 ( j 2 = 0) and Δ j 2 = 0, +2, as well as with H 2 ( j 2 = 2) and Δ j 2 = 0, −2. In addition and only for the 10 lowest energy levels of o-H 2 O, we provide state-to-state rate coefficients involving j 2 = 4 with Δ j 2 = 0, −2 and j 2 = 2 with Δ j 2 = +2. We give estimates of effective rate coefficients for j 2 = 6, 8. Methods. Calculations are performed with the close coupling (CC) method over the whole energy range, using the same 5D potential energy surface (PES) as the one employed in our latest publication on water. We perform comparisons with coupled states (CS) calculations, with thermalized quasi-classical trajectory (QCT) calculations using the same PES and with previous quantum calculations obtained between T = 20 K and T = 140 K with a different PES. Results. We find that the CS approximation fares extremely badly even at high energy for j 2 different from zero. Comparisons with thermalized QCT calculations show large factors at intermediate temperatures and factors from 1 to 3 at high temperature for the strongest rate coefficients. Finally we stress that scaled collisional rate coefficients obtained with He cannot be used in place of collisional rate coefficients with H 2 .

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“…The H 2 O observations have been abundantly successful, a summary of which has been presented by Hjalmarson et al ( , 2007. Emission and absorption in the 557-GHz H 16 2 O line have been detected in the Galactic centre towards the Sgr A * circumnuclear disk (CND), and the Sgr A +20 km s −1 and +50 km s −1 molecular clouds (Sandqvist et al 2003(Sandqvist et al , 2006. Good reviews on the Galactic centre region have been presented by Morris & Serabyn (1996) and Mezger et al (1996).…”

Section: Introductionmentioning

confidence: 99%

Odin observations of the Galactic centre in the 118-GHz band

Sandqvist¹,

Larsson²,

Hjalmarson

et al. 2008

A&A

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Odin observations of H₂O in the Galactic Centre

Cited by 26 publications

References 23 publications

The connection between W31, SGR 1806–20, and LBV 1806–20: Distance, extinction, and structure

The connection between W31, SGR 1806–20, and LBV 1806–20: Distance, extinction, and structure

Rotational excitation of ortho-H₂O by para-H₂ (j₂ = 0, 2, 4, 6, 8) at high temperature

Odin observations of the Galactic centre in the 118-GHz band

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Odin observations of H2O in the Galactic Centre

Cited by 26 publications

References 23 publications

The connection between W31, SGR 1806–20, and LBV 1806–20: Distance, extinction, and structure

The connection between W31, SGR 1806–20, and LBV 1806–20: Distance, extinction, and structure

Rotational excitation of ortho-H2O by para-H2 (j2 = 0, 2, 4, 6, 8) at high temperature

Odin observations of the Galactic centre in the 118-GHz band

Contact Info

Product

Resources

About

Odin observations of H₂O in the Galactic Centre

Rotational excitation of ortho-H₂O by para-H₂ (j₂ = 0, 2, 4, 6, 8) at high temperature