The Odin orbital observatory

Nordh, H. L.; Schéele, F. von; Frisk, U.; Ahola, Kimmo; Booth, R. S.; Encrenaz, P.; Hjalmarson, Å.; Kendall, D. J. W.; Kyrölä, E.; Kwok, Sun; Lecacheux, A.; Leppelmeier, G. W.; Llewellyn, E. J.; Mattila, K.; Mégie, G.; Murtagh, Donal; Rougeron, M.; Witt, G.

doi:10.1051/0004-6361:20030334

Cited by 93 publications

(79 citation statements)

References 2 publications

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“…Water has been observed previously in deeply embedded, low-mass protostars, primarily with space-based observatories such as ISO, SWAS, Odin and Spitzer (Kessler et al 1996;Melnick et al 2000;Nordh et al 2003;Werner et al 2004). ISO and Spitzer both observed spectrally unresolved water lines in the wavelength range of 5-180 μm (Ceccarelli et al 1998;Boogert et al 2000;Giannini et al 2001;Larsson et al 2002;Maret et al 2002;Watson et al 2007), where many higherexcited water lines (E up /k B ∼ few 100 K) were detected.…”

Section: Introductionmentioning

confidence: 95%

Water in star-forming regions withHerschel(WISH)

Kristensen

Dishoeck

Bergin

et al. 2012

A&A

250

587

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Context. Water is a key tracer of dynamics and chemistry in low-mass star-forming regions, but spectrally resolved observations have so far been limited in sensitivity and angular resolution, and only data from the brightest low-mass protostars have been published. Aims. The first systematic survey of spectrally resolved water emission in 29 low-mass (L < 40 L ) protostellar objects is presented. The sources cover a range of luminosities and evolutionary states. The aim is to characterise the line profiles to distinguish physical components in the beam and examine how water emission changes with protostellar evolution. Methods. H 2 O was observed in the ground-state 1 10 -1 01 transition at 557 GHz (E up /k B ∼ 60 K) as single-point observations with the Heterodyne Instrument for the Far-Infrared (HIFI) on Herschel in 29 deeply embedded Class 0 and I low-mass protostars. Complementary far-IR and sub-mm continuum data (including PACS data from our programme) are used to constrain the spectral energy distribution (SED) of each source. H 2 O intensities are compared to inferred envelope properties, e.g., mass and density, outflow properties and CO 3-2 emission. Results. H 2 O emission is detected in all objects except one (TMC1A). The line profiles are complex and consist of several kinematic components tracing different physical regions in each system. In particular, the profiles are typically dominated by a broad Gaussian emission feature, indicating that the bulk of the water emission arises in outflows, not in the quiescent envelope. Several sources show multiple shock components appearing in either emission or absorption, thus constraining the internal geometry of the system. Furthermore, the components include inverse P-Cygni profiles in seven sources (six Class 0, one Class I) indicative of infalling envelopes, and regular P-Cygni profiles in four sources (three Class I, one Class 0) indicative of expanding envelopes. Molecular "bullets" moving at > ∼ 50 km s −1 with respect to the source are detected in four Class 0 sources; three of these sources were not known to harbour bullets previously. In the outflow, the H 2 O/CO abundance ratio as a function of velocity is nearly the same for all line wings, increasing from 10 −3 at low velocities (<5 km s −1 ) to > ∼ 10 −1 at high velocities (>10 km s −1 ). The water abundance in the outer cold envelope is low, > ∼ 10 −10 . The different H 2 O profile components show a clear evolutionary trend: in the younger Class 0 sources the emission is dominated by outflow components originating inside an infalling envelope. When large-scale infall diminishes during the Class I phase, the outflow weakens and H 2 O emission all but disappears.

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Section: Introductionmentioning

confidence: 95%

Water in star-forming regions withHerschel(WISH)

Kristensen

Dishoeck

Bergin

et al. 2012

A&A

250

587

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“…Most of the water is rotationally cold throughout the cometary atmosphere (Crovisier, 1984;Weaver and Mumma, 1984;Bockelée-Morvan, 1987;Xie and Mumma, 1992; the Microwave Instrument for the Rosetta orbiter, MIRO, the Swedish-led satellite mission Odin (Nordh et al, 2003), and the Submillimeter Wave Astronomy Satellite, SWAS (Melnick et al, 2000). In this paper we present the results from the SWAS observing campaign for comet 9P/Tempel 1 and Deep NASA's Submillimeter Wave Astronomy Satellite is a complete space-borne radio observatory (Melnick et al, 2000).…”

Section: P/tempel 1 the Target Comet Of The Deep Impact Mission Ismentioning

confidence: 99%

Submillimeter Wave Astronomy Satellite observations of Comet 9P/Tempel 1 and Deep Impact

Bensch

Melnick

Neufeld

et al. 2007

Icarus

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“…The spectrum of the H 2 O (1 10 − 1 01 ) line at 557 GHz (λ = 538.29 µm) was observed by the Odin satellite towards W Hya using the autocorrelation spectrometer (Nordh et al 2003;Frisk et al 2003). The resulting spectrum is a combination of two separate observing sessions, in December 2002 and July 2003, of a total of 185 orbits.…”

Section: Observationsmentioning

confidence: 99%

W Hya through the eye of Odin

Justtanont¹,

Bergman²,

Larsson³

et al. 2005

A&A

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Abstract. We present Odin observations of the AGB star W Hya in the ground-state transition of ortho-H 2 O, 1 10 − 1 01 , at 557 GHz. The line is clearly of circumstellar origin. Radiative transfer modelling of the water lines observed by Odin and ISO results in a mass-loss rate of (2.5 ± 0.5) × 10 −7 M yr −1 , and a circumstellar H 2 O abundance of (2.0 ± 1.0) × 10 −3 . The inferred mass-loss rate is consistent with that obtained from modelling the circumstellar CO radio line emission, and also with that obtained from the dust emission modelling combined with a dynamical model for the outflow. The very high water abundance, higher than the cosmic oxygen abundance, can be explained by invoking an injection of excess water from evaporating icy bodies in the system. The required extra mass of water is quite small, on the order of ∼0.1 M ⊕ .

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The Odin orbital observatory

Cited by 93 publications

References 2 publications

Water in star-forming regions withHerschel(WISH)

Water in star-forming regions withHerschel(WISH)

Submillimeter Wave Astronomy Satellite observations of Comet 9P/Tempel 1 and Deep Impact

W Hya through the eye of Odin

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