Herschelmeasurements of the D/H and16O/18O ratios in water in the Oort-cloud comet C/2009 P1 (Garradd)

Bockelée‐Morvan, Dominique; Biver, Nicolás; Swinyard, Bruce; Val-Borro, M. de; Crovisier, J.; Hartogh, P.; Lis, D. C.; Moreno, R.; Szutowicz, S.; Lellouch, E.; Emprechtinger, M.; Blake, Geoffrey A.; Courtin, R.; Jarchow, Christopher; Kidger, M.; Küppers, M.; Rengel, Miriam; Davis, G. R.; Fulton, T.; Naylor, David; Sidher, S.; Walker, H. J.

doi:10.1051/0004-6361/201219744

Cited by 137 publications

(105 citation statements)

References 30 publications

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“…Recently however, a HDO/H 2 O ratio of 3.2 × 10 −4 was measured Appendix A is available in electronic form at http://www.aanda.org 1 A HDO/H 2 O ratio of "x" corresponds to a D/H ratio of "x/2". for the Jupiter class comet Hartley 2 with the Herschel Space Observatory (Hartogh et al 2011) and 4.2 × 10 −4 for the Oort cloud comet Garradd (Bockelée-Morvan et al 2012), indicating values closer to those of Earth's water.…”

Section: Introductionmentioning

confidence: 94%

Warm water deuterium fractionation in IRAS 16293-2422

Persson

Jørgensen

Dishoeck

2012

A&A

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Context. Measuring the water deuterium fractionation in the inner warm regions of low-mass protostars has so far been hampered by poor angular resolution obtainable with single-dish ground-and space-based telescopes. Observations of water isotopologues using (sub)millimeter wavelength interferometers have the potential to shed light on this matter. Aims. To measure the water deuterium fractionation in the warm gas of the deeply-embedded protostellar binary IRAS 16293-2422. Results. The 692 GHz H 182 O line is seen toward both components of the binary protostar. Toward one of the components, "source B", the line is seen in absorption toward the continuum, slightly red-shifted from the systemic velocity, whereas emission is seen off-source at the systemic velocity. Toward the other component, "source A", the two HDO and H 18 2 O lines are detected as well with the SMA. From the H 18 2 O transitions the excitation temperature is estimated at 124 ± 12 K. The calculated HDO/H 2 O ratio is (9.2 ± 2.6) × 10 −4 -significantly lower than previous estimates in the warm gas close to the source. It is also lower by a factor of ∼5 than the ratio deduced in the outer envelope. Conclusions. Our observations reveal the physical and chemical structure of water vapor close to the protostars on solar-system scales. The red-shifted absorption detected toward source B is indicative of infall. The excitation temperature is consistent with the picture of water ice evaporation close to the protostar. The low HDO/H 2 O ratio deduced here suggests that the differences between the inner regions of the protostars and the Earth's oceans and comets are smaller than previously thought.

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Section: Introductionmentioning

confidence: 94%

Warm water deuterium fractionation in IRAS 16293-2422

Persson

Jørgensen

Dishoeck

2012

A&A

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“…The HDO 1 10 -1 01 transition at 509.292 GHz was observed using the Heterodyne Instrument for the Far-Infrared (HIFI) in the Jupiter-family comets 103P/Hartley 2 and 45P/Honda-Mrkos-Pajdušáková , and in the Oort-cloud comet C/2009 P1 (Garradd) (Bockelée-Morvan et al 2012 2 O was measured to be 0.161 ± 0.017 for comet Hartley 2, i.e., consistent with the VSMOW value for this ratio of 0.1554 ± 0.0001. The HDO/H 18 2 O value of 0.215 ± 0.023 for comet Garradd suggests a significant difference (3-σ ) in deuterium content between the comet Garradd and Hartley 2. derived a D/H ratio of (1.61 ± 0.24) × 10 −4 for comet Hartley, assuming an H 16 2 O/H 18 2 O ratio of 500 ± 50 which encompasses the VSMOW value and values measured in cometary water (Jehin et al 2009, see Sect.…”

Section: Watermentioning

confidence: 99%

“…the fact that oxygen isotope variations in meteorites cannot be explained in any easy way (Yurimoto and Kuramoto 2004). Recently H 2 O, and H 18 2 O 1 10 -1 01 lines were observed with high signal-to-noise ratio in the Oort Cloud comet C/2009 P1 (Garradd) using the HIFI instrument onboard the IR Herschel space telescope (Bockelée-Morvan et al 2012). The measured oxygen ratio of 523 ± 32 is consistent with the terrestrial value.…”

Section: Oxygenmentioning

confidence: 99%

Cometary Isotopic Measurements

et al. 2015

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“…For water lines, radiation trapping effects are important and considered in both excitation and radiative transfer calculations. Details on the H 2 O and CH 3 OH excitation models can be found in Bockelée-Morvan et al (2012) and Biver et al (2000), and references therein.…”

Section: Excitation Modelsmentioning

confidence: 99%

Searches for HCl and HF in comets 103P/Hartley 2 and C/2009 P1 (Garradd) with theHerschelSpace Observatory

Bockelée‐Morvan

Biver

Crovisier

et al. 2014

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Context. Hydrogen chloride (HCl) and hydrogen fluoride (HF) are expected to be the main reservoirs of fluorine and chlorine over a wide range of conditions, wherever hydrogen is predominantly molecular. They are found to be strongly depleted in dense molecular clouds, suggesting freeze-out onto grains in such cold environments. We can then expect that HCl and HF were also the major carriers of Cl and F in the gas and icy phases of the outer solar nebula, and were incorporated into comets. Aims. We aimed to measure the HCl and HF abundances in cometary ices as they can provide insights on the halogen chemistry in the early solar nebula. Methods. We searched for the J(1−0) lines of HCl and HF at 626 and 1232 GHz, respectively, using the Heterodyne Instrument for the Far-Infrared (HIFI) onboard the Herschel Space Observatory. HCl was searched for in comets 103P/Hartley 2 and C/2009 P1 (Garradd), whereas observations of HF were conducted in comet C/2009 P1 (Garradd). In addition, observations of H 2 O and H 2 18 O lines were performed in C/2009 P1 (Garradd) to measure the H 2 O production rate at the time of the HCl and HF observations. Three lines of CH 3 OH were serendipitously observed in the HCl receiver setting. Results. HCl is not detected, whereas a marginal (3.6-σ) detection of HF is obtained. The upper limits for the HCl abundance relative to water are 0.011% and 0.022%, for comet 103P/Hartley 2 and C/2009 P1 (Garradd), respectively, showing that HCl is depleted with respect to the solar Cl/O abundance by a factor more than 6 +6 −3 in 103P/Hartley 2, where the error is related to the uncertainty in the chlorine solar abundance. The marginal HF detection obtained in C/2009 P1 (Garradd) corresponds to an HF abundance relative to water of (1.8 ± 0.5) × 10 −4 , which is approximately consistent with a solar photospheric F/O abundance. The inferred water production rate in comet C/2009 P1 (Garradd) is (1.1±0.3)×10 29 s −1 and (0.75±0.05)×10 29 s −1 on 17 and 23 February 2012, respectively. CH 3 OH abundances relative to water are 2.7 ± 0.3% and 3.4 ± 0.6%, for comets 103P/Hartley 2 and C/2009 P1 (Garradd), respectively. Conclusions. The observed depletion of HCl suggests that HCl was not the main reservoir of chlorine in the regions of the solar nebula where these comets formed. HF was possibly the main fluorine compound in the gas phase of the outer solar nebula. However, this needs to be confirmed by future measurements.

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Herschelmeasurements of the D/H and¹⁶O/¹⁸O ratios in water in the Oort-cloud comet C/2009 P1 (Garradd)

Cited by 137 publications

References 30 publications

Warm water deuterium fractionation in IRAS 16293-2422

Warm water deuterium fractionation in IRAS 16293-2422

Cometary Isotopic Measurements

Searches for HCl and HF in comets 103P/Hartley 2 and C/2009 P1 (Garradd) with theHerschelSpace Observatory

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