2010
DOI: 10.1051/0004-6361/201015240
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Heavy water around the L1448-mm protostar

Abstract: Context. L1448-mm is the prototype of a low-mass Class 0 protostar driving a high-velocity jet. Given its bright H 2 O spectra observed with ISO, L1448-mm is an ideal laboratory to observe heavy water (HDO) emission. Aims. Our aim is to image the HDO emission in the protostar surroundings, the possible occurrence of HDO emission also investigating off L1448-mm, towards the molecular outflow. Methods. We carried out observations of L1448-mm in the HDO(1 10 -1 11 ) line at 80.6 GHz, an excellent tracer of HDO co… Show more

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Cited by 62 publications
(82 citation statements)
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“…For IRAS 16293-2422, IRAS 4A, and IRAS 4B, the HDO fundamental 1 1,1 -0 0,0 transition was observed at high sensitivity with Herschel/HIFI, allowing us to strongly constrain the outer abundance of deuterated water. The estimate of the HDO inner abundance in L1448-mm by Codella et al (2010) is based on interferometric observations of the HDO 1 1,0 -1 1,1 line at 80.6 GHz. Using the spherical source structure determined by Jørgensen et al (2002), the abundance is then estimated at 4 × 10 −7 .…”
Section: Discussionmentioning
confidence: 99%
“…For IRAS 16293-2422, IRAS 4A, and IRAS 4B, the HDO fundamental 1 1,1 -0 0,0 transition was observed at high sensitivity with Herschel/HIFI, allowing us to strongly constrain the outer abundance of deuterated water. The estimate of the HDO inner abundance in L1448-mm by Codella et al (2010) is based on interferometric observations of the HDO 1 1,0 -1 1,1 line at 80.6 GHz. Using the spherical source structure determined by Jørgensen et al (2002), the abundance is then estimated at 4 × 10 −7 .…”
Section: Discussionmentioning
confidence: 99%
“…Velocity-resolved spectra of 12 CO up to J u = 10 (Yıldız et al 2010(Yıldız et al , 2012Bjerkeli et al 2011;Benedettini et al 2012) and of several H 2 O Codella et al 2010;Kristensen et al 2011Kristensen et al , 2012Santangelo et al 2012;Vasta et al 2012) and OH (Wampfler et al 2011) lines indicate that the bulk of the far-infrared emission has broad line wings with Δ > 15 km s −1 . The quiescent warm inner envelope is primarily seen in the narrow (Δ 5 km s −1 ) 13 CO and C 18 O isotopolog mid-J spectra centered at the source position but this component does not contribute to H 2 O emission.…”
Section: Origin Of Far-ir Line Emissionmentioning
confidence: 99%
“…Interestingly, L1157-B1 also shows emission in molecular ions, such as HCO + , HCS + , and N 2 H + (Bachiller & Perez Gutierrez 1997;Codella et al 2010Codella et al , 2013Yamaguchi et al 2012), making it a unique target for investigating the chemistry of molecular ions in protostellar shocks.…”
Section: Previous Work On L1157mentioning
confidence: 99%