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The Episodic, Precessing Giant Molecular Outflow from IRAS 04239+2436 (HH 300)
Astrophysics · Submitted 28 Mar 2001
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Lines drawn from IRAS 04239+2436 to each of these clumps have different orientations on the plane of the sky, and we conclude that HH 300 is a precessing and episodic outflow.
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The abstract, sentence by sentence
We present the first set of detailed molecular line maps of the region associated with the giant Herbig-Haro flow HH 300, from the young star IRAS 04239+2436. Our results indicate that the red lobe of the HH 300 flow is depositing a fair amount of momentum and kinetic energy over a notable volume of its host dark cloud. This makes HH 300 a key player in the evolution and fate of its parent cloud. The redshifted molecular outflow lobe of HH 300 is 1.1 pc long and 0.3 pc wide, and has a very clumpy structure. The density, velocity, and momentum distributions in the outflow indicate that the observed clumps arise from the prompt entrainment of ambient gas. Bow shock-shaped structures are associated with the clumps, and we hypothesize that the shocks are produced by different mass ejection episodes. Lines drawn from IRAS 04239+2436 to each of these clumps have different orientations on the plane of the sky, and we conclude that HH 300 is a precessing and episodic outflow. The observations include a map of the red lobe in the 12CO(2-1) line, with a beam size of 27'', and more extended maps of the outflow region in the 12CO(1-0) and 13CO(1-0) lines, with 45'' and 47'' beam sizes, respectively. We obtain a steep power-law mass spectrum for HH 300, which we believe is best explained by the evolution of the outflow mass kinematics. In addition, our 13CO observations show that the HH 300 flow has been able to redistribute (in space and velocity) considerable amounts of its surrounding medium-density gas.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present the first set of detailed molecular line maps of the region associated with the giant Herbig-Haro flow HH 300, from the young star IRAS 04239+2436. | contribution 1.00 | 0.95 | 0.04 | asserted 0.99 |
| s1 | Our results indicate that the red lobe of the HH 300 flow is depositing a fair amount of momentum and kinetic energy over a notable volume of its host dark cloud. | result 0.57 | 0.92 | 0.21 | hedged possibility 0.99 |
| s2 | This makes HH 300 a key player in the evolution and fate of its parent cloud. | interpretation 1.00 | 0.30 | 0.24 | asserted 1.00 |
| s3 | The redshifted molecular outflow lobe of HH 300 is 1.1 pc long and 0.3 pc wide, and has a very clumpy structure. | result 1.00 | 0.90 | 0.05 | asserted 1.00 |
| s4 | The density, velocity, and momentum distributions in the outflow indicate that the observed clumps arise from the prompt entrainment of ambient gas. | interpretation 0.95 | 0.91 | 0.08 | asserted 0.55 |
| s5 | Bow shock-shaped structures are associated with the clumps, and we hypothesize that the shocks are produced by different mass ejection episodes. | interpretation 0.95 | 0.78 | 0.05 | speculative 0.66 |
| s6 | Lines drawn from IRAS 04239+2436 to each of these clumps have different orientations on the plane of the sky, and we conclude that HH 300 is a precessing and episodic outflow. | interpretation 0.78 | 0.94 | 0.76 | asserted 0.97 |
| s7 | The observations include a map of the red lobe in the 12CO(2-1) line, with a beam size of 27'', and more extended maps of the outflow region in the 12CO(1-0) and 13CO(1-0) lines, with 45'' and 47'' beam sizes, respectively. | method 0.99 | 0.91 | 0.02 | asserted 0.99 |
| s8 | We obtain a steep power-law mass spectrum for HH 300, which we believe is best explained by the evolution of the outflow mass kinematics. | result 0.84 | 0.96 | 0.08 | asserted 0.50 |
| s9 | In addition, our 13CO observations show that the HH 300 flow has been able to redistribute (in space and velocity) considerable amounts of its surrounding medium-density gas. | result 0.92 | 0.96 | 0.08 | asserted 0.98 |
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Original abstract
We present the first set of detailed molecular line maps of the region associated with the giant Herbig-Haro flow HH 300, from the young star IRAS 04239+2436. Our results indicate that the red lobe of the HH 300 flow is depositing a fair amount of momentum and kinetic energy over a notable volume of its host dark cloud. This makes HH 300 a key player in the evolution and fate of its parent cloud. The redshifted molecular outflow lobe of HH 300 is 1.1 pc long and 0.3 pc wide, and has a very clumpy structure. The density, velocity, and momentum distributions in the outflow indicate that the observed clumps arise from the prompt entrainment of ambient gas. Bow shock-shaped structures are associated with the clumps, and we hypothesize that the shocks are produced by different mass ejection episodes. Lines drawn from IRAS 04239+2436 to each of these clumps have different orientations on the plane of the sky, and we conclude that HH 300 is a precessing and episodic outflow. The observations include a map of the red lobe in the 12CO(2-1) line, with a beam size of 27'', and more extended maps of the outflow region in the 12CO(1-0) and 13CO(1-0) lines, with 45'' and 47'' beam sizes, respectively. We obtain a steep power-law mass spectrum for HH 300, which we believe is best explained by the evolution of the outflow mass kinematics. In addition, our 13CO observations show that the HH 300 flow has been able to redistribute (in space and velocity) considerable amounts of its surrounding medium-density gas.
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