Using H3+ and H2D+ as probes of star-forming regions

The H3+ and H2D+ ions are important probes of the physical and chemical conditions in regions of the interstellar medium where new stars are forming. This paper reviews how observations of these species and of heavier ions such as HCO+ and H3O+ can be used to derive chemical and kinematic properties of nearby pre-stellar cores, and the cosmic-ray ionisation rate toward more distant regions of high-mass star formation. Future prospects in the field are outlined at the end.Comment: Refereed review, 6 pages, to appear in Phil. Trans. R. Soc.

An accelerated Monte Carlo method to solve two-dimensional radiative transfer and molecular excitation. With applications to axisymmetric models of star formation

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Detection of interstellar H2D+ emission

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Abundance profiles of CH3OH and H2CO toward massive young stars as tests of gas-grain chemical models

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Chemistry as a probe of the structures and evolution of massive star-forming regions

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Sulphur chemistry in the envelopes of massive young stars

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Water Line Strengths Toward High-Mass Star Forming Regions: Predictions for Herschel/HIFI

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Deep learning for galaxy mergers in the galaxy main sequence

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The young intermediate-mass stellar object AFGL 490 - a disk surrounded by a cold envelope

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