275 citations · 3.6k across the 46 of their papers we have counts for
46 papers
Origin of warm and hot gas emission from low-mass protostars: Herschel-HIFI observations of CO J=16-15. I. Line profiles, physical conditions, and H2O abundance
L. E. Kristensen, E. F. van Dishoeck, J. C. Mottram +18
(Abridged) Through spectrally unresolved observations of high-J CO transitions, Herschel-PACS has revealed large reservoirs of warm (300 K) and hot (700 K) molecular gas around low…
Water in star forming regions with Herschel (WISH) III. Far-infrared cooling lines in low-mass young stellar objects
A. Karska, G. J. Herczeg, E. F. van Dishoeck +22
(Abridged) Far-infrared Herschel-PACS spectra of 18 low-mass protostars of various luminosities and evolutionary stages are studied. We quantify their far-infrared line emission an…
OH far-infrared emission from low- and intermediate-mass protostars surveyed with Herschel-PACS
S. F. Wampfler, S. Bruderer, A. Karska +10
OH is a key species in the water chemistry of star-forming regions, because its presence is tightly related to the formation and destruction of water. This paper presents OH observ…
Water in star-forming regions with Herschel (WISH): II. Evolution of 557 GHz 110-101 emission in low-mass protostars
L. E. Kristensen, E. F. van Dishoeck, E. A. Bergin +22
(Abridged) Water is a key tracer of dynamics and chemistry in low-mass protostars, but spectrally resolved observations have so far been limited in sensitivity and angular resoluti…
The warm gas atmosphere of the HD 100546 disk seen by Herschel (Evidence of a gas-rich, carbon-poor atmosphere?)
Simon Bruderer, Ewine F. van Dishoeck, Steven D. Doty +1
(Abridged) Context. With the Herschel Space Observatory, lines of simple molecules (C+, O, and CO) have been observed in the atmosphere of protoplanetary disks. When combined with…
Modelling Herschel observations of hot molecular gas emission from embedded low-mass protostars
R. Visser, L. E. Kristensen, S. Bruderer +6
Aims. Young stars interact vigorously with their surroundings, as evident from the highly rotationally excited CO (up to Eup=4000 K) and H2O emission (up to 600 K) detected by the…