@inproceedings{oai:jaxa.repo.nii.ac.jp:00003037,
 author = {Bjerkeli, Per and Olofsson, Goran and Santangelo, Gina and Bergman, Per and Liseau, Rene and Larsson, Bengt},
 book = {宇宙航空研究開発機構特別資料, JAXA Special Publication: Proceedings of the SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe},
 month = {Mar},
 note = {SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, The star formation process is often revealed through the observations of molecular outflows. The ejection mechanism of these flows is most likely closely linked to the formation of protostellar disks. Swept up material from the parental cloud, excited in the interaction with the ambient medium, can be observed on parsec scale distances from the central source. The Herbig-Haro object HH 54 is a shock that can be studied in detail using a very limited amount of Herschel time. It is located relatively nearby in the Chamaeleon II cloud, situated at a distance of 180 pc. The shocked region has an angular extent of roughly 30" and is not contaminated with emission from other nearby objects. The nature of the central source has, however, been a matter of debate. Several IRAS point sources have in the past been suggested to be the driving source of the HH 54 flow. Here, we present spatially resolved observations of CO carried out with SPIRE and PACS onboard Herschel. The observations show a complicated picture and provide the possibility to measure the true CO abundance in a spatially resolved region., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027060, レポート番号: JAXA-SP-17-010E},
 pages = {277--279},
 publisher = {宇宙航空研究開発機構(JAXA), Japan Aerospace Exploration Agency (JAXA)},
 title = {Herschel Observations of the Shocked Gas in HH 54},
 volume = {JAXA-SP-17-010E},
 year = {2018}
}