TY - JOUR
T1 - SOFIA FIFI-LS spectroscopy of DR21 Main
T2 - Energetics of the spatially resolved outflow from a high-mass protostar
AU - Karska, A.
AU - Figueira, M.
AU - Mirocha, A.
AU - Kaåºmierczak-Barthel, M.
AU - Fischer, Ch
AU - Wiesemeyer, H.
AU - Skretas, I. M.
AU - Beck, A.
AU - Khan, S.
AU - Lê, N.
AU - Yang, Y. L.
AU - Looney, L.
AU - Krabbe, A.
AU - Wyrowski, F.
AU - Menten, K.
N1 - The authors would like to thank the referee, Alessio Caratti o Garatti, for the comments that helped to improve this manuscript. The authors also thank Volker Ossenkopf for useful discussions concerning the parallel analysis of the GREAT observations of DR21. A.K. and M.F. acknowledge support from the Polish National Agency for Academic Exchange grants No. BPN/BEK/2021/1/00319/DEC/1 and BPN/BEK/2023/1/00036/DEC/01, respectively. MF acknowledges also support from the Polish National Science Centre via the grant UMO-2022/47/D/ST9/00419. Y.-L.Y. acknowledges support from Grant-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan (20H05845, 20H05844, 22K20389), and a pioneering project in RIKEN (Evolution of Matter in the Universe). Based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. GREAT is a development by the MPI für Radioastronomie and the KOSMA/Universität zu Köln, in cooperation with the DLR Institut für Optische Sensorsysteme, financed by the participating institutes, by the German Aerospace Center (DLR) under grants 50 OK 1102, 1103 and 1104, and within the Collaborative Research Centre 956, funded by the Deutsche Forschungsgemeinschaft (DFG). Herschel was an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
The authors would like to thank the referee, Alessio Caratti o Garatti, for the comments that helped to improve this manuscript. The authors also thank Volker Ossenkopf for useful discussions concerning the parallel analysis of the GREAT observations of DR21. A.K. and M.F. acknowledge support from the Polish National Agency for Academic Exchange grants No. BPN/BEK/2021/1/00319/DEC/1 and BPN/BEK/2023/1/00036/DEC/01, respectively. MF acknowledges also support from the Polish National Science Centre via the grant UMO-2022/47/D/ST9/00419. Y.-L.Y. acknowledges support from Grant-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan (20H05845, 20H05844, 22K20389), and a pioneering project in RIKEN (Evolution of Matter in the Universe). Based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2–97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. GREAT is a development by the MPI für Radioastronomie and the KOSMA/Universität zu Köln, in cooperation with the DLR Institut für Optische Sensorsysteme, financed by the participating institutes, by the German Aerospace Center (DLR) under grants 50 OK 1102, 1103 and 1104, and within the Collaborative Research Centre 956, funded by the Deutsche Forschungsgemeinschaft (DFG). Herschel was an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
PY - 2025/5/1
Y1 - 2025/5/1
N2 - Context. Massive star formation is associated with energetic processes that may influence the physics and chemistry of parental molecular clouds and impact galaxy evolution. The high-mass protostar DR21 Main in Cygnus X possesses one of the largest and most luminous outflows ever detected in the Galaxy, but the origin of its structure and driving mechanisms are still debated. Aims. Our aim is to spatially resolve the far-infrared line emission from DR21 Main and to investigate the gas physical conditions, energetics, and current mass loss rates along its outflow. Methods. Far-infrared SOFIA FIFI-LS spectra covering selected high-J CO lines, OH, [O I], [C II], and [O III] lines are analyzed across almost the full extent of the DR21 Main outflow using 2.00′ × 3.75′ mosaic. Results. The spatial extent of far-infrared emission closely follows the well-known outflow direction of DR21 Main in the case of high-J CO, [O I] 63.18 μm, and the OH line at 163.13 μm. On the contrary, the emission from the [C II] 157.74 μm and [O I] 145.53 μm lines arises mostly from the eastern part of the outflow, and is likely linked with a photodissociation region. Comparison of non-LTE radiative transfer models with the observed [O I] line ratios suggest H2 densities of ∼105 cm-3 in the western part of the outflow and ∼ 104 cm-3 in the east. Such densities are consistent with the predictions of UV-irradiated non-dissociative shock models for the observed ratios of CO and [O I] along the DR21 Main outflow. Assuming that the bulk of the emission arises in shocks, the outflow power of DR21 Main of 4.3-4.8 × 102 L⊙ and the mass loss rate of 3.3-3.7 × 10-3 M⊙ yr-1 are determined, consistent with estimates using HCO+ 1-0. Conclusions. Spatially resolved far-infrared emission of DR21 Main provides a strong support for its origin in outflow shocks, and the stratification of physical conditions along the outflow. The total line cooling provides additional evidence that DR21 Main drives one of the most energetic outflows in the Milky Way.
AB - Context. Massive star formation is associated with energetic processes that may influence the physics and chemistry of parental molecular clouds and impact galaxy evolution. The high-mass protostar DR21 Main in Cygnus X possesses one of the largest and most luminous outflows ever detected in the Galaxy, but the origin of its structure and driving mechanisms are still debated. Aims. Our aim is to spatially resolve the far-infrared line emission from DR21 Main and to investigate the gas physical conditions, energetics, and current mass loss rates along its outflow. Methods. Far-infrared SOFIA FIFI-LS spectra covering selected high-J CO lines, OH, [O I], [C II], and [O III] lines are analyzed across almost the full extent of the DR21 Main outflow using 2.00′ × 3.75′ mosaic. Results. The spatial extent of far-infrared emission closely follows the well-known outflow direction of DR21 Main in the case of high-J CO, [O I] 63.18 μm, and the OH line at 163.13 μm. On the contrary, the emission from the [C II] 157.74 μm and [O I] 145.53 μm lines arises mostly from the eastern part of the outflow, and is likely linked with a photodissociation region. Comparison of non-LTE radiative transfer models with the observed [O I] line ratios suggest H2 densities of ∼105 cm-3 in the western part of the outflow and ∼ 104 cm-3 in the east. Such densities are consistent with the predictions of UV-irradiated non-dissociative shock models for the observed ratios of CO and [O I] along the DR21 Main outflow. Assuming that the bulk of the emission arises in shocks, the outflow power of DR21 Main of 4.3-4.8 × 102 L⊙ and the mass loss rate of 3.3-3.7 × 10-3 M⊙ yr-1 are determined, consistent with estimates using HCO+ 1-0. Conclusions. Spatially resolved far-infrared emission of DR21 Main provides a strong support for its origin in outflow shocks, and the stratification of physical conditions along the outflow. The total line cooling provides additional evidence that DR21 Main drives one of the most energetic outflows in the Milky Way.
KW - HII regions
KW - ISM: jets and outflows
KW - Photon-dominated region (PDR)
KW - Stars: formation
KW - Stars: massive
KW - Stars: protostars
UR - https://www.scopus.com/pages/publications/105006601654
UR - https://www.scopus.com/pages/publications/105006601654#tab=citedBy
U2 - 10.1051/0004-6361/202453109
DO - 10.1051/0004-6361/202453109
M3 - Article
AN - SCOPUS:105006601654
SN - 0004-6361
VL - 697
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A186
ER -