A dataset provided by the European Space Agency

Name OT1_mrllig_1
Title Hot CO in the Massive Star Forming Region DR21
URL

http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342245386&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342255769&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342255770&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342255772&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342255773&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342256305&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342256306&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342256307&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342256420&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342256463&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342256464&instrument_name=HIFI&product_level=LEVEL0&compress=true
...
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342256465&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342256468&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342256469&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342259721&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342259722&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342259726&instrument_name=HIFI&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342259750&instrument_name=HIFI&product_level=LEVEL0&compress=true

DOI https://doi.org/10.5270/esa-flrcvmo
Author rollig, m.
Description We plan to resolve the detailed physical and dynamical
structure of the massive star forming (SF) region
DR21virgulC which has a prominent bipolar outflow visible
in 2 micron emission of vibrationally excited H2,
tracing hot, shocked gas. While, the shock is hardly
affecting most of the molecular line emission of the
region (Lane et al. 1990, Ossenkopf et al. 2010),
only [CII] is showing an additional broad blue wing
indicating that the [CII] emission is not only
originating from that warm gas, but also from the
ionized wind in the blister outflow.
H2 and CO are at least partly co-existent and hence
should show similar signs of shocks, but surprisingly
13CO(10-9) doesn.t, so many question remains:

- Is there any CO that is directly affected by the
shock and if so, at at which AV does the shock
excitation stop?
- Why does CO up to 10-9 show no direct signature
of shock heating or outflowing material?
- Does the shock only affect H_2 and ionized material?
- Which volume of the source is affected/heated by
the shock?
- Which volume of the source is heated by the UV
radiation from the cluster?

The aim of this proposal is to understand how
shock/outflow and UV radiation from the embedded
OB cluster contribute to the excitation of the
surrounding material and where exactly the transition
from shocked to unshocked material occurs.
Publication
Instrument HIFI_HifiMapping_raster, HIFI_HifiPoint_dbs, HIFI_HifiMapping_fly
Temporal Coverage 2012-05-04T19:39:03Z/2013-01-16T05:44:31Z
Version SPG v14.1.0
Mission Description Herschel was launched on 14 May 2009! It is the fourth 'cornerstone' mission in the ESA science programme. With a 3.5 m Cassegrain telescope it is the largest space telescope ever launched. It is performing photometry and spectroscopy in approximately the 55-671 µm range, bridging the gap between earlier infrared space missions and groundbased facilities.
Creator Contact https://support.cosmos.esa.int/h®erschel/
Date Published 2013-07-16T05:36:07Z
Publisher And Registrant European Space Agency
Credit Guidelines European Space Agency, rollig, m., 2013, OT1_mrllig_1, SPG v14.1.0, European Space Agency, https://doi.org/10.5270/esa-flrcvmo