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J/A+A/602/A8        Cepheus E CO, OH and OI spectra             (Gusdorf+, 2017)

Nature of shocks revealed by SOFIA OI observations in the Cepheus E protostellar outflow. Gusdorf A., Anderl S., Lefloch B., Leurini S., Wiesemeyer H., Guesten R., Benedettini M., Codella C., Godard B., Gomez-Ruiz A.I., Jacobs K., Kristensen L.E., Lesaffre P., Pineau des Forets G., Lis D.C. <Astron. Astrophys. 602, A8 (2017)> =2017A&A...602A...8G (SIMBAD/NED BibCode)
ADC_Keywords: Infrared sources ; Interstellar medium ; Carbon monoxide Keywords: astrochemistry - stars: formation - ISM: jets and outflows - ISM: individual objects: Cepheus E - ISM: kinematics and dynamics - infrared: ISM Abstract: Protostellar jets and outflows are key features of the star-formation process, and primary processes of the feedback of young stars on the interstellar medium. Understanding the underlying shocks is necessary to explain how jet and outflow systems are launched, and to quantify their chemical and energetic impacts on the surrounding medium. We performed a high-spectral resolution study of the [OI]63um emission in the outflow of the intermediate-mass Class 0 protostar Cep E-mm. The goal is to determine the structure of the outflow, to constrain the chemical conditions in the various components, and to understand the nature of the underlying shocks, thus probing the origin of the mass-loss phenomenon. We present observations of the OI 3P1 -> 3P2, OH between 2Π1/2 J=3/2 and J=1/2 at 1837.8GHz, and CO (16-15) lines with the GREAT receiver onboard SOFIA towards three positions in the Cep E protostellar outflow: Cep E-mm (the driving protostar), Cep E-BI (in the southern lobe), and Cep E-BII (the terminal position in the southern lobe). Description: All spectra shown in Fig. 2 are provided in FITS format at their nominal spectral and spatial resolution x-axis is the lsr velocity (in km/s) y-axis is the main beam temperature (in K) they were obtained with the SOFIA-GREAT receiver (see Table 2 for details): - the CO, OH, and OI spectra shown in the upper panel (Cep E - mm position) are in the co-cepe-mm.fits, oh-cepe-mm.fits, and oI-cepe-mm.fits files; - the CO, OH, and OI spectra shown in the middle panel (Cep E - BI position) are in the co-cepe-BI.fits, oh-cepe-BI.fits, and oI-cepe-BI.fits files; - the CO, OH, and OI spectra shown in the upper panel (Cep E - BII position) are in the co-cepe-BII.fits, oh-cepe-BII.fits, and oI-cepe-BII.fits files. Objects: ----------------------------------------------------- RA (2000) DE Designation(s) ----------------------------------------------------- 23 03 12.78 +61 42 25.8 Cep E = IRAS 23011+6126 ----------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 135 9 List of spectra fits/* 0 9 Individual spectra
Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000) 10- 18 F9.5 deg DEdeg Declination of center (J2000) 20- 22 I3 --- Nx Number of pixels along X-axis 24- 42 A19 --- Obs.Date Observation date (YYYY-MM-DD:hh:mm:ss) 44- 54 F11.6 GHz RestFreq Rest frequency 56- 64 F9.6 GHz bFreq Lower value of frequency interval 66- 72 F7.5 GHz BFreq Upper value of frequency interval 74- 81 F8.5 MHz dFreq Frequency resolution 83 I1 Kibyte size Size of FITS file 85-100 A16 --- FileName Name of FITS file, in subdirectory fits 102-135 A34 --- Title Title of the FITS file
Acknowledgements: Antoine Gusdorf, antoine.gusdorf(at)
(End) Patricia Vannier [CDS] 07-Apr-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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