The structure of the Cepheus E protostellar outflow: The jet, the bowshock, and the cavity

B. Lefloch; A. Gusdorf; C. Codella; J. Eislöffel; R. Neri; A. I. Gómez-Ruiz; R. Güsten; S. Leurini; C. Risacher; M. Benedettini

doi:10.1051/0004-6361/201425521

Free Access

Issue		A&A Volume 581, September 2015


Article Number		A4
Number of page(s)		21
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201425521
Published online		21 August 2015

Online material

Appendix A: Complementary single-dish CO observations

	Fig. A.1 Map of the CO J = 2–1 emission integrated in channels of 3.25km from −13.5 to +113.1 km s^-1, as observed with the IRAM 30 m telescope. The position of the protostar is marked by a red star. The positions targeted by GREAT/SOFIA and HIFI/Herschel are marked by blue stars. The size of the telescope HPBW (10.7″) is indicated by the white circle.
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	Fig. A.2 Map of the CO J = 2–1 emission integrated in channels of 3.25km from −137.0 to −10.3 km s^-1, as observed with the IRAM 30 m telescope. The position of the protostar is marked by a red star. The positions targeted by GREAT/SOFIA and HIFI/Herschel are marked by blue stars. The size of the telescope HPBW (10.7″) is indicated by the white circle.
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	Fig. A.3 Map of the CO J = 3–2 emission integrated in channels of 3.25km from −13.5 to +113.1 km s^-1, as observed with the JCMT. The position of the protostar is marked by a red star. The positions targeted by GREAT/SOFIA and HIFI/Herschel are marked by blue stars. The size of the telescope HPBW (15″) is indicated by the white circle.
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	Fig. A.4 Map of the CO J = 3–2 emission integrated in channels of 3.25km from −137 to −10.3 km s^-1, as observed with the JCMT. The position of the protostar is marked by a red star. The positions targeted by GREAT/SOFIA and HIFI/Herschel are marked by blue stars. The size of the telescope HPBW (15″) is indicated by the white circle.
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Appendix B: Excitation conditions in the outflow cavity

	Fig. B.1 χ² distribution of LVG slab models for different velocity intervals in the low-excitation gas of the outflow cavity. The considered velocity intervals are indicated in each panel. The minimum value and the contour levels are indicated in each panel.
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	Fig. B.2 χ² distribution of LVG slab models for different velocity intervals in the high-excitation gas of the outflow cavity. The considered velocity intervals are indicated in each panel. The minimum value and the contour levels are indicated in each panel.
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	Fig. B.3 Best fitting solutions of the CO spectral line flux distribution as a function of the rotational number of the transition from our LVG analysis with the MADEX radiative transfer code. The fits to the low- and high-excitation components are shown by black solid and dashed lines, respectively. The fit to the total flux is shown in red.
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© ESO, 2015

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