Issue |
A&A
Volume 522, November 2010
|
|
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Article Number | A106 | |
Number of page(s) | 19 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/201014524 | |
Published online | 09 November 2010 |
Online material
Appendix A: Sofi imaging
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Fig. A.1
SOFI Js image of CG 1 head. Square root scaling has been used to enhance the appearance of the faint surface brightness structures. |
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Fig. A.2
SOFI H image of CG 1 head. Square root scaling has been used to enhance the appearance of the faint surface brightness structures. |
Open with DEXTER |
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Fig. A.3
SOFI Ks image of CG 1 head. Square root scaling has been used to enhance the appearance of the faint surface brightness structures. |
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Fig. A.4
SOFI Ks (in black) and H (in red) surface brightness contours superimposed on a grey scale Js image. The contour levels in SOFI counts are from 100 to 1100 in steps of 100 in Ks and from 10 to 90 in steps of 10 in H . The wedge in the right shows the Js grey scale levels. The image size is 23″ by 23″ and SOFI pixel scale is 0288. |
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Appendix B: C18O mapping
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Fig. B.1
Contour map of the integrated C18O(1–0) emission in CG 1 head in TMB scale. The contour levels are from 0.25 K km s-1 to 1.25 K km s-1 in steps of 0.25 K km s-1. The points indicate the measured points and the square the location of the YSO in the figure. The SEST HPBW at the C18O(1–0) frequency is shown in the upper left corner. |
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Fig. B.2
Contour map of the integrated C18O(2–1) emission in CG 1 head in TMB scale. The contour levels are from 0.4 K km s-1 to 2.0 K km s-1 in steps of 0.4 K km s-1. The points indicate the measured points and the square the location of the YSO in the figure. The SEST HPBW at the C18O(2–1) frequency is shown in the upper left corner. |
Open with DEXTER |
Appendix C: ESO archive data
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Fig. C.1
CO (3–2) map in the direction of the YSO. The spectra are plotted from 1 km s-1 to 7 km s-1 in velocity and from –1 K to 12 K in |
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© ESO, 2010
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