A spectral line survey of the starless and proto-stellar cores detected by BLAST toward the Vela-D molecular cloud

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Volume 543 (July 2012)

A&A, 543 (2012) A65

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Issue		A&A Volume 543, July 2012


Article Number		A65
Number of page(s)		33
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201218836
Published online		27 June 2012

Online material

Appendix A: Spectral line maps

	Fig. A.1 Maps of the line integrated intensities (from left to right, N₂H⁺(1 − 0), HCN(1 − 0), HCO⁺(1 − 0) and HNC(1 − 0), in units of [K km s^-1] ) of selected sources toward Vela-D. In this figure we show, from top to bottom, maps of BLAST009, BLAST013, BLAST024 and BLAST031. The white dashed contours represent the BLAST flux density at 250 μm.
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	Fig. A.2 Same as Fig. A.1 for sources BLAST034, BLAST040, BLAST041 and BLAST047.
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	Fig. A.3 Same as Fig. A.1 for sources BLAST050, BLAST055, BLAST056 and BLAST063.
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	Fig. A.4 Same as Fig. A.1 for sources BLAST081, BLAST082 and BLAST101. The bottom row shows the HCO⁺(1 − 0) integrated intensity maps of sources BLAST057, BLAST089 and BLAST109.
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Appendix B: Molecular line spectra

	Fig. B.1 Spectra of N₂H⁺(1 − 0) toward the Vela-D sources, in the T_mb scale, obtained with the Mopra telescope.
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	Fig. B.2 Same as Fig. B.1 for the HCN(1 − 0) line.
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	Fig. B.2 continued.
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	Fig. B.3 Same as Fig. B.1 for the HNC(1 − 0) line.
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	Fig. B.3 continued.
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	Fig. B.4 Same as Fig. B.1 for the HCO⁺(1 − 0) (lower spectra) and H¹³CO⁺(1 − 0) (upper spectra) lines. Only sources where H¹³CO⁺(1 − 0) was detected are shown.
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	Fig. B.5 Same as Fig. B.1 for the H¹³CN(1 − 0) (upper spectra) lines, shown together with the corresponding HCN(1 − 0) (lower spectra) lines. Only sources where H¹³CN(1 − 0) was detected are shown.
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	Fig. B.6 Spectra of the NH₃(1, 1) line obtained with the Parkes telescope.
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Appendix C: Molecular lines parameters

Table C.1

N₂H⁺ line parameters.

Table C.2

HCN and H¹³CN line parameters.

Table C.3

HNC line parameters.

Table C.4

HCO⁺ and H¹³CO⁺ line parameters.

© ESO, 2012

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