ALMA observations of TiO2 around VY Canis Majoris | Astronomy & Astrophysics (A&A)

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Volume 580 (August 2015)

A&A, 580 (2015) A36

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Issue		A&A Volume 580, August 2015


Article Number		A36
Number of page(s)		24
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201525990
Published online		23 July 2015

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Appendix A: Maps of titanium dioxide emission

Figures A.1 to A.15 show channel maps of the detected TiO₂ emission lines (Table 2, Fig. 1) at a velocity resolution of 2 km s^-1, covering the range −14 ≤ ν_LSR ≤ 78 km s^-1. This ν_LSR-range covers the bulk of all TiO₂ emission; emission at

more extreme velocities is no longer visible in the channel maps. Figure A.16 shows integrated-intensity maps for all listed lines, covering the ν_LSR-ranges indicated in Table 2. Figure A.17 shows a comparison of the TiO₂ line emission to the south-west tail detected at 310.78 GHz, which is discussed in Sects. 3.1 and 4.4.

Fig. A.1

Channel maps of the TiO₂ emission at 310.55 GHz, at a 2 km s^-1 velocity resolution. Black contours show the continuum measured with ALMA at 321 GHz (O+15; R+14). The stellar position is indicated with a white cross. Spatial scales are indicated in the top left panel and are the same for all panels. The colour scale starts at the 3σ level and is plotted as the square root of the flux for increased contrast.

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	Fig. A.2 Same as Fig. A.1, but for TiO₂ emission at 310.78 GHz.
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	Fig. A.3 Same as Fig. A.1, but for TiO₂ emission at 311.46 GHz.
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	Fig. A.4 Same as Fig. A.1, but for TiO₂ emission at 312.25 GHz.
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	Fig. A.5 Same as Fig. A.1, but for TiO₂ emission at 312.73 GHz.
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	Fig. A.6 Same as Fig. A.1, but for TiO₂ emission at 312.82 GHz.
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	Fig. A.7 Same as Fig. A.1, but for TiO₂ emission at 321.40 GHz. Artefacts in channels with ν_LSR ≥ 55 km s^-1 are due to the presence of strong SO₂ emission. See also Fig. 1.
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	Fig. A.8 Same as Fig. A.1, but for TiO₂ emission at 321.50 GHz.
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	Fig. A.9 Same as Fig. A.1, but for TiO₂ emission at 322.33 GHz.
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	Fig. A.10 Same as Fig. A.1, but for TiO₂ emission at 322.61 GHz.
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	Fig. A.11 Same as Fig. A.1, but for TiO₂ emission at 324.49 GHz.
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	Fig. A.12 Same as Fig. A.1, but for TiO₂ emission at 324.96 GHz.
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	Fig. A.13 Same as Fig. A.1, but for TiO₂ emission at 325.32 GHz.
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	Fig. A.14 Same as Fig. A.1, but for TiO₂ emission at 325.50 GHz.
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	Fig. A.15 Same as Fig. A.1, but for TiO₂ emission at 325.60 GHz.
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Fig. A.16

Integrated-intensity maps of TiO₂ emission. Colour maps show the intensity integrated over the ν_LSR-ranges indicated in Table 2 and Fig. 1 and cut off at 3σ. Contours show the ALMA 321 GHz continuum. Labels indicate the positions of the star (+, VY) and the continuum component (x, C) to the south-east (O+15; R+14), and the position and approximate extent of the south-west clump of Shenoy et al. (2013, SW and a dashed 1′′. The presence of cleaning artefacts, mainly at ~312 GHz, is addressed in Sect. 2.

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	Fig. A.17 Comparison of TiO₂ emission lines listed in Table 2 to south-west tail at 310.78 GHz (red contours) and HST image (black contours). Emission integrated over 19 ≤ ν_LSR ≤ 22 km s^-1 plotted at > 3σ (colour scale). Emission of 311.46 GHz was omitted since the relevant ν_LSR-range is not covered by the observations.
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© ESO, 2015

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