Table A.1.
Data for the stars observed within the ALMA proposal 2013.1.01200.S.
Input ALMA observationsb | ALMA continuum | ALMA CO(2-1) | ||||||||
---|---|---|---|---|---|---|---|---|---|---|
IDa | α(J2000.0) | δ(J2000.0) |
![]() |
α (peak flux) | δ (peak flux) | Peak intensity | σrms | σrms | vLSR | vLSR (c) |
[mJy/beam] | [mJy/beam] | [mJy/beam] | [km s−1] | [km s−1] | ||||||
F01 | 18 37 56.29 | −06 52 32.2 | 129.5 | 18 37 56.31 | −06 52 32.25 | 0.420 | 0.051 | 1.7 | 117.5 | 117.7 |
F02 | 18 37 55.28 | −06 52 48.4 | 114.2 | 18 37 55.29 | −06 52 48.50 | 0.359 | 0.051 | 1.9 | 120.5 | 119.7 |
F03 | 18 37 59.72 | −06 53 49.4 | 127.2 | 18 37 59.74 | −06 53 49.50 | 0.160 | 0.053 | 2.1 | 123.5 | − |
F04 | 18 37 50.90 | −06 53 38.2 | 121.2 | 18 37 50.89 | −06 53 38.45 | 0.097 | 0.055 | 2.0 | 123.5 | 124.3 |
F05 | 18 37 55.50 | −06 52 12.2 | 124.8 | 0.051 | 2.0 | − | ||||
F06 | 18 37 57.45 | −06 53 25.3 | 120.7 | 0.051 | 2.0 | − | ||||
F07 | 18 37 54.31 | −06 52 34.7 | 121.6 | 0.055 | 2.2 | − | ||||
F08 | 18 37 55.19 | −06 52 10.7 | 128.2 | 0.050 | 2.0 | − | ||||
F09 | 18 37 57.77 | −06 52 22.2 | 121.6 | 0.053 | 2.4 | − | ||||
F10 | 18 37 59.53 | −06 53 31.9 | 122.0 | 0.051 | 2.0 | − | ||||
F11 | 18 37 51.72 | −06 51 49.9 | 124.1 | 0.052 | 2.0 | − | ||||
F12 | 18 38 03.30 | −06 52 45.1 | − | 0.051 | 1.8 | − | ||||
F13 | 18 37 58.90 | −06 52 32.1 | 125.4 | 18 37 58.90 | −06 52 32.05 | 0.148 | 0.051 | 1.8 | 123.5 | 120.5 |
F14 | 18 37 47.63 | −06 53 02.3 | 122.0 | 0.052 | 1.7 | − | ||||
F15 | 18 37 57.78 | −06 52 32.0 | 120.8 | 0.051 | 1.9 | − |
Notes. First part of the table lists the target identifier, the input coordinates for the ALMA observations, and the vLSR as derived by Davies et al. (2008). The second part of the table lists for the four sources detected in the ALMA band 6 continuum data and in CO(2-1) the coordinates of the peak of the continuum emission, the peak flux, and the rms noise of the continuum observations. The third part lists the CO(2-1) line rms noise and the vLSR deduced from the ALMA CO(2-1) data. The last part list the vLSR values deduced by Nakashima & Deguchi (2006) from the analysis of SiO masers.
The stellar IDs from Figer et al. (2006).
From Davies et al. (2008).
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