Table 1.
Log of the NACO observations including observing conditions.
| RMS name | α (J2000) | δ (J2000) | MJD | KS | L′ | Distance | Lbol | Seeing | Contrast | Mult. |
|---|---|---|---|---|---|---|---|---|---|---|
| (h m s) | (° ′ ″) | (kpc) | (L⊙) | (mas) | (L′ mag) | |||||
| G194.9349−01.2224 | 06 13 16.12 | +15 22 43.8 | 56271.2 | 9.8 | 6.8 | 2.0 (a) | 2620 | 0.82 | 2.0 | N |
| G203.3166+02.0564 | 06 41 10.12 | +09 29 33.7 | 56307.2 | 4.9 | 1.7 | 0.74 (b) | 1080 | 1.25 | 7.2 | Y |
| G232.6207+00.9959 | 07 32 09.86 | −16 58 13.0 | 56295.3 | 8.3 | 5.3 | 1.68 (c) | 11 270 | 0.76 | 3.3 | Y |
| G254.0548−00.096108 | 08 17 52.51 | −35 52 50.2 | 56317.1 | 9.5 | 7.2 | 2.75 | 4910 | 1.27 | 2.2 | N |
| G263.7434+00.1161 | 08 48 48.74 | −43 32 29.0 | 56257.3 | 9.0 | 3.8 | 0.7 | 520 | 0.68 | 6.9 | N |
| G263.7759−00.4281 | 08 46 34.90 | −43 54 31.6 | 56295.3 | 9.6 | 5.7 | 0.7 (d) | 880 | 0.68 | 3.9 | Y |
| G265.1438+01.4548 | 08 59 27.40 | −43 45 03.7 | 56307.2 | 9.6 | 3.8 | 0.7 (d) | 670 | 0.85 | 3.6 | Y |
| G268.3957−00.4842 | 09 03 25.15 | −47 28 27.1 | 56308.3 | 8.3 | 3.9 | 0.7 (d) | 720 | 0.95 | 7.2 | Y |
| G269.1586−01.1383A | 09 03 32.1 | −48 28 43.3 | 56314.3 | 10.7 | 7.4 | 0.7 (d) | 220 | 1.20 | 1.4 | Y |
| G305.2017+00.2072A | 13 11 10.45 | −62 34 38.6 | 56314.2 | 9.4 | 5.5 | 4.0 (e) | 30 320 | 0.95 | 2.5 | Y |
| G310.0135+00.3892 | 13 51 37.92 | −61 39 07.5 | 56309.3 | 4.9 | 2.3 | 3.25 | 54 680 | 1.42 | 7.1 | Y |
| G314.3197+00.1125 | 14 26 26.3 | −60 38 31.5 | 56313.3 | 10.6 | 4.7 | 3.6 (f) | 12 870 | 1.06 | 3.2 | N |
| G318.0489+00.0854B | 14 53 42.7 | −59 08 58.9 | 56319.4 | 11.7 | 7.7 | 3.36 (f) | 6810 | 1.03 | 2.6 | N |
Notes. The first three columns list the names, Right Ascension (α) and Declination (δ), taken from the RMS survey (Lumsden et al. 2013). The KS magnitude is taken from 2MASS, considering that the nearest 2MASS source to the MSX position is assumed to be associated. The estimated L′ mag are extrapolated from the WISE W1-band and W2-band magnitudes. Distances are taken from the RMS catalogue (Urquhart et al. 2011) and we add further references in the notes of this table. Bolometric luminosities were derived in Mottram et al. (2011). The uncertainties on distances are rather large: of the order of ∼1 kpc and of about 20 to 35% for the bolometric fluxes. The L′-contrast magnitudes are derived following a method that consists in injecting artificial sources and that is described in Sect. 3.5. The last column named “Mult.” (for multiple) indicates the detection of any companion in the NACO images: N stands for NO while Y stands for YES. A more detailed analysis is given in Sect. 4.
References. (a) Kawamura et al. (1998); (b)H2O maser: Kamezaki et al. (2014); (c)maser parallax distance: Reid et al. (2009); (d) Liseau et al. (1992), Netterfield et al. (2009); (e)Parallax of 6.7 GHz methanol maser: Krishnan et al. (2017); (f)kinematic distance using the source velocity: Green & McClure-Griffiths (2011), Green et al. (2012).
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