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Table 3.

λ6 cm small-diameter H II regions that have WISE H II region counterparts but are not in the Paladini catalogue.

No. G-NAME GLong6 cm GLat6 cm θmaj θmin S6 cm GLongwise GLatwise diameter WISE type D Ref. Notes
(°) (°) (′) (′) (Jy) (°) (°) (′) (kpc)
1 G12.2−0.1 12.232 −0.110 8.4 5.7 5.405 12.145 0.000 13.4 K One λ6 cm source matches thirteen WISE H II regions
12.184 −0.113 0.7 K
12.192 −0.104 1.0 K
12.194 −0.144 0.6 K
12.194 −0.112 0.6 K
12.194 −0.129 1.6 K
12.199 −0.034 1.4 K
12.202 −0.110 0.8 K
12.209 −0.105 0.7 K
12.216 −0.119 0.8 K
12.217 −0.138 2.3 K
12.229 −0.115 2.0 K
12.311 −0.059 6.0 K
2 G19.8+0.3 19.775 0.285 <3.1 <3.1 0.655 19.741 0.280 1.4 K 14.20 ± 0.61 hh14 One λ6 cm source matches two WISE H II regions
19.781 0.287 3.7 K 17.28 ± 1.22 hh14
3 G23.5+1.6 23.547 1.589 <3.1 <3.1 0.147 23.569 1.582 3.9 K 2.94 ± 0.42 hh14
4 G26.4+1.5 26.373 1.451 8.1 5.7 1.216 26.385 1.399 19.8 K One λ6 cm source matches two WISE H II regions
26.385 1.401 3.8 K 3.03 ± 0.40 hh14

Notes. Columns 1 and 2: sequential number and G-name; Cols. 3 and 4: Galactic longitude and latitude of the λ6 cm source; Cols. 5 and 6: intrinsic size θmaj and θmin of the λ6 cm source, obtained following Eq. (1) by assuming the sources to be Gaussian. The observed sizes (θfit, maj and θfit, min) used for the deconvolution are taken from Reich et al. (2014). The Galactic position angle for each source can be found in Reich et al. (2014); Col. 7: integrated flux density at λ6 cm; Cols. 8 and 9: Galactic longitude and latitude of the matched WISE H II region; Col. 10: diameter of the matching WISE H II region; Col. 11: group type of the WISE H II region, K* indicates currently known H II regions (original C-type WISE H II regions) according to Kim et al. (2018); Columns 12 and 13: distance information and their references; Column 14: remarks for the source. Some other references in the 14th column: e.g. Suad et al. (2012). Full table is accessible from the CDS.

References. abb+14: Anderson et al. (2014); aaj+15: Anderson et al. (2015); aal+18: Anderson et al. (2018); cpt06: Comerón et al. (2006); fb15: Foster & Brunt (2015); hh14: Hou & Han (2014); mdf+11: Moisés et al. (2011); rus03: Russeil (2003); rag07: Russeil et al. (2007); xlr+13: Xu et al. (2013b).

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