Notes. A portion of this table is listed here. The entire version will be available as a machine-readable form at the CDS and at the authors’ webpage. Columns 1−3 list the Number, the Galactic longitude, and the Galactic latitude for HII regions, taken from the reference listed in Col. 4; Cols. 5 and 6 list the velocity and its uncertainty if available. The V_LSR are directly taken from references. The standard solar motion [20.0 km s^-1, toward RA (1900) = 18h and Dec (1900) = 30 deg] was generally adopted to get V_LSR ; Col. 7 is the measured electron temperature; Cols. 8 and 9 list the used telescope and the observed line(s) derived from the reference in Col. 10. The abbreviations for telescopes are: GBT – the Green Bank 100 m telescope; Are – the Arecibo 305 m telescope; B&M – the 7 m telescope of the Bell Telescope Laboratories and the 5 m telescope at the Millimeter Wave Observatory; SET – the Swedish-ESO Submillimeter telescope; OSO – the Onsala Space Observatory 20 m telescope; PKS – the Parkes 64 m telescope; GBO – the 42.6 m telescope of the NRAO at Green Bank; BRAL – the 25.8 m telescope of the Berkeley Radio Astronomy Laboratory; Eff – the Effelsberg 100 m telescope; XAO – the 25 m telescope of Xinjiang Observatory; LO – the 0.76 m telescope at the Leuschner Observatory; DRAO – The 25.6 m telescope at the Dominion Radio Astrophysical Observatory; ARO – the 46 m telescope of the Algonquin Radio Observatory. Columns 11−13 are the radio continuum flux of the HII region, the observation frequency and the reference if available. Columns 14−16 list the photometric or trigonometric distance when available, as well as the uncertainty and the reference; Col. 17 is a note for the kinematic distance ambiguity and Col. 18 is the reference(s) and note: knear – the nearer kinematic distance is adopted; kfar – the farther kinematic distance is adopted; ktan – the tracer is located at the tangential point and the distance to the tangent is adopted; kout – the tracer is in the outer Galaxy; n3kpc – the tracer is located in the Near 3 kpc Arm; f3kpc – the tracer is in the Far 3 kpc Arm; Cols. 19 and 20 list the distance to the GC and the distance to the Sun, the kinematic distances when adopted are calculated with a flat rotation curve with the IAU standard R₀ = 8.5 kpc and Θ₀ = 220 km s^-1 and the standard solar motions; Col. 21 is the excitation parameter re-scaled by the adopted distance; Cols. 22−24 are the same as Cols. 19−21, except with fundamental parameters R₀ = 8.3 kpc and Θ₀ = 239 km s^-1 (Brunthaler et al. 2011) and the solar motions of Schönrich et al. (2010); Cols. 25−27 are the same as Cols. 19−21, except with the rotation curve of Brand & Blitz (1993).

Reference. ab09: Anderson & Bania (2009); abbr11: Anderson et al. (2011); abbr12: Anderson et al. (2012); adps79: Altenhoff et al. (1979); adg+70: Altenhoff et al. (1970); ahck02: Araya et al. (2002); alb80: Abraham et al. (1980); bab12: Bania et al. (2012); bfs82: Blitz et al. (1982); bnm96: Bronfman et al. (1996); brba11: Balser et al. (2011); brm+09: Brunthaler et al. (2009); bwl09: Beuther et al. (2009); casw72: Caswell (1972); cf08: Crowther & Furness (2008); ch87: Caswell & Haynes (1987); cmh74: Churchwell et al. (1974); cor+07: Copetti et al. (2007); cpt06: Comerón et al. (2006); diet67: Dieter (1967); dlr+11: Dzib et al. (2011); dm72: Dickel & Milne (1972); dsa+10: Deharveng et al. (2010); dwbw80: Downes et al. (1980); dze+11: Duet al. (2011); fb84: Fich & Blitz (1984); fb14: Foster & Brunt (2014); fc72: Felli & Churchwell (1972); frwc03: Fish et al. (2003); fdt90: Fich et al. (1990); F3R: Furst et al. (1990); GB6: Gregory et al. (1996); gg76: Georgelin & Georgelin (1976); gm11: Green & McClure-Griffiths (2011); gmb+07: Garay et al. (2007); hab+08: Hirota et al. (2008a); hbc+07: Hirota et al. (2007); hbc+08: Hirota et al. (2008b); hbc+07b: Honma et al. (2007); hbm+09: Hachisuka et al. (2009); hls+00: Henning et al. (2000); hze+11: Han et al. (2011); hhi+11: Hirota et al. (2011); irm+13: Immer et al. (2013); jd12: Jones & Dickey (2012); kb94: Kuchar & Bania (1994); kc97: Kuchar & Clark (1997); kcw94: Kurtz et al. (1994); kjb+03: Kolpak et al. (2003); kns+11: Kurayama et al. (2011); kwc77: Kazes et al. (1977); lock79: Lockman (1979); lock89: Lockman (1989); lph96: Lockman et al. (1996); lra11: Lépine et al. (2011); lt08: Leahy & Tian (2008); lbbs14: Lima et al. (2014); mcr+11: Moscadelli et al. (2011); mdf+11: Moisés et al. (2011); mg68: McGee & Gardner (1968); mgps2: Murphy et al. (2007); mh67: Mezger & Hoglund (1967); mitg: Bennett et al. (1986); mn81: McGee & Newton (1981); mnb75: McGee et al. (1975); mrm+09: Moscadelli et al. (2009); mcg09: Moellenbrock et al. (2009); msh+11: Motogi et al. (2011); nnh+11: Niinuma et al. (2011); okh+10: Oh et al. (2010); pbd+03: Paladini et al. (2003); pbt77: Pankonin et al. (1977); pco10: Pinheiro et al. (2010); pdd04: Paladini et al. (2004); pedl80: Pedlar (1980); PMN: Wright et al. (1994, 1996); Griffith et al. (1994, 1995); qrbb06: Quireza et al. (2006); rag07: Russeil et al. (2007); rbr+10: Rygl et al. (2010); rbs+12: Rygl et al. (2012); rmb+09: Reid et al. (2009a); rmhg80: Rodriguez et al. (1980); rmz+09: Reid et al. (2009c); ross78: Rossano (1978); rus03: Russeil (2003); rwb+70: Reifenstein et al. (1970); shd+11: Shiozaki et al. (2011); shr+10: Sato et al. (2010a); srbm10: Sato et al. (2010b); srd+12: Sanna et al. (2012); srm+09: Sanna et al. (2009); srm+14: Sanna et al. (2014); st79: Silverglate & Terzian (1979); swa+04: Sewilo et al. (2004); uhl12: Urquhart et al. (2012); vch76: Viner et al. (1976); vgd+10: Vollmer et al. (2010); wa72: Wilson & Altenhoff (1972); wam82: Wink et al. (1982); was+03: Watson et al. (2003); wend70: Wendker (1970); wmgm70: Wilson et al. (1970); wsr+14: Wu et al. (2014); wwb83: Wink et al. (1983); wxm+12: Wu et al. (2012); xlr+13: Xu et al. (2013); xmr+11: Xu et al. (2011); xrm+08: Xu et al. (2009); xrm+09: Xu et al. (2009); xrzm06: Xuet al. (2006); zms+14: Zhang et al. (2014); zrm+13: Zhang et al. (2013); zzr+09: Zhang et al. (2009); 87GB: Gregory & Condon (1991).