^a The peak H₂ column density at the peak derived from Herschel data at the original resolution of the 500 μm surface brightness maps (${36}_{\cdot }^{\mathrm{\prime }\mathrm{\prime }}3$). The dust temperature is reported in Table B.1. The values are taken from catalogs provided by the Herschel Gould Belt Survey Archive.

^b S: The Sepia345 receiver used in two tunings covering the frequency ranges 1) 271.8–279.7 GHz (LSB) and 288.0–295.9 GHz (USB), and 2) 287.3-295.3 GHz (LSB) and 303.6–311.5 GHz (USB); so the frequencies ~288–295 GHz were observed twice. F: The nFLASH230/460 dual channel receiver tuned to cover the frequency ranges 224.4–232.3 GHz (LSB), 240.6–248.5 GHz (USB), 462.2–466.2 GHz (LSB), and 474.6–478.6 GHz (USB).

^c An asterisk next to the HGBSA name indicates association with a YSO; see main text.

References: ^A André et al. (1993); ^C Chen et al. (2019); ^Chini Chini et al. (2003); ^D04 Di Francesco et al. (2004); ^D08 Di Francesco et al. (2008); ^E Eden et al. (2019); ^F09 Friesen et al. (2009); ^F10 Friesen et al. (2010b); ^G Gaczkowski et al. (2015); ^Gro Groppi et al. (2007); ^H Haas et al. (2008); ^HGBS,B Bresnahan et al. (2018); ^HGBS,M Marsh et al. (2016); ^HGBS,L Ladjelate et al. (2020); ^H–U Hardegree-Ullman et al. (2013); ^Ka Kamazaki et al. (2019); ^Ke Kerr et al. (2019); ^Ki Kirk et al. (2017); ^M Motte et al. (1998); ^N Nutter et al. (2005); ^P Pattle et al. (2015); ^S Stanke et al. (2006); ^Y Yonekura et al. (1999)