Notes. Columns 1–3 list the names and coordinates of sources (the top four sources with SOFIA observations). Column 4 list the variability type: M (Mira) and SR (Semi-regular), as adopted from Ramstedt & Olofsson (2014), with the type for S Cep taken from the American Association of Variable Star Observers (AAVSO; https://www.aavso.org/). Columns 5–8 provide the distance, the stellar LSR velocity ($V_{\text{LSR}}^{\ast }$), the terminal expansion velocity of the envelope (V_exp), the mass-loss rate (Ṁ) and the stellar pulsation period, respectively. ^(a) Stellar parameters for IRC+10216, CIT 6, and II Lup are adopted from Menten et al. (2018), and the distances derived from the Mira period-luminosity relation are used in this work. We caution that the adopted $V_{\text{LSR}}^{\ast }$ may be slightly overestimated as the contribution from microturbulence has not been subtracted. ^(b) Stellar parameters for Y CVn, S Cep, IRC+50096, V Cyg, and CRL 3068 are adopted from Massalkhi et al. (2018), except for their stellar pulsation periods that are derived from the AAVSO.