Notes. Velocities and flux densities refer to individual maser components identified through multi-Gaussian fits to the spectral profiles. V_range indicates the total velocity interval over which maser emission was detected (shaded blue regions in Fig. 1). For each transition, the subcolumns report the peak velocity and flux density of each Gaussian component, listed in order of increasing velocity. Typical 1σ uncertainties are ∼0.1 km s⁻¹ in velocity and ∼10% in flux density (median values). Where possible, components from different (sub)millimeter transitions are placed on the same row when their peak velocities are similar (within a few km s⁻¹). Blank entries indicate either non-detection or lack of a velocity match across transitions. The 22 GHz maser properties are drawn from previous studies across different epochs and resolutions: SerpensFIRS1 (Furuya et al. 2003; Bae et al. 2011), L1641N,MM1/3 (Bae et al. 2011; Kang et al. 2013), YLW16A (Furuya et al. 2003; Sunada et al. 2007), and IRAS16293–2422 (Furuya et al. 2003; Sunada et al. 2007). When multiple nearby components are reported, we bin them in 0.5 km s⁻¹ intervals and average the velocity; for repeated observations, we adopt the mean peak flux density. The last column indicates the following references (Ref.): Furuya et al. (2003), R2: Sunada et al. (2007), R3: Bae et al. (2011), R4: Kang et al. (2013), and R5: Ortiz-León et al. (2021).