Classifying the embedded young stellar population in Perseus and Taurus and the LOMASS database

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Table 2

Cloud-average central spectra properties.

		HCO⁺ 4–3			C¹⁸O 3–2

Cloud	V_lsr		T_mb	Δv		T_mb	Δv

Perseus^a	4.7	0.7	0.3	2.3	0.4	0.3	1.7
Perseus^b	8.0	3.2	1.3	2.3	2.5	1.0	2.4
Taurus	6.4	2.4	1.2	2.3	1.5	1.0	1.6

Notes. Central spectra are within a 15″ beam. Local standard of rest velocity, integrated intensity, and line width are derived from the Gaussian fit. Δv is the FWHM of the Gaussian fit. Peak main beam temperature is taken as the maximum value from the data.

^(a)

Fit to the weak blue component of Perseus spectra.

^(b)

Fit to the strong red component of Perseus spectra.

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