Survey of (sub)millimeter water masers in low-mass star-forming regions

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Volume 701 (September 2025)

A&A, 701 (2025) A167

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Table 1.

Proposed evolutionary scenario.

Region	MMcIsJ₋₁		H₂O				T_DD [K]	Relative age
	J = 7	J = 10	22	183	321	325
	70.6	133.2	643.5	204.71	1861.3	469.9

IRAS 16293	✗	✗	✓	✓	✓	✓	16.92 $_{- 4.70}^{+ 10.20}$ $_{-4.70}^{+10.20}$	quite young
CARMA 7	✓	✓	✓	✓	✗	✗	29.56 $_{- 2.50}^{+ 2.89}$ $_{-2.50}^{+2.89}$	very young
YLW16A	✗	✗	✓	✓	✗	✗	37.93 $_{- 11.14}^{+ 28.00}$ $_{-11.14}^{+28.00}$	young
Serpens FIRS	✗	✓	✓	✓	✓	✗	42.07 $_{- 17.61}^{+ 15.42}$ $_{-17.61}^{+15.42}$	slightly evolved
L1641N	✓	✓	✓	✓	✗	✗	48.493 $_{- 11.54}^{+ 6.18}$ $_{-11.54}^{+6.18}$	evolved
NGC 2024	✗	✓	✓	✗	✗	✗	94.04 $_{- 44.80}^{+ 62.58}$ $_{-44.80}^{+62.58}$	very evolved

Notes. Frequencies of the water masers are indicated in GHz, with upper energy levels in Kelvin shown below each transition label. The diffuse dust temperatures (T_DD) were derived from SED fits (see Appendix B).

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