Tracing the sulfur depletion in starless and pre-stellar cores

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Table 3

Line properties of L1495A-S, showing Gaussian fit results for the observed transitions and upper limits for non-detections.

Source /Molecule	Frequency (GHz)	T_MB (K)	rms (mK)	W (K km s⁻¹)	v_LSR (km s⁻¹)	∆v (km s⁻¹)	τ	N_tot (10¹¹ cm⁻²)
L1495A-S
HCS⁺	85.347	0.38	10	0.118 ± 0.013	7.375	0.293	0.056 ± 0.006	6.8 ± 0.7
SO	86.093	0.43	14	0.130 ± 0.005	7.267	0.288	0.063 ± 0.002	102.6 ± 3.6
CCS	86.181	0.30	11	0.083 ± 0.004	7.217	0.261	0.044 ± 0.003	25.2 ± 1.2
C₃S	92.488	0.05	6	0.012 ± 0.002	7.314	0.203	0.008 ± 0.002	3.5 ± 0.5
¹³CS	92.494	0.39	9	0.190 ± 0.004	7.389	0.457	0.065 ± 0.002	9.7 ± 0.2
HDCS	92.981	0.17	8	0.058 ± 0.003	7.344	0.319	0.025 ± 0.001	9.0 ± 0.4
S¹⁸O	93.267	0.07	3	0.031 ± 0.001	7.385	0.406	0.011 ± 0.000	4.1 ± 0.2
CCS	93.870	0.66	5	0.223 ± 0.002	7.317	0.318	0.100 ± 0.001	32.8 ± 0.3
C³⁴S	96.412	0.46	14	0.232 ± 0.007	7.273	0.471	0.078 ± 0.003	11.3 ± 0.4
OCS	97.301	0.14	6	0.045 ± 0.002	7.298	0.296	0.021 ± 0.001	62.1 ± 2.2
³⁴SO	97.715	0.31	4	0.115 ± 0.001	7.264	0.352	0.045 ± 0.001	14.5 ± 0.2
SO	99.299	1.36	8	0.610 ± 0.003	7.223	0.422	0.223 ± 0.015	82.7 ± 0.7
CCS	99.866	0.17	7	0.042 ± 0.002	7.345	0.233	0.025 ± 0.001	14.8 ± 0.6
H₂CS	101.477	1.024	15	0.300 ± 0.005	7.215	0.275	0.164 ± 0.003	87.1 ± 1.4
H₂CS	103.040	0.75	10	0.230 ± 0.004	7.247	0.290	0.116 ± 0.002	46.1 ± 0.7
CCS	103.640	0.14	5	0.046 ± 0.002	7.321	0.315	0.020 ± 0.001	20.6 ± 0.9
SO₂	104.029	0.14	10	0.048 ± 0.003	7.321	0.334	0.020 ± 0.001	13.1 ± 0.8
H₂CS	104.617	0.80	7	0.262 ± 0.002	7.272	0.309	0.124 ± 0.001	73.6 ± 0.6
SO	109.252	0.41	6	0.137 ± 0.002	7.431	0.315	0.062 ± 0.001	97.5 ± 1.3
OCS	109.463	0.14	5	0.048 ± 0.001	7.294	0.326	0.020 ± 0.001	86.7 ± 2.5
CCS	113.410	0.12	14	0.030 ± 0.003	7.312	0.232	0.018 ± 0.002	13.7 ± 1.4

Notes. Line properties were derived using Gaussian fits. Upper limits were determined as $3 σ \sqrt{Δv δ v}$ $Mathematical equation: $3\sigma \sqrt {{\rm{\Delta v}}\delta {\rm{v}}} $$ , following Jiménez-Serra et al. (2016), where σ is the rms noise, ∆v the full width at half maximum, and δv the spectral velocity resolution. The reported v_LSR and ∆v values are given without uncertainties, as the statistical uncertainties are significantly smaller than the spectral resolution.

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