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Table 1

Observed integrated intensities ( in K km s-1) and half-power beam widths (θ in arcsec)a.

Source HCO+ 6–5 H13CO+ 1–0 H13CO+ 3–2 H13CO+ 4–3 N2H+ 1–0b N2H+ 6–5b References
W θ W θ W θ W θ W θ W θ

L1448 MM 1.37 43 2.0 43 1.9 19 0.92 21 12.48 27 0.19 41 1, 2, 3, 4
NGC 1333 IRAS2A 1.36 43 1.8 43 2.1 19 2.7 14 14.2 40 0.41 41 1, 2, 5
NGC 1333 IRAS4A 2.29 43 2.3 43 1.4 19 0.86 21 15.9 40 0.78 41 1, 2, 5, 6
NGC 1333 IRAS4B 1.88 43 2.1 43 0.57 19 ··· 13.5 40 0.64 41 1, 2, 5
L1527 1.06 43 2.2 43 1.1 19 0.47 14 3.91 27 <0.030 41 1, 2, 4
Ced110 IRS4 ··· ··· ··· 0.38 18 4.8 54 ··· 7, 8
BHR71 0.95 43 ··· ··· ··· 8.1 54 ··· 1, 8
IRAS 15398 0.75 43 ··· 0.52 28 ··· 9.4 54 ··· 8, 9
L483 MM 1.25 43 1.5 43 1.7 19 1.2 14 14.05 27 0.29 41 1, 2, 4
Ser SMM1 4.30 43 1.56 c 5.8 19 3.1 21 28 27 1.48 41 1, 5, 8, 10
Ser SMM4 2.08 43 1.13 c 2.9 19 1.2 21 49 27 ··· 1, 8, 10
Ser SMM3 1.74 43 <0.1 c 1.6 19 0.2 21 23 27 ··· 1, 8, 10
L723 MM 0.77 43 0.61 43 0.94 19 0.70 14 5.70 27 ··· 1, 2, 4
B335 0.63 43 0.24 24 0.46 28 ··· 6.05 27 ··· 1, 4, 11
L1157 0.54 43 0.89 29 0.61 19 0.52 14 8.38 27 0.07 41 1, 2, 4

L1489 0.40 43 0.96 43 0.82 19 0.61 14 0.26 40 ··· 2, 5
L1551 IRS5 ··· 1.55 19 2.4 19 2.2 14 15.7 40 ··· 2, 12
TMR1 ··· 1.1 43 0.51 19 0.20 14 0.37 40 ··· 2
TMC1A ··· 0.44 19 <0.27 19 <0.13 14 7.1 40 ··· 2, 12
TMC1 ··· 1.26 19 <0.27 19 <0.12 14 5.8 40 ··· 2, 12
HH46 IRS ··· ··· ··· 1.1 18 ··· ··· 7
Elias 29 0.28 43 0.36 72 0.09 28 ··· ··· ··· 13
RNO91 ··· 0.93 72 ··· ··· 11 27 ··· 8, 14

Notes.

(a)

Throughout the paper, Class 0 sources appear above the horizontal line and Class I sources below it. Tmb is the main-beam temperature, corrected for beam efficiencies as detailed in the references. Typical uncertainties on the integrated intensities are 10–25%. Upper limits are at the 3σ level. See Yıldız et al. (2013) for a compilation of C18O intensities and beam sizes.

(b)

The N2H+ intensities are summed over all hyperfine components (see text).

(c)

Integrated intensity over a 20′′ × 20′′ region (Hogerheijde et al. 1999).

Reference. (1) this work; (2) Jørgensen et al. (2004); (3) Gregersen et al. (1997); (4) Emprechtinger et al. (2009); (5) San José-García et al. (2015) and Benz et al. (2015); (6) Blake et al. (1995); (7) van Kempen et al. (2009); (8) Mardones et al. (1997); (9) Gregersen et al. (2000); (10) Hogerheijde et al. (1999); (11) Evans et al. (2005); (12) Onishi et al. (2002); (13) Boogert et al. (2002); (14) Butner et al. (1995).

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