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Table 2.

Summary of the molecular lines in our compiled data set towards the centre of NGC 6946.

νrest νobs Eu nH2 (ϵmax) neff Project code Setup
Molecules [GHz] [GHz] [K] [cm−3] [cm−3]
(1) (2) (3) (4) (5) (6) (7) (8) (9)
C2H N = (1 − 0), J = 3/2 − 1/2 87.316 87.302 4.19 Q059+R02C A
HCN (1 − 0) 88.632 88.617 4.25 2 × 105 4.5 × 103 Q059+R02C+P069 A
HCO+ (1 − 0) 89.188 89.173 4.28 4 × 104 5.3 × 102 Q059+R02C A
HNC (1 − 0) 90.664 90.648 4.35 1 × 105 2.3 × 103 Q059+R02C C
3 mm HC3N (10 − 9) 90.979 90.964 16.69 4.3 × 104 R09F C
N2H+ (1 − 0) 93.174 93.158 4.47 5.5 × 103 R09F C
CH3OH JK = 20 − 10 96.741 96.725 6.96 Q059+R02C B
CS (2 − 1) 97.980 97.965 7.10 1.2 × 104 R09F+S08E B
12CO (1 − 0) 115.271 115.252 5.53 1 × 102 M032 D

CH3OH JK = 30 − 20 145.100 145.073 18.80 S02A B
HC3N (16 − 15) 145.561 145.534 41.27 S02A B
2 mm p-H2CO N = (2 − 1), J = 0/2 − 0/1 145.603 145.576 10.48 6.3 × 104 S02A B
CS (3 − 2) 146.969 146.942 14.11 3.3 × 104 S02A B

1.3 mm 12CO (2 − 1) 230.538 230.499 16.59 1 × 103 M032+P069 One mm

Notes. (1) and (2) Molecular lines with their transition ordered by their rest frequencies; Throughout the paper, for simplicity, we refer to the transitions of C2H as (1−0), of CH3 OH as (2−1) and (3−2), and of H2CO as (2−1). (3) and (4) Rest and observational frequencies. (5) Upper energy levels. (6) Minimum density at which the emissivity of the line reaches 95% of its peak value for T = 25 K (see Table 2 within Leroy et al. 2017 and references therein). (7) Taken from Shirley (2015) (Table 1, for 20 K), and have been defined by radiative transfer modelling as the density that results in a molecular line with an integrated intensity of 1 K km s−1. (8) and (9) PdBI project code and setup. A = configuration C and D; B = configuration A, B, C, D; C = configuration B, C, D.

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