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Table 3.

Observed and derived parameters of the CO lines.

Galaxy d I 12 CO 10 $ \rm~I_\mathrm{^{12}CO_{\mathrm{10}}} $ v12CO10 I 13 CO 10 $ \rm~I_\mathrm{^{13}CO_{\mathrm{10}}} $ v13CO10 I 12 CO 21 $ \rm~I_\mathrm{^{12}CO_{\mathrm{21}}} $ v12CO21 12 CO 10 13 CO 10 $ \frac{^{12}\mathrm{CO}_{\mathrm{10}}}{^{13}\mathrm{CO}_{\mathrm{10}}} $ 12 CO 21 12 CO 10 $ \frac{^{12}\mathrm{CO}_{\mathrm{21}}}{^{12}\mathrm{CO}_{\mathrm{10}}} $ τ(13CO) TK
(kpc) (K km s−1) (km s−1) (K km s−1) (km s−1) (K km s−1 ) (km s−1) (K)
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12)
N2613-1 −7.5 14.3 ± 0.6 291 . 5 2.4 + 2.6 $ -291.5^{+2.6}_{-2.4} $ 2.5 ± 0.3 −294.8 ± 4.6 10.7 ± 0.5 302 . 6 3.0 + 3.9 $ -302.6^{+3.9}_{-3.0} $ 5 . 2 0.5 + 0.3 $ 5.2^{+0.3}_{-0.5} $ 0.28 ± 0.01 0 . 21 0.06 + 0.02 $ 0.21^{+0.02}_{-0.06} $ 19 . 4 2.3 + 1.4 $ 19.4^{+1.4}_{-2.3} $
N2613-2 −2.5 11.9 ± 0.8 −150.6 ± 4.5 < 0.8 −173.4 ± 8.6 4.0 ± 0.6 193 . 4 6.4 + 7.6 $ -193.4^{+7.6}_{-6.4} $ 0 . 15 0.03 + 0.01 $ 0.15^{+0.01}_{-0.03} $
N2613-3 0.0 9.9 ± 0.6 −32.0 ± 3.7 < 0.6 −68.6 ± 5.0 5.9 ± 0.5 −73.9 ± 8.2 0 . 24 0.02 + 0.01 $ 0.24^{+0.01}_{-0.02} $

Notes. Listed items (The full table is available at the CDS): (1) Galaxy labels for different observational regions, as shown in Fig. 3. The bold name indicates companion galaxies or locations off the main disc, as listed in Table 2. (2) d denotes the projected distance to the galaxy’s minor axis. (3), (5), (7) The integrated line intensities for the 12CO J = 1 − 0, 13CO J = 1 − 0, and 12CO J = 2 − 1 lines, corrected for main beam and forward efficiencies. If the lines were not firmly detected, we list the 3σ upper limit and use ‘–’ in the velocity column and other parameter calculations. (4), (6), (8) The centroid velocities were derived from the intensity-weighted average velocity of the Gaussian components. (9), (10) The intensity line ratios of 12CO J = 1 − 0 to 13CO J = 1 − 0, and 12CO J = 2 − 1 to 12CO J = 1 − 0 were corrected for beam dilution as discussed in Sect. 2.2. (11), (12) τ(13CO) and TK represent the optical depth and kinetic temperature, respectively, under LTE. The uncertainties only account for the statistical errors from the measurements.

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