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Table A.1.

Fine-structure lines in the mid- to far-IR range.

Line λ ν IP E ncr Spec. res. Ang. res.
(μm) (GHz) (eV) (K) (cm−3) (km s−1) (arcsec)
[Ne VI]2P3/22P1/2 7.65 39188.56 126.21 1888 2.5 × 105 ∼1500 14 × 20
H2 (0,0) S(3) 9.66 31034.41 4.48 2504 9 × 105(a) ∼500 4.7 × 11.3
[S IV]2P3/22P1/2 10.51 28524.50 34.79 1369 5.39 × 104 ∼500 4.7 × 11.3
H2 (0,0) S(2) 12.28 24413.07 4.48 1682 2 × 105(a) ∼500 4.7 × 11.3
[Ne II]2P1/22P3/2 12.81 23403.00 21.56 1123 7.00 × 105 ∼500 4.7 × 11.3
[Ne V]3P23P1 14.32 20935.23 97.12 1892 3 × 104 ∼500 4.7 × 11.3
[Ne III]3P13P2 15.56 19266.87 40.96 925 2.68 × 105 ∼500 4.7 × 11.3
H2 (0,0) S(1) 17.03 17603.78 4.48 1015 2 × 104(a) ∼500 4.7 × 11.3
[S III]3P23P1 18.71 16023.11 23.34 769 2.22 × 104 ∼500 4.7 × 11.3
[Ne V]3P13P0 24.32 12326.99 97.12 596 5.0 × 105 ∼500 11.1 × 22.3
[O IV]2P3/22P1/2 25.89 11579.47 54.94 555 104 ∼500 11.1 × 22.3
[Fe II]a6D7/2–a6D9/2 25.98 11539.35 7.9 553 2.2 × 106 ∼500 11.1 × 22.3
H2 (0,0) S(1) 17.03 17603.78 4.48 1015 2 × 104(a) ∼500 4.7 × 11.3
[S III]3P13P0 33.48 8954.37 23.34 430 7.04 × 103 ∼500 11.1 × 22.3
[Si II]2P3/22P1/2 34.81 8612.25 8.15 413 3.4 × 105(a), 103 ∼500 11.1 × 22.3
[O III]3P23P1 51.81 5787.57 35.12 441 3.6 × 103 ∼105 9.4 (c)
[N III]2P3/22P1/2 57.32 5230.43 29.60 251 3.0 × 103 ∼105 9.4
[O I]3P23P1 63.18 4744.77 228 4.7 × 105(a) ∼86 9.4
[O III]3P13P0 88.36 3393.01 35.12 163 510 ∼124 9.4
[N II]3P23P1 121.90 2459.38 14.53 118 310 ∼290 9.4
[O I]3P13P0 145.52 2060.07 98 9.5 × 104(a) ∼256 10.3
[C II]2P3/22P1/2 157.74 1900.54 11.26 91 20,[2.2 (a), 4.4 (b)] × 103 ∼238 11.2
[N II]3P13P0 205.3 1460.27 14.53 70 48 ∼297 ∼16.8

Notes. The columns correspond to the central wavelength, frequency, ionisation potential, excitation temperature, critical density, spectral and spatial resolution of the data presented in this work, and the number of AGN, starburst, and dwarfs galaxies with line detections above 3 × rms. Critical densities and excitation temperatures from: Launay & Roueff (1977), Tielens & Hollenbach (1985), Greenhouse et al. (1993), Sturm et al. (2002), Cormier et al. (2012), Goldsmith et al. (2012), Farrah et al. (2013).

(a)

Critical density for collisions with hydrogen atoms.

(b)

Critical density for collisions with H2 molecules.

(c)

The beam size for Herschel PACS is dominated by the spaxel size () below ∼120 μm.

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