Table 3
[C I] and CO line fluxes from Herschel archive galaxies.
Name | Observed line flux | Herschel | Ref.a | ||||||
CO (4−3) | CO (7−6) | [C I] (1−0) | [C I] (2−1) | CO (2−1) | 13CO (2−1) | obsid | |||
461 GHz | 807 GHz | 492 GHz | 809 GHz | 230 GHz | 220 GHz | ||||
(10-17 W m-2) | (10-19 W m-2) | ||||||||
|
|||||||||
NGC 1275/Per A | 0.86 | 0.56 | 0.48 | 1.05 | 13 | 2.0 | 1342249055 | BI98 | |
NGC 1482 | 0.52 | 0.19 | 0.32 | 0.61 | 61 | − | 1342248233 | A07 | |
NGC 2798 | 1.48 | 2.65 | 0.67 | 2.11 | − | − | 1342252892 | ||
NGC 3521 | 0.49 | 0.09 | 0.59 | 0.50 | − | − | 1342247743 | ||
NGC 3627/M66 | 0.80 | 0.26 | 0.68 | 0.61 | 92 | 7.3 | 1342247604 | I | |
NGC 4254/M99 | 0.82 | 0.18 | 1.14 | 1.20 | 58 | 5.4 | 1342236997 | I | |
NGC 4321/M100 | 0.60 | 0.18 | 0.38 | 0.47 | 100 | 7.8 | 1342247572 | I | |
NGC 4536 | 1.71 | 1.99 | 0.23 | 2.27 | 90 | 7.4 | 1342237025 | I | |
NGC 4631 | 1.65 | 0.57 | 0.83 | 1.60 | 119 | 5.5 | 1342247553 | I09a, * | |
NGC 4736/M94 | 0.68 | 0.26 | 0.51 | 0.86 | 69 | 5.9 | 1342245851 | GP00, Ba06 | |
NGC 4826/M64 | 0.75 | 0.34 | 0.82 | 1.04 | 301 | 40 | 1342246992 | IB02, I09a, * | |
NGC 4945 | 34.9 | 90.8 | 21.5 | 91.7 | 1570 | 131 | 1342212343 | W04 | |
NGC 5055/M63 | 1.08 | 0.31 | 0.95 | 1.60 | 78 | 13 | 1342237026 | I | |
NGC 5194/M51 | 1.67 | 0.62 | 1.21 | 2.36 | 205 | 28 | 1342201202 | IB02, ITB, * | |
NGC 5713 | 0.57 | 0.23 | 0.26 | 0.42 | 49 | 5.6 | 1342248250 | I | |
Circinus | 41.3 | 36.2 | 17.1 | 41.8 | 592 | 56 | 1342251313 | H08 | |
NGC 6946 | 5.07 | 5.74 | 2.20 | 5.36 | 789 | 79 | 1342243603 | IB01, IB02, * | |
NGC 7331 | 1.03 | 0.16 | 0.56 | 0.95 | 20 | 3.4 | 1342245871 | IB99, * |
Notes.
References to ground-based J = 2−112CO and 13CO observations: A07 = Albrecht et al. (2007); Ba06 = Bayet et al. (2006); BI98 = Bridges & Irwin (1998); GP00 = Gerin & Phillips (2000); H08 = Hitschfeld et al. (2008); I09a = Israel (2009a); I = Israel (JCMT, this paper); IB01 = Israel & Baas (2001); IB02 = Israel & Baas (2002); ITB = Israel et al. (2006); W04 = Wang et al. (2004). For galaxies marked by an asterisk (*) we have determined J = 2−112CO and 13CO fluxes corresponding to the SPIRE aperture by integration over the (JCMT) map.
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