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Home All issues Volume 566 (June 2014) A&A, 566 (2014) A147 Full HTML
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Table 1

CO mapping along the major axis of the M 63 disk.

CO(1–0) CO(2–1)
r gal r gal Time rmsa FWHM b F c rmsa FWHM b F c r 2,1 d M H2 e ΣH2 f
(″) (r25) (min) (mK) (kms-1) (K km s-1) (mK) (kms-1) (K km s-1) (106M⊙) (M⊙ pc2)
0 0 31 11 200 49.8 ± 2.2 16 192 39.8 ± 3.1 0.24 321.8 ± 14.2 125.7 ± 5.6
22 0.06 8 18 53 24.5 ± 0.9 28 27 12.6 ± 0.8 0.16 158.3 ± 5.8 61.8 ± 2.3
44 0.12 8 19 41 16.4 ± 0.8 33 21 9.0 ± 0.7 0.17 106.0 ± 5.2 41.4 ± 2.0
66 0.19 8 19 23 9.8 ± 0.4 32 16 4.2 ± 0.5 0.13 63.3 ± 2.6 24.7 ± 1.0
88 0.25 8 18 20 6.3 ± 0.4 32 20 3.4 ± 0.6 0.17 40.7 ± 2.6 15.9 ± 1.0
110 0.31 8 19 26 12.6 ± 0.5 30 21 8.2 ± 0.6 0.20 81.4 ± 3.2 31.8 ± 1.3
132 0.37 8 21 22 5.1 ± 0.5 35 20 2.6 ± 0.7 0.16 33.0 ± 3.2 12.9 ± 1.3
154 0.44 23 13 29 5.3 ± 0.4 22 39 2.5 ± 0.9‡ 0.15 34.3 ± 2.6 13.4 ± 1.0
176 0.50 23 13 19 5.4 ± 0.2 24 27 2.8 ± 0.6 0.16 34.9 ± 1.3 13.6 ± 0.5
198 0.56 23 13 21 1.8 ± 0.3 22 18 0.82 ± 0.40‡ 0.14 11.6 ± 1.9 4.5 ± 0.8
220 0.62 31 11 16 0.98 ± 0.17 11 † 10 <0.33 <0.11 6.3 ± 1.1 2.5 ± 0.4
242 0.68 101 6 11 0.30 ± 0.06 8 6 0.17 ± 0.05 0.17 1.9 ± 0.4 0.76 ± 0.15
264 0.75 101 6 14 0.45 ± 0.08 4 † 10 <0.12 <0.08 2.9 ± 0.5 1.1 ± 0.2
286 0.81 55 10 21 0.88 ± 0.21 9 † 10 <0.27 <0.10 5.7 ± 1.4 2.2 ± 0.5
308 0.87 47 11 14 0.81 ± 0.15 11 † 10 <0.33 <0.13 5.2 ± 1.0 2.0 ± 0.4
330 0.93 63 7 22 0.85 ± 0.15 9 34 0.38 ± 0.31‡ 0.14 5.5 ± 1.0 2.1 ± 0.4
352 0.99 155 5 9 0.23 ± 0.04 6 34 0.29 ± 0.21‡ 0.38 1.5 ± 0.3 0.58 ± 0.10
374 1.06 109 4 † 10 <0.12 4 † 10 <0.12
396 1.12 117 4 † 10 <0.12 3 † 10 <0.09
418 1.18 93 5 † 10 <0.15 5 † 10 <0.15
... ...
473 1.34 381 2 † 10 <0.06 2 † 10 <0.06 <0.39 <0.15

Notes. The radius of the B-band 25 mag arcsec-2 isophote, the so-called isophotal radius, is equal to r25 = 354″ = 17.4 kpc in M 63. It is often used as a reference to express the relative galactocentric radius, rgal. The last separate line of the Table gives the values obtained when summing all scans at the 10 outermost pointings from 1.06 r25 to 1.6 r25 with no CO detection and by smoothing the resulting 3 mm and 1 mm spectra to a resolution of 9.7 km s-1 and 10.4 km s-1, respectively.

(a)

Rms noises at, respectively, 3 mm and 1 mm, measured per channel of 3.2 km s-1 and 1.3 km s-1. The values marked with † correspond to rms noises measured per smoothed channel of 9.7 km s-1 and 10.4 km s-1, respectively.

(b)

Full widths at half maximum of, respectively, CO(1–0) and CO(2–1) lines as determined from fitting Gaussian profiles.

(c)

Integrated CO(1–0) and CO(2–1) line fluxes as determined from fitting Gaussian profiles. The values marked with ‡ correspond to potentially less reliable measurements, because of a CO line detection at 2σ only. Upper limits are 3σ and are calculated assuming a 10 km s-1 line width.

(d)

CO luminosity ratios defined as , needed to correct the lower Rayleigh-Jeans brightness temperature of the 2–1 transition relative to 1–0. We would like, however, to stress that CO(1–0) and CO(2–1) do not exactly map the same regions, because the CO(1–0) beam area equals 4 × the CO(2–1) beam area. The CO luminosity is calculated using the formula (3) from Solomon et al. (1997).

(e)

H2 masses calculated from the CO(1–0) luminosity and by adopting the “standard” Galactic CO-to-H2 conversion factor, XCO = 2 × 1020 cm-2 (K km s-1)-1 (Dickman et al. 1986). The applied formula is: , where a factor of 1.36 is included to account for helium.

(f)

H2 surface densities calculated from the integrated CO(1–0) line flux and by adopting the CO-to-H2 conversion factor given under.

(e)

The applied formula is: ΣH2 (M⊙ pc-2) = 4.4cos(i)FCO(1−0) (K km s-1), where i = 55° is the inclination of M 63 (Leroy et al. 2008).

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