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Table 1

Fluxes and widths of resolved H2 lines in local AGN.

Source z fS1 FWHMS1a fS2 FWHMS2a fS3 FWHMS3a Mwarm T Mcoldb
– – 10-17 W m-2 km s-1 10-17 W m-2 km s-1 10-17 W m-2 km s-1 107 M⊙ K 109 M⊙
3C 236 0.0989 1.06  ±  0.07 582 (750) 0.49  ±  0.08 557 (719) 0.81  ±  0.09 624 (767) 6.10 345  < 5.1
3C 293 0.0450 5.30  ±  0.38 510 (716) 1.79  ±  0.31 553 (732) 2.96  ±  0.38 519 (714) 6.62 323 23
IRAS 09039+0503 0.1254 3.09  ±  0.54 519 (700) 1.34  ±  0.06 575 (730) 2.04  ±  0.13 569 (751) 31.6 334 ...
MCG-2-58-22 0.0472 3.86  ±  0.42 544 (740) 1.50  ±  0.25 636 (796) 3.40  ±  0.46 662 (824) 4.19 359 5.7
Mrk 463E 0.0507 3.37  ±  0.59 556 (748)  <1.98 ... (...) 3.76  ±  0.44 590 (767) 4.06 378 1.2
4C 12.50 (mainc) 0.1217 1.64  ±  0.21 ... (519) 1.20  ±  0.11 ... (552) 1.78  ±  0.46 ... (652) 13.9 374 15
4C 12.50 (wingc) 0.1196d 0.62  ±  0.21 ... (568) 0.44  ±  0.11 521 (690) ... ... (...) 5.19 374e ...

Notes. None of these sources had a reliable S0 detection owing to the high noise levels in the long wavelength array.

(a)

Rest-frame, instrumental-broadening-corrected FWHM. Their measured values appear in parenthesis. Their error bars correspond to 5−10% of their values.

b

Cold H2 gas masses calculated from CO observations (Evans et al. 1999, 2002; Bertram et al. 2007; Saripalli & Mack 2007) using an H2/CO mass conversion factor of 1.5 M⊙/(K km s-1 pc2) for the IR-bright systems Mrk 463E and 4C 12.50 (Evans et al. 2002), and a standard Galactic value of 4.8 M⊙/(K km s-1 pc2) for all other sources. They are converted to the adopted cosmology.

(c)

The main and wing components correspond to the primary and the secondary Gaussian functions in Fig. 2.

(d)

The Gaussians that best fit the S1 and S2 line wings peak at  − 646 km s-1 and  − 634 km s-1 from systemic velocity, respectively.

(e)

The excitation temperature of the rapidly moving H2 gas is assumed to be identical to that of the H2 at systemic velocity to facilitate the comparison of their masses.

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