Astronomy & Astrophysics

All Tables

Table 1: Basic properties of the NUGA sources taken from NED. ^a $i\equiv$ inclination of the galaxy. H = HII-region, S = Seyfert and L = LINER.
Table 2: Radio observations for seven NUGA sources. ^a NGC 4579 was excluded since MERLIN observations were already carried out; the data are taken from the MERLIN archive. ^b NGC 3147 and NGC 4579 were not observed because VLBA data were already available from Ulvestad & Ho (2001). ^c The first observations in 2002 were not successful due to technical problems with some of the antennas and were thus repeated in 2003; the results of both observations are consistent with each other but only the 2003 data sets are used for further discussion due to the higher quality of the data. ^d Eb $\equiv$ Effelsberg, Jb $\equiv$ Jodrell Bank, Wb $\equiv$ Westerbork, Mc $\equiv$ Medicina, Nt $\equiv$ Noto, On85 $\equiv$ Onsala 25m, Sh $\equiv$ Shanghai, Ur $\equiv$ Urumqi, Tr $\equiv$ Torun (see EVN homepage for more information on the respective telescopes: http://www.evlbi.org/).
Table 3: Radio positions of the seven NUGA sources, mainly derived from the EVN 6 cm (core) or MERLIN 18 cm/6 cm (jet) observations by fitting Gaussian profiles to the emission (the positions are coincident within the uncertainties of the different observations). The positional uncertainties are estimated from the Gaussian fits and also include the most recent (i.e., determined in the past 4 years) astromectric errors of the used phase-calibrators.
Table 4: Results of the radio and mm continuum observations with MERLIN, EVN and PdBI. ^a From the MERLIN archive (PI: N.Nagar). ^b Taken from VLBA observation carried out by Ulvestad & Ho (2001; $\equiv$ Ulv01). Please note that the flux errors do not include the calibration uncertainties of 5-10% and represent only the statistical uncertainties of the fit. The given angles are derived from North to East.
Table 5: Spectral indices of the respective sources. $S_\nu \propto \nu ^\alpha$ . ^a taken from Ulvestad & Ho (2001).
Table 6: Brightness temperatures estimated with the formula given in Condon et al. (1982). The frequency ( $\nu$ ), the flux density ( $S_\nu$ ) and the deconvolved size ( $\theta$ ) as an upper limit are taken from Table 4.
Table 7: Black hole masses, bolometric and Eddington luminosities for the seven galaxies.