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tokens: other hand, in more extended BCDs the observed CO emission corresponds only to the most luminous regions of the starbursts, so it may be considered as a lower limit to the total CO emission. For all the observed galaxies our CO observations cover at least 50% of the projected size of starburst (, see Sect. 3), while for three objects this fraction, , is 100%. Table 3 Multiwavelength properties of galaxies from the literature. Notes. Columns: (2) radius at the mag arcsec isophote; (3) radius of the star-forming region from 2D surface photometry ( Amorín et al. 2009 ); (4) inclination; (5) H i gas mass; (6) logarithm of H i gas surface density; (7) stellar mass; (8) logarithm of star-formation rate density; (9) gas-phase metallicity; (10) logarithm of H surface density assuming a Galactic CO-to-H conversion factor. Reference. For metallicity: References for : (a) Shi et al. (2006) ; (b) Cairós et al. (2007) ; (c) García-Lorenzo et al. (2008) ; (d) López-Sánchez Esteban (2010) ; (e) Zhao et al. (2010) ; (f) Pérez-Montero Díaz (2003) ; (g) Gil de Paz et al. (2003) . (h) Frayer et al. (1998) ; (i) Leroy et al. (2005) ; (j) Barone et al. (2000) ; (k) Albrecht et al. (2004) ; (l) Leon et al. (1998) ; (m) Verdes-Montenegro et al. (1998) ; (n) Taylor et al. (1998) ; (o) Tacconi Young (1987) ; (p) Wei et al. (2010) . A wobbler switching mode was used at a frequency of 0.5 Hz with a beam throw up to 240 in azimuth. Two independent SIS receivers at each frequency (A100, B100 at 3 mm and A230, B230 at 1.3mm) were used to observe both polarizations of the CO 10 and 21 transitions simultaneously. The receivers were tuned in single side band, using only the lower band (LSB), which improves the calibration procedure and avoids contamination by other spectral lines in the image band, especially in observations of the calibration sources. The SIS receivers were connected to two filter-banks with resolutions of 1 MHz and 4 MHz at 115 GHz and 230 GHz, respectively, which yields velocity resolutions, , of 2.6 km s and 5.2 km s, respectively. These backends have 512 channels each, covering a total instantaneous velocity range of 1300 and 2600 km s. Pointing and focus were checked before each integration on continuum sources and planets. The pointing accuracy was better than 2.5 on average. Calibrations were done using the chopper wheel method, by observing strong radio sources (Orion A, CW Leo, and W51d). System temperatures at both frequencies varied between 290–470 K, the higher values being due to bad weather conditions. Thus, we obtained a range for the antenna temperature sensitivity of –15 mK. The CO spectra was reduced using CLASS 2 ( Buisson et al. 1997 ). To increase the signal-to-noise ratio (S/N), averaged spectra for each pointing were obtained by weighting multiple scans by a factor of , where is the integration time and is the system temperature. In all cases, baselines of zeroth order were subtracted. The spectra was then scaled to a main-beam