All Tables

Table 1: This table presents the sample of cooling flow clusters of galaxies observed with the IRAM 30 m telescope. Central frequencies of the CO(1-0) and CO(2-1) lines observed, as the exposure time are indicated for each galaxy. Sources observed in the second run (August) are with indicated by a star. The others were observed during the first run (July). Several sources were not observed in CO(2-1) since the redshifted J=2-1 transition lines were out of the 30 m telescope receiver's band.
Table 2: Summary of observational data for the two runs. Lines characteristics are presented, spectra are shown in Fig. 8. $I_{\rm CO}$ (Col. 8) were evaluated from a Gaussian fit of the CO(1-0) and CO(2-1) lines for detections and hints of detections. $I_{\rm CO}$ upper limits were evaluated by equation 2 for non-detections. A detection is asserted in one transition line when the peak of the Gaussian fit is above three times the rms (in 55 km s^-1 channels) and a hint of detection when it is between two and three times the rms. To claim a cold molecular gas detection, we require a detection in both transition lines. A possible detection was claimed when was present a detection in one transition line or a hint of detection in both lines, unless the line appear clearly in one transition only (Abell 262, Abell 1068, Zw8193).
Table 3: Summary of observational data for the two runs. Lines characteristics (Table 2 continuation).
Table 4: Derived parameters of the observed sources. Optical line luminosities are from Crawford et al. (1999). Mass deposition rates and cooling radius are from (1) Peres et al. (1998) and (2) White et al. (1997). Dust masses are evaluated from 60 $\mu$ m data compiled in Edge (2001), assuming $T_{\rm dust}=35$ K.