J/A+AS/115/407 J/A+AS/115/407 Short WSRT HI observations of spiral galaxies M -H Rhee T S Van Albada Astron. Astrophys. Suppl. Ser. 115 407 1996 1996A&AS..115..407R Galaxies, radio galaxies: fundamental parameters galaxies: ISM galaxies: kinematics and dynamics galaxies: spiral galaxies: structure radio lines: galaxies We have obtained short HI observations of 60 late type spiral galaxies with the Westerbork Synthesis Radio Telescope (WSRT). Several HI properties are presented, including the radial surface density distribution of HI and a position-velocity map. When possible these are compared to those measured from single-dish observations. We confirm earlier results that there is no serious systematic difference between the WSRT and single-dish observations in total flux and linewidths.

Name Galaxy name --- RAh Right ascension of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database h RAm Right ascension of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database min RAs Right ascension of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database s DEd Declination of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database deg DEm Declination of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database arcmin DEs Declination of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database arcsec MType Morphological type number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database --- Dist Distance to the galaxy number=2 Calculated from the systemic velocity (column 2 of Table 5), corrected for the Virgo-centric flow and H0=75km/s/Mpc Mpc Inclin Inclination number=3 Calculated from the axial ratio b/a of the disc: cos^2(i)=[(b/a)^2-q_0_^2]/(1-q_0_^2) deg AbB Galactic extinction in the B-band mag AiB Internal extinction in the B-band mag D25 Uncorrected blue major-axis isophotal diameter at the 25 mag/arcsec^2 number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database arcmin Dbi25 Corrected blue major-axis isophotal diameter kpc BTmag Uncorrected total apparent blue magnitude number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database mag MBabs Corrected absolute blue magnitude number=4 MBasb= BTmag - AbB - AiB -5log(Dist) -25 mag Name Galaxy name --- RAh Right ascension of the optical center (1950) h RAm Right ascension of the optical center (1950) min RAs Right ascension of the optical center (1950) s DEd Declination of the optical center (1950) deg DEm Declination of the optical center (1950) arcmin DEs Declination of the optical center (1950) arcsec ObsDay Day of observation d ObsMon Month of observation "month" ObsYear Year of observation yr ObsTime Observation length h BasMin Minimum baseline m BasMax Maximum baseline m Phi Position angle of the resolution axis deg Vobs Radial velocity of the central channel km/s BW Bandwidth of the observation MHz DeltaV Velocity spacing of the channels number=1 The velocity resolution is twice this value km/s Name Galaxy name --- l Integration length perpendicular to the resolution axis arcmin Phi Position angle of the resolution axis deg Theta Half power beam width of the integrated antenna pattern arcsec Noise Noise level in the position-velocity map (mJy/beam) mJy Name Galaxy name --- FHI Total H I flux integral Jy.km/s MHI Total H I mass 10+9solMass DHI H I isophotal diameter at the level of 1 solMass/pc^2 kpc Reff H I effective radius, enclosing 50% of the H I mass kpc mueff H I surface density at the H I effective radius solMass/pc2 Name Galaxy name --- Vsyst1 Systemic velocity determined from global profiles with the method 1 number=1 The HI profile linewidths are defined as the radial velocity differences between the high and low velocity edges, measured at the signal levels equal to 20 and 50% of: Method 1: the peak flux of the profile (e.g. Tully 1988; Bottinelli et al. 1990) Method 2: the peak fluxes in each half of the profile, separately; Method 3: the average of the peak fluxes in the two halves of the profile (e.g. Sullivan et al. 1981; Bothun et al. 1985) Method 4: the mean flux of the profile (e.g. Haynes and Giovanelli 1984; Bicay and Giovanelli 1986) km/s e_Vsyst1 Error on Systemic velocity km/s LW201 H I linewidth determined from method 1 (1), W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW201 Error on W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW501 H I linewidth determined from method 1 (1), W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW501 Error on W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s Vsyst2 Systemic velocity determined from global profiles with the method 2 number=1 The HI profile linewidths are defined as the radial velocity differences between the high and low velocity edges, measured at the signal levels equal to 20 and 50% of: Method 1: the peak flux of the profile (e.g. Tully 1988; Bottinelli et al. 1990) Method 2: the peak fluxes in each half of the profile, separately; Method 3: the average of the peak fluxes in the two halves of the profile (e.g. Sullivan et al. 1981; Bothun et al. 1985) Method 4: the mean flux of the profile (e.g. Haynes and Giovanelli 1984; Bicay and Giovanelli 1986) km/s e_Vsyst2 Error on Systemic velocity km/s LW202 H I linewidth determined from method 2 (1), W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW202 Error on W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW502 H I linewidth determined from method 2 (1), W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW502 Error on W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s Vsyst3 Systemic velocity determined from global profiles with the method 3 number=1 The HI profile linewidths are defined as the radial velocity differences between the high and low velocity edges, measured at the signal levels equal to 20 and 50% of: Method 1: the peak flux of the profile (e.g. Tully 1988; Bottinelli et al. 1990) Method 2: the peak fluxes in each half of the profile, separately; Method 3: the average of the peak fluxes in the two halves of the profile (e.g. Sullivan et al. 1981; Bothun et al. 1985) Method 4: the mean flux of the profile (e.g. Haynes and Giovanelli 1984; Bicay and Giovanelli 1986) km/s e_Vsyst3 Error on Systemic velocity km/s LW203 H I linewidth determined from method 3 (1), W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW203 Error on W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW503 H I linewidth determined from method 3 (1), W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW503 Error on W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s Vsyst4 Systemic velocity determined from global profiles with the method 4 number=1 The HI profile linewidths are defined as the radial velocity differences between the high and low velocity edges, measured at the signal levels equal to 20 and 50% of: Method 1: the peak flux of the profile (e.g. Tully 1988; Bottinelli et al. 1990) Method 2: the peak fluxes in each half of the profile, separately; Method 3: the average of the peak fluxes in the two halves of the profile (e.g. Sullivan et al. 1981; Bothun et al. 1985) Method 4: the mean flux of the profile (e.g. Haynes and Giovanelli 1984; Bicay and Giovanelli 1986) km/s e_Vsyst4 Error on Systemic velocity km/s LW204 H I linewidth determined from method 4 (1), W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW204 Error on W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW504 H I linewidth determined from method 4 (1), W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW504 Error on W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW201c H I linewidth determined from method 1 (1), W20 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW501c H I linewidth determined from method 1 (1), W50 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW202c H I linewidth determined from method 2 (1), W20 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW502c H I linewidth determined from method 2 (1), W50 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW203c H I linewidth determined from method 3 (1), W20 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW503c H I linewidth determined from method 3 (1), W50 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s Name Galaxy name --- Vmax.sini Maximum rotation velocity, uncorrected for inclination km/s e_Vmax.sini Error on maximum rotation velocity, uncorrected for inclination km/s Vmax Maximum rotation velocity, corrected for inclination km/s Simona Mei CDS 1995Sep25 J_A+AS_115_407.xml