Kinematics of gas and stars in the circumnuclear star-forming ring of NGC3351

HÄGELE, GUILLERMO F.; DÍAZ, ÁNGELES I.; CARDACI, MÓNICA V.; TERLEVICH, ELENA; TERLEVICH, ROBERTO

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

WILEY-BLACKWELL PUBLISHING, INC

Año: 2007 vol. 378 p. 163 - 178

0035-8711

We have measured gas and stellar velocity dispersions in five circumnuclear star-forming regions (CNSFRs) and the nucleus of the barred spiral galaxy NGC3351. The stellar dispersions have been obtained from high-resolution spectra of the Ca II triplet (CaT) lines at lambdalambda 8494, 8542, 8662 Å, while the gas velocity dispersions have been measured by Gaussian fits to the Heta lambda 4861Å line on high-dispersion spectra. The CNSFRs, with sizes of about 100 to 150 pc in diameter, are seen to be composed of several individual star clusters with sizes between 1.7 and 4.9 pc on a Hubble Space Telescope (HST) image. Using the stellar velocity dispersions, we have derived dynamical masses for the entire star-forming complexes and for the individual star clusters. Values of the stellar velocity dispersions are between 39 and 67 km/s. Dynamical masses for the whole CNSFRs are between 4.9×10^6 and 4.3×10^7 Msun and between 1.8 and 8.7×10^6 Msun for the individual star clusters. Stellar and gas velocity dispersions are found to differ by about 20 km/s with the Heta lines being narrower than both the stellar lines and the [O III] lambda 5007 Å lines. We have found indications for the presence of two different kinematical components in the ionized gas of the regions. The radial velocity curve shows deviation from circular motions for the ionized hydrogen consistent with its infall towards the central regions of the galaxy at a velocity of about 25 km/s. To disentangle the origin of these two components it will be necessary to map these regions with high spectral and spatial resolution and much better signal-to-noise ratio in particular for the O2+ lines.