Kinematics and metallicities of globular clusters in M104

Details Kinematics and metallicities of globular clusters in M104 Kinematics and metallicities of globular clusters in M104

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.284..376b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 284, Issue 2, pp. 376-384.

Astronomy and Astrophysics

Astronomy

33

Galaxies: Haloes, Galaxies: Individual: M104, Galaxies: Kinematics And Dynamics, Galaxies: Spiral, Galaxies: Star Clusters.

Scientific paper

We have obtained spectra for globular cluster candidates in M104 with the Low Dispersion Survey Spectrograph (LDSS-2) on the William Herschel Telescope, confirming 34 objects as M104 globular clusters. We find a cluster velocity dispersion of ~260kms^-1, and the projected mass estimator gives a mass of 5.0 (3.5,6.7)x10^11Msolar for M104 within a projected radius of ~330arcsec (14kpc for D=8.55Mpc). Our best estimate for the mass-to-light ratio is M/L_V_T=16^+5.5_-5.0 within the same radius. Considering all of the possible sources of uncertainty, we find a lower limit of M/L_V=5.3, which is larger than the M/L_V ratio found from rotation curve analyses inside 180arcsec. We thus conclude that the mass-to-light ratio increases with radius, or in other words that M104 possesses a dark matter halo. There is a marginal detection of rotation in the M104 cluster system at the 92.5 per cent confidence level; larger samples will be needed to investigate this possibility. Interestingly, the M104 globular cluster and planetary nebulae (PNe) kinematics are roughly consistent inside ~100arcsec. Finally, we find a mean cluster metallicity of [Fe/H]=-0.70+/-0.3, which is more typical of clusters in giant elliptical (gE)/cD galaxies than it is of clusters in other spirals.

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