Kinematics of Globular Clusters in M49 and M87

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dc.creatorBridges, Terry
dc.date2001-06-08
dc.date.accessioned2026-07-07T01:58:51Z
dc.date.available2026-07-07T01:58:51Z
dc.descriptionWe present recent multi-object spectroscopy of globular clusters in the Virgo gEs M49 and M87. In M49, we have a total of 144 confirmed clusters out to 8 arcmin radius (~6 R_eff or 35 kpc). We find that the blue (metal-poor) clusters have both a higher velocity dispersion and rotation than the red (metal-poor) clusters. For the metal-rich population we place an upper limit of (v/sigma)_proj < 0.34 at 99% confidence. We calculate the velocity dispersion as a function of radius, and show that this is consistent with isotropic cluster orbits and the M49 mass distribution determined from X-ray data. For M87, we combine new CFHT data with previous data to obtain a total sample of 278 clusters out to 10 arcmin radius (~45 kpc). We find a similar global rotation for the metal-poor and metal-rich clusters of 160-170 km/sec. Beyond ~ 2 R_eff (15 kpc), both the metal-poor and metal-rich clusters appear to rotate about the photometric minor axis. The combined cluster sample is consistent with isotropic orbits, but when considered separately, the metal-poor clusters show significant tangential bias of beta_cl ~ -0.4, while the metal-rich clusters show a radial bias with beta_cl ~ +0.4. In both galaxies, the metal-rich and metal-poor clusters share different kinematics, but there is no clear preference for any one formation scenario.
dc.description6 pages, latex, 7 figures. To appear in the proceedings of IAU Symp. 207, "Extragalactic Star Clusters", eds E. Grebel, D. Geisler, D. Minniti. IAU207_pasp.sty included
dc.identifierhttps://arxiv.org/abs/astro-ph/0106148
dc.identifierhttp://arxiv.org/abs/astro-ph/0106148
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/2883
dc.subjectAstrophysics
dc.titleKinematics of Globular Clusters in M49 and M87
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