FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W4289800876> ?p ?o ?g. }

• W4289800876 endingPage "A52" @default.
• W4289800876 startingPage "A52" @default.
• W4289800876 abstract "Globular clusters (GCs) are tracers of the gravitational potential of their host galaxies. Moreover, their kinematic properties may provide clues for understanding the formation of GC systems and their host galaxies. We use the largest set of GC velocities obtained so far of any elliptical galaxy to revise and extend the previous investigations (Richtler et al. 2004) of the dynamics of NGC 1399, the central dominant galaxy of the nearby Fornax cluster of galaxies. The GC velocities are used to study the kinematics, their relation with population properties, and the dark matter halo of NGC 1399. We have obtained 477 new medium-resolution spectra (of these, 292 are spectra from 265 individual GCs, 241 of which are not in the previous data set). with the VLT FORS 2 and Gemini South GMOS multi-object spectrographs. We revise velocities for the old spectra and measure velocities for the new spectra, using the same templates to obtain an homogeneously treated data set. Our entire sample now comprises velocities for almost 700 GCs with projected galactocentric radii between 6 and 100 kpc. In addition, we use velocities of GCs at larger distances published elsewhere. Combining the kinematic data with wide-field photometric Washington data, we study the kinematics of the metal-poor and metal-rich subpopulations. We discuss in detail the velocity dispersions of subsamples and perform spherical Jeans modelling. The most important results are: the red GCs resemble the stellar field population of NGC 1399 in the region of overlap. The blue GCs behave kinematically more erratic. Both subpopulations are kinematically distinct and do not show a smooth transition. It is not possible to find a common dark halo which reproduces simultaneously the properties of both red and blue GCs. Some velocities of blue GCs are only to be explained by orbits with very large apogalactic distances, thus indicating a contamination with GCs which belong to the entire Fornax cluster rather than to NGC 1399. Also, stripped GCs from nearby elliptical galaxies, particularly NGC 1404, may contaminate the blue sample. We argue in favour of a scenario in which the majority of the blue cluster population has been accreted during the assembly of the Fornax cluster. The red cluster population shares the dynamical history of the galaxy itself. Therefore we recommend to use a dark halo based on the red GCs alone. The dark halo which fits best is marginally less massive than the halo quoted previously. The comparison with X-ray analyses is satisfactory in the inner regions, but without showing evidence for a transition from a galaxy to a cluster halo, as suggested by X-ray work." @default.
• W4289800876 created "2022-08-05" @default.
• W4289800876 creator A5009613358 @default.
• W4289800876 creator A5022741391 @default.
• W4289800876 creator A5024925390 @default.
• W4289800876 creator A5043620022 @default.
• W4289800876 creator A5053053215 @default.
• W4289800876 creator A5054162614 @default.
• W4289800876 creator A5078342408 @default.
• W4289800876 date "2010-04-01" @default.
• W4289800876 modified "2023-10-14" @default.
• W4289800876 title "The globular cluster system of NGC 1399" @default.
• W4289800876 cites W1511199250 @default.
• W4289800876 cites W1513618424 @default.
• W4289800876 cites W1543298386 @default.
• W4289800876 cites W1627431398 @default.
• W4289800876 cites W1671791007 @default.
• W4289800876 cites W1877953985 @default.
• W4289800876 cites W1965396900 @default.
• W4289800876 cites W1965941590 @default.
• W4289800876 cites W1973331810 @default.
• W4289800876 cites W1974866549 @default.
• W4289800876 cites W1978075820 @default.
• W4289800876 cites W1979494770 @default.
• W4289800876 cites W1980350013 @default.
• W4289800876 cites W1980790187 @default.
• W4289800876 cites W1981506893 @default.
• W4289800876 cites W1984462263 @default.
• W4289800876 cites W1988145451 @default.
• W4289800876 cites W1988935076 @default.
• W4289800876 cites W1990934390 @default.
• W4289800876 cites W1992885010 @default.
• W4289800876 cites W1993244035 @default.
• W4289800876 cites W1993839984 @default.
• W4289800876 cites W1995033962 @default.
• W4289800876 cites W1997001715 @default.
• W4289800876 cites W1999188890 @default.
• W4289800876 cites W2000790004 @default.
• W4289800876 cites W2004536451 @default.
• W4289800876 cites W2005434195 @default.
• W4289800876 cites W2010758978 @default.
• W4289800876 cites W2013101677 @default.
• W4289800876 cites W2017612006 @default.
• W4289800876 cites W2018185424 @default.
• W4289800876 cites W2019028512 @default.
• W4289800876 cites W2023344562 @default.
• W4289800876 cites W2026204466 @default.
• W4289800876 cites W2029540172 @default.
• W4289800876 cites W2031203298 @default.
• W4289800876 cites W2037400398 @default.
• W4289800876 cites W2044896216 @default.
• W4289800876 cites W2046839445 @default.
• W4289800876 cites W2047172810 @default.
• W4289800876 cites W2059468604 @default.
• W4289800876 cites W2061968438 @default.
• W4289800876 cites W2062166184 @default.
• W4289800876 cites W2065595147 @default.
• W4289800876 cites W2067239832 @default.
• W4289800876 cites W2069353545 @default.
• W4289800876 cites W2074255988 @default.
• W4289800876 cites W2084691636 @default.
• W4289800876 cites W2087142598 @default.
• W4289800876 cites W2088089730 @default.
• W4289800876 cites W2088694231 @default.
• W4289800876 cites W2092756578 @default.
• W4289800876 cites W2102825905 @default.
• W4289800876 cites W2111682619 @default.
• W4289800876 cites W2114813636 @default.
• W4289800876 cites W2122948592 @default.
• W4289800876 cites W2131785502 @default.
• W4289800876 cites W2134127792 @default.
• W4289800876 cites W2141453531 @default.
• W4289800876 cites W2148672165 @default.
• W4289800876 cites W2158093180 @default.
• W4289800876 cites W2161997838 @default.
• W4289800876 cites W2599734048 @default.
• W4289800876 cites W2601053151 @default.
• W4289800876 cites W3098109397 @default.
• W4289800876 cites W3098332098 @default.
• W4289800876 cites W3099368291 @default.
• W4289800876 cites W3099441451 @default.
• W4289800876 cites W3099826761 @default.
• W4289800876 cites W3099860733 @default.
• W4289800876 cites W3099884128 @default.
• W4289800876 cites W3100110286 @default.
• W4289800876 cites W3100205966 @default.
• W4289800876 cites W3100370271 @default.
• W4289800876 cites W3100403128 @default.
• W4289800876 cites W3101795484 @default.
• W4289800876 cites W3103036378 @default.
• W4289800876 cites W3103306379 @default.
• W4289800876 cites W3103318976 @default.
• W4289800876 cites W3103368470 @default.
• W4289800876 cites W3103438512 @default.
• W4289800876 cites W3103816948 @default.
• W4289800876 cites W3104103327 @default.
• W4289800876 cites W3105443329 @default.
• W4289800876 cites W3105503988 @default.

• next