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Query : 2015ApJ...807...56B |
2015ApJ...807...56B - Astrophys. J., 807, 56 (2015/July-1)
Structure and formation of cD galaxies: NGC 6166 in Abell 2199.
BENDER R., KORMENDY J., CORNELL M.E. and FISHER D.B.
Abstract (from CDS):
However, our photometry does not confirm the widespread view that cD halos are identifiable as an extra, low-surface-brightness component that is photometrically distinct from the inner, steep-Sérsic-function main body of an otherwise-normal giant elliptical galaxy. Instead, all of the brightness profile of NGC 6166 outside its core is described to ±0.037 V mag/arcsec2 by a single Sérsic function with index. The cD halo is not recognizable from photometry alone. This blurs the distinction between cluster-dominated cD halos and the similarly-large-Sérsic-index halos of giant, core-boxy-nonrotating ellipticals. These halos are believed to be accreted onto compact, high-redshift progenitors (''red nuggets'') by large numbers of minor mergers. They belong dynamically to their central galaxies. Still, cDs and core-boxy-nonrotating Es may be more similar than we think: both may have outer halos made largely via minor mergers and the accumulation of tidal debris.
We construct a main-body+cD-halo decomposition that fits both the brightness and dispersion profiles. To fit, we need to force the component Sérsic indices to be smaller than a minimum- photometric decomposition would suggest. The main body has of the total galaxy light. The cD halo has, ∼1/2 mag brighter than the brightest galaxy in the Virgo cluster. A mass model based on published cluster dynamics and X-ray observations fits our observations if the tangential dispersion is larger than the radial dispersion at -. The cD halo is as enhanced in α element abundances as the main body of NGC 6166. Quenching of star formation in ≲1 Gyr suggests that the center of Abell 2199 has been special for a long time during which dynamical evolution has liberated a large mass of now-intracluster stars.
Abstract Copyright: ∼
Journal keyword(s): galaxies: elliptical and lenticular, cD - galaxies: evolution - galaxies: formation - galaxies: kinematics and dynamics - galaxies: photometry - galaxies: structure
Simbad objects: 19
Number of rows : 19 |
N | Identifier | Otype |
ICRS (J2000) RA |
ICRS (J2000) DEC |
Mag U | Mag B | Mag V | Mag R | Mag I | Sp type |
#ref
1850 - 2024 |
#notes |
---|---|---|---|---|---|---|---|---|---|---|---|---|
1 | M 32 | GiG | 00 42 41.82480 | +40 51 54.6120 | 9.51 | 9.03 | 8.08 | ~ | 2157 | 2 | ||
2 | NGC 1399 | BiC | 03 38 29.083 | -35 27 02.67 | 11.05 | 9.74 | 9.59 | 8.12 | ~ | 1572 | 1 | |
3 | * 62 Aur | PM* | 06 59 02.8473250152 | +38 03 08.346327696 | 7.245 | 6.021 | K2III | 84 | 0 | |||
4 | HD 74377 | PM* | 08 45 10.3964048108 | +41 40 18.605049150 | 9.48 | 8.55 | 8.0 | K3V | 96 | 0 | ||
5 | NGC 3311 | EmG | 10 36 42.821 | -27 31 42.02 | 11.93 | 10.93 | 10.00 | 9.67 | ~ | 300 | 2 | |
6 | NAME Virgo Cluster | ClG | 12 26 32.1 | +12 43 24 | ~ | 6669 | 0 | |||||
7 | M 49 | Sy2 | 12 29 46.8 | +08 00 01 | 13.21 | 12.17 | ~ | 2098 | 2 | |||
8 | M 87 | AGN | 12 30 49.42338414 | +12 23 28.0436859 | 10.16 | 9.59 | 8.63 | 7.49 | ~ | 7231 | 3 | |
9 | NAME NGC 4839 Group | GrG | 12 57 21.5 | +27 31 54 | ~ | 80 | 0 | |||||
10 | NGC 4839 | rG | 12 57 24.3563164776 | +27 29 52.203087132 | 13.56 | 13.02 | 12.06 | ~ | 468 | 3 | ||
11 | NGC 4874 | LIN | 12 59 35.7093764280 | +27 57 33.293892204 | 13.01 | 13.7 | 11.40 | 12.122 | 11.386 | ~ | 785 | 3 |
12 | ACO 1656 | ClG | 12 59 44.40 | +27 54 44.9 | ~ | 4819 | 2 | |||||
13 | NGC 4889 | EmG | 13 00 08.097 | +27 58 37.29 | 12.93 | 13.0 | 11.30 | 11.652 | 10.906 | ~ | 708 | 1 |
14 | IC 1101 | rG | 15 10 56.100 | +05 44 41.19 | 15.10 | ~ | 155 | 2 | ||||
15 | ACO 2029 | ClG | 15 10 56.2 | +05 44 42 | ~ | 944 | 0 | |||||
16 | MCG+07-34-050 | GiC | 16 28 31.0733294184 | +39 31 16.009809528 | 16 | ~ | 41 | 1 | ||||
17 | NGC 6166 | Sy2 | 16 28 38.24470063 | +39 33 04.2335319 | 12.78 | 11.78 | ~ | 764 | 5 | |||
18 | ACO 2199 | ClG | 16 28 43.31 | +39 34 07.6 | ~ | 1172 | 1 | |||||
19 | NAME Local Group | GrG | ~ | ~ | ~ | 8435 | 0 |
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