1997A&A...319..747A


Query : 1997A&A...319..747A

1997A&A...319..747A - Astronomy and Astrophysics, volume 319, 747-756 (1997/3-3)

Structural classification of galaxies in clusters.

ANDREON S. and DAVOUST E.

Abstract (from CDS):

The traditional method of morphological classification, by visual inspection of images of uniform quality and by reference to standards for each type, is critically examined. The rate of agreement among traditional morphologists on the morphological type of galaxies is estimated from published classification works, and is estimated at about 20%, when galaxies are classified into three bins (E, S0, S+Irr). The advantages of the quantitative method of structural classification for classifying galaxies in clusters are outlined. This method is based on the isophotal analysis of galaxy images, and on the examination of quantitative structural parameters derived from this analysis, such as the profiles of luminosity, ellipticity and deviations from ellipticity of the galaxy. The structural and traditional methods are compared on a complete sample of 190 galaxies in the Coma cluster. The morphological types derived by both methods agree to within 15 or 20%, the same rate as among traditional morphologists alone, thus showing that our morphological classes do coincide with the traditional ones. The galaxies with discrepant types are mostly faint (magB>16.0), or have features typical of spirals, but which have not been detected, noticed or taken into account by traditional morphologists. The rate of agreement is also good for galaxies in a distant cluster (z∼0.4). The structural method, which requires an image quality adapted to the difficulty of classifying a given galaxy, gives highly reproducible results, never reached by traditional estimations of the morphological type. Thus, the morphological types obtained with this method should be preferred, even if their determination is more time and telescope consuming, because they are less subjective, therefore more reproducible, and based on images of adequate resolution. The advantages of the method are further demonstrated by new results on the properties of galaxies in clusters.

Abstract Copyright:

Journal keyword(s): galaxies: fundamental parameters - elliptical and lenticular, cD - spiral - clusters: individual: Coma cluster

Simbad objects: 23

goto View the references in ADS

Number of rows : 23
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 ACO 370 ClG 02 39 50.5 -01 35 08           ~ 684 0
2 ACO 851 ClG 09 42 56.6 +46 59 22           ~ 313 0
3 NGC 3115 GiG 10 05 13.9270507008 -07 43 06.982712292   11   9.37   ~ 968 2
4 M 105 LIN 10 47 49.600 +12 34 53.87   10.56 9.76 9.12 8.18 ~ 1417 0
5 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4502 2
6 LEDA 126738 GiC 13 01 39.088 +28 14 45.16           ~ 8 0
7 GMP 1925 GiC 13 01 40.97 +28 14 56.6           ~ 4 0
8 GMP 1878 GiC 13 01 45.0 +28 18 00           ~ 2 0
9 GMP 1844 G 13 01 47.2 +27 46 16           ~ 2 0
10 GMP 1834 G 13 01 47.9 +27 30 18           ~ 2 0
11 LEDA 1815605 GiC 13 02 04.3413142968 +27 41 58.370141040           ~ 7 0
12 GMP 1373 G 13 02 37.8 +27 59 55           ~ 2 0
13 GMP 1300 G 13 02 46.6 +28 19 44           ~ 2 0
14 2MASX J13025690+2643233 G 13 02 56.9171849016 +26 43 23.535317280           ~ 2 0
15 2MASX J13025942+2816313 GiC 13 02 59.4401155344 +28 16 31.216793016           ~ 7 0
16 GMP 1154 G 13 03 01.1 +26 39 46           ~ 2 0
17 GMP 1035 G 13 03 16.7 +27 57 42           ~ 2 0
18 GMP 999 GiC 13 03 23.050 +29 06 44.10           ~ 8 0
19 2MASX J13032999+2733044 G 13 03 30.0079823544 +27 33 04.303117440           ~ 2 0
20 GMP 694 G 13 03 56.6 +28 05 59           ~ 2 0
21 NGC 4941 Sy2 13 04 13.1036380320 -05 33 05.752803672   13.18 12.23 10.74   ~ 332 0
22 GMP 565 G 13 04 13.8 +27 13 04           ~ 2 0
23 5C 4.161 GiC 13 04 18.4208038560 +28 28 05.287857708   15.46       ~ 17 0

To bookmark this query, right click on this link: simbad:objects in 1997A&A...319..747A and select 'bookmark this link' or equivalent in the popup menu


2022.05.29-08:04:09

© Université de Strasbourg/CNRS

    • Contact