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VII/96 Catalog of morphological properties of Abell clusters (Struble+, 1987)
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A catalog of morphological properties of the 2712 Abell clusters
Struble M.F., Rood H.J.
<Astrophys. J. Suppl. Ser., 63, 555 (1987)>
=1987ApJS...63..555S
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ADC_Keywords: Clusters, galaxy ; Morphology
Keywords: galaxies: clusters: general - galaxies: distances and redshifts -
galaxies: structure
Description:
A catalog is presented which contains Rood-Sastry (1971, hereafter RS)
morphological types for all 2712 Abell clusters.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1 132 2712 Catalog of morphological properties of
Abell clusters
table2 114 372 Additional data for resolved F clusters
table3 122 142 Additional data for Abell clusters with
non-cluster population
notes 80 3209 Comments of table1
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Byte-by-byte Description of file: table1
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Bytes Format Units Label Explanations
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1- 4 I4 --- Abell Abell cluster identification
5 A1 --- n_Abell [*] An '*' indicates that the cluster is not
in Abell's (1980) statistical sample
7 I1 --- Dist Distance class as given by Abell (1980)
9- 11 I3 --- nGal Abell's (1980) number count of galaxies
13- 14 I2 mm Radius Radius of the circular observation window
which our data were obtained (1mm=67.14")
16- 18 A3 --- RS1 Basic RS type (1)
20- 21 A2 --- RS2 Subsidiary property of RS type (2)
23- 24 I2 --- RS3 []? Number of bright galaxies used to determine
RS type for both the C and L types
26- 31 A6 --- T1 First brightest cluster galaxy Hubble type
33- 36 F4.2 mm Sep1a []? Separation, see note (3)
38- 41 F4.2 mm Sep1b []? Separation, see note (3)
43- 48 A6 --- T2 Second brightest cluster galaxy Hubble type
50- 53 F4.2 mm Sep2a []? Separation, see note (3)
55- 58 F4.2 mm Sep2b []? Separation, see note (3)
60- 65 A6 --- T3 Third brightest cluster galaxy Hubble type
67- 70 F4.2 mm Sep3a []? Separation, see note (3)
72- 75 F4.2 mm Sep3b []? Separation, see note (3)
77- 81 F5.2 mm r12 Separation between the first and second most
luminous cluster galaxies (1mm=67.14")
83- 87 F5.2 mm r13 Separation between the first and third most
luminous cluster galaxies (1mm=67.14")
89- 93 F5.2 mm r23 Separation between the second and third most
luminous cluster galaxies (1mm=67.14")
95- 96 I2 --- Nb []? Number of apparent galaxies that are not
among the three most luminous cluster galaxies
98 I1 --- Nt []? Number of apparent triple galaxies not
among the three most luminous cluster galaxies
99 A1 --- n_Nt [n] A 'n' indicates that a galaxy with a
multiple nucleus is observed in the cluster
100-101 A2 --- FRS1a Basic RS type for the first subcluster in an
F cluster (1)
103-104 A2 --- FRS1b Subsidiary property of RS type of FRS1 (2)
106-107 I2 --- FRS1c []? Number of bright galaxies used to determine
FRS1 RS type for both the C and L types
109-110 A2 --- FRS2a Basic RS type for the second subcluster in an
F cluster (1)
112-113 A2 --- FRS2b Subsidiary property of RS type of FRS2 (2)
115-116 I2 --- FRS2c []? Number of bright galaxies used to determine
FRS2 RS type for both the C and L types
118-119 A2 --- FRS3a Basic RS type for the third subcluster in an
F cluster (1)
121-122 A2 --- F3RS3b Subsidiary property of RS type of FRS3 (2)
124-125 I2 --- F3RS3c []? Number of bright galaxies used to determine
FRS3 RS type for both the C and L types
127-131 A5 --- Other Other source data (4)
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Note (1): Basic RS type: cD, B, L, C, F or I
Note (2): Appendage or subscript which indicates a subsidiary property :
p=peculiar cD galaxy
n=multiple nucleus cD galaxy
s=satellite of a cD galaxy
b=connected supergiant binary galaxy within a B-type cluster
p=peculiarity associated with a supergiant binary galaxy or the
B cluster itself
a=arc shape of the line of galaxies defining an L-type cluster
c=clumpy
s=smooth I-type cluster
Note (3): The number following a 'b' or 's' designation is the measured
separation (1mm=67.14") between the components of a binary galaxy
or between a cD_s_ galaxy ant its nearby satellite, respectively
Note (4): c: presence of a comment concerning the cluster in "notes" file
r: continuum radio emission in a passband centered at a frequency of
1400MHz was detected in the survey by Owen et al. (1982)
u: the cluster was observed but not detected at the sensitivity limit
of 0.10Jy in the 1400MHz radio survey by Owen et al. (1982)
v: the cluster is listed in the catalog of
Leir and van den Bergh (1977)
x: X-ray emission was detected in the HEAO 1 2-6 keV passband survey
of Abell clusters by Johnson et al. (1983)
z: the redshift of the cluster is contained in the catalog compiled
by Struble and Rood (1986a)
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Byte-by-byte Description of file: table2
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Bytes Format Units Label Explanations
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1- 4 I4 --- Abell Abell cluster identification
5 A1 --- u_Abell [:] Uncertainty flag on F type of the cluster
(RS1 in table1)
7 A1 --- m_Abell [EWNSM] Component of the cluster (1)
10- 11 A2 --- RS Basic revised RS type
13- 18 A6 --- T1 First brightest cluster galaxy Hubble type
20- 23 F4.2 mm SepT1a []? Separation, see note (2)
25- 28 F4.2 mm SepT1b []? Separation, see note (2)
30- 35 A6 --- T2 Second brightest cluster galaxy Hubble type
37- 40 F4.2 mm SepT2a []? Separation, see note (2)
42- 45 F4.2 mm SepT2b []? Separation, see note (2)
47- 52 A6 --- T3 Third brightest cluster galaxy Hubble type
54- 57 F4.2 mm SepT3a []? Separation, see note (2)
59- 62 F4.2 mm SepT3b []? Separation, see note (2)
64- 68 F5.2 mm r12 Separation between the first and second most
luminous cluster galaxies (1mm=67.14")
70- 74 F5.2 mm r13 Separation between the first and third most
luminous cluster galaxies (1mm=67.14")
76- 80 F5.2 mm r23 Separation between the second and third most
luminous cluster galaxies (1mm=67.14")
82- 83 I2 --- Nb []? Number of apparent galaxies that are not
among the three most luminous cluster galaxies
85 I1 --- Nt []? Number of apparent triple galaxies not
among the three most luminous cluster galaxies
87- 88 A2 --- RS1 Basic RS type for the first subcluster
90- 91 A2 --- RS2 Subsidiary property of RS type (3)
93- 94 I2 --- RS3 []? Number of bright galaxies used to determine
FRS1 RS type for both the C and L types
97-100 F4.1 mm Sep []? Separation of the components (1mm=67.14")
102-103 A2 --- m_Sep [SENWM] Component designation
105-107 I3 deg PA []? Position angle of the separation vector of
the components
109 A1 --- n_PA [SENWM] Component designation
114 A1 --- Com Comments (4)
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Note (1): M for middle
Note (2): The number following a 'b' or 's' designation is the measured
separation (1mm=67.14") between the components of a binary galaxy
or between a cD_s_ galaxy ant its nearby satellite, respectively
Note (3): Appendage or subscript which indicates a subsidiary property :
p=peculiar cD galaxy
n=multiple nucleus cD galaxy
s=satellite of a cD galaxy
b=connected supergiant binary galaxy within a B-type cluster
p=peculiarity associated with a supergiant binary galaxy or the
B cluster itself
a=arc shape of the line of galaxies defining an L-type cluster
c=clumpy
s=smooth I-type cluster
Note (4): c: presence of a comment concerning the cluster in "notes" file
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Byte-by-byte Description of file: table3
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Bytes Format Units Label Explanations
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1- 4 I4 --- Abell Abell number
5 A1 --- u_Abell Uncertainty flag on the type of the cluster
7 A1 --- n_Abell [CX] C: confused,
X: probable cluster in the foreground
of an Abell cluster
9- 10 A2 --- RS1 Basic RS type (1)
13 A1 --- RS2 Subsidiary property of RS type (2)
16 I1 --- RS3 []? Number of bright galaxies used to determine
RS type for both the C and L types
18- 23 A6 --- T1 First brightest cluster galaxy Hubble type
25- 28 F4.2 --- SepT1a []? Separation, see note (3)
35- 40 A6 --- T2 Second brightest cluster galaxy Hubble type
42- 45 F4.2 --- SepT2a []? Separation, see note (3)
52- 57 A6 --- T3 Third brightest cluster galaxy Hubble type
59- 62 F4.2 --- SepT3a []? Separation, see note (3)
64- 67 F4.2 --- SepT3b []? Separation, see note (3)
69- 73 F5.2 --- r12 Separation between the first and second most
luminous cluster galaxies (1mm=67.14")
75- 79 F5.2 --- r13 Separation between the first and third most
luminous cluster galaxies (1mm=67.14")
81- 85 F5.2 --- r23 Separation between the second and third most
luminous cluster galaxies (1mm=67.14")
88 I1 --- Nb []? Number of apparent galaxies that are not
among the three most luminous cluster galaxies
92- 93 A2 --- FRS1a Revised RS type for the first subcluster
99 I1 --- FRS1c []? Number of bright galaxies used to determine
FRS1 RS type for both the C and L types
102 A1 --- FRS2a Revised RS type for the second subcluster
108 I1 --- FRS2c []? Number of bright galaxies used to determine
FRS2 RS type for both the C and L types
122 A1 --- Com Comments (4)
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Note (1): Basic RS type: cD, B, L, C, F or I)
Note (2): Appendage or subscript which indicates a subsidiary property :
p=peculiar cD galaxy
n=multiple nucleus cD galaxy
s=satellite of a cD galaxy
b=connected supergiant binary galaxy within a B-type cluster
p=peculiarity associated with a supergiant binary galaxy or the
B cluster itself
a=arc shape of the line of galaxies defining an L-type cluster
c=clumpy
s=smooth I-type cluster
Note (3): The number following a 'b' or 's' designation is the measured
separation (1mm=67.14") between the components of a binary galaxy
or between a cD_s_ galaxy ant its nearby satellite, respectively
Note (4): c: presence of a comment concerning the cluster in "notes" file
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References:
Abell G.O., 1980, (Catalogue published in 1989, ApJS 70, 1)
Johnson M.W. et al., 1983, ApJ, 266, 425
Leir A. & van der Bergh S., 1977, ApJS, 34, 381
Owen F.W. et al., 1982, AJ, 87, 1083
Rood H.J., Sastry G., 1971, Pub. A.S.P., 83, 313
Struble M.F. & Rodd H.J., 1986, ApJS, 63 543
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Courtesy: Struble M.F., Rood H.J.
First prepared by W.H. Warren (ADC/NASA)
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(End) Patricia Bauer [CDS] 20-Jan-1995