J/AJ/124/2453 Spectroscopy of active galaxies in nearby clusters (Miller+, 2002)
Evolution of star-forming and active galaxies in nearby clusters.
Miller N.A., Owen F.N.
<Astron. J. 124, 2453 (2002)>
=2002AJ....124.2453M 2002AJ....124.2453M
ADC_Keywords: Clusters, galaxy ; Radio continuum ; Galaxies, spectra
Keywords: galaxies: clusters: general - galaxies: evolution - radio continuum
Abstract:
We have used optical spectroscopy to investigate the active galaxy
populations in a sample of 20 nearby Abell clusters. The targets were
identified on the basis of 1.4GHz radio emission, which identifies
them as either active galactic nuclei (AGNs) or galaxies forming stars
at rates comparable to or greater than that of the Milky Way. The
spectra were used to characterize the galaxies via their emission and
absorption features.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 78 619 D4000 and Balmer equivalent widths for
cluster radio galaxies
table4.dat 96 619 Forbidden-line equivalent widths for
cluster radio galaxies
table5.dat 73 236 Balmer line fluxes for cluster radio galaxies
table6.dat 94 234 Forbidden-line fluxes for cluster radio galaxies
table8.dat 39 229 Galaxy classifications
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See also:
J/ApJS/134/355 : Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- [MO2002] Galaxy identification (G1)
15 A1 --- Apt Extraction aperture (G2)
17- 20 F4.2 --- D4000 ? The 4000Å break strength (2)
22- 25 F4.2 --- e_D4000 ? Error in D4000
27- 31 F5.1 0.1nm EWHd Hδ equivalent width in Å (3)
33- 36 F4.1 0.1nm e_EWHd Error in EWHd
38- 41 F4.1 0.1nm EWHg Hγ equivalent width in Å (3)
43- 46 F4.1 0.1nm e_EWHg Error in EWHg
48- 51 F4.1 0.1nm EWHb Hβ equivalent width in Å (3)
53- 55 F3.1 0.1nm e_EWHb Error in EWHb
57- 61 F5.1 0.1nm EWHa+NII Hα+[N II] equivalent width in Å (3)
63- 66 F4.1 0.1nm e_EWHa+NII Error in EWHa+NII
68- 72 F5.1 0.1nm EWHa ? Hα equivalent width in Å (3)
74- 77 F4.1 0.1nm e_EWHa ? Error in EWHa
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Note (2): The ratio of average Fν evaluated in the ranges 4050-4250Å
to 3750-3950Å (Bruzual, 1983ApJ...273..105B 1983ApJ...273..105B).
Note (3): With the exception of Hα + [N II], these equivalent widths
have been corrected for the assumed Balmer absorption component caused
by starlight in the galaxies. The adopted convention has positive
equivalent widths representing emission lines and negative equivalent
widths representing absorption. Where blends occur, the deblending has
been performed in IRAF using the task SPLOT as described in the text.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- [MO2002] Galaxy identification (G1)
15 A1 --- Apt Extraction aperture (G2)
17- 21 F5.1 0.1nm EWOII ? The [O II] λ3727 equivalent width (2)
23- 26 F4.1 0.1nm e_EWOII ? Error in EWOII
28- 31 F4.1 0.1nm EWO4959 The [O III] λ4959 equivalent width (2)
33- 35 F3.1 0.1nm e_EWO4959 Error in EWO4959
37- 40 F4.1 0.1nm EWO5007 The [O III] λ5007 equivalent width (2)
42- 44 F3.1 0.1nm e_EWO5007 Error in EWO5007
46- 49 F4.1 0.1nm EWOI The [O I] λ6300 equivalent width (2)
51- 54 F4.1 0.1nm e_EWOI Error in EWOI
56- 60 F5.1 0.1nm EWNII ? The [N II] λ6584 equivalent width (2)
62- 65 F4.1 0.1nm e_EWNII ? Error in EWNII
67- 70 F4.1 0.1nm EWSII ? The [S II] doublet equivalent width (2)
72- 75 F4.1 0.1nm e_EWSII ? Error in EWSII
77- 80 F4.1 0.1nm EWS6717 ? The [S II] λ6717 equivalent width (2)
82- 85 F4.1 0.1nm e_EWS6717 ? Error in EWS6717
87- 90 F4.1 0.1nm EWS6731 ? The [S II] λ6731 equivalent width (2)
92- 95 F4.1 0.1nm e_EWS6731 ? Error in EWS6731
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Note (2): The adopted convention has positive equivalent widths representing
emission lines and negative equivalent widths representing absorption.
Where blends occur, the deblending has been performed in IRAF using
the task SPLOT as described in the text.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- [MO2002] Galaxy identification (G1)
15 A1 --- Apt Extraction aperture (G2)
17- 21 F5.2 10-15mW/m2 FHd Hδ flux (in 10-15erg/s/cm2) (2)
23- 26 F4.2 10-15mW/m2 e_FHd Error in FHd (3)
28- 32 F5.2 10-15mW/m2 FHg Hγ flux (in 10-15erg/s/cm2) (2)
34- 37 F4.2 10-15mW/m2 e_FHg Error in FHg (3)
39- 43 F5.2 10-15mW/m2 FHb Hβ flux (in 10-15erg/s/cm2)(2)
45- 48 F4.2 10-15mW/m2 e_FHb Error in FHb (3)
50- 55 F6.2 10-15mW/m2 FHa+NII Hα+[N II] flux
(in 10-15erg/s/cm2) (2)
57- 60 F4.2 10-15mW/m2 e_FHa+NII Error in FHa+NII (3)
62- 67 F6.2 10-15mW/m2 FHa Hα flux (in 10-15 ergs/s/cm2) (2)
69- 72 F4.2 10-15mW/m2 e_FHa Error in FHa (3)
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Note (2): Only galaxies with emission lines are presented in this table.
Values of 0.00 indicate that the line was not detected in emission.
Where blends occur, the deblending has been performed in IRAF using
the task SPLOT as described in the text.
Note (3): Errors are based on the error in the continuum around the line,
bootstrapped to the line region taking into account the relative sizes
of the line and continuum regions. For deblended lines, a line
extraction region of 20Å was assumed.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- [MO2002] Galaxy identification (G1)
15 A1 --- Apt Extraction aperture (G2)
17- 22 F6.2 10-15mW/m2 FlOII The [O II] λ3727 flux
(in 10-15erg/s/cm2) (2)
24- 27 F4.2 10-15mW/m2 e_FlOII Error in FlOII (3)
29- 33 F5.2 10-15mW/m2 FlO4959 The [O III] λ4959 flux
(in 10-15erg/s/cm2) (2)
35- 38 F4.2 10-15mW/m2 e_FlO4959 Error in FlO4959 (3)
40- 44 F5.2 10-15mW/m2 FlO5007 The [O III] λ5007 flux
(in 10-15erg/s/cm2) (2)
46- 49 F4.2 10-15mW/m2 e_FlO5007 Error in FlO5007 (3)
51- 55 F5.2 10-15mW/m2 FlOI The [O I] λ6300 flux
(in 10-15erg/s/cm2) (2)
57- 60 F4.2 10-15mW/m2 e_FlOI Error in FlOI (3)
62- 66 F5.2 10-15mW/m2 FlNII The [N II] λ6584 flux
(in 10-15erg/s/cm2) (2)
68- 71 F4.2 10-15mW/m2 e_FlNII Error in FlNII (3)
73- 77 F5.2 10-15mW/m2 FlS6717 The [S II] λ6717 flux
(in 10-15erg/s/cm2) (2)
79- 82 F4.2 10-15mW/m2 e_FlS6717 Error in FlS6717 (3)
84- 88 F5.2 10-15mW/m2 FlS6731 The [S II] λ6731 flux
(in 10-15erg/s/cm2) (2)
90- 93 F4.2 10-15mW/m2 e_FlS6731 Error in FlS6731 (3)
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Note (2): Only galaxies with emission lines are presented in this table.
Values of 0.00 indicate that the line was not detected in emission.
Where blends occur, the deblending has been performed in IRAF using
the task SPLOT as described in the text.
Note (3): Errors are based on the error in the continuum around the line,
bootstrapped to the line region taking into account the relative sizes
of the line and continuum regions. For deblended lines, a line
extraction region of 20Å was assumed.
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- CName Abell cluster name
12- 24 A13 --- [MO2002] Galaxy identification (G1) (1)
26- 28 A3 --- SpClass Spectral classification (2)
30- 33 A4 --- MORPHS MORPHS classification (3)
35 A1 --- f_MORPHS [ab] Flag on MORPHS (4)
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Note (1): From J2000 coordinates.
Note (2): Spectral classification:
SF = star-forming galaxy;
SF? = emission-line galaxy presumed to be star-forming, although line
ratios are somewhat noisy;
Abs = absorption-line spectrum with no apparent emission lines;
Ab+ = predominantly absorption-line spectrum, although with slight
emission of [N II] and sometimes [S II];
Sey = emission-line galaxy shown to be a Seyfert in line ratio tests;
Lin = emission-line galaxy shown to be a LINER in line ratio tests;
Mix = nuclear spectrum that of a Seyfert or LINER, with off-nuclear
spectrum showing star formation.
Note (3): Determined from full aperture spectrum.
Table 7: MORPHs spectral classification scheme
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Class [OII]λ3727 Hδ Comments
EW in Å EW in Å
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k Absent <3 Passive
k+a Absent 3-8 Moderate Balmer absorption
without emission
a+k Absent ≥8 Strong Balmer absorption without
emission
e(c) Yes, <40Å <4 Moderate Balmer absorption plus
emission, spiral-like
e(a) Yes ≥4 Strong Balmer absorption plus
emission
e(b) Yes, ≥40Å ... Starburst
e(n) ... ... AGN from broad lines or
[O III]λ5007/Hβ
ratio
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Adapted from Dressler et al., 1999, Cat. J/ApJS/122/51.
The [O II] equivalent widths are for emission lines, and
the Hδ are for absorption lines.
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Note (4): Flag on MORPHS classification:
a: The [O II] line was not available in this spectrum.
b: The wavelength coverage for the spectrum did not include the full
blue continuum band for [O II], and hence no equivalent width or
line flux is reported. However, the [O II] line is apparent in
the spectrum.
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Global notes:
Note (G1): Nomenclature note:
The identification names are HHMMSS+DDMMSS in the tables, and
[MO2002] JHHMMSS+DDMMSS in Simbad
Note (G2): Extraction aperture code:
A: full 15" aperture;
N: the 2" aperture;
O: the difference between A and N.
M: Denotes that the spectrum was obtained with the MX multifiber
spectrometer and no spatial information can be obtained. Such
spectra are not flux-calibrated, and consequently, meaningful
values of D4000 cannot be calculated. For this reason, no
correction for Balmer absorption has been applied to these
spectra. Values are not presented in two cases: (1) all or some
portion of the defined continuum region lay off the CCD, and
(2) blended lines that were too weak to be deblended.
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History:
From electronic version of the journal
Some modifications of name (from authors) on 09-Apr-2003
(End) Greg Schwarz [AAS], Patricia Bauer [CDS] 13-Jan-2003