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J/A+A/283/805 Integrated spectral properties of star clusters (Bica+ 1994)
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Integrated spectral properties of star clusters in the the near-ultraviolet
Bica E., Alloin D., Schmitt H.R.
<Astron. Astrophys. 283, 805 (1994)>
=1994A&A...283..805B
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Keywords: globular clusters - open clusters - galaxies: star clusters -
Magellanic Clouds - ultraviolet: stars - galaxies: evolution
Abstract:
We study integrated spectra of 37 star clusters in the range 3100 - 4200
A . The sample includes Galactic globular and open clusters, as well as
Magellanic Cloud clusters. Feature equivalent widths (W)and continuum
distribution are analyzed as a function of age and metallicity. In
particular we discuss the behaviour of the Balmer Jump and of the 4000 A
Break, which are measured by the same continuum ratio C3660 A / C4020 A.
For ages t < 500 Myr the Balmer Jump is dominant over the 4000 A Break and
for t < 50 Myr it is an excellent age discriminator. The effects of blue
Horizontal Branch morphology on globular cluster spectra are also
discussed: they increase the Balmer line W, but do not dilute substantially
the Near-UV metallic features. The present data will provide a means to
connect optical to W integrated star cluster spectra, with important
applications in stellar population analyses, in particular for distant
galaxies at redshift up to 1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1 61 37 Cluster Properties
table3 100 37 Equivalent Widths
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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 A4 --- Group See note 1 (1)
7- 13 A7 --- NGC NGC denomination
18- 24 A7 --- Other Other name
35- 39 I5 Myr Age Age
40 A1 --- r_Age Reference to Age (2)
42- 46 F5.2 Sun Z Metallicity
48 A1 --- r_Z Reference to metallicity (2)
50- 53 F4.2 mag E(B-V) Foreground reddening
55- 58 F4.2 --- B/B+R []? Mironov Horizontal branch morphology
parameter for the old clusters
59 A1 --- u_B/B+R uncertainty flag on B/B+R
61 A1 --- r_B/B+R Reference to B/B+R (3)
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Note (1): SMCC: Small Magellanic Cloud Cluster
LMCC: Large Magellanic Cloud Cluster
GOP: Galactic Open Cluster
GGC: Galactic Globular Cluster
Note (2): Age metallicity and reddening as compiled in the BA86a except
a Mould et al. 1989;
b Vallenari et al. 1992;
c Richtler & Nelles (1983) and Walker(1985);
d Arp & Cuffey (1962) and Christian, Heasly & Janes (1985).
Note (3): Horizontal branch morphology parameter B/B+R from Zinn(1980) except
our estimates from
e Walker (1992);
f Stetson (1981);
g Cannon, Sagar & Hawkins (1990);
h Alcaino et al. (1991);
i Janes & Heasley (1991);
j Bica, Barbuy & Ortolani (1993);
k Alcaino (1981);
l Martins, Harvel & Miller (1980);
m Ortolani, Bica & Barbuy (1992);
n Ortolani, Bica & Barbuy (1990);
o Liller & Carney (1978);
p Ortolani, Bica & Barbuy (1993).
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Table 2 = Equivalent width in the spectral Windows
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Window Limits (A) Main the Absorbers
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a 3290-3332 NH; TiII; NiI
b* 3332-3392 NH; TiII; TiI; CN
c 3392-3420 NiI; FeI; CrII; CN
d* 3420-3460 NiI; FeI; CoI; CN
e 3460-3500 FeI; CN
f 3500-3540 FeI; NiI
g 3540-3596 FeI; CN
h 3596-3626 FeI
i 3626-3660 FeI; Balmer Limit; CrII; CN
j 3660-3696 FeI
k* 3696-3760 {HI12,13,...}; FeI M
l 3760-3780 {HI11}; FeI M
1L 3780-3810 {HI10}; CN Lband
1C 3810-3822 mostly continuum in the blue clusters
2L 3822-3858 {HI9}; CN Lband; FeI; MgI; HeI
2C* 3858-3872 mostly continuum in the blue clusters
3L* 3872-3908 {HI8}; CN Lband; FeI; SiI; HeI
4 3908-3952 CaII K
5* 3952-3988 CaII H;{H_epsilon_}
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Notes on Table 2:
{ } indicates that the line can be in the absorption and/or emission.
* indicates windows where emission lines in the e.g. HII regions and
Seyfert galaxies occur ([NeV] 3346 A, [NeV] 3426 A, [OII] 3727 A,
[NeIII] 3869 A and [NeIII] 3968 A).
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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 A4 --- Groupe See note 1
6- 9 I4 --- NGC NGC number
10- 14 F5.1 0.1nm b []? Equivalent width in the [3332-3392] range
16- 19 F4.1 0.1nm d []? Equivalent width in the [3420-3460] range
21- 24 F4.1 0.1nm e []? Equivalent width in the [3460-3500] range
26- 28 F3.1 0.1nm f []? Equivalent width in the [3500-3540] range
30- 33 F4.1 0.1nm g []? Equivalent width in the [3540-3596] range
35- 37 F3.1 0.1nm h []? Equivalent width in the [3596-3626] range
39- 41 F3.1 0.1nm i []? Equivalent width in the [3626-3660] range
48- 53 F6.1 0.1nm k Equivalent width in the [3696-3760] range
55- 58 F4.1 0.1nm 1L Equivalent width in the [3780-3810] range
60- 62 F3.1 0.1nm 1C Equivalent width in the [3810-3822] range
64- 67 F4.1 0.1nm 2L Equivalent width in the [3822-3858] range
69- 73 F5.1 0.1nm 2C Equivalent width in the [3858-3872] range
75- 79 F5.1 0.1nm 3L Equivalent width in the [3872-3908] range
81- 84 F4.1 0.1nm 4 Equivalent width in the [3908-3952] range
85- 89 F5.1 0.1nm 5 Equivalent width in the [3952-3988] range
92- 95 F4.2 --- C3540/C4020 Intensities ratio in the continuum at the
wavelengths 3540/4020
97-100 F4.2 --- C3660/C4020 Intensities ratio in the continuum at the
wavelengths 3660/4020
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Note (1):
SMCC: Small Magellanic Cloud Cluster
LMCC: Large Magellanic Cloud Cluster
GOP : Galactic Open Cluster
GGC : Galactic Globular Cluster
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(End) Patricia Bauer [CDS] 19-Oct-1993