J/ApJ/424/599 Abundances in barred spiral galaxies (Martin+ 1994)
The influence of bars on the chemical composition of spiral galaxies
Martin P., Roy J-R.
<Astrophys. J. 424, 599 (1994)>
=1994ApJ...424..599M 1994ApJ...424..599M (SIMBAD/NED BibCode)
ADC_Keywords: H II regions ; Abundances
Keywords: galaxies: abundances - galaxies: kinematics and dynamics -
galaxies: structure - galaxies: spiral - H II regions
Abstract:
Imaging spectrophotometry in the nebular lines Hα, Hβ,
[OIII]λ5007 and [NII]λ6584, using narrow-band
interference filters, has been performed of 82, 55, and 79 H II
regions in the barred spiral galaxies NGC 925, NGC 1073, and NGC 4303,
respectively. The O/H abundance gradients were derived from the
abundance indicators [O III]/Hβ and [N II]/[O III], calibrated by
Edmunds & Pagel (1984MNRAS.211..507E 1984MNRAS.211..507E). The global O/H gradients in NGC
925 [{DELTA}log(O/H)/{DELTA}R=0.033dex/kpc] and NGC 1073
[{DELTA}log(O/H)/{DELTA}R=0.048dex/kpc] are flatter than the gradients
observed in normal galaxies of the same morphological type. The
abundance gradient in NGC 4303 is identical to that found in normal
spiral galaxies. A comparison is made between the O/H gradients of
normal galaxies and of a sample of galaxies showing a barred
morphology it is concluded that the global abundance gradients of
spiral galaxies with a barred structure are in general shallower than
gradients of normal galaxies. The slopes of O/H gradients are analyzed
as a function of two properties of bars: the relative length of the
bar with respect to the size of the disk, and the bar ellipticity,
defined by the axis ratio of the bar. It is found that gradients are
flatter when the length or the ellipticity of the bar increases. This
result is consistent with recent models of radial flows. These
observations indicate that large-scale mixing of the interstellar gas
occurs across the disks of barred spiral galaxies and affects the
radial distribution of elements.
Objects:
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RA (2000) DE Designation(s)
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02 27.3 +33 35 NGC 925
02 43.7 +01 23 NGC 1073
12 21.9 +04 28 NGC 4303
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5 55 82 Properties of H II regions in NGC 925
table6 55 55 Properties of H II regions in NGC 1073
table8 70 24 Properties of galaxies with abundance gradients
with samples ≥10 H II regions
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See also:
VII/112 : RC2 Catalogue (de Vaucouleurs+ 1976)
Byte-by-byte Description of file: table5 table6
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq Region sequential number
4- 8 F5.2 --- log([OIII]/Hb) Corrected [O III]/Hβ line ratio
10- 13 F4.2 --- e_log([OIII]/Hb) rms uncertainty on log([OIII]/Hb)
15- 19 F5.2 --- log([NII]/[OIII]) ? Corrected [N II]/[O III] line ratio
21- 24 F4.2 --- e_log([NII]/[OIII]) ? rms uncertainty on log([NII]/[OIII])
26- 30 F5.2 --- log([NII/Ha) ? Corrected [N II/Hα line ratio
32- 35 F4.2 --- e_log([NII/Ha) ? rms uncertainty on log([NII/Ha)
37- 40 F4.2 --- R/Reff Galactocentric distance corrected for
inclination
42- 45 F4.2 --- c(Hb) Logarithmic extinction at Hβ
47- 50 F4.2 --- e_c(Hb) rms uncertainty on c(Hb)
52- 55 F4.2 --- O/H O/H gradient
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Byte-by-byte Description of file: table8
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Bytes Format Units Label Explanations
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1- 8 A8 --- NGC Galaxy name
11- 19 A9 --- Type Morphological type
21- 22 I2 --- T T parameter (de Vaucouleurs et al., 1976,
Cat. VII/112)
24- 25 I2 deg i Inclination angle
27- 29 I3 deg PA [-30/170] Position angle
31- 34 F4.1 Mpc Dist Distance
36- 38 I3 --- N Number of H II regions used to derive the
O/H gradient
40- 42 I3 arcsec Rad25 ? Radius at the 25 magnitude/arcsec2
isophote in blue light
44- 46 I3 arcsec a ? Semi-major axis
48- 49 I2 arcsec b ? Semi-minor axis
52 I1 --- Ebar ? Bar ellipticity (Ebar=10(1-b/a))
54- 57 F4.2 --- a/Rad25 ? a/Rad25 ratio
59- 64 F6.3 kpc-1 Slope Slope of the global O/H gradient normalized
for the adopted distance
66- 67 I2 --- r_PA References for inclination & position angle (1)
69- 70 I2 --- r_N References for N and slopes of gradients (1)
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Note (1): References :
1: Vila-Costas & Edmunds 1992MNRAS.259..121V 1992MNRAS.259..121V
2: Belley & Roy 1992ApJS...78...61B 1992ApJS...78...61B
3: Wevers et al. 1986A&AS...66..505W 1986A&AS...66..505W
4: Our study
5: England, Gottesman, & Hunter 1990ApJ...348..456E 1990ApJ...348..456E
6: Roy et al. 1996ApJ...460..284R 1996ApJ...460..284R
7: Walsh & Roy 1989ApJ...341..722W 1989ApJ...341..722W
8: Martin 1992, Ph.D. thesis, Univ. d'Aix-Marseille I
9: Oey & Kennicutt 1993ApJ...411..137O 1993ApJ...411..137O
10: Martin et al. 1989ApJ...345..707M 1989ApJ...345..707M
11: Warmels 1988A&AS...72...57W 1988A&AS...72...57W
12: Martin & Roy 1992ApJ...397..463M 1992ApJ...397..463M
13: Scowen, Dufour & Hester 1992AJ....104...92S 1992AJ....104...92S
14: Zaritsky et al. 1994ApJ...420...87Z 1994ApJ...420...87Z
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History: Prepared via OCR at CDS.
(End) James Marcout, Patricia Bauer [CDS] 21-Mar-1997