J/A+A/393/389 Hα in HII regions in spiral galaxies (Marquez+, 2002)
Rotation curves and metallicity gradients from H II regions in spiral galaxies.
Marquez I., Masegosa J., Moles M., Varela J., Bettoni D., Galletta G.
<Astron. Astrophys. 393, 389 (2002)>
=2002A&A...393..389M 2002A&A...393..389M
ADC_Keywords: Clusters, galaxy ; Photometry, CCD ; Equivalent widths
Keywords: spiral - galaxies: kinematics and dynamics - galaxies: structure -
galaxies: interaction - galaxies
Abstract:
In this paper we study long slit spectra in the region of
Hα emission line of a sample of 111 spiral galaxies with
recognizable and well defined spiral morphology and with a well
determined environmental status, ranging from isolation to
non-disruptive interaction with satellites or companions. The
form and properties of the rotation curves are considered as a
function of the isolation degree, morphological type and
luminosity. The line ratios are used to estimate the metallicity of
all the detected H II regions, thus producing a composite
metallicity profile for different types of spirals. We have found that
isolated galaxies tend to be of later types and lower
luminosity than the interacting galaxies. The outer parts of the
rotation curves of isolated galaxies tend to be flatter than in
interacting galaxies, but they show similar relations between global
parameters. The scatter of the Tully-Fisher relation
defined by isolated galaxies is significantly lower than that of
interacting galaxies. The [NII]/Hα ratios, used as a
metallicity indicator, show a clear trend between Z and morphological
type, t, with earlier spirals showing higher ratios;
this trend is tighter when instead of t the gradient of the inner
rotation curve, G, is used; no trend is found with the change in
interaction status. The Z-gradient of the disks depends on the type,
being almost flat for early spirals, and increasing for
later types. The [NII]/Hα ratios measured for disk H II regions
of interacting galaxies are higher than for
normal/isolated objects, even if all the galaxy families present
similar distributions of Hα equivalent width.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 67 528 Results from the line measurements for the
different H II regions along the slits
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See also:
J/A+A/268/419 : HII Regions in NGC 4258 (Courtes+ 1993)
J/A+A/309/446 : HII Regions in M51 (Petit+, 1996)
J/A+A/354/823 : HII region catalogue of NGC 3359 (Rozas+, 2000)
J/ApJS/112/29 : HII regions in southern spiral galaxies (Feinstein 1997)
J/AJ/116/2805 : HII regions in spiral galaxies (Van Zee+, 1998)
J/A+A/416/475 : Long slit spectroscopy of HII regions (Marquez+, 2004)
Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Galaxy Name of the galaxy
11- 16 F6.1 arcsec Dist Distance to the center
18- 25 F8.3 0.1nm EW Equivalent width of Hα
27- 31 F5.3 --- [OI]/Halpha ? Intensity ratio [OI]/Hα
33- 37 F5.3 --- e_[OI]/Halpha ? rms uncertainty on [OI]/Hα
39- 43 F5.3 --- [NII]/Halpha ? Intensity ratio [NII]/Hα
45- 49 F5.3 --- e_[NII]/Halpha ? rms uncertainty on [NII]/Hα
51- 55 F5.3 --- [SII]/Halpha ? Intensity ratio [SII]/Hα
57- 61 F5.3 --- e_[SII]/Halpha ? rms uncertainty on [SII]/Hα
63- 67 F5.3 --- [SII]1/[SII]2 ? Intensity ratio [SII]1/[SII]2
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Acknowledgements: Isabel Marquez
References:
Marquez & Moles, Paper I 1996A&AS..120....1M 1996A&AS..120....1M
(End) Patricia Bauer [CDS] 15-Jul-2002