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85#85
86#86
87#87
88#88
89#89
The WFPC2 F606W images. The orientation in all the images is North
up and East to the left. The images show the morphological characteristics of
the inner galaxy: a) NGC 7130 shows dust lanes running from North to South.
The displayed field size is roughly 9 by 9 kpc. b) NGC 5135 shows arc-like
segments spiraling to the center of the galaxy. The displayed field size is
roughly 6.5 by 6.5 kpc.
c) IC 3639 shows its bar and its spiral arms emerging from the edge of the bar.
The displayed field size is roughly 6.7 by 6.3 kpc
The UV surface brightness profiles of the new galaxies in the
sample. These were measured from the FOC
23#23
images, after
sky subtraction, and using circular annuli centered on the origins mentioned
in the text. The solid line shows the mean surface brightness within the
annuli, while the dotted lines show the effects of changing the adopted sky
level by its
90#90
uncertainty. The arrow indicates the adopted outer
radius of the inner high surface brightness structure.
The FOC F210M image of the ultraviolet continuum in NGC 7130. The field displayed (roughly 2.6 by 2.9 kpc)
shows knots that are located in the
arc-like segments that could be associated with the leading edge of the bar.
The central 211#112 arcsec2 (620 by 620 pc) of NGC 7130 in optical
light (a) and in UV light (b). The origin of the plot is the knot with the
highest UV surface brightness.
The presumed nucleus is placed at 0.2 arcsec West and 0.1 arcsec South of the
origin.
Overall view of the UV continuum emission detected in the FOC image of NGC 5135. The arc structure is coincident with the arc segment seen in the optical WFPC2 image that is spiraling to the center. The displayed field size is
about 2.2 kpc.
Central 311#113 arcsec2 (540 by 540 pc)
field of NGC 5135: a) WFPC2, b) UV. The origin of this plot is the pixel with
the highest UV surface brigtness. Based on the morphology of the WFPC2 image,
we believe that the nucleus is the knot located at 1.05 arcsec North and 0.4 arcsec East.
Central 111#111 arcsec2 (210 by 210 pc) field
of IC 3639: a) WFPC2, b) UV. The origin of this plot is the center of the 41#41
structure seen in the WFPC2 image, which is coincident with the pixel of the highest surface brightness in the central 0.111#110.1
arcsec of the UV image. We suggest that the nucleus of the galaxy is placed there.
The GHRS spectra of: a) NGC 7130, b) NGC 5135, c) IC 3639. They are
displayed in log (F
60#60)
to show the emission and absorption lines. The
most important stellar wind and photospheric absorption lines in the galaxy
(NGC 7130) are labeled.
The normalized GHRS spectrum of IC 3639 and one simulation in which scattered light from a hidden Seyfert 1 nucleus produces 591#91
of the UV continuum. (dashed line)
55#55
parameter of the fits to the profile of SiIV in
NGC 7130 for burst models (a,b) and continuous star formation models (c,d) with different Mupp (a,c) and IMF slope (b,d).
The size of the bubble is proportional to 55#55,
with a larger size indicating a worse fit. The scale in the small boxes indicates the value of 55#55.
As in Figure 12 for NGC 5135
As in Figure 12 for IC 3639
The GHRS spectrum of NGC 7130 dereddened by E(B-V)=0.046 using the MW extinction law and by E(B-V)=0.25 using the Calzetti et al (1994) extinction law (thick line) and the synthetic 4 Myr burst model (in relative units) (thin line). The IMF slope is Salpeter and Mupp=80 M16#16.
The GHRS spectrum of NGC 5135 dereddened by E(B-V)=0.094 using the MW extinction law and by E(B-V)=0.2 using the Calzetti et al (1994) extinction law (thick line) and the synthetic 5 Myr burst model (in relative units) (thin line). The IMF slope is Salpeter and Mupp=80 M16#16.
The GHRS spectrum of IC 3639 dereddened by E(B-V)=0.138 using the MW extinction law and E(B-V)=0.2 using the Calzetti et al (1994) extinction law (thick line) and the synthetic 4 Myr burst model (in relative units) (thin line). The IMF slope is Salpeter and Mupp=60 M16#16.
Ground-based optical spectrum of NGC 7130 (a), NGC 5135 (b) and IC 3639 (c) obtained through a 1.511#113.5 arcsec2 aperture displayed as log (F
60#60)
to show the emission and absorption lines. The inset shows the region around 3650-3850
Å expanded to highlight the high-order Balmer series and HeI 1#13819
lines. Other photospheric absorption lines are labeled in the figure. The wavelength axis is in the rest frame of the galaxy.
The normalized spectrum of NGC 7130 (dashed line) plotted with the normalized spectrum of a B0V star combined with a G0V star (thick line). 6091#91
of the light is from a B0V and 4091#91
from a G0V star. The comparison shows that most of the
stellar features in NGC 7130 are well reproduced by a combination of young (B0V) and old (G0V) stars.
The normalized spectrum of NGC 5135 (dashed line) plotted with the normalized spectrum of the super-star cluster B in NGC 1569 (thick line).
The stellar features in NGC 1569 B are well
reproduced by a combination of young (70 91#91
of the light from B0V) and old (30 91#91
of the light from G0V) stars. There is a good match between NGC 5135 and NGC 1569 B.
The normalized spectrum of IC 3639 (dashed line) plotted with the combination of the normalized spectrum of the super-star cluster B in NGC 1569 and the galaxy NGC 4339 (thick line). 6091#91
of the light is from NGC 1569 and 4091#91
from
NGC 4339. The stellar lines of NGC 4339 are the typical features from an old bulge population.
The CaII triplet region in NGC 7130. The absorption features and some emission lines are labeled.
Profile of the emission lines in NGC 5135: a) H10#10,
b) [OIII], c) HeII 1#14686. The observed profile (solid line), the two model components (dashed lines) and their sum (solid line) are shown.
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Rosa Gonzalez
1998-06-20