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Date and Time of the Query: 2019-04-26 T09:58:44 PDT
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Notes for object NGC 6890

11 note(s) found in NED.


1. 2003ApJS..146..353M
Re:NGC 6890
NGC 6890 (GD)
This is another prototype of the grand-design nuclear spiral class,
and it illustrates the effect of inclination in enhancing and
suppressing the dust contrast on the near and far sides of the galaxy,
respectively.

2. 2000ApJ...544..747S
Re:NGC 6890
The CR of 0.7 indicates the presence of a PL/YS continuum contributing
with ~30% to the flux at 4020 A, in agreement also with the W values. Some
contribution of an intermediate-aged population is also possible, and a
model including 10% mass contribution of a 1 Gyr stellar population,
combined with 20% in flux of a PL gives a slightly improved fit in the
H9-H10 region, as shown in Figure 16b. Ne III {lambda}3968 + H {epsilon}
emission are filling the Ca II H + H{epsilon} absorption.

3. 1999A&AS..140....1M
Re:NGC 6890
Despite its classification as a non-barred galaxy, the K' image of
NGC 6890 reveals a strong bar (Figs. 17a and e), together with the
beginning of two spiral arms at the extremities of the bar, the northern
arm being brighter than the southern one (Fig. 17b). These features are
also apparent in the K' image by Mulchaey et al. (1997), but these
authors give PA = 179 ^deg^ corresponding to a radius ~ 14 arcsec, where
the PA strongly decreases. However, their plots of the PA and {epsilon}
show that the bar actually extends up to about 6 arcsec with
PA ~ 15 ^deg^, in agreement with our values. We also note that, even
considering the differences in the photometry (see Table 4) the
isophotal levels differ by more than 6 magnitudes, those by
Mulchaey et al. being extremely bright and most probably incorrect.
The difference image reveals a beautiful spiral structure as well as a
possible inner ring (10-15 arcsec) (Fig. 17c). This inner ring seems
confirmed by the J/K' image (Fig. 17d), where J appears to be somewhat
larger around the nucleus than in the very central region. Notice a
smooth decrease of J relative to K' with increasing radius from 2 arcsec
outwards (Fig. 17h). The NICMOS HST image shows spiraling structure
reaching the central arsecond, with some hints of dust at 0.5 arcsec
(Fig. 33).
The bulge + disk fit is quite good except in the arm regions (Figs. 17f
and 17g).

4. 1998MNRAS.297..579C
Re:NGC 6890
NGC 6890. Storchi-Bergmann et al. (1990) studied the nuclear optical spectrum
of this galaxy, finding that the stellar population is old and that H{alpah} may
have a broad component. The Ws show a gradient in Ca K and the G band. which
change from S4 at the nucleus to S3 in the outer regions, but not in Mg, which
has values typical of an S3 template, with no gradient (Fig. 27). The continuum
ratios have values larger than S1 at the nucleus, decreasing to S2 in the outer
regions. These results are similar to those obtained by Storchi-Bergmann
et al. (1990).

5. 1997ApJS..110..299M
Re:NGC 6890
Bar is visible in both the ellipse fits and the K_S_image. Unbarred in the
RSA.

6. 1994CAG1..B...0000S
Re:NGC 6890
Sb(s)II-III
CD-1503-S/Br
Aug 4/5, 1980
103aO + GG385
45 min
Two zones of different surface brightness
exist in the disk of NGC 6890. The tightly wound
thick spiral arms in the inner disk have very high
surface brightness. Sets of lower-surface-brightness
arms begin from the ends of the inner arms
and wind outward, stopping abruptly to form an
apparent edge to the pattern.

7. 1985SGC...C...0000C
Re:NGC 6890
Plate 5235r
Overexposed center (probable bar and ring), knotty arms form (R'): 1.0 x 0.7.
Very faint plume to south-preceding.
Plate 5281
Overexposed center.

8. 1982ESOU..C...0000L
Re:ESO 201449-4457.8
=ESO 284- G 54
in cluster

9. 1979AJ.....84..472S
Re:NGC 6890
Two well-defined arms in a high-surface-brightness disk.

10. 1976RC2...C...0000d
Re:NGC 6890
In group.
Spectrum:
Bull. A.A.S., 4, 237, 1972.

11. 1964RC1...C...0000d
Re:NGC 6890
Very small, bright nucleus in a bright inner lens with 2 main, poorly resolved
arms. Pseudo (r): 0.5 arcmin x 0.3 arcmin. Outer part has a fairly sharp
edge with traces of spiral structure forming a pseudo (R): 0.95 arcmin x 0.65
arcmin.
HA 88, 2 classification (E:) is erroneus.


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