Date and Time of the Query: 2019-04-25 T11:15:22 PDT
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Notes for object NGC 5427

13 note(s) found in NED.

1. 2003ApJS..146..353M
Re:NGC 5427
NGC 5427 (LW)
This galaxy is unusual as it appears to have star formation along the
leading edges of a two-arm, symmetric dust spiral. However, these arms
are the continuation of the main disk, Sc grand-design spiral pattern.
Interior to these arms, at less than approximately 700 pc radius,
there are four or five nuclear dust spirals; therefore, we classify
this galaxy as loosely wound, rather than grand-design type.

2. 2002ApJS..143...73E
Re:NGC 5427
NGC 5427.---Sc: System is nearly face-on. Bright nucleus embedded in a
small, slightly elliptical bulge. Some evidence for a weak oval
distortion with a P.A. skewed by ~45 from that of the bulge.
Grand-design two-armed spiral pattern emerges from the bulge. The arm
that emerges from the west side of the bulge is HSB for ~250deg and
has many bright knots. It then fades, but it can be traced through a
full 360deg winding. The east arm has fewer knots and is HSB for only
~150deg. It can also be traced at lower surface brightness levels
through a full 360deg. Both arms have spurs at ~180deg. There is a LSB
bridge to the interacting companion to the south.

3. 2002A&A...389...68G
Re:NGC 5427
NGC 5427: here the two methods and the three catalogs give
different results, which again are very different from the
literature values. This is not surprising as the galaxy is
not very inclined and there is no derived velocity field in
the literature. For lack of any stronger criteria and looking
at the deprojected images obtained with all these values, we
decided to adopt the result of the first method and the richer
catalog. However, it should be stressed that these are very
ill defined values.

4. 1999AJ....118.2331V
Re:NGC 5427
Only a single F606W image of NGC 5427 is available. We used the
nuclear offset position for the SN (35" east and 34" north) from the
online Asiago catalog. The SN site is very near the edge of the chip,
near a spiral arm. Within the 10" radius error circle are a number of
bright nebulae, presumably H II regions and star clusters.

5. 1997ApJS..108..155G
Re:NGC 5427
NGC 5427 is an S2 nucleus in an Sc host galaxy. It is interacting with
NGC 5426. The disk has strong H{alpha} emission; 164 H II regions located
mainly in the spiral arms have been detected. More emission is located in
the part of the disk opposite to NGC 5426; this effect seems to be a
consequence of the interaction. The nuclear emission represents 5% of the
total emission, and the isophotal contours seem to be elongated to the
north, especially in the [O III] image (see the [O III] and expanded
H{alpha} images in Figure 11j). The [O III] image also shows emission
associated with the H II regions. A circumnuclear ring of H II regions is
detected at 1 kpc from the nucleus. A more detailed analysis of the
H{alpha} and [O III] was presented by Gonzalez Delgado & Perez (1992).

6. 1997A&AS..125..479J
Re:NGC 5427
NGC 5427 (SAc/Seyfert 2, 1"~86 pc, I=35.1^deg^)
The ellipticity profile shows four clear maxima, the highest of which (at
a~21") corresponds to the two-arm spiral structure. The two innermost ones
(a~5" and 8") do not correspond to well defined plateaus in PA, however the
changes in ellipticity and PA occur at roughly the same places. We agree with
W95 that these features are oval structures whose nature remains controversial,
which is perhaps connected to the interacting nature of NGC 5427. Nevertheless,
we note that after deprojection, the PA is defined much better in the inner
region: it is constant up to 6", i.e. within the first ellipticity peak which
could indicate a nuclear bar in this region. This interpretation is tempting
also because of the Seyfert nucleus.

7. 1996ApJS..105...93E
Re:NGC 5427
4.12. NGC 5427
NGC 5427 is one component of the interacting pair of galaxies Arp 271. The
other component is NGC 5426, which is separated from NGC 5427 by ~25 kpc
(Dahari 1984). Optical spectra of the nucleus of NGC 5427 have been obtained by
Kennicutt & Keel (1984), who suggest that the nuclear activity may have been
induced through the galaxy-galaxy interactions. Optical nuclear emission-line
(Keel et al. 1985), infrared (Giuricin 1994), and radio (Giuricin et al. 1990)
fluxes are available in the literature.
Figure 1 reveals the presence of a possible nuclear ring of H II regions with a
radius of ~5". Numerous H II region complexes trace the distorted spiral arms
out to at least 1' from the nucleus. The H II regions appear brightest in the
eastern spiral arm, although there is a bright complex located in the western
arm at the point at which the arm abruptly changes direction. One can speculate
that mechanical interactions due to changes in the direction of the gas flows
in the local ISM may be responsible for the star formation that has produced
the H II region complex at this location.

8. 1994CAG1..B...0000S
Re:NGC 5427
Pair [with NGC 5426]
April 29/30, 1979
103aO + GG385
40 min
Both NGC 5426 and NGC 5427 have normal
Sbc morphologies. They evidently form a
physical pair; the redshifts are v_o = 2455 km/s
and v_o = 2565 km/s, respectively. The angular
separation of 2.3' corresponds to a projected
linear separation of 34 kpc at the mean redshift
distance of 50 Mpc (H = 50).
The only evidence for a close tidal encounter
are the two thin straight strands of the multiple
outer arms of NGC 5426 that overlap the outer
thin spiral arms of NGC 5427, where the spiral
pattern is of the grand design. Otherwise, each
galaxy has beautifully formed arms that are so
regular that each is assigned the earliest
luminosity class because of the small geometrical
entropy. Evidently, close encounters at some
phase in their action have had nearly negligible
perturbative effects on the visible morphology.

9. 1976RC2...C...0000d
Re:NGC 5427
= Holm 573a
In Arp 271 = VV 021
Interacting pair with NGC 5426 at 2.3 arcmin, connected.
HI 21cm:
A.J., 79, 767, 1974 (Velocity and flux attributed to NGC 5427).

10. 1974UGCA..C...0000N
Re:UGCA 381
UGCA 381:
= NGC 5427
paired with UGCA 380 (connected): UGCA 380 + UGCA 381 = VV 021 = Arp 271;
UGCA 380 at 2.4, 187, , connecting filaments;
"Arms linked. Note bifurcation in arm of N spiral" (Arp)

11. 1964RC1...C...0000d
Re:NGC 5427
= Holm 573a
Very bright nucleus in a bright lens: 0.23 arcmin x 0.17 arcmin. 2 main bright
spiral arms, knots and branches.
Interacting pair with NGC 5426 at 2.3 arcmin.
Photograph and Spectrum:
Ap. J., 116, 64, 1952.

12. 1963MCG3..C...0000V
Re:MCG -01-36-003
Remarkable interacting pair with MCG -01-36-004, {rho} = 2.3 arcmin
with two bridges. This is Holmberg double No. 573. Photo: VV Atlas No. 21.
Type: vB - Sc(t), Vauc - SA(s)c p. Redshift: +2588 (not corrected),
{lambda} 3727 (Page); B-V = 0.64, U-B = -0.06, CI = 0.52.

13. 1959VV....C...0000V
Re:VV 021a
= NGC 5427
V = +2,528 km/sec from {lambda}3727
(Page, T., Ap. J., 116, 63, 1952)

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