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Notes for object NGC 5474

15 note(s) found in NED.


1. 2008MNRAS.388..500E
Re:UGC 09013
UGC 9013 (NGC 5474). This late-type peculiar dwarf galaxy is the nearest
companion of M101 (44 arcmin) and is tidally deformed into a very asymmetric and
disturbed object. Our H{alpha} velocity field cannot help us finding the
rotation centre as it shows a solid body shape. Knapen et al. (2004) show an
H{alpha} map in good agreement with ours. The H{alpha} rotation curve derived
from long-slit spectroscopy data by Catinella, Haynes & Giovanelli (2005) cannot
be compared directly with ours, because their centre has been chosen to be the
'pseudo-nucleus'. Several H I studies are available in the literature
(Huchtmeier & Witzel 1979; van der Hulst & Huchtmeier 1979; Rownd, Dickey &
Helou 1994; Kornreich et al. 2000). Kornreich et al. (2000) and Rownd et al.
(1994) used the same data set from the VLA array (35-arcsec beam). The optical
part of the galaxy is not affected by the severe warp seen in H I and the solid
body rotation seen in H{alpha} is compatible with H I data. These authors place
the kinematical centre as the symmetry centre of the warp. It is closer to the
centre of the outermost optical isophotes than the 'pseudo-nucleus'. Rownd et
al. (1994) assumed an inclination of 21^deg^ from a tilted ring model. Their PA
of the major-axis at the centre (~158^deg^) is in agreement with ours but almost
perpendicular to the photometric PA. Due to the presence of the strong tidal arm
and the relative low spatial H{alpha} coverage, the inclination and centre are
in fact difficult to recover. That is why we preferred using the H I kinematical
centre and inclination (21^deg^) consistent with the external axial ratio of the
outermost isophotes from the XDSS image. The strange behaviour of the resulting
H{alpha} rotation curve in the first 40 arcsec could be the signature of strong
non-circular motions. We find a maximum velocity rotation ~120 km s^-1^ at about
70 arcsec, significantly higher than the velocities found by Kornreich et al.
(2000) even when assuming a very low inclination for the H I disc. A lso the
amplitude of our H{alpha} velocity field is higher than the H I velocity field
amplitude.

2. 2008MNRAS.385..553D
Re:NGC 5474
NGC 5474: The H{alpha} distribution of this peculiar galaxy is composed
of several H II regions and clumpy diffuse ionized gas which are
rotating weakly. The H I disc also displays a clumpy but fairly
symmetric distribution. The H I velocity field exhibits normal
differential rotation but warping near the edge of the H I disc can be
seen (Rownd, Dickey & Helou 1994, see also van der Hulst & Huchtmeier
1979).

3. 2007ApJS..173..538T
Re:NGC 5474
NGC 5474 (Fig. 16.34).-This companion of M101 (NGC 5457) is well known optically
for hosting an off-center nucleus, most likely indicative of prior interaction
(with M101?). Imaging from GALEX shows that scattered SF complexes exist in the
outer disk of this SA(s)cd pec H II galaxy, most especially to the west and
southeast. NGC 5474 is a galaxy in which the distribution of UV-bright sources
falls off smoothly with galactocentric distance, even if extended. The H I
structure of NGC 5474 was studied in Rownd et al. (1994), who noted the clumpy
nature of the gas distribution without any clear evidence for spiral features.
At a limit of ~2 * 10^20^ cm^-2^, the H I disk covers an area of 9' * 7' .
Curiously, the GALEX data show spiral arm structure, as do H{alpha} observations
(Hodge & Kennicutt 1983). Moreover, these features begin at the position of the
offset nucleus, rather than the center of the overall optical distribution. SDSS
data again suggest a dramatic disconnection between the stars contributing to
the visible light morphology and the (spiral) pattern of recent star birth,
similar to what we found for UGC 04393.

4. 2002AJ....124..675C
Re:UGC 09013
Extended galaxy. Uncataloged diffuse NVSS source, very uncertain flux
density.

5. 2000A&AS..142..425D
Re:NGC 5474
3.5 NGC 5474 = UGC 9013 = VV 344 = Arp 26 = PGC 50216 = IRAS 14031+5354
The structure of this nearest companion to M 101 is strongly disturbed
by tidal interaction. A view of the galaxy imaged in the R band is shown
in Fig. 11. It has been taken from the archive of the Isaac Newton
telescope (La Palma). Positions of two CCD frames obtained with the 6-m
telescope are indicated by boxes. The reproduction of the southern image
in the I band is presented in Fig. 12. The results of photometry of 298
brightest stars in both fields are given in the diagram V proportional
to V-I (Fig. 13). For three brightest blue supergiant candidates we
derived the mean apparent magnitude = 20.37, which coincides
with the previous estimate, 20.36, made by Karachentsev et al. (1994).
The distance modulus of NGC 5474, (m - M)_0_ = 29.15, agrees well with
the modulus of M 101 (29.26) measured via cepheids (Alves & Cook 1995).

6. 1999ApJS..125..409C
Re:UGC 09013
UGC 09013. - Position of the eccentric nucleus.

7. 1999A&AS..137..337B
Re:NGC 5474
NGC 5474: highly asymmetrical galaxy. Too large for the field of view
for accurate photometry due to sky subtracion difficulties.

8. 1997AstL...23..644G
Re:NGC 5474
NGC 5474. A companion of M 101. Vorontsov-Vel'yaminov (1959) considered M 101
and NGC 5474 to be the members of an interacting pair. It follows from the CCD
photometry of Karachentsev et al. (1994) that the distances to M 101 and NGC
5474 are essentially the same. Only two red stars were detected. We include
this galaxy, the largest among the companions of M 101, in our list in order
that M 101 would not appear to be simultaneously the largest and the most
distant galaxy in our sample.

9. 1997ApJS..108..155G
Re:NGC 5474
The continuum emission shows a disk that is completely shifted toward the
south with respect to the bulge, and the same happens with the H{alpha}
emission. The nucleus is weak and compact, but diffuse emission connects
the nucleus to a bright H II region at 7" (200 pc) to the east. A well-
formed shell of H II regions at 1.2 kpc west from the nucleus surrounds a
continuum source. Although the H{alpha} and continuum emission have a
distorted appearance, the H I emission is quite regular in this galaxy.

10. 1994CAG1..B...0000S
Re:NGC 5474
M101 Group
Scd(s)IV pec
PH-82-B
June 9/10, 1950
103aO
30 min
NGC 5474 is one of the five late-type dwarf
companions to M101. The others are NGC 5204
(SdIV; panel 324), NGC 5477 (not in the RSA;
panel 326 here), NGC 5585 (SdIV; panel 323),
and Ho IV (not in the RSA or this atlas), all
shown together for comparison, as enlarged nearly
to a common scale (Sandage and Tammann
1974c, Fig. 1).
NGC 5474 is well resolved into individual
stars beginning at V = 20.5. This is about 2 mag
fainter than in M101, which is at the same
distance. This magnitude difference for the
brightest stars illustrates the dependence of M
(brightest star) on the absolute luminosity of the
parent galaxy.
Many HII regions exist across the disk. The
largest several are complex and have total (halo)
diameters of about 10".
The asymmetrical pattern of the multiple-armed
system may be due to tidal interaction
with M101, at an angular separation of 44'. At
the distance of 7.2 Mpc (m - M = 29.3) the
projected linear separation is small at 92 kpc.

11. 1976RC2...C...0000d
Re:NGC 5474
= VV 344
In M101 Group.
Photograph:
Ap. J., 194, 223, 1974.
HII Regions:
"Atlas and Catalogue", Univ. Washington, Seattle, 1966.
Ap. J., 156, 847, 1969. 194, 223, 1974.
Distance Modulus:
Ap. J., 194, 223, 1974.
HI 21cm:
Proc. 1st European Ast. Meet., Vol. 3, 15, 1974. Confused by M101.

12. 1973UGC...C...0000N
Re:UGC 09013
SA(s)cd pec (de Vaucouleurs), Sc+ (Holmberg)
VV 344b
Amorphous
Eccentric nucleus, probably interacting with UGC 08981 = M 101 at 45'.

13. 1964RC1...C...0000d
Re:NGC 5474
Low surface brightness. Smooth, partially resolved center with very small
faint nucleus. Several partially resolved arms. Strongly asymmetric.
In the M101 Group.
Photometry:
Medd. Lund II, 128, 1950.
HII Regions:
Zeit. fur Ap., 50, 168, 1960.

14. 1959VV....C...0000V
Re:VV 344b
= NGC 5474
V = +394 km/sec
Yerkes Type: fS1p

15. 1956AJ.....61...97H
Re:NGC 5474
HMS Note No. 176
The redshift indicates that this nebula is a member of the M101 Group
studied by Holmberg, E.E. 1950, Medd. Lunds Astr. Obs., Ser. II, No. 128.


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