Date and Time of the Query: 2019-06-27 T00:28:52 PDT
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Notes for object NGC 4298

8 note(s) found in NED.

1. 2006MNRAS.366..812C
Re:NGC 4298
This apparently flocculent galaxy (Elmegreen et al. 1999) has a companion NGC
4302 only at a distance 2.3 arcmin (or 10.7 kpc projected) and with nearly the
same systemic velocity ({nu}^N4302^_sys_ = 1149 km s^-1^, Binggeli et al. 1985).
According to Koopmann & Kenney (2004), the truncated gas disc is due to RPS and
the stellar asymmetry to a tidal interaction with a companion. The velocity
field appears however mildly perturbed. Notice that the southern arm presents
velocities more redshifted than the nearby parts of the disc at the same
azimuthal angles. This perhaps indicates streaming motions along it or, less
probably, a locally warped arm. A steep velocity rise is detected in the PV
diagram in the core of the galaxy.

2. 2002AJ....124..675C
Re:UGC 07412
F12190+1452 is a blend of UGC 07412 and UGC 07418.

3. 2001A&A...379...54H
Re:KPG 332A
KPG332A. The galaxy is classified as SA(rs)c and our (B-I) and
sharp/filtered images show a bright nucleus and blue knotty arms. We do not
find evidence for an internal ring or s-shaped structure. We classify this
galaxy as Sc. The colour is representative of Sa type. Our EE class is 3.

4. 1994CAG1..B...0000S
Re:NGC 4298
VCC 483
March 22/23, 1980
panel 289
75 min
NGC 4298 forms an apparent pair with
NGC 4302 (Sc on edge; panel 289) at a separation
of 2.4'. The redshifts listed in the RSA are
identical at v_o = 1004 km/s. However, as the
pair is in the Virgo Cluster, the similarity of
redshifts does not assure a dynamical relation
because of the large virial velocities of parts of
the cluster complex. If the pair is at the same
distance of 21.9 Mpc (m - M = 31.7), their
projected linear separation is small at 15 kpc.
As in NGC 5949 above, and NGC 7314 on
the preceding panel, the nucleus of NGC 4298 is
pointlike. There is no central bulge or evidence
of a halo.

5. 1994CAG1..B...0000S
Re:NGC 4298
VCC 483
Karachentsev 332 [with NGC 4302]
March 22/23, 1980
panel 279
75 min
NGC 4302 and NGC 4298 in the Virgo
Cluster may form a physical pair. Their redshifts
are identical at v_o = 1004 km/s, as listed in the
RSA2. The angular separation of 2.4' corresponds
to a projected linear separation of only
15 kpc at the distance of 21.9 Mpc. There is no
evidence for tidal distortion in either NGC 4298
or NGC 4302. Note that the thin disk seen edge
on in NGC 4302 is not warped; yet NGC 4298,
in projection, is nearly in the pole of NGC 4302.
The lack of morphological distortion in
either galaxy suggests that the true separation is
considerably larger than the projected separation.
Similarity of redshift in the Virgo Cluster
does not necessarily mean a common distance
because of the large (virial) spread in the
velocities of cluster members.

6. 1976RC2...C...0000d
Re:NGC 4298
= Holm 377a
= Kara[72] 332a
Non-interacting pair with NGC 4302 at 2.4 arcmin

7. 1973UGC...C...0000N
Re:UGC 07412
SA(rs)c (de Vaucouleurs), Sc- (Holmberg)
Paired with UGC 07418 at 2.4, 102

8. 1964RC1...C...0000d
Re:NGC 4298
= Holm 377a
Very small, bright nucleus. Many knotty, filamentary arms with dark lanes.
Non-interacting pair with NGC 4302 at 2.4 arcmin.

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