Date and Time of the Query: 2019-07-19 T17:33:47 PDT
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Notes for object NGC 3414

15 note(s) found in NED.

1. 2008MNRAS.386.2242H
Re:NGC 3414
The black hole masses of NGC 2974, NGC 3414, NGC 4552, NGC 4621, NGC
5813 and NGC 5846 are taken from Cappellari et al. (2007b) with a formal
error of 10 per cent (1{sigma} CL), which is approximately converted
from the 30 per cent error at 3{sigma} CL.

2. 2008MNRAS.386.2242H
Re:NGC 3414
The black hole masses of NGC 2974, NGC 3414, NGC 4552, NGC 4621, NGC 5813 and
NGC 5846 are taken from Cappellari et al. (2007b) with a formal error of 10 per
cent (1{sigma} CL), which is approximately converted from the 30 per cent error
at 3{sigma} CL.

3. 2006MNRAS.369..497K
Re:NGC 3414
This disturbed galaxy (Arp 162) contains a kinematically decoupled component
(hereafter KDC; see Paper III) within the central 10 arcsec. The line strength
maps appear to have regular gradients.

4. 2006MNRAS.366.1151S
Re:NGC 3414
This peculiar S0 galaxy (Arp 162) shows a spiral pattern in the distribution of
the gas, which is more evident in the EW maps and is accompanied by a 90^deg^
twist of the velocity field. In the central regions, the gas rotates almost
perpendicularly with respect to the stars, as noticed by Sil'chenko & Afanasiev
(2004). The {sigma}_gas_ map show a very sharp peak, which is elongated in the
same direction as the zero-velocity curve, as in the case of NGC 2768. Weak
filamentary absorption features are visible in the southern part of this galaxy,
consistent with Tran et al. (2001).

5. 2005MNRAS.362.1319L
Re:NGC 3414
NGC 3414. This is a peculiar galaxy, which looks like a barred system with a
large oval, but different interpretations have been given of its true nature.
For example, Whitmore et al. (1990) suggested that it is a galaxy seen edge-on
with a large-scale polar ring in the R band, whereas according to Bagget, Bagget
& Anderson (1998; hereafter BBA98) and Chitre & Jog (2002) it might be a nearly
face-on galaxy with a prominent bar.

6. 2004MNRAS.352..721E
Re:NGC 3414
NGC 3414: A central counter-rotating component is visible in the
velocity map of this peculiar galaxy (Arp 162), with the h_3_ field
showing a corresponding sign reversal just outside this kinematically
decoupled structure. The decoupled nature of this central component has
not been previously reported in the literature, although long-slit data
exist (Bertola et al. 1995).

7. 2002AJ....124..675C
Re:UGC 05959
Low FIR fluxes (Knapp et al. 1989) suggest that the radio source is
powered by an AGN.

8. 2000A&AS..141..385V
Re:NGC 3414
C-35 = NGC 3414. (A,E,G,N) Has unusual isophotes, considered to be a box
or X-galaxy by Whitmore & Bell (1988), and faint extensions
perpendicular to the major axis suggest the possibility of a ring (PRC).
Has an optical LINER emission line spectrum (Ho et al. 1995, 1997) The
central stellar velocity dispersion is 253 km s^-1^ (see Prugniel &
Simien 1996, and references therein), and the maximum stellar rotation
velocity about 55 km s^-1^ (Lake & Dressler 1986). Three other objects
were found within the Nancay search area: (1.) NPM1G +28.0180 (Klemola
et al. 1987), a 16.1 mag object at a redshift of 1142 km s^-1^, at 2'
distance, (2.) NGC 3418, a 14.1 mag early-type (SAB(s)0/a:) spiral with
an optical redshift of 1251 +/- 52 km s^-1^, at 8.5' distance, and (3.)
UGC 5958, a 15.3 mag Sbc spiral at 7.6' distance, detected in H I at
Arecibo with a line flux of about 2.6 Jy km s^-1^ at a redshift of
1182 km s^-1^ with a FWHM of 185 km s^-1^ (Bicay & Giovanelli 1986;
Giovanelli et al. 1997; Schneider et al. 1986). The PRC object has a
well-established optical redshift of 1445 +/- 63 km s^-1^. Our Nancay and
Effelsberg spectra do not even show an overlap in velocity (the measured
mean velocities and {DELTA}V_20_ widths are 1173, 325: km s^-1^ and 1526,
322 km s^-1^, respectively), and the Effelsberg integrated line flux is
2.5 times smaller than the Nancay value. The two published Arecibo
profiles of the PRC object, which should be free of confusion with
NGC 3418 and UGC 5958, do not have any overlap in velocity either, as
their mean velocities and FWHMs are 1414, 330 km s^-1^ (Bieging &
Biermann 1977) and 1592, 256 km s^-1^ (DuPrie & Schneider 1996),
respectively. DuPrie & Schneider actually mapped the NGC 3414 group at
Arecibo and found no evidence of extended H I features within the group.

9. 1994CAG1..B...0000S
Re:NGC 3414
Feb 1/2, 1981
12 min
NGC 3414 is the single best example in the
RSA of a galaxy having a dominant central bulge
and a rudimentary disk of very low surface
brightness. The disk in NGC 3414 is of much
lower mass than the well-developed disks of S0
and spiral galaxies at every stage of the spiral
(disk) sequence.
The simplest conclusion, independent of the
details of the generally unknown process of
galaxy formation, is that disks form by dissipation.
In a dissipative collapse, the potential energy
of position in the protogalactic gas is radiated
away by atomic processes. This permits the gas
that has not turned into stars in an initial formation
episode to settle into a plane, forming a disk,
as is described in Chapter 4. Bulges and halos of
E galaxies have turned their protogalactic gas
into stars on a time scale short compared with the
free-fall collapse time, and no disk is formed.
Disks are dissipative structures; halos are not.
NGC 3414 is an important link between the
pure E sequence where no disks exist and the
disk sequence of the S0 and spiral galaxies. It has
a dominant bulge indicating rapid star formation
relative to the free-fall collapse time and therefore
little dissipation, yet it has the rudiments of
a disk, showing that some very small fraction of
the protogalactic gas suffered dissipation and
collapsed to the plane. The disk-to-halo ratio in
NGC 3414 is among the smallest of any galaxy in
the RSA.

10. 1994CAG1..B...0000S
Re:NGC 3414
Feb 1/2, 1981
12 min
[This is an example] of a rudimentary disk in a dominant bulge galaxy.

11. 1994AJ....107...99R
Re:NGC 3414
C-35 = NGC 3414. Our upper limit of 5.1 x 10^8^ M_sun_ with GB 140'
implies a small gas-to-light ratio of M_HI_/L_B_ <= 0.07. This galaxy
has unusual isophotes and is considered by Whitmore and Bell (1988) to be
a box or X-galaxy; it has three neighbors with separations within 10' and
redshifts within 300 km s^-1^.

12. 1994A&AS..105..481M
Re:NGC 3414
NGC 3414: A sharply tipped S-shaped feature, together with a large
twist, is interpreted as evidence for a spiral pattern in the disk of
this remarkable object. It forms the close pair Arp 162 with NGC 3418.

13. 1976RC2...C...0000d
Re:NGC 3414
= Arp 162
Pair with NGC 3418 at 8.2 arcmin. Faint diffuse bar in halo.

14. 1973UGC...C...0000N
Re:UGC 05959
SB(s)0? (de Vaucouleurs)
Arp 162
In Arp's class "galaxies with diffuse counter-tails, diffuse filaments"
See UGC 05958
UGC 05963 at 8.5, 12
Companion 2.0, 338, 0.4 x 0.4

15. 1964RC1...C...0000d
Re:NGC 3414
Classification doubtful.
Pair with NGC 3418 at 8.2 arcmin.

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