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Notes for object NGC 1614

18 note(s) found in NED.

1. 2008ApJS..178..189W
Re:NGC 1614
A14. NGC 1614 (Arp 186, Mrk 617) Veilleux et al. (1995) classify the optical
spectrum of NGC 1614 as H ii, although the [N II] lines suggest a LINER
classification. Neff et al. (1990) find no direct evidence for an AGN component
in their 4.6 GHz maps. Fritz et al. (2006) fit the infrared spectral energy
distribution with a type II AGN model; however, these model fits suggest that
starburst emission is likely the dominant component at 880 {mu}m.
High-resolution radio, near-infrared, and mid-infrared imaging reveal a
star-forming ring with diameter 1.2" (Soifer et al. 2001; Alonso-Herrero et al.
2001; Neff et al. 1990). NGC 1614 is the only object in our sample besides Mrk
231 to show clear evidence of a nonthermal component from the ratio of its
millimeter continuum fluxes. The peak 880 {mu}m and 1.3 mm continuum fluxes are
almost identical (Tables 3 and 7). If we assume that any nonthermal component
depends inversely on frequency, then dust emission represents perhaps 60% of the
total 880 {mu}m flux and only 40% of the peak 880 {mu}m flux. However,
correcting for this putative nonthermal component produces the highest peak
gas-to-dust ratio of any galaxy in our sample (Table 7).

2. 2008A&A...488...83S
Re:MRK 0617
This is a strongly interacting galaxy in a late stage of the merging process,
which displays star forming regions observed in H{alpha}(Dopita et al. 2002).
X-ray spectroscopy suggests that Mkn 617 may harbor an obscured AGN (Risaliti et
al. 2000). VLBI studies did not detect a compact radio core (Hill et al. 2001).
The 11.7 micron image acquired by Miles et al. (1996) provided a similar
measurement of the size as the VISIR image (Fig. 2) but did not resolve the
detailed structure of the central 1", where individual clumps on top of a
diffuse component are detected. The radio emission follows the MIR morphology in
the outer parts, but this correlation no longer exists in the central sub-arcsec
region. However, differences may be related to insufficient spatial resolution
in the VLA map of beam size of 0.6" (FWHM).

3. 2006ApJS..164...52S
Re:NGC 1614
The 3.6 cm image of this galaxy consists of a strong point source, surrounded by
faint emission, extended by 25" in the E-W direction (Fig. 14, middle right).
The structure of the radio emission is similar to that seen in H{alpha} (Armus
et al. 1990).

4. 2006A&A...457...61R
Re:NGC 1614
NGC 1614. This is a strongly interacting galaxy in a late stage of a
merging process with spectacular tidal features. It is one of the four
starburst galaxies of our sample, also cataloged as a luminous infrared
galaxy (LIRG Alonso-Herrero et al. 2002). The HST/NIR camera and
multiobject spectrometer (NICMOS) observations reported by
Alonso-Herrero et al. (2001) show deep CO stellar absorption, tracing a
starburst nucleus about 45 pc in diameter surrounded by a ~600 pc
diameter ring of supergiant H II regions. The luminosities of these
regions are extremely high, an order of magnitude brighter than 30
Doradus. The spectrum presented in Fig. 2 agrees with the starburst
nature of this source. Only narrow nebular emission lines are detected,
all spectroscopically unresolved. The molecular H2 spectrum is
particularly weak. The continuum is dominated by stellar absorption
features, with strong CO bandheads in K and numerous CO absorptions in

5. 2004AJ....127..736H
Re:NGC 1614
A9. NGC 1614 NGC 1614 (Fig. 1i) is one of the most well-studied objects
in our sample. It is a strongly interacting galaxy in a late stage of
the merging process, with spectacular tidal features. Our H{alpha} image
has identical features to the H{alpha}+[N II] image by AHM and Dopita et
al. (2002): a bright nuclear source, the inner spiral arms, and H II
regions along the southwestern linear tail. The nuclear source is very
compact, and the nuclear ring (Alonso-Herrero et al. 2001) is not
spatially resolved in our image (with ~1.8" [~0.5 kpc] seeing).

6. 2002ApJS..143...47D
Re:IRAS 04315-0840
IRAS 04315-0840 (NGC 1614).---This object is a well-known galaxy
merger. Strong tidal arms can be seem in our R-band image, and our
H{alpha} image shows knots of star formation in the southern tidal
tail. We have classified this galaxy as H II region--like from
optical spectra (Kewley et al. 2001b). X-ray spectroscopy suggests
that NGC 1614 may harbor an obscured AGN (Risaliti et al. 2000), but
VLBI studies with a sensitivity limit of 0.9 mJy do not detect a
compact radio core in NGC 1614 (Hill et al. 2001).

7. 2000A&A...357...13R
Re:NGC 1614
NGC 1614: The spectrum of NGC 1614 is well fitted by a powerlaw with
{GAMMA} = 1.55 +/- 0.4, while a thermal component is rejected. There is
no evidence of an iron line. The measured 2-10 keV flux is
5.6 10^-13^ erg cm^-2^ s^-1^.

8. 1999AJ....118.2331V
Re:NGC 1614
Only a single 500 s F606W image is available for NGC 1614. We used
the nuclear offset, 6[&farcs;]6 east (Drissen et al. 1996), with a 2"
radius uncertainty, to isolate the environment of the SN Ic 1996D, which
is shown in Figure 13. The SN occurred along a bright spiral arm in the
vicinity of a number of stellar objects with median m_F606W_ ~ 24.5 mag
and several unresolved objects with m_F606W_ ~ 21.0 to 20.8 mag. For a
distance modulus to NGC 1614 of m - M = 34.02 (assuming cz = 4778
km s^-1^ and H_0_ = 75 km s^-1^ Mpc^-1^), these apparent magnitudes
correspond to M_V_ ~ -9.5 mag for the fainter objects and M_V_ ~ -13.0
to -13.2 mag for the brighter probable star clusters. The image data do
not allow us to be more specific about the stellar populations in the SN
site, other than to note the likelihood that these are recently formed
young, massive stars and star clusters.

9. 1999A&AS..136...35S
Re:NGC 1614
NGC 1614 -- A broad WR bump is detected by Pindao (1998). The
measurement of Vacca & Conti (1992) provides an upper limit on broad
He II {lambda}4686.

10. 1997ApJS..108..449G
Re:NGC 1614
The weather was marginal on this night. To correct for differences in the
brightnesses of the before-and-after star measurements, the fluxes and
error bars of the galaxy spectrum were multiplied by 23%. The line
luminosities from this corrected spectrum are in rough agreement with the
quantities calculated by Puxley & Brand (1994). However, although our
fitted continuum slope agrees with that of Ridgway, Wynn-Williams, &
Becklin (1994, hereafter RWB), we get a significantly smaller value of
CO_ph_ than either RWB or Doyon (1990). The CO index as measured from
the spectrum of Puxley & Brand (1994) is 0.19 (Puxley, private
communication), consistent with that measured by RWB and Doyon.
Examination of our continuum fit has failed to reveal any obvious errors
on our part in fitting the continuum. It appears that there is some
increase in flux to the red end of our spectrum. We speculate that very
poor cancellation of the atmospheric water vapor bands past 2.3 {mu}m
might be responsible for this effect. Our value of the CO index is quite
likely in error, and we suggest that the reader use a value of 0.19 for
the CO index.

11. 1996ApJ...465..191M
Re:NGC 1614
3.2. NGC 1614
An image of NGC 1614 at 11.7 microns is shown in Figure 6. The brighter source
has a disk of emission extending some 200-300 kpc away from the nucleus on all
sides except the northeast. The fainter source (3 {sigma} detection) to the
northeast (PA 38^deg^) is elongated approximately 200 kpc.
The telescope was guided by hand for this image since there was no nearby star
bright enough for the offset auto-guider. While the hand-guided PSF image has
a FWHM of 0.7" (Fig. 18), the longer exposure on the galaxy may have slightly
poorer resolution but no worse than 1".
Keto et al. (1992) imaged this galaxy at 12.5 microns with 1" resolution. They
found two nuclei of similar brightness, oriented east-west and separated by
~1", with an arm reaching north of the western component and then arching
over to the east. There seems to be no correspondence at all between their
image and ours, except that the general size of the galaxy is about the same
in both images.
The radio map by CHSS, with a resolution of 1.4", cannot provide information
on the detailed structure at this small scale. However, they do resolve the
galaxy, finding a FWHM size of 2" (600 pc), in excellent agreement with the
size scale of our observations. The radio image also shows a slight northeast
extension, consistent with the direction of the secondary source in the
infrared image.
Optical maps show distorted, asymmetric spiral arms with tidal tails emanating
from a possible double nucleus with separation ~2 kpc(Fig. 1; Armus, Heckman,
& Miley 1990).

12. 1996A&AS..115..439E
Re:NGC 1614
NGC 1614 is an IR-luminous merger with barred structure which has been
observed extensively in the optical, infrared and radio regions by Neff et al.
(1990). Interferometric observations of CO have been performed by Scoville et
al. (1989).

13. 1996A&AS..115..253L
Re:NGC 1614
NGC 1614 & Mrk 331: The 5" diameter of the aperture used to observe NGC 1614
and Mrk331 corresponds to ~2.5 kpc and to approximately twice the currently
estimated dimension of the galaxies' starburst cores (Neff et al. 1990; Zenner
& Lenzen 1993). This limits the contribution of the underlying spiral galaxy
population to the emission.
Both spectra have very similar continua and lines. Their common corrected CO
index of 0.29+/-0.02 magnitudes (in agreement with Doyon 1991, for NGC 1614),
confirms that CO is deeper in the two starbursts than in typical elliptical
galaxies (CO <= 0.24, see also Frogel et al. 1978). The molecular bands
throughout the H atmospheric window (third overtone CO and OH) appear dearly
on the smoothed average of the two spectra, also deeper than in elliptical
galaxies. The CO features indicate supergiants as the dominant contributors to
the near-IR emission. This is consistent with the H_2_O absorption, too weak
to allow for a large contribution from late-type M giants (see Sect. 42).
NGC 1614 and Mrk 331 both show strong Brackett {gamma} (4617 cm^-1^) and
[Fe II] (6083 cm^-1^) emission, with the same ratio [Fe II]/Br{gamma} ~1.3.
This value is typical for starburst galaxies (Greenhouse et al. 1991; Moorwood
& Oliva 1988). The He I to Br{gamma} ratio measured for NGC 1614
(0.44+/-0.20) is consistent with the measurement of Doyon et al. (1992). The
main difference between the two starburst spectra arises in the molecular
hydrogen lines, which are much stronger in Mrk 331.

14. 1993ApJ...412..535W
Re:NGC 1614
NGC 1614.-The position of the galaxy at 10 microns is within 1" of
Condon et al.'s (1990) radio position. The optical peak and the 2.2
micron peak were independently determined to lie within 1.5" of the radio
peak. Multiaperture photometry at 10 microns (Fig. 1) suggests a scale
length of order 300 pc, a result not inconsistent with the high value
obtained for the compactness (Fig. 3) and compatible with that implied by
Wright et al. (1988). The 10 micron size would thus appear to be
comparable to the 2" (600 pc) diameter measured by Neff et al. (1990) at
6 cm and the 0.9" diameter measured by Eales et al. (1990) at 2.2
microns. It is well within the 7" upper limit on the size of the
millimeter-wave Co emission (Scoville et al. 1989).

15. 1976RC2...C...0000d
Re:NGC 1614
= Arp 186
= II Zw 015
= MRK 0617
Note correction to NGC R.A.
IAU Symp. No. 29, 421, 1968.
Photometry: (I.R.: 5, 10 and 21 microns)
Bull. A.A.S., 4, 223, 1972.
Ap. J. (Letters), 176, L95, 1972.
IAU Symp. No. 29, 421, 1968.
Ap. J., 178, 113, 1972.
Discordant velocity (V_0 = 6706 km/sec from Source K3,
Ap. J., 160, 405, 1970) rejected.
Dynamics and Mass Determination:
Ap. J., 178, 113, 1972.

16. 1971CGPG..C...0000Z
Re:CGPG 0431.6-0841
II Zw 015
NGC 1614
Blue post-eruptive galaxy.
Compact patchy core.
Spiral plumes.
Long blue jet [south-south-west], m(pg) = 14.0
Spectrum: Emission: Balmer, [ 011], [ 0111].
= +6,790 km/sec.
Literature: Zwicky 1965a, Sargent 1970a.
m(pg) = 14.0

17. 1964RC1...C...0000d
Re:NGC 1614
Extremely bright nucleus.
2 main, massive bright arms.
Strongly asymmetric.
Faint outer streamer.
Radio Emission: (possible identification with Mills 04-012)
Australian J. Phys., 10, 162, 1957.

18. 1963MCG3..C...0000V
Re:MCG -01-12-032
These are probably two merged interacting galaxies. [1{back-s}fa]
and [sswa] spring from its two ends.

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