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Notes for object NGC 7714

15 note(s) found in NED.

1. 2006ApJS..164...52S
Re:NGC 7714
The radio emission of this galaxy presents a strong point source at the nucleus
(Fig. 15, bottom) and some diffuse emission around it, extending by
approximately 30" in the NW-SE direction. This structure is similar to the one
seen in H{alpha} by Gonzalez Delgado et al. (1995).

2. 2006A&A...457...61R
Re:NGC 7714
NGC 7714. Is described by Weedman et al. (1981) as an archetype of the
starburst nucleus galaxies. According to Kinney et al. (1993), the
burst of star formation is thought to be caused by interaction with the
companion NGC 7715. The central region of about 330 pc has been the
site of active star formation at a rate of about 1 M_sun_ yr^-1^ for
some 10^8^ years (Brandl et al. 2004). NGC 7714 is also classified as a
Wolf-Rayet galaxy because of its strong He II 4686 Angstrom line
(Gonzalez Delgado et al. 1995). Recent Spitzer observations of this
object by Brandl et al. (2004) show that it has an H II region-like
spectrum with strong polycyclic aromatic hydrocarbon emission features.
No evidence of an obscured AGN was found. With very little silicate
absorption and a temperature of the hottest dust component of 340 K,
NGC 7714 is defined by Brandl et al. (2004) as the perfect template for
a young, unobscured starburst. However, we measured an E(B-V)=0.47 from
our spectrum, based on three different indicators , implying the
existence of dust along the line of sight to this source. Although it
has been extensively studied in the mid-infrared, see, e.g., O'Halloran
et al. (2000); Brandl et al. (2004); Dudley (1999), our SpeX spectrum
is the first one published with simultaneous JHK spectroscopy. Our data
shows unresolved emission lines of [S III], He I, H I, [C I], [Fe II],
and H2. The continuum emission is steep, decreasing in flux towards
longer wavelengths and dominated by absorption lines and bands across
the whole NIR region, the strongest ones being those of Ca II and CO,
including the bandheads at 23 000 Angstrom.

3. 2005ApJS..157...59L
Re:NGC 7714
This Sc spiral at a distance of 36.9 Mpc is interacting with its dwarf irregular
companion NGC 7715. ULX1 is an extreme ULX with L_X_ ~40 * 10^39^ ergs s^-1^ and
is located on the tenuous plume on the outer edge of a spiral arm in NGC 7714.

4. 2004MNRAS.355..728F
Re:NGC 7714
NGC 7714. Weedman et al. (1981) called this object a 'prototype
starburst' galaxy. van Breugel et al. (1985) noted the spectral
similarity of NGC 7714 to Minkowski's object and extragalactic H II
regions. They reported this galaxy as having weak WR emission features
near He II{lambda}4686. Conti (1991) called attention to the
importance of NGC 7714 for understanding the relation between
starbursts and the presence of WR stars in this type of galaxy. We
found WR stars in two regions of NGC 7714. In the nuclear region we
find WR/O = 0.08, while in the secondary H II region, WR/O = 0.14. In
the nuclear regions we were able to measure the C III{lambda}5696 and
C IV{lambda}5808 broad emission lines due to WC stars.

5. 2003ApJS..146....1W
Re:NGC 7714
NGC 7714.-This direction lies within the tip of the Magellanic Stream
and there is H I at = -316 km s^-1^. The high- velocity O VI component
lies at slightly less negative velocities. It may or may not be
associated with the Magellanic Stream.
Absorption in NGC 7714 is seen in the Ly{beta}, C II, Si II
{lambda}1020.699, Fe II {lambda}1144.938, and Fe H {lambda}1063.176
lines, centered at a velocity of 2725 km s^-1^. This places the
intrinsic Si II {lambda}1020.699 line at 1029.975 {angstrom}
(-565 km s^-1^ on the O VI velocity scale). This line therefore does
not contaminate the Galactic O VI.

6. 2002MNRAS.329..747T
Re:NGC 7714
4.5 NGC 7714 (Arp 284) Weedman et al. (1981) classified NGC 7714 as an
archetypal starburst galaxy, and it is well studied via optical,
ultraviolet and near-infrared spectroscopy (e.g. Garcia-Vargas et al.
1997; Gonzalez et al. 1999; O'Halloran et al. 2000; Kotilainen et al.
2001). The starburst is estimated to be 3-9 Myr old, and is known to contain
Wolf-Rayet stars. The optical and H I maps clearly show a bridge of
emission connecting the galaxy with its irregular companion NGC 7715,
1.9 arcmin away. Detailed VLA H I maps of the pair are presented by
Smith & Wallin (1992) and Smith et al. (1997). The peak in the H I is
offset from the centre of NGC 7714. This apparent offset is probably
due to the absorption of gas against the bright continuum source. The
850 micron emission associated with this galaxy is essentially
unresolved, but the peak in the emission is in reasonable agreement
with the peak in the 1.4-GHz emission (Condon 1990).

7. 2002ApJS..143...47D
Re:IRAS 23336+0152
IRAS 23336+0152 (NGC 7714).---This is a well-known starburst galaxy
which is part of a strongly interacting pair. The companion galaxy, NGC
7715, is ~1.9' to the west of NGC 7714. The diffuse glow in the lower
left-hand corner of the continuum image is due to light scattered from
a very bright star, just off the frame. Strong tidal features are
observed in the red continuum image, with a concentrated peak of red
continuum emission occurring in the center of NGC 7714. The red
continuum emission in the companion however, is much more diffuse. The
H{alpha} image is strikingly different from the red continuum image.
The companion is not seen in H{alpha} at all, and a strong tidal tail
is observed to the west of NGC 7714, which is absent from the red
continuum image. This is clearly a site of strong current star
formation. The nucleus of NGC 7714 is very strong in H{alpha}, and
several star-forming knots are observed to the northeast and
southeast, along the spiral arm.

8. 1999A&AS..136...35S
Re:NGC 7714
NGC 7714 -- Van Breugel et al. (1985) reported weak WR features near
4686A and possible nebular He II emission in the nucleus of this
"prototypical starburst" galaxy, and call attention to the similarity
with Minkowski's object (above) and extragalactic HII regions. New
long-slit observations at several position angles were obtained by
Gonzalez-Delgado et al. (1995), confirming the presence of broad
He II {lambda}4686 in the nucleus. Nebular emission can also be
suspected from their spectrum. From the same observations Garcia-Vargas
et al. (1997) find broad WR bumps (~4660A) in three extra-nuclear
giant HII regions. One of them shows a definite detection of
C IV {lambda}5808; for the remaining regions upper limits on
C IV {lambda}5808 are given. Pindao (1998) also signals the presence of
a broad WR bump; no information about the observed location given.

9. 1997MNRAS.286..183T
Re:UM 167
UM 167 (NGC 7741). This galaxy is an archetype of the starburst nucleus
galaxies (Weedman et al. 1981). The contour map of this starburst galaxy is
affected by a bright star in the south. Nevertheless, one can clearly see this
interacting pair, which consists of two spiral galaxies. They appear to be
bridged by their arms from the east of UM 167. The companion of UM 167 does not
show emission lines in the narrow-band images. The nuclear starburst in UM 167
is very intense and compact. It also has circumnuclear activity regions. A
detailed spectroscopic study of this starburst galaxy has recently been made by
the GEFE collaborators (Gonzalez-Delgado et al. 1995; Garcia-Vargas et al.

10. 1993ApJS...86....5K
Re:NGC 7714
NGC 7714 (Mrk 538); Sdm pec, starburst.
NGC 7714 is the prototype starburst galaxy (Weedman et al. 1981). The P
Cygni profiles of Si IV and C IV, whose absorption wings are blueshifted
by 1000 and 500 km s^-1^, respectively, manifest the presence of an
evolved population of massive post-main-sequence stars (Leitherer &
Lamers 1991). The burst of star formation is thought to be caused by
interaction with the companion NGC 7715. The spectrum shows evidence of
dust absorption at 2200 A. It might be dust intrinsic to NGC 7714, since
the extinction from our Galaxy (see Table 1) is not high enough to
produce the observed 2200 A feature.

11. 1976RC2...C...0000d
Re:NGC 7714
= MRK 0538
= Arp 284
= VV 051
= Holm 810a
= Kara[72] 587a
Interacting pair with NGC 7715 at 1.9 arcmin
A.J., 73, 890, 1968.
Ap. J., 153, 31, 1968.
Photometry (I.R. 2-10 microns):
Ap. J. (Letters), 159, L165, 1970.
Ap. J., 176, L95, 1972.
Bull. A.A.S., 4, 223, 1972.
Spectrum, Rotation Curve, and Mass Determination:
Ap. J., 153, 31, 1968.
HI 21cm:
A.J., 79, 767, 1974.
Radio Observations (NGC 7714 + NGC 7715):
M.N.R.A.S., 167, 251, 1974.

12. 1973UGC...C...0000N
Re:UGC 12699
VV 51a, Arp 284
SB(s)b pec: (de Vaucouleurs)
Paired with UGC 12700 at 1.9 following
"Some very small knots in connecting streamer" (Arp)

13. 1964RC1...C...0000d
Re:NGC 7714
= Holm 810a
Extremely bright nucleus. Bright, distorted, knotty lens 0.8 arcmin x
0.8 arcmin. One main smooth arm or loop. Outer extensions, one linking with
NGC 7715 at 1.9 arcmin.
Lund 6 and Heidelberg Veroff. Vol. 9, 1926 dimensions are for the lens only.
IAU Symp., No. 5, 1958 = Lick Contr. II, 82, 1958.

14. 1959VV....C...0000V
Re:VV 051a
= NGC 7714
V = +3,001 km/sec
For VV 051A there is {lambda}3727 and other emission
(Mayall, H., I.A.U. Symposium No., 1958).

15. 1956AJ.....61...97H
Re:NGC 7714
HMS Note No. 222
Slit simultaneously on nuclear regions of both members of close pair.
Strong early-type continuum with numerous emission lines, from which
the redshift was determined.

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