Date and Time of the Query: 2019-05-23 T05:15:49 PDT
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Notes for object NGC 2782

20 note(s) found in NED.

1. 2007ApJS..173..538T
Re:NGC 2782
NGC 2782 (Fig. 16.9).-The clearly disturbed ultraviolet and optical morphology
of this SAB(rs)a; Seyfert 1 starburst galaxy has been attributed to a previous
galaxy merger by Smith (1991). The merger remnant exhibits a very large,
double-sided H I tail (Smith 1991, 1997; Noordermeer et al. 2005) which has
modest extent directly east of the galaxy (coincident with low surface
brightness plume in DSS imaging) but more significantly reaches 5' to the
northwest in the form of a long curving feature. Our GALEX images show clumpy UV
emission within the NW tail, matching the morphology of the atomic gas, and a
component of more diffuse and redder UV light originating from the eastern H I
cloud. Smith (1991) reports that LSB ({mu}_B_ mag arcsec^-2^) optical emission
can be seen within the NW tail, but the UV clumps seen in our data are more
conspicuous and demonstrate that SF is occurring in the structure. SDSS image
data is not sensitive to the young clusters in the NW tail. NGC 2782 is the
brightest galaxy in a small group of four objects.

2. 2007A&A...468..129T
Re:NGC 2782
4.2.5 NGC 2782 - The X-ray source has 597 net counts. It can be seen in Fig. 4
that the extracted spectrum has a pronounced bump at energies below 1.5 keV
which is well fitted by a hot diffuse-gas model. The high energy region is
fitted by a power law which appears to be flat. The best fit ({chi}^2^_v_ = 1.0)
requires a gaussian component at 6.4 keV, (EW ~ 1.5 keV) with a
high-significance F-statistic value of 17.0 and associated random probability 3
x 10^-4^. FC shows that all 2000 simulated spectra lead to smaller F-values.
As in the case of NGC 3310, if the line energy is left free, XSPEC places the
line at 6.4 +/- 0.1 keV. Fitting a line at 6.7, rather than 6.4, keV requires
fixing all line components, the fit is clearly poorer ({chi}^2^_v_ = 1.4) and,
as the number of degrees of freedom is the same as without a line, the F-test is

3. 2005ApJS..157...59L
Re:NGC 2782
This ringed Sa spiral galaxy (at a distance of 37.3 Mpc) is a starburst galaxy
with tidal plumes/tails. ULX1 is an extreme ULX with L_X_ ~ 2 * 10^40^ ergs
s^-1^ and is located on the dusty plume near the disk.

4. 2005A&A...442..137N
Re:UGC 04862
UGC 4862 (NGC 2782) has a large, banana-shaped tail of gas northwest of the main
disk. The gas in the central regions is clearly disturbed as well and does not
show signs of regular rotation around the center. The optical image is peculiar
too, with some striking shells. These facts were already noted by Smith (1994),
who interpreted the peculiar structure as evidence for a recent merger of the
main galaxy with a low-mass companion. Schiminovich et al. (1995,1994) studied H
I in shells around elliptical galaxies. It seems not unreasonable to assume that
UGC 4862 is a similar case as their galaxies, but in an earlier stage of its

5. 2004A&A...415..941E
Re:NGC 2782
NGC 2782: Suggested by Jogee et al. (1999). As they point out, the evidence for
a nuclear bar is rather good, but the case for an outer bar (or outer oval, in
this case) is uncertain.

6. 2001AJ....121.2483U
Re:NGC 2782
NGC 2782. - Smith (1994) considered this galaxy to be in the process of
a merger. A separate component can be seen at a distance of 4 kpc from the
nucleus in the spectra of P.A. = 90^deg^ and 180^deg^. This component is
also seen in the H{alpha} image. While the [N II]/H{alpha} and
[S II]/H{alpha} ratios are constant for the spectra of P.A. = 90^deg^
(see also Fig. 1a), these ratios are enhanced on the southern region of
P.A. = 135^deg^ and P.A. = 180^deg^ (see also Fig. 1b). This region was
shown to be shock-excited by Boer, Schulz, & Keel (1992). Despite the
rather face-on appearance, the rotation curve rises steeply in the spectra
of P.A. = 90^deg^. The kinematics of this galaxy may be complicated as
proposed by Yoshida, Taniguchi, & Murayame (1999).

7. 2001AJ....121..710S
Re:NGC 2782
4.2. NGC 2782 and NGC 4438
At the other extreme from the NGC 7714/5 bridge in terms of CO
brightness is the eastern tail of NGC 2782 and the extra-disk gas
cloud near NGC 4438, with low L_H{alpha}_/M_H_2__ ratios compared to
the other features (see Fig. 4). These features have strong CO
emission, but little on-going star formation (Combes et al. 1988;
Kenney et al. 1995; Smith et al. 1999). None of the features in our
new sample are as rich in CO as the NGC 2782 and NGC 4438 features.
As discussed at length in Smith et al. (1999), the gas in these
features may be metal-rich material removed from the interiors of
their disks by near head-on collisions, leading to high CO fluxes.
Star formation may be inhibited in these features because of the
collision (Smith et al. 1999). Gas clouds pushed out of a galactic
disk by a high-velocity collision may compress and then adiabatically
expand, reducing their self-gravity. This may decrease the rate of
star formation and therefore the L_H{alpha}_/M_H_2__ ratio.

8. 2001A&A...378...51B
Re:NGC 2782
NGC 2782 (Arp 215): Smith et al. (1999) detected CO in what appears to be
the base of the eastern tidal tail. The tail seems dynamically separate
from the main galaxy but interpretation of the CO emission requires much
higher angular resolution.

9. 2001A&A...368...16M
Re:NGC 2782
9. NGC 2782 = Arp 215 is an isolated face-on Sa galaxy showing HI gas
plumes extending 5' to the east and 2' to the northwest (Smith 1991),
probably formed during a merger event. The eastern plume is associated with
a stellar tail of similar size. However, this feature is outside our 3'
field of view. The main disk of NGC 2782 is fairly undisturbed
(Jogee et al. 1998). Our residuum shows some irregularities near the
centre, which are probably due to the strong central star-formation region
(Boer et al. 1992; Jogee et al. 1998, 1998; Yoshida et al. 1999).

10. 1998AJ....116.2166U
Re:NGC 2782
This galaxy is sometimes classified as a Seyfert galaxy, but Boer,
Schulz, & Keel (1992) showed that the nuclear spectrum is typical of
nuclear starbursts and the high-excitation gas due to shocks is 4"-8"
south of the center. In the Carnegie Atlas, low surface brightness
components extend far beyond D_25_, and fragments of dust lanes in
spiral arms exist through the central bulge. Smith (1994) considered
this galaxy to be merging with a dwarf galaxy. H{alpha} emission is
strong in the central region and also seen on the northwestern arc. The
southern component corresponding to the high excitation gas is weak in
H{alpha} emission compared with the center.

11. 1997A&A...319...52V
Re:NGC 2782
NGC 2782 is a galaxy which, although it belongs to the original list of
Seyfert (1943), has been classified as a starburst galaxy by Sakka et al.
(1973) and Kinney et al. (1984) on the basis of the nuclear emission line
ratios; the [NII] and [SII] line strengths are however abnormally large for a
HII region; medium resolution spectroscopy revealed that the H{beta} and [OIII]
lines have dramatically different profiles, with [OIII] showing both a broad
core and high velocity wings (Kennicutt et al., 1989).

12. 1996ApJS..105...93E
Re:NGC 2782
4.5. NGC 2782
NGC 2782 (Arp 215) is a well-studied, peculiar, early-type spiral galaxy
containing a nuclear starburst and several H II regions reported by Hodge &
Kennicutt (1983). Using spatially resolved spectrophotometry, Boer, Schulz, &
Keel (1992) identify a shell of highly ionized material 4"-8" S of the central
starburst. They conclude that the local ISM is either shock heated or
photoionized by warmers (Terlevich & Melnick 1985). Smith (1994) has obtained
high-quality broadband BVRI images and presents a contour map of the brightest
H{alpha} emission.
Our data (Fig. 1) reveal diffuse H{alpha} emission covering the entire region
within ~14" of the nucleus, in addition to the emission detected by Boer et
al. A complex of bright but relatively diffuse H II regions is visible clearly
20"-25" N of the nucleus, and a string of bright, compact H II regions is
visible ~30" W of the nucleus. Fainter diffuse H{alpha} emission is detected
at larger radii.

13. 1996A&AS..115..439E
Re:NGC 2782
NGC 2782 is an "arm class 1" galaxy (Elmegreen & Elmegreen 1982b) which
implies chaotic appearance, no symmetry and fragmented arms with different
pitch angles. There is prominent diffuse optical component. The galaxy is an
X-ray emitter (Fabbiano et al. 1992). CO is detected with certainty only in
the central position. We failed to detect any emission outside 15" from the

14. 1994MNRAS.268..203C
Re:NGC 2782
NGC 2782 is a peculiar spiral galaxy classified as a starburst by many
authors (e.g. Balzano 1983). Boer, Schulz & Keel (1992) suggested the
highly excited gas to be due to a ~3 x 10^6^ yr old supernova-driven
nuclear outflow along the minor axis of the galaxy. The starburst
activity could have been triggered by the merger of two galaxies, at
least one of which was gas-rich (Smith 1991). The galaxy has a plume of
neutral hydrogen which extends to about 50 kpc (Smith 1991).
Radio continuum observations with the VLA C-array at 20 cm show the
source to be extended along a position angle of about 160^deg^. Higher
resolution observations with a restoring beam of about an arcsec show a
dominant compact component and radio emission both along and roughly
perpendicular to the plane of the galaxy (Wilson & Willis 1980; Condon et
al. 1982; Saikia et al. 1993). The compact component was not detected at
15 GHz with a resolution of 0.3 arcsec to a limit of 0.3 mJy beam^-1^
(Carral, Turner & Ho 1990). In our MERLIN image at 18 cm, the brightest
feature has a peak brightness of 0.19 mJy beam^-1^ and its position is
consistent with it being a nuclear component.

15. 1994CAG1..B...0000S
Re:NGC 2782
Sa(s) pec
Nov 4/5, 1978
IIIaJ + GG13
60 min
The two prints of NGC 2782 on this page
are made from the same original plate but are
printed to different contrast to show the faint
and the bright surface features, keeping the
blackness of the sky the same by darkroom
contrast-control techniques.
This demonstration shows that it is impossible
to judge levels of absolute surface brightness
by inspecting photographic prints using the
apparent surface brightness of the sky as reference.
Darkroom procedures can give any desired
relative intensity levels between object and sky,
and also within the different parts of an object.
An example is the plume to the main image in the
left print, where the feature appears to have
nearly the same surface brightness as parts of the
center. That this is not the case is seen in the
right-hand print, where the plume is nearly
No close companions to NGC 2782 can be
identified as a partner in a close encounter. No
companion galaxy can be seen as possible cause
of the plume. A few knots exist in the bridge that
connects the plume with the main body, but a
high rate of recent star formation in the plume
itself is absent.

16. 1994CAG1..B...0000S
Re:NGC 2782
Sa(s) pec
Nov 4/5, 1978
IIIaJ + GG13
60 min
NGC 2782 is classed as Sa pee on the basis
of the tightly wound and generally smooth spiral
arms in the main body shown in this lightly
printed image from the same plate used for the
print at the left. Bright knots, presumed to be
HII regions, are seen in one of the nearly circular
arms to the left of the bright central region.
Fragments of dust lanes in spiral patterns exist
throughout the central bulge. The luminous arms
are smooth in the outer part of the image visible

17. 1993ApJS...86....5K
Re:NGC 2782
NGC 2782; SAB(rs)a, starburst.
This starburst galaxy has a UV continuum and strong UV absorption lines
which resemble those in the spectrum of the starburst prototype NGC 7714
(Kinney et al. 1984). The nucleus is a strong, extended (1 kpc) radio
source, whose emission is probably due to supernova remnants from the
active star formation in the galaxy center. The star formation may be
triggered by the anonymous companion (Condon et al. 1982). However, the
source of the radio spectrum is controversial: Heckman et al. (1983) find
a nonthermal component in addition, leading to the composite
classification of LINER plus starburst. This idea is supported by Keel
(1984), who notes the flatness of the radio spectrum. The high
far-infrared luminosity and the strength of the CO emission support the
scenario of an intense burst of star formation (Sanders & Mirabel 1985).

18. 1976RC2...C...0000d
Re:NGC 2782
= Arp 215
Narrow emission lines; removed from Seyfert class.
Peculiar nucleus.
Interacting (?) pair with anonymous SB(s) sp at 11.8 arcmin.
Description and Photograph:
Publ. Dept. Astr. Univ. Texas, (II), 2, No. 7, 1968.
Publ. A.S. Japan, 25, 153, 1973.
Diameter of Nucleus:
A.J., 73, S175, 1968.
A.J., 73, 858, 1968.
Publ. A.S. Japan, 25, 153, 1973.
Photometry: (UBVRI)
A.J., 73, 866, 1968.
Publ. Dept. Astr. Univ. Texas, (II), 2, No. 7, 1968.
Photometry: (I.R.: 1.6 to 10 microns)
A.J., 73, 868, 1968.
Ap. J., (Letters), 159, L165, 1970.
Ap. J., (Letters), 176, L95, 1972.
M.N.R.A.S., 169, 357, 1974.
Spectrum and Spectrophotometry:
Publ. A.S. Japan, 25, 153, 1973.
Rotation Curve and Mass Determination:
J. Observateurs, 48, 247, 1965 = Publ. O.H.P., 8, No. 16.
Publ. A.S. Japan, 25, 153, 1973.
Radio Observations:
Astr. Ap., 15, 110, 1971. 33, 351, 1974.

19. 1973UGC...C...0000N
Re:UGC 04862
Arp 215, in Arp's class "galaxies with adjacent loops"
"Diffuse outer arms" (Arp)
SAB(rs)a pec (de Vaucouleurs)
Very broad asymmetric arm north-following

20. 1964RC1...C...0000d
Re:NGC 2782
Extremely bright nucleus. Smooth, broad bar with a strong dark lane.
Hexagonal pseudo (r): 1.0 arcmin x 1.0 arcmin. Asymmetric smooth arms with
dark lanes, asymmetric extensions extending out to 2.5 arcmin.
See also M.N.R.A.S., 74, 239, 1914.
Interacting(?) pair with anonymous SB(s) south-preceding at 11.8 arcmin.
C.R. Acad.Sc., Paris, 250, 2516, 1960.

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