Date and Time of the Query: 2019-07-21 T13:03:31 PDT
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Notes for object NGC 2276

15 note(s) found in NED.

1. 2008MNRAS.388..500E
Re:UGC 03740
UGC 3740 (NGC 2276, Arp 25). Its spiral pattern is unusual, perhaps because of a
tidal encounter with the probable companion NGC 2300 (Karachentsev 1972) or more
likely, due to tidal stripping. Indeed, it is a member of a group where
stripping has been evidenced (Rasmussen, Ponman & Mulchaey 2006). The western
side of our H{alpha} imagE and the velocity field show compression due to
stripping by the intragroup medium. Our H{alpha} data also reveal low surface
brightness filaments extending towards the east, in agreement with James et al.
(2004). Our H{alpha} rotation curve is very peculiar and asymmetric. A steep
velocity rise is observed in the galaxy core. The width of the H I profile at 20
per cent (167 km s^-1^ from Springob et al. 2005) is slightly larger than our
H{alpha} velocity field amplitude. Nevertheless, the shape of our H{alpha}
rotation curve suggests that the maximum is reached just after the optical
radius (D_25_/2). The CO emission (Elfhag et al. 1996) is distributed in a
lopsided fashion, with more emission towards the north-western region.

2. 2005ApJS..157...59L
Re:NGC 2276
This Sc spiral galaxy at a distance of 36.8 Mpc shows unusual asymmetric spiral
patterns perhaps because of a tidal encounter with its E3 companion NGC 2300.
There are many bright knots on the spiral arms, some of them are known to be
recent supernovae. ULX1 is an extreme ULX on the spiral arm and close to a
bright knot. Its luminosity increased from (24 +/- 4) * 10^39^ to (34 +/- 8) *
10^39^ ergs s^-1^ in half a year.

3. 2005ApJ...630..269N
Re:NGC 2276
NGC 2276, NGC 6701.The narrow single-Gaussian line profiles for these galaxies
are likely due to viewing these spiral galaxies ~face-on.

4. 2003ApJS..146..353M
Re:NGC 2276
NGC 2276 (CS)
This is one of the galaxies in which we disputed the nuclear
classification. There is only one obvious dust spiral arm in the V-H
color map, although this is mostly because the nucleus is near the
edge of the H image. The V image clearly shows several additional dust
spiral arms to the south.

5. 2002AJ....124..675C
Re:UGC 03740
Asymmetric (cometary) radio source. Unusually low q =1.83 for a

6. 1999A&AS..138..253B
Re:NGC 2276
NGC 2276 - SNe 1962Q, 1968V, 1968W: no R band observations are
available. The first two SNe lie in crowded regions. South-east of
SN 1962Q a bright and compact patch of light is seen. At least four
relatively bright patches are identified at around the location of
SN 1968V. Further observations are needed (in the R band for example).
At the SN 1968W position some blue emission brighter than a 3{sigma}
magnitude is visible. The last supernova is close to the nucleus of the

7. 1996A&AS..115..439E
Re:NGC 2276
NGC 2276 is a spiral galaxy with multiple arm structure. We have mapped a
substantial part of the galaxy with 15" spacing. The CO is distributed in a
lopsided fashion with more emission towards the northwestern region. We have
also observed four positions 1' from the centre along both major and minor
axes but fail to detect any emission.

8. 1994CAG1..B...0000S
Re:NGC 2276
Karachentsev 127 [with NGC 2300]
Dec 4/5, 1939
60 min
NGC 2276 forms a pair with NGC 2300
(E3; panel 6). The redshifts measured by
Karachentsev are v_o(2276) = 2598 km/s and
v_o(2300) = 2332 km/s. The separation of 6.3'
corresponds to a projected linear separation of
90 kpc at the mean redshift distance of 49 Mpc.
The difference in morphological type of the
pair is particularly to be noted (Sc and E3) if the
two galaxies form a bound system. Other listed
nearby Dreyer galaxies are IC 455 (S0) and
IC 469. Many fainter early-type galaxies and
several candidates for dwarf dE galaxies also
exist in the field.
The image here of this field near the celestial
pole is from a plate taken with the Mount Wilson
60-inch telescope. For comparison, an image
from a plate taken with the Palomar 200-inch
Hale reflector is shown at the right.

9. 1994CAG1..B...0000S
Re:NGC 2276
Karachentsev 127 [with NGC 2300]
Nov 7/8, 1978
12 min
Compare the image of NGC 2276 taken with
the Palomar Hale 200-inch telescope in the print
here with that taken with the Mount Wilson
60-inch reflector in the print to the left.
The spiral pattern is unusual, perhaps
because of a tidal encounter with the probable
companion NGC 2300 (E3; panel 6), whose
projected linear separation is small at 90 kpc.

10. 1976RC2...C...0000d
Re:NGC 2276
= Arp 025
= VII Zw 134
= NB 85.4 (radio source)
= Kara[72] 127a
Interacting pair with NGC 2300 at 6.0 arcmin (= Arp 114).
Astrofizika, 4, 319, 1968.
Astrofizika, 6, 367, 1970.
Astrofizika, 9, 21, 1973.
Astrofizika, 6, 367, 1970.
Astrofizika, 9, 21, 1973.
Ast. Tsirk. No. 339, 1967.
Astrofizika, 3, 133, 1967.
Ast. Tsirk. No. 458, 1968.
Ast. Tsirk. No. 461, 1968.
Ast. Tsirk. No. 466, 1968.
Astrofizika, 4, 319, 1968.
Ast. Tsirk. No. 468, 1968.
Ast. Tsirk. No. 480, 1968.
Astrofizika, 9, 21, 1973.
HI 21cm: (extension towards NGC 2300)
A.J., 79, 767, 1974
Radio Observations:
M.N.R.A.S., 135, 149, 1967.

11. 1973UGC...C...0000N
Re:UGC 03740
Arp 25 (and 114, see UGC 03798), VII Zw 134
SAB(rs)c (de Vaucouleurs), Sc+ (Holmberg)
"Tubular arm, straight at first, then bent. Secondary arm from straight
portion" (Arp)
"Spiral somewhat peculiar, may be perturbed" (Arp, comment to number 114)
"Blue, badly disrupted post-eruptive Sc with many compact knots" (CGPG)
Paired with UGC 03798 at 7.5, 115, interaction
SN 1962q, SN 1968v, SN 1968w

12. 1971CGPG..C...0000Z
Re:CGPG 0710.0+8551
VII Zw 134
NGC 2276
Badly disrupted post-eruptive Sc with many compact knots.
= +2,391 km/sec. (Humason. 1956.)
m(pg) = 12.3 [CGCG]

13. 1964RC1...C...0000d
Re:NGC 2276
Small, very bright nucleus.
Weak bar.
Hexagonal pseudo (r): 0.52 arcmin x 0.43 arcmin.
Many knotty, filamentary arms.
Sharp outline.
Heidelberg Veroff. Vol. 9, 1926 dimensions for bright part only.
Paired with NGC 2300 at 6.3 arcmin.
A.J., 61, 97, 1956.
Ap. J., 82, 62, 1935.
Ap. J., 85, 325, 1937.

14. 1956AJ.....61...97H
Re:NGC 2276
HMS Note No. 036
Slit oriented through nucleus and emission patch 42 arcsec [north-west]
(HMS Plate IVj)
The smaller redshift is from absorption lines in the nucleus,
the larger from emission lines in the patch.
The difference of 101 km/sec probably is entirely accidental and
is not due to rotation, because the spiral is nearly normal to
the line of sight.

15. 1956AJ.....61...97H
Re:NGC 2276
HMS Note No. 037
The inclusion of this elliptical nebula with resolved nebulae
(Hubble, E.P. 1936, Ap. J., 84, 158. Table II)
was due to a misidentification of NGC 2300.
The object listed by Hubble is NGC 2276.

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