Date and Time of the Query: 2019-03-19 T18:39:53 PDT
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Notes for object NGC 2623

14 note(s) found in NED.

1. 2008ApJS..178..189W
Re:NGC 2623
A12. NGC 2623 (Arp 243, UGC 4509) Heckman et al. (1983) classify the optical
spectrum as LINER. 8.4 GHz images from the VLA show a strong compact radio
source (Condon et al. 1991). Maiolino et al. (2003) classified this galaxy as an
obscured AGN using X-ray observations from Chandra. Near- and mid-infrared
images show a single compact nucleus (Scoville et al. 2000; Soifer et al. 2001).
The combination of the 1.3 mm continuum flux from Table 3 with the 880 {mu}m
continuum flux from this paper suggests that some small nonthermal component may
be present. If we assume the nonthermal emission scales inversely with frequency
and that the dust emissivity goes as {beta} = 1.5, then any nonthermal
contribution at 880 {mu}m would be less than 10% of the total.

2. 2004AJ....127..736H
Re:NGC 2623
A10. NGC 2623 NGC 2623 (Fig. 1j) is a nearly completed merger showing an
r^1/4^ profile at K band (Wright et al. 1990; Stanford & Bushouse 1991;
Chitre & Jog 2002) and two long tidal tails. Extensive observations of
this galaxy have been made from the X-ray to the radio. The radio
continuum (Condon et al. 1991), mid-infrared (Soifer et al. 2001), CO
(Bryant & Scoville 1999), and H{alpha}+[N II] (AHM) emission
distributions are dominated by a nuclear compact source. In our H{alpha}
image the nucleus also dominates the emission, and there is little
emission in the outer regions, except for a faint source ~8" (~3 kpc)
southeast of the nucleus.

3. 2000AJ....119..991S
Re:NGC 2623
NGC 2623 has a highly reddened nucleus with a possible short tidal
feature or spiral arm at ~1" radius to the southwest (seen best in the
1.1 micron image). In the optical, prominent tails are seen, suggesting
that this system underwent a significant merging event in the past
(Toomre 1977; Joseph & Wright 1985). However, at 1.6 and 2.2 microns,
the light profiles are smooth, following approximately an r^1/4^ law
(Wright et al. 1990; see below). The latter morphology suggests that the
galaxies that may have merged have coalesced into a common nucleus. A
weak VLBI radio core is seen in the nucleus of NGC 2623 (cf. Lonsdale,
Smith, & Lonsdale 1993). In CO (1-0) the emission complex is ~1.6" in
diameter with kinematic major axis east-west (Bryant & Scoville 1999),
similar to the reddening distribution shown in Figure 3.

4. 2000A&A...357...13R
Re:NGC 2623
NGC 2623: NGC 2623 was detected by the MECS at 3.5{sigma}, thus we can
only estimate the 2-10 keV flux, F_2-10_ ~ 8 x 10^-14^ erg cm^-2^ s^-1^.
The detection in the PDS is weak and cannot be associated with certainty
to NGC 2623, because of the presence in the PDS field (~ 100) of another
source that could emit in the hard X rays.

5. 1999ApJS..125..409C
Re:UGC 04509
UGC 04509. - The two northern components of this UGC "triple system"
straddle a compact ({THETA} < 0.7") radio source (Condon et al. 1990),
so we believe they are just two halves of a single galaxy (our
UGC 04509a) bisected by a dust lane to give the "appearance of fission"
(Nilson 1973).

6. 1998MNRAS.297..143R
Re:ARP 243
NGC 2623 (Arp 243), appearing eighth in the Toomre sequence, is, like Arp 220, a
superluminous IRAS galaxy, and is also very bright in the radio. Very long tails
are visible but the central masses have become indistinguishable. Only one true
nucleus is thought to exist.

7. 1996ApJS..104..217S
Re:UGC 04509
3.8. UGC 4509
UGC 4509 = NGC 2623 is a well-studied triple system included in Arp's atlas of
peculiar galaxies (Arp 1966). Bright tidal tails are observed in both the
optical and near-infrared; these tails suggest that a merger has occurred. The
parent nuclei have not been resolved in either the radio or near-infrared. The
K-band light profile is well fit by a {gamma}^1/4^ law out to a radius of 3 kpc
(Stanford & Bushouse 1991). The optical line ratios are more consistent with
those observed from LINERs than H II regions (Armus, Heckman, & Miley 1989).
Condon et al. (1991b) conclude that the emission is dominated by a compact

8. 1996A&AS..115..253L
Re:ARP 243
Other galaxies in Group I: The H + K spectra of Arp 243 and NGC 3690A & B are
obtained through apertures of 12", 8" and 12" respectively, and include
emission from large quiescent regions around the nuclei (Arp 1966; Stanford &
Bushouse 1991; Gehrz et al. 1983). Although the S/N ratios around 10 prevent
the use of the molecular features to identify the nature of the stellar
populations, the presence of CO absorption (clear in Arp 243, marginally
detected in NGC 3690) and the curved H band energy distributions indicate
predominantly stellar emission.

9. 1993ApJ...412..535W
Re:NGC 2623
NGC 2623.-The 10 micron peak coincides to within 1" with both the radio
peak and the visible peak of the galaxy. No sign of extended emission is
seen in the multiaperture photometry (Fig. 1). Eales et al. (1990)
reported that most of the 2 micron emission comes from a region smaller
than 1" (350 pc) in diameter.

10. 1985ApJS...57..643D
Re:VV 079
Very distorted spiral -- aftermath?
Nucleus is approximately 10 arcsec in diameter.
See Vorontsov-Vel'yaminov, B. 1977, Astr. Ap. Suppl., 28, 1.

11. 1976RC2...C...0000d
Re:NGC 2623
= Arp 243
= VV 079
Chaotic bright central part with
bright knots and two long streamers at opposite ends.
P.A.S.P., 77, 94, 1965.
P.A.S.P., 77, 94, 1965.

12. 1973UGC...C...0000N
Re:UGC 04509
VV 79, Arp 243
SBb (de Vaucouleurs)
In Arp's class "galaxies with appearance of fission"
Triple central region 0.55 x 0.45, 2 long curved streamers (or arms)
"Some very small bright knots resolved in interior" (Arp)

13. 1964RC1...C...0000d
Re:NGC 2623
Possible radio source (unconfirmed): see Humason et al. (1956).

14. 1959VV....C...0000V
Re:VV 079
= NGC 2623
V = +5,342 km/sec
Left photograph is by Baade: Vistas in Astronomy.
Right photograph POSS-1355B, on which the high velocity
S to the south is in contact with the small E.

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