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Date and Time of the Query: 2019-04-20 T17:43:58 PDT
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Notes for object NGC 4819

7 note(s) found in NED.


1. 2009AJ....137.4450M
Re:NGC 4819
This galaxy has a relatively red optical color with {DELTA}(u - g) = -2.45 and
is better fit by a de Vaucouleurs profile. Consistent with these factors is its
(NUV -r) = 5.07, which is near the red sequence but potentially slightly offset
to the blue (see Figure 8). Its morphological classification in NED is
(R')SAB(r)a, and visually there is the suggestion of slightly blue patches of
its disk. Its synthesized spectrum from K_CORRECT is primarily that of a passive
galaxy, although with weak emission of [O II] and H{alpha}+[N II]. Prior studies
have indicated that it is highly H I deficient and only marginally detected in
H{alpha}+[N II] (e.g., Gavazzi et al. 2002), consistent with its red color and
fitted spectrum. The radio emission is compact and coincident with the nucleus
and not the disk, and this along with its red colors leads us to an AGN
classification. Alternatively, it might have very low residual star formation in
its nucleus (0.2 M_sun_ yr^-1^) prior to its landing on the red sequence.

2. 1999MNRAS.310...30C
Re:B2 1254+27
B2 1254+27
There is a large discrepancy between the positions given for this object
in the NASA Extragalactic Database (NED) and the SIMBAD Astronomical
Database. This is because the radio source has, in some cases, been
incorrectly associated with the galaxy NGC 4819 rather than with the
true host galaxy for the radio emission which is NGC 4839.
NGC 4839 is classified confusingly as morphological type S0 (Eskridge
& Pooge 1991), E/S0 (Jorgensen, Franx & Kjaegaard 1992) or as a cD
(Gonzalez-Serrano, Carballo & Perez-Fournon 1993; Fisher, Illingworth
& Franx 1995). Andreon et al. (1996) mention that the low average
surface brightness suggests that this galaxy is dominated by an extended
disc. The X-ray map of the source shows extended large-scale emission to
the south-west [described by Dow & White (1995) as being in the process
of interacting with the intracluster medium of the main (Coma) cluster].
This goes beyond the size of the optical galaxy and has been excluded
here so as not to affect the background emission. About 88 per cent of
the net counts arise from a point-like emission component.

3. 1997A&AS..126..335M
Re:B2 1254+27
1254+27 Using the 2.7 GHz polarization position angle in Parma & Weiler (1981),
we obtain a rotation measure of -165 rad m^-2^ (n=-2, see Sect. 4.1).

4. 1986A&AS...64..135P
Re:B2 1254+27
The radio galaxy belongs to the Coma cluster and is located at its
periphery. The optical image of the galaxy is very large (~ 1 arcmin) and
the optical center is therefore poorly defined.

5. 1976RC2...C...0000d
Re:NGC 4819
= Holm 490a
Pair with NGC 4821 at 1.8 arcmin.
In the Coma Cluster

6. 1973UGC...C...0000N
Re:UGC 08060
12 54.1 +27 13 = NGC 4821 at 1.9, 170, 0.5 x 0.3, v = 6974, v(0) = 6980, m=15.0

7. 1964RC1...C...0000d
Re:NGC 4819
= Holm 490a
Pair with NGC 4821 at 1.8 arcmin.
Color (P-V) = 0.86
Proc. 4th Berkeley Symp. No.Vol.III, 1960.


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