Date and Time of the Query: 2019-07-18 T01:53:45 PDT
Help | Comment | NED Home

Notes for object NGC 4889

12 note(s) found in NED.

1. 2009AJ....137.3314H
Re:NGC 4889
The surface brightness profiles are from Jorgensen et al. (1992; dashed line)
and Peletier et al. (1990; solid line). For this galaxy, the results fall into a
familiar pattern whereby the GCS is moderately more extended (shallower) than
the halo light throughout the entire run of our data, though both have steeper
profiles than their counterparts in NGC 4874. Combined with the moderate
specific frequency and high metallicity distribution that we find for NGC 4889
(see below), we interpret it as a normal, though extremely high luminosity,
elliptical. For both NGC 4889 and 4874, much wider-field imaging with similar
depth will be needed to gauge properly how extended their cluster systems are at
larger radius, since for r >~ 5' they overlap each other rather heavily. The
hints from the current data are that the NGC 4874 system probably dominates more
and more at larger radii because of its shallower profile, but this remains to
be seen. Wider-field data are also the only way to assess the true contribution,
if any, of intracluster GCs within the Coma core. A roughly similar case has
been studied in the Hydra cluster (Wehner et al. 2008), where two giants NGC
3309 and 3311 sit close to each other in the cluster core and one of them (NGC
3311) is a central cD. With the right data, a numerical solution can be
performed to derive the two total GC populations and spatial distributions
simultaneously. For Hydra, the result shows that the cD NGC 3311 is dominant and
NGC 3309 unimportant; but in Coma, both the central giants have very large
cluster popula tions and the actual degree of overlap is not yet known.

2. 2009AJ....137.3314H
Re:NGC 4889
NGC 4889 For the second of the two supergiants, the GC radial density curve is
steeper. For this reason, it approaches much more closely to the background
(Figure 6) at the edges of the WFPC2 field, and so the the estimate of N_t_ can
converge reasonably. Using V < 27 and the global background, we obtain
{sigma}_b_ = 0.040 and a total of 3200 +/- 400 clusters for radii 4" < r < 150",
and add another ~= 50 for r < 4". Extrapolating over all magnitudes gives
N_t_ = 11000 +/- 1340. The outward extrapolation to account for clusters beyond
the observed field is a much smaller correction than for NGC 4874: we find with
r(max) the same as used for NGC 4874 above that it is necessary to increase N_t_
by at most 10%-15%, i.e., N_t_ ~= 12000 +/- 2000. With M^t^_V_ = -23.54 we
have S_N_ = 4.7 +/- 0.6. This result is squarely in the normal range established
by the giants in Virgo and Fornax; its huge total GC population simply goes
along with its very high luminosity.

3. 2008MNRAS.391.1009L
Re:NGC 4889
NGC 4889: a large cD galaxy with a very extended envelope. This is the brightest
galaxy of the Coma cluster. The surface brightness profile was published by
Peletier et al. (1990) and the HST imaging by Laine et al. (2003). The radial
velocity profile clearly shows a KDC.

4. 2000A&AS..141..449M
Re:NGC 4889
(2) D Galaxy GMP 2921 (NGC 4889) Weak H{beta} emission contaminates the
H{beta} absorption index in the center and at r ~ 8". The Mgb peak at
r ~ 4" is real as well as the differences of the index at different
sides of the galaxy. There is no evidence for further emission or
systematic errors in the continuum shape.

5. 1996A&AS..116..429A
Re:NGC 4889
1039 (= NGC 4889): A large cD galaxy with a very extended envelope. The field
of the CCD was not sufficient to extend the analysis to low SuBr.

6. 1996A&AS..116..429A
Re:NGC 4889
1039 (= NGC 4889): Global photometry cannot be obtained from small field
frames of this huge object.

7. 1996A&AS..116..429A
Re:NGC 4889
1039 (= NGC 4889): It is the eastern component of the famous pair of cD
galaxies near the cluster center. It displays a very extended envelope.

8. 1995ApJ...438..539F
Re:NGC 4889
The brightest galaxy in Coma, NGC 4889 has one bright lenticular and
two fainter galaxies within its envelope. On the basis of surface
photometry from PDIDC we classify NGC 4889 as a gE. Rood-Sastry cluster
type: B (Struble & Rood 1987).

9. 1994CAG1..B...0000S
Re:NGC 4889
Coma Cluster
May 25/26, 1965
103aD + GG11
30 min
NGC 4489 is the brightest galaxy in the
Coma Cluster and is the center of one of the two
main galaxy concentrations in the cluster. The
other is centered on NGC 4874 (panel 21). The
adopted redshift of the Coma Cluster is =
7143 km/s.

10. 1976RC2...C...0000d
Re:NGC 4889
= NGC 4884.
Brightest in Coma Cluster
Ap. J., 173, 485, 1972.
P.A.S.P., 80, 424, 1968.
Ap. J. (Letters), 169, L3, 1971.
A.J., 79, 671, 1974.
Ap. J., 139, 284, 1964.
Photometry (P,V):
A.J., 71, 635, 1966.
Photometry (UBV):
A.J., 73, 442, 1968.
A.J., 77, 642, 1972.
P.A.S.P., 80, 424, 1968.
Ap. J., 158, 657, 1969.
Ap.J., 173, 485, 1972.
Ap.J., 178, 1, 1972.
Astrophys. Lett., 5, 219, 1970.
Ap. J. (Letters), 169, L3, 1971.
A.J., 79, 671, 1974.
Dynamics and, Mass Determination:
Ap. J., 139, 284, 1964.
X-RAYS from Cluster
Ap. J., 146, 955, 1966. Ap.J., 183, 15, 1973.
Ap. J. (Letters), 167, L81, 1971.
Ap. J. (Letters), 173, L99, 1972.
Ap. J. (Letters), 183, L57, 1973.
Ap. J. (Letters), 185, L13, 1973.
Ap. J. (Letters), 193, L57, 1974.
Nature, 231, 107, 1971.
Bull. A.A.S., 6, 429, 437, 1974.

11. 1973UGC...C...0000N
Re:UGC 08110
E4 (de Vaucouleurs)
RA = 12 57 42, DEC = 28 14.7 (CGCG)
Following of 2 bright galaxies in the center of Coma I cluster
See UGC 08103
A large number of cluster galaxies near

12. 1964RC1...C...0000d
Re:NGC 4889
= NGC 4884
Misidentified as NGC 4872 in HA 88, 2.
NGC 4872 is 0.8 arcmin south-preceding.
NGC 4886 is 1.1 arcmin north-preceding.
Hubble, E. Obs. App. to Cosmology, Plate III, 1936.
Ap. J., 74, 36, 1931.
Ap. J., 135, 734, 1962.

Back to NED Home