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Date and Time of the Query: 2019-02-21 T17:09:03 PST
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Notes for object NGC 4144

6 note(s) found in NED.


1. 2007MNRAS.382.1552L
Re:NGC 4144
NGC 4144: There is no obvious nucleus in this galaxy. The spectrum of source 1
corresponds to the brightest knot seen in the optical images. The spectrum shows
low-ionization emission lines and significant absorption features from a young
population of stars. Source 3 corresponds to the brightest infrared peak and it
is located approximately 1 arcsec to the east of source 1. The spectra of
sources 1 and 3 are very similar. Source 2 corresponds to a high-excitation
star-forming region located 4 arcsec north from source 1.

2. 2000MNRAS.319...17L
Re:NGC 4144
NGC 4144: This galaxy was observed for the first time in X-rays, and no
emission was detected in the ROSAT HRI data. A 2{sigma} upper limit for a
point source located in the nuclear region of the galaxy can be found in
Table 5.

3. 1994CAG1..B...0000S
Re:NGC 4144
Canes Venatici II Group
ScdIII
PH-7147-S
Feb 1/2, 1976
103aO + GG13
30 min
Racine wedge
NGC 4144 is very nearby, judged by the
easy resolution into individual stars beginning at
about B = 20. The galaxy is in the complex Ursa
Major region wherein at least three separate
groups can be identified. The mean redshift is
about = 285 km/s for the CVn I Group, as
named by de Vaucouleurs (1975), where he lists
five members. The group is called B4 by
Kraan-Korteweg and Tammann (1979), where they list
21 members, including NGC 4144.
The second group in the Ursa Major region,
called the CVn II Cloud by de Vaucouleurs
(1975), has of about 750 km/s. It contains
such galaxies as NGC 3675 (Sb; panels 139, S4,
S13, S14) and NGC 4051 (Sbc; panel 180) as
listed by de Vaucouleurs (1975). It also contains
others such as NGC 4242 (SBd; panel 322),
IC 749/750 (SBc; Sb?; panels 195, 306),
NGC 3782 (SBcd; panel 328), and NGC 3949 (Sc;
panel 265). The third aggregate in the region is
the loose Ursa Major Cluster, with of about
980 km/s.
The redshift of NGC 4144 is small at 316 km/s.
The galaxy is clearly in the nearby B4 (or CVn I)
Group.
The spiral pattern can be discerned by the
characteristic hooks that bend in opposite directions
at the ends of the nearly edge on image.
Note that the plate was taken with a Racine
wedge; the bright stars have secondary images 5
mag fainter at 18" separation.

4. 1976RC2...C...0000d
Re:NGC 4144
HI 21cm:
Discordant Source R2 (Astr. Ap., 3, 292, 1969) rejected.

5. 1973UGC...C...0000N
Re:UGC 07151
SAB(s)cd? (de Vaucouleurs)

6. 1964RC1...C...0000d
Re:NGC 4144
Bright middle, no bright nucleus. Poorly resolved.
Lund 9 dimensions are for the bright part only.


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