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Date and Time of the Query: 2019-05-22 T09:15:09 PDT
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Notes for object NGC 3949

9 note(s) found in NED.


1. 2007MNRAS.380..506G
Re:NGC 3949
NGC 3949 is an Sc galaxy belonging to the Ursa Major cluster. NGC 3949 presents
quite regular Fe5015 and Mgb line strength maps, peaking in an extended central
region and decreasing rather smoothly moving outwards. The H{beta} index is low
in the central region and higher in the surroundings; interestingly, it reaches
a minimum in a zone south of the centre where the emission line ratio [O
III]/H{beta} is particularly depressed (see relative figure in Ganda et al.
2006). The values measured for the H{beta} index are the highest in the sample,
as one can see from Table 2 and from Fig. A2. Ages (from the one-SSP approach)
are young (~=1.0 Gyr) in the central region, somewhat higher around it and
decreasing again towards the edge of the field. The metallicity is everywhere
low, and decreasing outwards.
Constant star formation cannot be ruled out; it is likely to characterize the
star formation mode over most of the field (see the {tau} map for age fixed to
10 Gyr in Fig. 10: {tau} assumes high values). Actually, when performing the fit
allowing the code to choose among exponentially declining and constant star
formation, constant is selected over most of the field.

2. 2005ApJS..160...76B
Re:NGC 3949
High discordance and fair S/N. Clear rotation and irregular {sigma}_*_ field.
Constant curve of growth. Significant high-velocity components in the central
LOSVD. Thin dust lane (Hughes et al. 2003). These are the first measures of
{sigma}_*_ in NGC 3949. See Figures 16 and 20a.

3. 2003AJ....126..742H
Re:NGC 3949
The morphological classification as determined by us is indicated in
parentheses next to the galaxy name, with our "chaotic circumnuclear
dust" (C) category now not including those galaxies with obvious dust
lanes (DL). Where the classification has already been made by Martini
et al. (2003), we indicate this with "-mp."
.
3.17. NGC 3949 (DL)
Figure 8 (bottom).
Spectra: Continuum only in the NUC spectrum. Only extended emission
lines are present in any of the spectra.
Images: Carollo et al. (2002) find a photometrically distinct nucleus,
a barlike feature, and a red dust lane 0.7" north of the nucleus. A
bar cannot be seen in these images; however, the thin dust lane is
clear in the STIS image and color map.

4. 2002ApJS..143...73E
Re:NGC 3949
NGC 3949.---SABcd (type example---see Fig. 3h): Very elliptical bulge.
Irregular, flocculent spiral structure in disk, with many filaments,
and knots of star formation.

5. 2002AJ....123..159C
Re:NGC 3949
Nuclear barlike feature (?); red (dust) lane ~0.7" N of nucleus

6. 1994CAG1..B...0000S
Re:NGC 3949
Sc(s)III
S-476-H
June 16/17, 1925
E40
40 min
NGC 3949 is in the highly complex Ursa
Major region, within which at least four separate
kinematic groups can be identified. The
lowest-redshift group contains the highly resolved
late-type spirals NGC 4144, 4214, 4244, 4449,
4736, and IC 4182. The mean redshift of this
group is = 285 km/s. The second kinematic
group at = 595 km/s is associated with
M51, and contains also NGC 4258, 4490, 4616,
and others. A group with near 750 km/s
contains NGC 3675, 3769, 3782, IC 750,
NGC 4051, 4242, and NGC 3949 shown here. The
fourth group is the great Ursa Major Cluster,
with about 980 km/s.
The image here of NGC 3949 is from a
Mount Wilson 60-inch plate. The surface brightness
of the disk is high. Useful resolution into
stars from the ground seems unlikely.
The redshift is v_o = 857 km/s.

7. 1976RC2...C...0000d
Re:NGC 3949
= Holm 301a.
NGC 3950 (Holm 301b) type EO: at 1.6 arcmin north.
Another companion 4.4 arcmin preceding.

8. 1973UGC...C...0000N
Re:UGC 06869
SA(s)bc: (de Vaucouleurs)
Companion 4.4, 273, 0.3 x 0.1

9. 1964RC1...C...0000d
Re:NGC 3949
= Holm 301a
Bright center. Several knotty bright arms. Poorly resolved.
NGC 3950 (= Holm 301b) at 1.6 arcmin noted as being a star in Ap. J., 91, 350,
1940 = MWC 626; however it appears to be nebulous on POSS chart.
Lund 9 dimensions are for the bright part only.


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