Date and Time of the Query: 2019-06-27 T03:20:40 PDT
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Notes for object NGC 3049

9 note(s) found in NED.

1. 2006MNRAS.366.1265B
Re:NGC 3049
This Makarian galaxy harbours a "double nucleus", as stated by Nordgren et al.
(1995). This feature, invisible in IR, is easily seen in H{alpha} and it does
not seem to affect the galaxy's kinematics. The "second nucleus" is most
probably just a strong starburst H II region. Still, according to Nordgen, this
galaxy does not show any trace of merging. The galaxy is totally dominated by a
bar, and the signal is too weak outside the bar to resolve the kinematics,
rendering the extraction of kinematical parameters impossible.

2. 2000ApJ...531..776G
Re:NGC 3049
0952+095 = NGC 3049 = Mrk 710.-Kunth & Schild (1986) detected broad
N III {lambda}4640, He II {lambda}4686, and C IV {lambda}5808 emission
lines. A broad WR bump in the blue region was also seen by Vacca & Conti
(1992). Schaerer et al. (1999a) discussed the presence of
N III {lambda}4640, He II {lambda}4686, C III {lambda}5696, and
C IV {lambda}5808 broad features indicating the presence of early and
late WC and late WN stars. We confirm their findings. Additionally, we
find N III {lambda}4512, Si III {lambda}4565 and N V {lambda}4619
features, implying the presence of WNE and WNL stars.

3. 2000AJ....120..244B
Re:NGC 3049
NGC 3049: NGC 3049 is a barred spiral with clumps of star formation
(Contini, Considere, & Davoust 1998; Mazzarella & Boroson 1993 and
references therein). The radio emission is nonthermal. The total
spectral indices are -1.2 and -0.7 from 20 to 6 and 6 to 2 cm,
respectively, and the 6/2 spectral index as mapped ranges from -1.0 to
-0.6. This is typical of a classic starburst spiral galaxy. The radio
emission is entirely from the galaxy core; the weaker H{alpha} source at
(09^h^54^m^50.0^s^, 09^deg^16'24") has no radio counterpart.

4. 1999A&AS..136...35S
Re:NGC 3049
NGC 3049 -- This Virgo Cluster galaxy shows broad [N II] {lambda}5755
and He II {lambda}4686 (Kunth & Schild 1986). The WR bump is confirmed
by Mas-Hesse & Kunth (1991, 1998), Masegosa et al. (1991), and Pindao
(1998). Broad He II {lambda}4686 was detected in region A by Vacca &
Conti (1992); an upper limit is given for region B. The high S/N
observations of Schaerer et al. (1999) reveal broad features of
N III {lambda}4640, He II {lambda}4686, C III {lambda}5696, and
C IV {lambda}5808 testifying of the presence of late-type WN and
late-type WC stars. These features are confirmed by Guseva et al.

5. 1999A&A...341..399S
Re:NGC 3049
In NGC 3049 and NGC 3125, the W-R regions coincide with the peaks of
the continuum emission and nebular lines distributions. NGC 3049 is a
barred spiral galaxy belonging to the Virgo cluster. This low-mass
galaxy has a small bulge and a thin bar of constant surface brightness
surrounded by an inner ring (Contini et al., 1997). The optical
appearance of NGC 3125 is an amorphous elliptical shape with a bright
central starburst region dominated by two bright knots (regions A and B)
apparently connected by a bridge of fainter intensity.

6. 1999A&A...341..399S
Re:NGC 3049
In NGC 3049, the W-R region first noted by Kunth & Schild (1986) is
located in the bar, ~2.5" North-East of the galaxy nucleus (see
Fig. 2). The blue W-R bump is defined by two broad emission lines
identified as He II {lambda}4686 and N III {lambda}4640 +
C III {lamda}4650 (see Fig. 7), with approximatively the same
strength as already reported in previous observations (Kunth &
Schild 1986, VC92). In addition to the C IV {lambda}5808 line, a
broad (FWHM ~45 A) emission line of C III {lambda}5696 is also
detected at ~2{sigma} level in the spectrum of NGC 3049 (see
Fig. 8). After Phillips & Conti (1992) this is the second detection
of this W-R emission line in an extra-galactic HII region. The C III
emission is attributed to late WC stars, whose presence is indeed
expected in high metallicity regions (Maeder, 1991).

7. 1999A&A...341..399S
Re:NGC 3049
The predictions of the standard model (instantaneous burst, Salpeter
IMF) for the high metallicity region in NGC 3049 show an excellent
agreement with all observed W-R line strengths. This is also the case
for the C III {lambda}5696 feature (not shown here) which is only
detected in NGC 3049.

8. 1995ApJS...99..461N
Re:MRK 0710
Markarian 710 is a distinct barred spiral with the two nuclear sources
lying along the axis of the bar (Figure 5a). The brightest part of the
larger of the two nuclei lies to the southwest away from the direction of
the smaller second source. Table 3 and Figure 17 show source b to have an
H{alpha} flux of only one tenth that of source a. The northeastern end of
the bar kinks southward before three arms emerge and trail to the west
(this is most clearly seen in the H{alpha} image of figure 5b). From the
southwestern end of the bar, one very prominent arm loops to the east. At
a distance of 21 Mpc, the distance between the central sources is 0.6 kpc
(the entire length of the bar is on the order of five to six
kiloparsecs). The velocity difference between the sources is 20 (+/-54)
km s^-1^. Figure 5b shows the H{alpha} emission from Mrk 710. The two
central sources are connected by a thin bridge and from source b there
extends a faint knot to the northeast along the bar. Two knots connected
by faint emission trace out the northeastern arm, while the southwestern
arm is clearly composed of many clumps of emitting material. A faint
eastern arm, defined by three knots, extends east from source b, while a
western spur stretches west from source a.

9. 1993ApJS...86....5K
Re:NGC 3049
NGC 3049 (Mrk 710); SBbc, starburst.
This spiral galaxy belongs to the Virgo Cluster and is a starburst
(Balzano 1983) that has also been called a W-R galaxy. (a galaxy whose
spectrum exhibits the emission from Wolf- Rayet stars) by Kunth & Schild
(1986). Our UV spectrum does not show clear P Cygni profiles or He II
emission, as would be expected if W-R stars were present. The near-IR
emission has been attributed to a thermal source (Balzano & Weedman
1981). A discussion of the visible, UV, and far-infrared properties of
Mrk 710, together with a population synthesis model, can be found in
Mas-Hesse, Arnault, & Kunth (1989), who conclude that the present burst
of star formation is probably only about 5 Myr old.

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