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Date and Time of the Query: 2019-04-22 T07:12:27 PDT
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Notes for object NGC 3003

11 note(s) found in NED.


1. 2008MNRAS.388..500E
Re:UGC 05251
UGC 5251 (NGC 3003). As already noted by Rossa & Dettmar (2003), except in the
nucleus and in several bright H II regions, the H{alpha} emission is rather
faint and its distribution asymmetric, like the spiral arms of the galaxy. Such
an asymmetry suggests that this galaxy may be disturbed by a dwarf companion.
The velocity field is also rather asymmetric. No H I velocity field is
available. The width of the H I profile at 20 per cent (305 km s^-1^ from
Springob et al. 2005 and 289 km s^-1^ from Bottinelli et al. 1990) is slightly
higher (by ~30 km s^-1^) than the velocity amplitude of our H{alpha} velocity
field. Thus, the maximum rotation velocity is probably not reached with our
H{alpha} rotation curve.

2. 2003AJ....126..742H
Re:NGC 3003
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."
.
3.10. NGC 3003
Figure 5 (top).
Spectra: Strong emission in H{alpha} and other lines is obvious in the
OFF 2 and NUC spectra. There is no obvious signs of rotation. The
continuum is weak in each spectrum.
Images: Three cluster-like features in the center. The location of the
nucleus is not obvious.

3. 2003A&A...406..505R
Re:NGC 3003
NGC 3003 NGC 3003 has been investigated spectroscopically by Ho et al.
(1995) in search of dwarf Seyfert nuclei, who concluded, based on a
detected broad emission complex centered at {lambda}4650 {Angstrom},
that this galaxy is a Wolf-Rayet galaxy. NGC 3003 has a modest
L_FIR_/D^2^_25_ ratio (1.65), however, the S_60_/S_100_ ratio of ~0.34
hints that there is some SF activity due to enhanced dust temperatures.
Furthermore, due to the slight deviation from its edge-on character, no
extraplanar emission can be identified reliably. The H{alpha}
distribution, however, reveals strong planar DIG, consistent with the
observations by Hoopes et al. (1999). Several bright emission knots can
be discerned. About four decades ago a SN has been detected 34"E, and
17"N of the nucleus (SN 1961 F).

4. 1999ApJ...522..669H
Re:NGC 3003
The morphology of this galaxy (Fig. 2) suggests that it may be
disturbed, in that the spiral arms appear asymmetric. There is a small
dwarf galaxy (or possibly a background galaxy) at the lower right edge
of Figure 2, but other than this there are no close companions visible
in our images, which cover an area of 300 x 300 kpc at the distance of
NGC 3003. However, just outside of our field of view is the small spiral
NGC 3021. These two galaxies are separated by about 200 kpc in projected
distance and about 50 km s^-1^ in velocity (Tully 1988). The total
H{alpha} luminosity of 1.18 x 10^41^ ergs s^-1^ indicates that active
star formation is ongoing. This H{alpha} luminosity is about an order of
magnitude higher than for the starbursts NGC 253 and M82. In fact, of
the galaxies observed by Young et al. (1996), one of the largest sample
of galaxies observed in H{alpha} in the literature, only six of the 120
spirals have higher observed H{alpha} luminosities than NGC 3003 (not
corrected for extinction). The H{alpha} image shows a bright nucleus and
many bright H II regions, including a very bright region in the outer
western part of the disk. A projected spiral arm protrudes below the
galaxy in the image, with a bright H II region at the end. The
H{alpha}-emitting disk is about 35 kpc across. The galaxy is not quite
edge on, so it is difficult to make any statements about the vertical
extent of the DIG, though there is pervasive diffuse emission in the
disk.

5. 1999A&AS..136...35S
Re:NGC 3003
NGC 3003 -- A complex broad WR-bump was signaled by Ho et al. (1995),
who also note the absence of a broad H{alpha} component in contrast to
their spectra of other WR galaxies (cf. NGC 1156, NGC 1569, NGC 4214).

6. 1995ApJS...98..477H
Re:NGC 3003
The blue spectrum shows a broad emission complex centered at 4650 A,
indicating that NGC 3003 is a W-R galaxy. Unlike other objects in this
class (e.g., NGC 1156, NGC 1569, NGC 4214), the H{alpha} emission line
does not show an obvious broad component.

7. 1994CAG1..B...0000S
Re:NGC 3003
Sc(s)II
PH-7958-S
Nov 8/9, 1980
103aO
12 min
NGC 3003 is seen nearly on edge, making
its spiral pattern difficult to trace. The absence
of a halo and the smallness of the central nucleus
is evident.
The redshift of is v_o = 1461 km/s.

8. 1976RC2...C...0000d
Re:NGC 3003
SN1961F:
Contr. Asiago No. 174, 1965.
"Stars and Stellar Systems", Vol. VIII, 396, 1965.
Photograph:
Contr. Asiago No. 174, 1965.
"Stars and Stellar Systems", Vol. VIII, 396, 1965.
Spectrum:
Ann. Ap., 27, 300, 1964.
Coll. Int. "Novae & SN", CNRS, Paris, 175, 1965.

9. 1973UGC...C...0000N
Re:UGC 05251
Sbc? (de Vaucouleurs), Sc (Holmberg)
SN 1961f

10. 1964RC1...C...0000d
Re:NGC 3003
No definite nucleus. Bright middle. Dark markings and knots. Filamentary
arms. Classification is doubtful, possibly SB(s)d.
SN 1961:
Sov. A.J., 220, 1961.
IAU Circ. 1753.

11. 1918PLicO..13....9C
Re:NGC 3003
Rather bright; 6' x 1'; faint nucleus. An irregular spiral with very clearly
marked absorption effect on the s. side. See Abs. Eff. 41 s.n.


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