Date and Time of the Query: 2019-06-17 T02:10:53 PDT
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Notes for object NGC 5005

19 note(s) found in NED.

1. 2007AJ....134..648M
Re:NGC 5005
NGC 5005 (Figs. 7.55, 9.55, 20.55): The nucleus has both clumpy and diffuse
emission, with a very broad dust lane obscuring the north part of the image. A
spiral arm is visible to the south, with several isolated star clusters and
richer star-forming regions.

2. 2005ApJS..160...76B
Re:NGC 5005
Low discordance and excellent S/N. Clear, well-defined rotation and complex
{sigma}_*_ field. Highly variable curve of growth. Large inclination
(~67{degree}) and complicated dust morphology (Hughes et al. 2003).
These are the first measures of {sigma}_*_ in NGC 5005. See Figures 28
and 30c.

3. 2003ApJS..146..353M
Re:NGC 5005
NGC 5005 (C)
CO observations by Sakamoto, Baker, & Scoville (2000) of this highly
inclined LINER find 109 M_solar_ of gas within the central 5", and
both the V-H and V-I color maps of Pogge et al. (2000) show that there
is a large amount of chaotic, circumnuclear dust. The nucleus at V is
very indistinct, although the H-band image shows that the nucleus is
approximately coincident with the northernmost emission feature at V.
The peak at H is still south of the location of the radio and CO peak
shown by Sakamoto et al. (2000).

4. 2003ApJ...582..190D
Re:NGC 5005
NGC 5005.In the K band, this galaxy appears to have a strong bulge and
a fairly round bar. But there are two features that at first glance
appear inconsistent with this. First, there are two straight
structures parallel to the length of the bar; they make the bar appear
more elliptical than our estimate from isophote fitting. On closer
inspection they appear offset from one another, rather like dust
lanes. However, dust emission should not be prominent in the K band,
so these structures cannot represent dust lanes; their origin is thus
not clear and requires further investigation. An alternative estimate
of how round a bar is can be obtained from the bar strength parameter
Q_b_. E. Laurikainen (2002, private communication) found a low value
of Q_b_ = 0.16 for the bar strength in this galaxy. The second feature
is the velocity field, which exhibits prominent shocks that are
typically considered a feature of strong bars, not weaker bars such as
NGC 5005. However, using the Piner, Stone, & Teuben (1995) hyd
rodynamical code, we simulated a galaxy with a bar axis ratio similar
to NGC 5005 and found strong shocks similar to that observed. Thus we
conclude that despite the strong shocks, a weak bar with Q_b_ = 0.16
+/- 0.5 is possible.
The rotation curve of this galaxy is affected by beam smearing, which
is made worse by the high inclination angle of this galaxy
(61.4^deg^). Also, since the bar is fairly closely aligned with the
major axis in this galaxy, the position-velocity (PV) plot is affected
by the elliptical streaming of gas in the bar. This explains why the
rotation curve has a velocity at the bulge radius lower than that seen
in the PV diagram; this was also evident when we compared our rotation
curve with the PV plot of Sakamoto, Baker, & Scoville (2000). However,
the beam smearing effect is important for mainly the inner 2-3
beamwidths, which is well within the bulge radius for this galaxy.
Also, the effect of elliptical streaming is considerably reduced in
deriving the rotation curve because velocities are azimuthally
averaged over annuli. We thus believe our isophote measurement of the
bar ellipticity and the rotation curve determination of fmc are both
reasonable estimates for NGC 5005.

5. 2003AJ....126..742H
Re:NGC 5005
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."
3.30. NGC 5005 (C) (C-mp)
Figure 14 (bottom).
Spectra: Complicated emission-line structure. The continua are
generally weak. Emission does not extend to large distances.
Images: Complicated dust morphology.

6. 2002ApJS..143...73E
Re:NGC 5005
NGC 5005.---SBa: System is fairly inclined. Bright, elliptical bulge
with a flattened nuclear source. Bulge is threaded by a bar with a
P.A. skewed ~30deg from that of the bulge. The outer bulge isophotes
are boxy, and the bar crosses the diagonal of the bulge. There are two
ansae near the ends of the bar. Two very narrow spiral arms. The inner
arms have some evidence for star-forming knots and are quite open.
However, the outer arms tighten and appear to wrap several times
around the system. The outer disk shows an occasional knot, but there
is no coherent star-forming pattern associated with the outer arms.

7. 2002ApJS..139....1T
Re:NGC 5005
NGC 5005 (L1.9).-The ASCA data show the presence of a pointlike hard
X-ray nucleus with an X-ray luminosity consistent with that expected
from the H{alp[ha} luminosity (Terashima et al. 2000a). Furthermore,
comparison between the ASCA and BeppoSAX data (Table 15) indicates that
the 2- 10 keV flux has varied by a factor of 2.4 between the two
observations. These characteristics strongly suggest that the nuclear
source is an LLAGN. A soft X-ray image taken with the ROSAT HRI shows an
extended component (13% of the total flux; Rush & Malkan 1996) and is
presumably associated with the soft thermal plasma emission seen in
our ASCA spectrum.

8. 2000ApJ...542..186N
Re:NGC 5005
NGC 5005.-Vila et al. (1990) find S_20 cm_^peak^ = 14.6 mJy beam^-1^
and S_6 cm_^peak^ = 2.7 mJy beam^-1^ at resolutions of ~1.1" and ~1.0",
respectively (a spectral index of {alpha}_6_^20^ = -1.8). The source is
resolved at both wavelengths, in P.A. ~ 135 ^deg^ on a ~5" scale, again
more or less along the minor axis of the host galaxy. Hummel et al.
(1985) find a 20 cm peak flux density of 70 mJy beam^-1^ at 14"
resolution, with extended emission (about 2' extent) in P.A. 67^deg^,
along the major axis of the galaxy. FIRST also lists this source with a
peak 20 cm flux density of 35.9 mJy beam^-1^ (at 5" resolution), with
extended emission in P.A. 124^deg^. The relatively steep spectral slope
between 20 and 6 cm and the extended radio morphology at these
frequencies are consistent with our 2 cm nondetection.

9. 1999ApJS..124..403S
Re:NGC 5005
5.14. NGC 5005
The CO map shows a ring of diameter 1' (6 kpc) and a strong central
peak about 15" (1.5 kpc) in extent. The axial ratio of the ring, ~ 0.45,
is close to cos i = 0.47 (i = 62^deg^); hence, the ring is almost
circular when deprojected. The major-axis diameter of the ring is
comparable to the size of our field of view, which does not allow us to
rule out the possibility that the ring really is a pair of tightly wound
spiral arms going out of our primary beam from near the major axis. The
ring feature consists of several gas clumps of sizes 5"-10" (0.5-1 kpc).
The central concentration has a mass of M_gas_ = 2 x 10^9^ M_sun_. The
position-velocity plot shows a steep velocity gradient reaching the
maximum velocity of ~ 420 km s^-1^ (inclination-corrected) within a
radius of ~ 0.5 kpc. A dwarf active nucleus has been suggested within
the central gas concentration at the nucleus (Ho, Filippenko, & Sargent
1997a). Gasdynamics in this galaxy has been discussed at length in
Sakamoto, Baker, & Scoville (1999).

10. 1998ApJ...496..133B
Re:NGC 5005
NGC 5005.--The optical morphology of the nucleus is suggestive of a clumpy,
dusty starburst region. The faint patch of UV emission appears at the same
location as the peak of the optical emission.

11. 1997ApJS..112..391H
Re:NGC 5005
NGC 5005.--Despite the extremely complicated velocity structure and severe
blending of the narrow lines, once again caused by a steep gradient in the
inner rotation curve, a rather significant (f_blend_~33%; Fig. 14a broad
H{alpha} component is suggested if one requires that narrow H{alpha} and [N II]
have the same profiles as [S II]. The sizable residuals notwithstanding, it is
remarkable that such simple constraints can reproduce most of the features of
the complex blend.

12. 1997A&A...319...33A
Re:NGC 5005
NGC 5005 This Seyfert lies 4.1' NW of the Seyfert NGC 5033 (discussed in the
section after the following). NGC 5005 is smaller, has a much higher surface
brightness than NGC 5033 and a redshift 145 kms^-1^ higher. By the precepts of
Arp (1994) we could consider NGC 5005 as a companion to NGC 5033 and a
companion which is in a star bursting phase.
There are no strong pairs across NGC 5005 although there is an apparent line of
sources, C=27.8, 10.0, 3.8, 2.2, 3.3 and 3.5 coming through the Seyfert at p.a.
15^deg^. The two brighter sources are optically identified as a very compact,
bluish gal ~18mag. and an E=18.8 mag. BSO respectively. The fainter X-ray
sources are not reliably identified. No figure is shown here.

13. 1994CAG1..B...0000S
Re:NGC 5005
Hubble Atlas, p. 13
June 29/30, 1941
45 min
The spiral pattern in NGC 5005 is defined
mainly by dust lanes that exist throughout the
disk. The most prominent dust lane has a
different pitch angle than that of the general spiral
fragments. The dust lane cuts across the main
spiral pattern on one side of the image. The
feature is similar to that in NGC 4450 (Sab pec;
panels 110, S14 here; Hubble Atlas, p. 13). The
lane does not begin in the nuclear region but on
the periphery of the high-surface-brightness
inner lens.
The current star-formation rate is low
although finite; a few small HII regions exist that
are unresolved at the 1" level.

14. 1993A&AS...97..887B
Re:NGC 5005
NGC 5005 is one of the few galaxies where the CO is wider than the HI,
making CO(2-1) observations difficult. Either some mechanism is ejecting
dense gas at high velocity or the rotation curve rises very sharply
indicating a large central mass. H87 nuclear 20cm emission from this
LINER (K83).

15. 1976RC2...C...0000d
Re:NGC 5005
= Bol.2 1308+37
Mem. S.A. Ital., 38, 189, 1967 = Cont. Asiago, No. 194.
Photometry (5 Color):
A.J., 73, 313, 1968.
Dynamics, Rotation Curve, and Mass Determination:
Astr. Ap., 8, 364, 1970.
Ap. J., 184, 735, 1973.

16. 1973UGC...C...0000N
Re:UGC 08256
SAB(rs)bc (de Vaucouleurs), Sb+ (Holmberg)
Paired with UGC 08307 at 41., 133

17. 1964RC1...C...0000d
Re:NGC 5005
Extremely bright nucleus in a bright inner lens: 0.8 arcmin x 0.3 arcmin.
Several knotty arms with strong dark lanes.
Lund 9 dimensions (5.0 arcmin x 0.9 arcmin) are inconsistent.
Lund 10 and MWC 132 dimensions are for the bright part only.
Ap. J., 133, 815, 1961.
Ap. J., 46, 43, 1917 = MWC 132.
Ap. J., 135, 698, 1962.
Orientation, Rotation, Mass.
Ap. J., 97, 117, 1943.
Ap. J., 127, 487, 1958.
Ap. J., 133, 814, 1961.

18. 1961Hubbl.B...0000S
Re:NGC 5005
June 29/30, 1941
45 min
Enlarged 3.6X
This galaxy is not of the NGC 4569 type but is illustrated here
to show the prominent dust lane similar to the one in NGC 4450
(above). As in NGC 4450, the lane does not begin in the nuclear
region but rather on the periphery of the high-surface-brightness
central region. This central region is not amorphous
but contains a spiral structure traceable to
within 7 sec of arc (2 mm on the illustration) of the center.
Dust lanes and luminous spiral filaments are present to
within this distance. The rather abrupt change of surface
brightness from the outer to the inner spiral arms (which
occurs at a radius of 8 mm from the center on this illustration)
is similar to the same feature in NGC 5055 (pg. 15),
NGC 3521 (pg. 15), NGC 4699 (pg. 16), NGC 1068 (pg. 16), and others.

19. 1918PLicO..13....9C
Re:NGC 5005
A very bright spiral 5' x 1.5' in p.a. 68^deg^; bright, elongated nucleus. The
whorls are somewhat patchy, and show a few condensations. Several well-marked
dark lanes on the s. See Abs. Eff. 17 s.n.

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