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Date and Time of the Query: 2019-05-27 T05:25:11 PDT
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Notes for object NGC 5033

29 note(s) found in NED.


1. 2009A&A...503..409H
Re:NGC 5033
The polarized emission in this galaxy is associated with the bright inner
continuum disk reported by Braun et al. (2007). It has a roughly X-shaped
appearance, which may be indicative of minor axis outflows, as seen elsewhere in
our sample. The polarized brightness declines to a minimum in the direction of
the receding major axis (PA = 352^deg^, as tabulated in Table 1). In the central
parts the polarized fraction is of the order of <~1%. At larger radii the
polarized fraction increases to about 5-7%. Although there are no well resolved
double radio sources in the field, at least one source is observed to be
somewhat extended with an RM of +9 +/- 2 rad m^-2^. The various other unresolved
sources in the field show scatter about this value.

2. 2008MNRAS.385..553D
Re:NGC 5033
NGC 5033: The H{alpha} velocity field displays a strong velocity
gradient (~100 km s^-1^ kpc-1) in the centre of this galaxy, agreeing
with CO emission (Helfer et al. 2003). The broad profiles found near the
centre of the galaxy are characteristic of a Seyfert galaxy. [O iii] and
H{alpha} observations show, respectively, an asymmetric morphology and
an off-centred active nucleus which can be understood in terms of a past
merger (Mediavilla et al. 2005). The H I large-scale velocity field is
well ordered and streaming motions can be seen near the spiral
structures (see Bosma 1981; Thean et al. 1997). The H{alpha} and H I
rotation curves present a constant rotational velocity of ~215 km s^-1^
and a warp developing beyond the optical disc.

3. 2007AJ....134..648M
Re:NGC 5033
NGC 5033 (Figs. 7.24, 9.24, 20.24): This galaxy shows an unresolved nucleus
together with an ionization cone open to the east (see Mediavilla et al.
2005). Heavy absorption to the west may be responsible for this asymmetry.
There is an interesting feature consisting of a bright bar of light coming
from the nucleus and extending 2" to the north. This might be
scattered light from the AGN or part of the extended narrow-line region.

4. 2004A&A...415..941E
Re:NGC 5033
NGC 5033: Suggested as a triple bar system by Laine et al. (2002). Martini
et al. (2001) did not find any bars in their analysis of the same images, and
Laurikainen et al. (2002) found no sign of a bar in their tangential-force
analysis of this galaxy using 2MASS images. Inspection of HST NICMOS1 and
NICMOS2 images (and a WFPC2 F606W image) shows extremely strong spiral dust
lanes in a highly inclined galaxy, with small, luminous bulge in center (see
also Martini et al. 2003). The K-band image of Peletier et al. (1999) does
suggest that the outermost bar of Laine et al. might be real, but the inner
ellipticity peaks are almost certainly due to dust.

5. 2003ApJS..146..353M
Re:NGC 5033
NGC 5033 (C)
While this galaxy was considered to have a nuclear dust spiral by
Martini & Pogge (1999), inclination effects make it difficult to
determine if these dust lanes actually form spiral structure.

6. 2003ApJ...583..145T
Re:NGC 5033
NGC 5033 (S1.5). A result on the same data set is presented in
Ho et al. (2001). The nucleus is significantly piled up in the Chandra
observation. The five off-nuclear sources shown in Table 3 are located
within the ASCA beam. The sum of the counts from these sources is less
than 44 counts in the 2-8 keV band, while 380 counts are detected from
the nucleus before correction for pileup. Therefore, the ASCA flux
(5.5 x 10^-12^ ergs s^-1^ cm^-2^; Terashima, Kunieda, & Misaki 1999;
Terashima et al. 2002) is probably larger than the true nuclear flux
by ~10% or less, unless the off-nuclear sources show drastic time
variability. We used the ASCA flux without any correction for the
off-nuclear source contribution. The 10% uncertainty does not affect
any of the conclusions.
.
We performed a spectral fit to the brightest off-nuclear source
(CXOU J131329.7+363523). An absorbed power-law model was applied, and
N_H_ = 0.40(< 1.2) x 10^22^ cm^-2^ and a photon index {GAMMA} = 1.5
+/- 1.1 were obtained.

7. 2002MNRAS.329..877C
Re:GB6 J1313+3635
120-redshift from Falco et al. (1999); spectrum in Ho et al. (1995);
classification (Sy1.5) from Ho et al. (1997).

8. 2002ApJS..139....1T
Re:NGC 5033
NGC 5033 (S1.5).-A detailed analysis of the ASCA data is presented in
Terashima et al. (1999). The ROSAT HRI image is pointlike (Koratkar et
al. 1995), as is the Chandra image (Ho et al. 2001).

9. 2002AJ....124..675C
Re:UGC 08307
The listed flux density includes the radio halo. CfA Seyfert 1
(Huchra & Burg 1992).

10. 2002A&A...389...68G
Re:NGC 5033
NGC 5033: a number of estimates are available for the
deprojection angles of this galaxy, and all cluster in a
relatively narrow range of values. The results of our two
methods are in good agreement between them and with the
rest of the estimates. The deprojection of the HII region
distribution is particularly sensitive to the adopted value
of the IA. We tired several averages of the individual
estimates both straight and weighted by our judgment of the
quality which resulted in identical values. We adopt these
mean values.

11. 2001ApJS..133...77H
Re:NGC 5033
NGC 5033 (S1.5). - Previous 6 and 20 cm VLA data show an unresolved
(Ulvestad & Wilson 1989; Collison et al. 1994; Kukula et al. 1995) or
slightly resolved (van der Hulst et al. 1981) core. Kukula et al. remark
that their C array 3.6 cm map contains extended emission on a scale of
30". Our 1" maps show a slightly resolved, steep-spectrum
({alpha}_6_^20^ = -0.52) core surrounded by a fluffy envelope with a
major-axis diameter of ~10" (0.9 kpc), roughly along the east-west
direction. The extended emission is more prominent toward the east. The
tapered maps further show a spectacular ridge of emission extended over
~40" (3.6 kpc), running nearly north-south, along the galaxy major axis
(P.A. = 170^deg^). This large-scale feature lies roughly orthogonal to the
10" structure.

12. 2001ApJ...562..139M
Re:NGC 5033
NGC 5033. - This nearly edge-on galaxy hosts a Seyfert 1.9 nucleus and
is conspicuously brighter in the NIR than at visible wavelengths,
suggesting that host galaxy dust contributes to the obscuration of the
nuclear region. The position angle of ~160^deg^ measured in the (poor)
elliptical isophote fits is in good agreement with the value measured by
Thean et al. (1997).

13. 2000ApJ...542..186N
Re:NGC 5033
NGC 5033.-FIRST lists a peak flux density of 1.4 mJy beam^-1^ at 20 cm
at a resolution of 5". The inner radio emission in the FIRST map is
extended in P.A. 91^deg^, along the minor axis of the host galaxy, and
there is an outer diffuse component that is more aligned with the host
galaxy major axis. Combining the FIRST peak flux density with our 2 cm
peak flux density (1.4 mJy beam^-1^) results in a nonsimultaneous
spectral index {alpha}_2_^20^ >= 0.

14. 1998PASJ...50..427S
Re:NGC 5033
NGC 5033: The nuclear component is superposed by a broad H{alpha}
emission feature from the unresolved nucleus, as wide as ~1000 km s^-1^.
The [N II] line does not suffer from this nuclear emission, and thus
better trace the kinematics. The [N II] PV diagram shows a steep rise of
rotation within ~ 2", and then a minimum at ~ 10", followed by flat
rotation at R > 15".

15. 1998ApJ...500..685P
Re:NGC 5033
9. NGC 5033.--NGC 5033 has a Seyfert type 1 nucleus in an Sac galaxy. The
optical images show bright H II regions in the inner spiral arms and giant star
formation regions in the spiral arms (Zaritsky, Kennicutt, & Huchra 1994). The
SED is reproduced with three distinct thermal components at 18, 40, and 151K.
The widths of these components are, respectively, 8, 16, and 40 K. The more
intense component is the cold one, in agreement with the presence of many
conspicuous star-forming regions in the disk of this galaxy.

16. 1997ApJS..112..391H
Re:NGC 5033
NGC 5033.--The nucleus of NGC 5033 has been detected in X-rays (Halpern &
Steiner 1983), and the emission comes from an unresolved source (Koratkar et
al. 1995). The very prominent and variable (Paper I) broad H{alpha} line,
originally noted by Shuder (1980) and Stauffer (1982), can be fitted fairly
accurately with a Gaussian of FWHM~2850 km s^-1^ (Fig. 14b). The narrow
components of H{alpha} and [N II], all of which show asymmetric wings, were
modeled using the [S II] lines. H{beta} also has a visible broad component.

17. 1997A&A...319...33A
Re:NGC 5033
NGC 5033 This Seyfert field, as shown in Fig. 10, contains a large number of
strong X-ray sources. The source C=25.5 represents the adjoining Seyfert
NGC 5005 discussed previously. Table 3 lists optical identifications for most
of the remaining sources.
Three of the X-ray sources, C=10.9 and the pair C=21.1 and 5.7, involve
multiple BSO candidates. If confirmed as quasars they would represent the
densest groupings of quasars yet discovered and continue the trend for such
tight groupings to fall near active, low redshift galaxies (Arp 1987 p64;
1995c). Two of these three groups of BSO's are well aligned and one, C=21.1,
has a blue galaxy central to the line of BSO's!

18. 1996ApJS..105...93E
Re:NGC 5033
4.11. NGC 5033
The late-type X-ray-bright spiral is classified as a Seyfert 1 on the basis of
observations of broad Balmer emission from the nucleus (Shuder 1980; Keel
1983c; Filippenko & Sargent 1985). Large (3') aperture H{alpha} + [N II]
{lambda}{lambda}6548,6583 photometry is reported by Kennicutt & Kent (1983),
while near (0.35-3.5 microns) infrared and IRAS photometry are presented by
McAlary et al. (1983) and Rodriguez Espinoza, Rudy, & Jones (1987),
respectively. Optical emission-line imaging is reported by several authors
(e.g., Keel 1983a; Elmegreen & Elmegreen 1983; Pogge 1989a).
Zaritsky et al. (1994) use optical spectrophotometry to estimate the abundances
of eight H II regions in the disk of NGC 5033, and they conclude that there is
a strong abundance gradient, with an inferred nuclear (zero radius) oxygen
abundance that is approximately twice solar. Our continuum-subtracted H{alpha}
image (Fig. 1) reveals the presence of bright H II regions in the inner spiral
arms down to a distance of ~5" from the nucleus. Giant extragalactic H II
regions clearly trace the spiral arms out to at least 4' radius, providing an
excellent sample for abundance measurements.

19. 1996ApJS..105...75C
Re:NGC 5033
4.2.6. NGC 5033
A patchy ring of H II regions shows up well in our H{alpha} + [N II] image
(Fig. 2f). The field of view of our CCD is small (5') compared to the large
optical size of the galaxy (~10' x 5'), so our H{alpha} + [N II] image is not
very useful for looking for emission from extraplanar gas. The morphology of
the H{alpha} + [N II] emission within the stellar (R-band) envelope is not
elongated along the minor axis. We did not find double-peaked line profiles or
any evidence for ELRs extending out of the disk in our minor axis spectra. This
galaxy has been very well studied, but we did not find any evidence in the
literature for a minor axis outflow.

20. 1995MNRAS.276.1262K
Re:NGC 5033
NGC 5033: Type 1(1.9). Host galaxy: Sc (UGC). Radio: the compact object in
the C-array map is slightly resolved and is surrounded by a region of
diffuse emission 30 arcsec (~1.5 kpc) in extent. The A-array image shows
a unresolved point source coincident with the peak of the C-array
emission, but with only half the flux. Ulvestad & Wilson (1989) report a
steep radio spectrum. The C-array map also shows a compact object 1
arcmin (3 kpc) to the south-west of the nuclear component. Although this
object lies within the bounds of the host galaxy it is unlikely to be
associated with the weak active nucleus, and has therefore been treated
as a field source in this survey.

21. 1995ApJS...98..477H
Re:NGC 5033
As mentioned in Paper I, the emission-line spectrum of NGC 5033 has
characteristics of both a LINER and a Seyfert galaxy. A comparison of
the spectra obtained at three different epochs (see Table 2) reveals that
the fairly prominent broad H{alpha} emission is variable. ROSAT
observations detected emission consistent with an unresolved X-ray source
(Koratkar et al. 1995).

22. 1994MNRAS.268..203C
Re:NGC 5033
NGC 5033 is an Sbc(s)I-II galaxy (Sandage & Tammann 1981) with signs of
Seyfert activity. VLA observations with a resolution of 54 arcsec show
that the flux density of the source is 178 mJy at 20 cm (Condon 1987;
Condon et al. 1990). VLA A-array observations show an unresolved
component with flux densities of 7 and 3.3 mJy at 20 and 6 cm
respectively (Ulvestad & Wilson 1989). The compact component has a steep
spectrum with {alpha} about 0.8 between 1.4 and 8.5 GHz.

23. 1994CAG1..B...0000S
Re:NGC 5033
Sb(s)I
PH-8034-S
Feb 3/4, 1981
103aO
12 min
The thinness and regularity of the multiple arms in NGC 5033 are
the characteristics of the high-luminosity class given to this
galaxy. The star-formation rate in the arms is moderate.
Many small HII regions exist in the arms. It is probable that
some of these images are individual stars as well; the redshift is
small, at v_o = 897 km/s, suggesting a distance modulus of about m - M
= 31. Brightest blue stars in galaxies reach absolute magnitude of
M_B_ = -10. Such stars in NGC 5033 will begin to resolve at B = 21,
which is well above the plate limit here.
Many intricate, thin dust lanes exist within the disk, seen best
in silhouette against the evident near side of the bulge.

24. 1993A&AS...97..887B
Re:NGC 5033
NGC 5033 was observed by S88 and SEC. The SEC intensity is closer to our
own. The rotation curve rises very sharply as the entire 450 km/s width
appears within 13" < 800 pc) of the nucleus and the central velocity is
essentially absent in the CO(2-1) spectra taken at radii of 10" along the
major axis. H{alpha} observations would be of interest to see if a
nuclear ring is present in this LINER (K83) or Seyfert 1 (SM). Strong
central 20 cm emission is present (C87, H87).

25. 1976RC2...C...0000d
Re:NGC 5033
= B2 1311+36
Photograph:
P.A.S.P., 82, 736, 1970.
A.J., 76, 22, 1971.
Photometry:
Bull. Ap. Inst. Duschambe, No. 48, 22, 1966.
Spectrum:
A.J., 76, 22, 1971.
Rotation Curve and Systemic Velocity:
Astr. Ap., 8, 364, 1970.
A.J., 76, 22, 1971.
SN1950C
P.A.S.P., 82, 736, 1970.

26. 1973UGC...C...0000N
Re:UGC 08307
SA(s)c (de Vaucouleurs), Sc- (Holmberg)
SN? 1957 (Carpenter, unconfirmed discovery)
See UGC 08256

27. 1964RC1...C...0000d
Re:NGC 5033
Small, very bright, diffuse nucleus in a bright bulge with a spiral pattern of
dark lanes. Several partially resolved, filamentary arms with branches.
HA 88, 2 dimensions: (6 arcmin x 3 arcmin) after Lick 13 for bright part only.
Unusual decline of (B-V) with log A/D(0), interpolated value.

28. 1956AJ.....61...97H
Re:NGC 5033
HMS Note No. 165
Auroral spectrum superimposed.

29. 1918PLicO..13....9C
Re:NGC 5033
A fine, rather open spiral 6' x 3' in p.a. 175^deg^. The nucleus is very bright,
almost stellar, and the portion near the nucleus is fan-shaped. The outer whorls
are rather faint, with a few almost stellar condensations. Well-marked
absorption effects on western side of major axis. See Abs. Eff.


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