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Date and Time of the Query: 2019-08-19 T16:42:12 PDT
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Notes for object NGC 5533

7 note(s) found in NED.


1. 2007MNRAS.376.1513N
Re:UGC 09133
UGC 9133 (NGC 5533) has the most extended rotation curve in our sample, with the
outermost point in the rotation curve lying at a projected radius of 103 kpc
(>11 R-band disc scalelengths). With a rotation velocity at this radius of 225
km s^-1^, the total enclosed mass is 1.3 x 10^12^ M_sum_. Most gas at large
radii lies in a giant spiral arm which extends from the north-east side of the
gas disc and is warped with respect to the inner parts of the galaxy. Although
the arm is clearly rotating and the fitted position and inclination angles are
well behaved, the lack of symmetry in the arm makes it difficult to exclude the
possibility that the gas in the arm is not rotating at perfectly circular
orbits. Therefore, care should be taken with the rotation velocities outside R
~= 200 arcsec. Note, however, that we have assumed rather conservative values
for the uncertainty {DELTA}i in the inclinations, such that the corresponding
uncertainties {DELTA}V_i_ in the rotation curve (indicated with the shaded area
in the figures in Appendix C) also include, at least partly, the uncertainties
introduced by the orientation of the spiral arm. Note also that the residual
velocities with respect to the tilted ring model are small, indicating that the
non-circular motions are not dominant.
The optical observations do not have sufficient resolution to trace the rise
of the rotation velocities in the centre. Furthermore, a bright central
component complicates the interpretation of the spectrum in the inner few
arcseconds (see also Appendix B). At larger radii, however, the spectrum is
highly regular and symmetric.
The rotation curve of UGC 9133 keeps declining almost to the outermost points
in the H I rotation curve. The asymptotic velocity is about 25 per cent lower
than the maximum. Only at a radius of approximately 80 kpc does the rotation
curve flatten out.

2. 2005A&A...442..137N
Re:UGC 09133
UGC 9133 (NGC 5533) has a large one-armed spiral in the outer regions which
seems to be warped with respect to the main disk. The inner parts are highly
regular. The xv-diagram indicates that the rotation velocities are declining. In
the outer parts, this can be explained as a result of the warp, but the decline
sets in well within the radius of the warp and must reflect a truly falling
rotation curve.

3. 2001A&A...378..370V
Re:NGC 5533
NGC 5533: short Westerbork H I synthesis observations
(Broeils & van Woerden 1994) show that its radial H I distribution is
symmetric and that it extends out to 2.4 times the optical D_25_ diameter
of the galaxy (3.2'), measured at a surface density level of
1 M_sun_ pc^-2^. The integrated line flux measured at Westerbork
(35.3 Jy km s^-1^) is much larger than the Nancay and Green Bank single
dish fluxes (19 and 12 Jy km s^-1^, respectively), and the Arecibo flux
(8 Jy km s^-1^) is even smaller. The linewidths of the Westerbork and
single-dish profiles are comparable, however. The discrepancy between the
Westerbork and Green Bank line fluxes is puzzling, as the Green Bank
10.7' HPBW should cover the bulk of the H I emission, seen the
7.7' H I disk major axis measured at Westerbork.

4. 1996ApJ...473..117S
Re:NGC 5533
NGC 5533.--This large Sab galaxy is the earliest type in the sample. The H I
surface densities are rather low, and the distribution in the outer parts is
quite patchy. There are also significant side-to-side asymmetries in the outer
velocity field, as well as kinematic evidence for a warp (Broeils 1992).
Because of this and the low spatial resolution, the galaxy would not have met
the BBS criteria. The double-exponential bulge-disk decomposition was provided
by Y. C. Andredakis (1996, private communication) and implies that a large
fraction of the total light is in the bulge. However, the MOND fit to the
rotation curve requires that an even larger fraction of the mass be in the
bulge. This leads to a bulge M/L of seven and a disk M/L of about one (both in
the blue band). While the overall mass-to-light ratio of three in the blue
implies that MOND successfully accounts for the magnitude of the discrepancy
in this galaxy, near-infrared photometry would he of considerable interest in
this case to estimate the distribution of the stellar mass in the central
regions.

5. 1994CAG1..B...0000S
Re:NGC 5533
Sb(s)I
PH-720-S
April 6/7, 1954
103aO + WG2
30 min
NGC 5533 would closely resemble NGC 3642 (panel 126) if seen more
nearly face on. The type is early Sb. The form is somewhat later than
Sa and is certainly earlier than Sc; hence the classification is Sb by
elimination. The spiral pattern is of the MAS type, similar to that of
NGC 488 (Sab), but is later in the sequence.

6. 1973UGC...C...0000N
Re:UGC 09133
SA(rs)ab (de Vaucouleurs)
RC1 v and v0 refer to NGC 5529 = UGC 09127
Companion 2.6, 48, 0.3 x 0.1

7. 1964RC1...C...0000d
Re:NGC 5533
Very bright nucleus in a pseudo (r): 0.7 x 0.3 arcmin. Weak irregular outer
arms.
Lund 9 dimensions (0.9 arcmin x 0.9 arcmin) is an error or for nucleus only.


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