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Date and Time of the Query: 2019-04-24 T07:03:48 PDT
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Notes for object NGC 5529

9 note(s) found in NED.


1. 2005MNRAS.358..481K
Re:NGC 5529
NGC 5529. The inner fitting boundary was positioned beyond the region that shows
strong non-circular motions in H{alpha} (see Paper III). The circular velocity
curve is unknown in this region. Therefore, models were constructed for two
extreme cases, taking a solid-body and a flat rotation curve (down to R= 0). The
solid-body rotation is adopted here because it better matches the stellar
rotation at radii smaller than the inner fitting boundary. The results for the
flat curve yield a product [IMAGE] and {sigma}_R_(h_R_) = 98 km s^[IMAGE]1^,
consistent with the values for the solid-body curve (Table 3). The models
overpredict the velocity dispersions measured in the outermost bins and cannot
reproduce the strong asymmetries (h_3_ and h_4_). These features in conjunction
with the high disc 'temperature'{sigma}_R_(h_R_)/v_max_[IMAGE] 0.4 constitute
further evidence that the disc is strongly perturbed.

2. 2004MNRAS.352..768K
Re:NGC 5529
NGC 5529. This spiral is probably barred (Paper III, appendix). In
addition, its H I layer is warped, and, like the stellar disc, strongly
perturbed on the approaching side. Hence, it is likely that a
substantial fraction of the H I follows non-circular orbits, at least in
the inner parts (R <~ 50 arcsec). In that region, the extreme-velocity
envelope is not representative of the circular velocity curve. On the
approaching side, the envelope rises sharply and peaks at a velocity of
approximately 290 km s^-1^ at R ~ 90 arcsec. Further out, at R ~ 120
arcsec it shows a steep drop with a minimum of 245 km s^-1^, which is
followed by a gradual increase. Two small companions are located south
of and close to the perturbed H I layer at a velocity close to the
systemic velocity of NGC 5529. Interestingly, these companions are
connected to the main galaxy via low column density H I bridges (see
also Section 3.4). On the receding side, the envelope is less steep but
again shows a local minimum at R ~ 120 arcsec. The H I on the receding
side is also warped. It further shows a faint extension to larger
projected radii with an H I mass of approximately 3.1 x 10^8^
M_sun_. This gas cannot be identified with an optical companion and may
be part of the warped H I layer.

3. 2004MNRAS.352..768K
Re:NGC 5529
NGC 5529. MCG +06-31-085a is located at a projected distance of 3.5
arcmin (2.5 arcmin from the galaxy plane) and is connected to NGC 5529
via an H I bridge. The H I associated with this bridge amounts to
approximately 6.5 x 10^8^ M_sun_. Companion B is found at a projected
distance of approximately 30 arcsec from the plane of NGC 5529 and also
appears to be connected to NGC 5529 via a bridge.

4. 2004MNRAS.351.1247K
Re:NGC 5529
NGC 5529. The velocity curve is asymmetric. On the approaching side, it
reaches a distinct plateau at projected radii around 10 arcsec, then
rises sharply and slowly flattens out to the last measured point at 3
scalelengths. The central velocity dispersion is the largest in the
sample, and declines slowly with projected radius. The h_3_ and h_4_
parameters reveal very strong asymmetries in the velocity profiles and
show several sign reversals with projected radius.

5. 2003ApJS..148..383M
Re:NGC 5529
A15. NGC 5529 An H{alpha}+[N II] image of NGC 5529 is shown in Figure
15. This Sc-type galaxy is reported to be perfectly edge-on. It is also
one of the farthest galaxies in our sample, so resolving HII regions is
a challenge. The two bright knots 1-2 kpc west of the nucleus and 2-3
kpc above and below the disk of the galaxy are stars that did not
completely subtract out. Given an inclination angle of 90deg, there
appears to be faint (EM = 2-5 pc cm^-6^), widespread extraplanar gas
over the inner 10 kpc of the galaxy, but not nearly as bright as has
been detected in NGC 891. No obvious plumes or filaments are detected.
The total H{alpha} luminosity /D^2^_25_ is only 0.8 x 10^37^ ergs s^-1^,
kpc 16% of which is attributed to extraplanar gas. The scale height of
the gas is greater on the southeast side (6.8 kpc) than that on the
northwest side (4.5 kpc). But both of these numbers are uncertain
because they are based on the detection of very faint emission. The
total ionized mass associated with this extraplanar gas is 2.0 x 10^8^
M_{sun}_, considerably higher than most galaxies (but then NGC 5529 is
one of the larger galaxies in the sample, with an optical radius of 78.8
kpc). Both the large deviations of the extraplanar gas from the average
vertical profile and the strong correlations between disk and halo
emission suggest that the northeast side of the galaxy is characterized
by filamentary eDIG.

6. 2001A&A...378..370V
Re:NGC 5529
NGC 5529: short Westerbork H I synthesis observations (Rhee & van Albada
1996) show an H I diameter of 6.6' at a surface density level of
1 M_sun_ pc^-2^, the same as its optical D_25_ diameter. Their
position-velocity map indicates that the Nancay beam with its 3.6' E-W HPBW
does not cover all of the H I emission of this edge-on E-W oriented spiral.
In fact, our line flux value of 26.4 Jy km s^-1^ is significantly lower
than the 36.3 Jy km s^-1^ measured at Westerbork, while the latter is in
agreement with ~40 Jy km s^-1^ measured at Green Bank and Jodrell Bank,
whose beams should cover the entire H I disk.

7. 1973UGC...C...0000N
Re:UGC 09127
Sc: (de Vaucouleurs)
14 13.6 +36 24 at 3.8, 146, 0.6 x 0.35, m=15.7
Companion 3.5, 244, 0.9: x 0.6:, dwarf irregular

8. 1964RC1...C...0000d
Re:NGC 5529
Very poorly resolved. Almost exactly edge-on.

9. 1918PLicO..13....9C
Re:NGC 5529
Edgewise spiral 6' x 0.6' in p.a. 115; central portion is brighter, but no
nucleus is apparent. See Abs. Eff. 47 s.n.


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