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Date and Time of the Query: 2019-06-16 T12:08:24 PDT
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Notes for object NGC 4030

11 note(s) found in NED.


1. 2012ApJ...754...67F
Re:NGC 4030
NGC 4030 .SAS4..-The flocculent spiral structure-easily seen in HST
F606W-extends all the way to the center with star-forming knots in the inner
disk (Eskridge et al. 2002). Fisher & Drory (2008) classify it as pseudobulge.
The major axis rotational velocity reaches ~=100 km s^-1^ at about +/-10". The
velocity dispersion stays moderately flat within the bulge region and drops off
outside; this was also observed by Ganda et al. (2006). The h_3_ moments are
clearly anti-correlated with velocity and reach values of up to 0.1 at a radius
of about 7". h_4_ moments are compatible with zero at all radii that are covered
by our data. The bulge is small (r_b_ = 3.0") and we do not sufficiently resolve
it to include this galaxy in any of our structural plots.

2. 2007MNRAS.380..506G
Re:NGC 4030
This Sbc galaxy is characterized by very regular kinematics for both the stellar
and gaseous components (Ganda et al. 2006). The line strength maps also have a
smooth appearance, with Fe5015 and Mgb decreasing at larger radius and H{beta}
increasing. The H{beta} map seems to be asymmetric with respect to the centre,
since the western side displays higher values than the eastern one. The stellar
populations are young over the whole field and the metallicity, among the
highest in our sample (the third after NGC 488 and 772), decreases moving
outwards; the abundance ratio is approximately solar. The {tau} map for age
fixed to 10 Gyr in Fig. 11 shows a large central depression. The analysis of the
{DELTA}{chi}^2^ contours, in the continuous star formation approach, shows that
this galaxy is probably not very well described by an SSP, nor by a constant
SFR.

3. 2003ApJS..146..353M
Re:NGC 4030
NGC 4030 (TW)
This galaxy has a spectacular, tightly wound nuclear spiral that
matches the criteria for acoustic turbulence extremely well as the
dust spirals fill the disk at all radii and decrease in contrast near
the nucleus. This is one of the prototypes of the tightly wound
nuclear spiral class.

4. 2003AJ....126..742H
Re:NGC 4030
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."
.
3.18. NGC 4030 (CS) (TW-mp)
Figure 9 (top).
Spectrum: Only the continuum is obvious in the NUC spectrum.
Images: A faint spiral structure can be seen going down to the nucleus
but is not obvious in the NICMOS image.

5. 2002ApJS..143...73E
Re:NGC 4030
NGC 4030.---Sab: Centrally condensed nucleus embedded in a large
elliptical bulge. Flocculent spiral pattern, with at least three arms.
Arms are patchy and wispy, still showing signs of dust lanes in the H
band. Inner disk has many star-forming knots. Outer disk appears
quiescent.

6. 1998AJ....116...68C
Re:NGC 4030
Tightly wound (ringlike), flocculent nuclear spiral arms (inside the
R_e_ of the fitted exponential bulge).

7. 1976RC2...C...0000d
Re:NGC 4030
Faint anonymous Im at 16.5 arcmin south-following.

8. 1973UGC...C...0000N
Re:UGC 06993
SA(s)bc (de Vaucouleurs)

9. 1964RC1...C...0000d
Re:NGC 4030
Small, bright nucleus. Many knotty, filamentary arms. Possible (rs) type.
Faint anonymous Im at 16.5 arcmin south-following.
Lick 13 major-axis dimension (2 arcmin) is for the bright part only.

10. 1956AJ.....61...97H
Re:NGC 4030
HMS Note No. 120
Slit on nucleus and emission patch in an arm
40 arcsec [south-east] of the center.
Redshift is mean of all lines measurable in nucleus and patch,
since slit was oriented only about 3 degrees from minor axis.
Spectrum is progressively out of focus toward H{beta} because
of presence of emulsion lump at end of plate.

11. 1918PLicO..13....9C
Re:NGC 4030
A rather bright, slightly oval spiral 2' long. Nucleus almost stellar; numerous
almost stellar condensations in the rather open whorls.


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