Date and Time of the Query: 2019-04-19 T02:11:07 PDT
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Notes for object NGC 3432

12 note(s) found in NED.

1. 2009A&A...493..871S
Re:UGC 05986
UGC 5986 is warped and has a strong asymmetry between the approaching and the
receding side, both in kinematics and in density. A possible cause is an
interaction with a small companion to the south west.

2. 2003ApJS..148..383M
Re:NGC 3432
A12. NGC 3432 The H{alpha}+[N II] image of NGC 3432, an SB(s)m galaxy
with an inclination of 84deg, is presented in Figure 12. Our analysis of
the halo gas was complicated by the presence of three very bright
foreground stars located near NGC 3432, which did not subtract out very
well. The regions contaminated by these stars were excluded from the
calculations of the eDIG properties. Some eDIG is apparent over the
inner 2 kpc of the galaxy, extending out about 1.5 kpc in height and
ranging in EM from 2 to 10 pc cm^-6^. A faint arc of gas (possibly a
superbubble) with an average EM {approx}10 pc cm^-6^ is located ~3 kpc
from the center of the galaxy, extending out into the northwest halo. It
is only ~500 pc in diameter but reaches a height of 1 kpc.
The derived H{alpha} luminosity /D^2^_25_ is 8.6 x 10^37^ ergs s^-1^
kpc-^2^, only ~7% of which is attributed to extraplanar gas. The scale
height of the gas is ~1.0 kpc on either side of the galaxy, and the
ionized mass associated with this extraplanar gas is 5.5 x 10^7^
M_{sun}_. The disk and halo components of NGC 3432 are not strongly
correlated with each other. The relatively small 1 {sigma} deviations
indicate relatively smooth eDIG morphology.
English & Irwin (1997) observed NGC 3432 in H{alpha} and 20 cm radio
continuum. They detect one extraplanar fiIament extending away from the
galaxy (what we called in the first paragraph a "faint arc of gas") but
conclude that extraplanar emission detected in NGC 3432 is due to tidal
interactions with UGC 5983 (at the time of observation, it was not
apparent to us that NGC 3432 was an interacting galaxy, and so was
included in our survey) and not indicative of any disk-halo
interaction. Other than this one fiIament, they do not detect any other
eDIG, but they point out that their H{alpha} observations were not done
under photometric conditions and therefore were not very sensitive to
faint diffuse emission.

3. 2002AJ....124..675C
Re:UGC 05986

4. 2000AJ....119.1592I
Re:NGC 3432
NGC 3432 is an interacting galaxy (Arp 206, together with
UGC 5983), which shows considerable distortion. Two distinct tidal tails
are also visible in the H I images of Wilcots, Lehman, & Miller (1996).
A dwarf galaxy, it has a low star formation rate and departs from the
FIR-radio continuum correlation (English & Irwin 1997). English & Irwin
do not detect any diffuse extraplanar H{alpha} component (except for
several features which have a stellar component), even though there is a
prominent radio halo. Previous lower resolution 20 cm radio continuum
images can be found in Condon (1987), Gioia & Fabbiano (1987), and
Paper I. Our high-resolution image shows very weak distributed emission.
The luminosity of the brightest component (on the far northeast major
axis) is also low (Table 3). A UV HST image can be seen in Maoz et al.

5. 1995ApJS...98..477H
Re:NGC 3432
It is difficult to identify the location of the nucleus in the 2-D
spectrum because NGC 3432 is an edge-on Scd galaxy. Emission from H II
regions extends along most of the slit. The spectrum of the adopted
position of the nucleus shows narrow emission lines superimposed on a
blue continuum with broad Balmer absorption lines.

6. 1994CAG1..B...0000S
Re:NGC 3432
NGC 3368 Group
Scd(on edge)
Feb 5/6, 1981
panel 320
5 min
Racine wedge
Robust star formation is occurring in the
high-surface-brightness disk of NGC 3432.
High-surface-brightness HII knots dominate the
image. Individual stars probably begin to resolve
at about B = 21.
A large, very-low-surface-brightness dwarf
with an unresolved nucleus exists at a separation
of 3.1'. It resembles the huge dE,N type in the
Virgo Cluster, illustrated elsewhere (Sandage and
Binggeli 1984) and listed in the VCC, Table XIV.
NGC 3432 is listed by de Vaucouleurs
(1975) as a member of the NGC 3368 Group,
whose mean redshift is about = 750 km/s.
The redshift of NGC 3432 itself is v_o = 607 km/s.
At a redshift distance of 15 Mpc, the
projected linear separation of the companion
from NGC 3432 is small at 14 kpc.

7. 1994CAG1..B...0000S
Re:NGC 3432
NGC 3368 Group
Scd(on edge)
Feb 5/6, 1981
5 min
Racine wedge
The image of NGC 3432 is repeated here
from the previous panel, taken from the same
original plate.
The redshift is v_o = 607 km/s.

8. 1976RC2...C...0000d
Re:NGC 3432
= Arp 206
= VV 011
Dwarf companion close to south-preceding end.
Mem. S.A. Ital., 37, 433, 1966 = Cont. Asiago No. 186.
IAU Symp. No. 29, 97, 1968.
Astr. Ap., 29, 249, 1973.
Mem. S.A. Ital., 37, 433, 1966.
Spectrum, Rotation Curve and Mass Determination:
Mem. S.A. Ital., 37, 433, 1966.
IAU Symp. No.29, 97, 1968.
Astr. Ap., 8, 364, 1970.
Radio Observations:
Astr. Ap., 29, 249, 1973.

9. 1973UGC...C...0000N
Re:UGC 05986
VV 11, Arp 206
SB(s)m (de Vaucouleurs), Sc+ (Holmberg)
See UGC 05983

10. 1964RC1...C...0000d
Re:NGC 3432
Bright narrow knotty bar: 1.4 arcmin x 0.3 arcmin. Faint knotty outer arms.
Nebulous patch 4 arcmin south-preceding.
A.J., 61, 97, 1956.
Ap. J., 97, 117, 1943.

11. 1959VV....C...0000V
Re:VV 011a
= NGC 3432 is double?
V = +588 km/sec;
Yerkes Type: a?S7? or a?I7
Lower photograph is from Manova.

12. 1956AJ.....61...97H
Re:NGC 3432
HMS Note No. 105
Very strong {lambda} 3727 with early-type continuum,
and H{gamma} and H{beta} in emission (HMS Plate IVo).

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