Date and Time of the Query: 2019-05-20 T20:04:28 PDT
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Notes for object MESSIER 085

15 note(s) found in NED.

1. 2006MNRAS.369..497K
Re:NGC 4382
This well-known object shows a distinct depression in Mg b within the central 10
arcsec, consistent with Fisher et al. (1996), which appears slightly more
flattened than the isophotes. This is coincident with an enhancement in the
H{beta} absorption map (see also Kuntschner et al. 2001), as well as
corresponding closely to a region of peculiar kinematic behaviour (decoupled
rotation, low-velocity dispersion, and complex higher order terms (see Paper
III). There is also evidence for a flattened feature in the iron absorption maps
within this region, most evident in the Fe5015 map.

2. 2006MNRAS.366.1151S
Re:NGC 4382
Only weak [O III] emission is detected in this galaxy, mostly towards the
centre. The HST unsharp-masked image suggests the presence of a dust lane
running across the nucleus along the minor axis direction. However, Lauer et al.
(2005) show the absence of dust reddening in the centre and find that NGC 4382
displays a central minimum in its surface brightness distribution.

3. 2006ApJS..164..334F
Re:VCC 0798
VCC 798 (M85, NGC 4382).The isophotes are very boxy within 1"; the boxiness
persists all the way to the center, where there almost seems to be a "butterfly"
pattern, extending about 0.3" on either side and aligned with the major axis of
the galaxy. The isophotes become distorted beyond ~50". The residual image shows
the possible presence of two small dust patches about 4"; southwest of the
center. There is no evidence of a nucleus.

4. 2006ApJ...639...95P
Re:VCC 0798
VCC 798.This galaxy appears to be the best candidate in our sample for having a
trimodal color distribution.

5. 2004MNRAS.352..721E
Re:NGC 4382
NGC 4382: The velocity field is nearly cylindrical in the outer part. It
exhibits a strong twist inwards, with the signature of a decoupled
component in the central 2 arcsec, where there is also a sign reversal
in h_3_ (Bender et al. 1994). A clear counter-rotation is visible from
higher-resolution OASIS maps (McDermid et al. 2004). The dispersion
shows a remarkably strong depression in the central 8-10 arcsec, clearly
seen in Fisher (1997). There is a ring of positive h_4_ values at about 8
arcsec, hinted in the long-slit data of Bender et al. (1994).

6. 1999A&AS..138..253B
Re:NGC 4382
NGC 4382 - SN 1960R: two very faint patches are detected within the
immediate SN regions. All images appear to be very noisy. Patch 1 is
within a 3{sigma} detection limit.

7. 1997AJ....113..950F
Re:NGC 4382
NGC 4382. This is the only galaxy in our sample to show signs of minor-axis
stellar rotation. The inner regions of our CCD image of NGC 4382 (M85) do not
show obvious isophote distortions though the outermost contours are visibly
twisted with respect to the inner body of the galaxy (see Fig. 10 contour
plot). An ellipse fitting algorithm applied to our R-band image indicates that
the position angle changes from P.A.=60^deg^ in the central regions to
P.A.=0^deg^ for r>100". The major- and minor-axis Kinematic profiles of
NGC 4382 are quite similar. Our slit positions were P.A.=179^deg^ and
P.A.=89^deg^ for the major and minor axes, respectively. Because this galaxy
is orientated nearly face-on, the observed rotation speeds are low, with
V_max_=65 km s^-1^. The minor-axis rotation amounts to ~25 km s^-1^. The
major- and minor-axis velocity dispersion profiles show that the central +/-5"
of NGC 4382 has a lower {sigma} than the surrounding main body of the galaxy.
The nuclear H{beta} fine strengths in NGC 4382 are high (2.57 A) and suggestive
of a young, <3 Gyr, nuclear population (FFI). A B-R color image of NGC 4382 is
presented in FFI which shows a blue inner ring corresponding to the young
stellar component. Schweizer & Seitzer (1992) gave NGC 4382 the second highest
fine structure parameter({sigma}=6.85) from their sample of 69 elliptical and
S0 galaxies. This galaxy is a likely candidate for having experienced a
late-time, possibly merger-induced episode of star formation (see, e.g.,
Schweizer 1995).

8. 1996ApJ...459..110F
Re:NGC 4382
NGC 4382
An ellipse-fitting algorithm applied to our R-band CCD image of NGC 4382 (M85)
shows that the isophotes change position angle with radius (from P.A.=60^deg^
in the nuclear regions to P.A.=10^deg^ for r > 100"). The high central H{beta}
strength (2.57 A) is suggestive of the presence of young stars in the inner
regions. This conclusion is supported by the observation of a blue inner ring
in the color image (Fig. 5). The lack of emission features in our spectra
indicates that current star formation is likely not occuring.

9. 1994CAG1..B...0000S
Re:NGC 4382
S0_2_(3) pec
April 20/21, 1950
30 min
NGC 4382 forms a physical pair with NGC 4394 (SBb; panel 165) at
7.8' angular separation. The similarity of redshifts at v_o(4382) =
648 km/s and v_o(4394) = 853 km/s suggests a physical pair. At an
adopted redshift distance of 15 Mpc (H = 50), the projected linear
separation is small at 34 kpc.
The inner region of NGC 4382, shown in the insert, resembles a
normal E5. The extensive outer envelope in the negative print has
edges, said by Schweizer (1982, 1983, 1986), by Toomre quoted by
Schweizer (1983), and by Quinn (1984), to be owed to a dynamical
encounter with a dominant giant. The result is a composite galaxy,
which they would identify in this case as NGC 4382. Other examples of
shells and ripples in the outer envelopes of galaxies in this atlas
are NGC 474 (RS0/a; panel 84), NGC 7585 (S0/Sa; panel 84), and NGC
5018 (to the right here).
An example of a nucleated dwarf elliptical (dE0,N) is near the
edge of the frame near the middle on the right-hand side of the
print. It is a likely companion to the NGC 4382/4394 pair.

10. 1994A&AS..105..481M
Re:NGC 4382
NGC 4382: The envelope of this large S0 displays a low contrast spiral
pattern, as indicated by the isophotal twist and the large f_4_ values.

11. 1993ApJS...86....5K
Re:NGC 4382
NGC 4382 (M85); S0 pec.
M85, a gas-poor galaxy of high surface brightness, belongs to the Virgo
Cluster and forms a strongly interacting pair with NGC 4394 (Cutri &
McAlary 1985). This interaction might explain its bluer visible color in
comparison with typical S0 galaxies (Veron & Veron-Cetty 1985),
interpreted as due to enhanced star formation in the disk as opposed to
star formation in the nucleus. It is a radio quiet galaxy with an
X-ray/optical luminosity of about 1.3 X 10^-4^ (Dressel & Wilson 1985),
easily explained as the integrated contribution of low-mass binaries
(Trinchieri, Fabbiano, & Canizares 1986). The UV spectrum of the nucleus
of this normal galaxy has been studied and synthesized by Rocca-
Volmerange & Guiderdoni (1987), who conclude that it has a dominant
contribution from F and early G dwarf stars.

12. 1976RC2...C...0000d
Re:NGC 4382
= M85
= Holm 397a
= Kara[72] 334a
Pair with NGC 4394 at 7.8 arcmin
Faint diffuse companion at 3 arcmin south.
A.J., 69, 236, 1964.
"Stellar Structure", Stars and Stellar Systems, 8, 396, 1965.
Ap. J., 169, 209, 1971.
Ap. J. Suppl., 26, No. 230, 1973.
A.J., 69, 236, 1969.
"Stellar Structure", Stars and Stellar Systems, Vol. 8, 395, 1965.

13. 1973UGC...C...0000N
Re:UGC 07508
SA(s)0+ pec (de Vaucouleurs), S0 (Holmberg)
SN 1960r
Paired with UGC 07523 at 7.8, 80
Companion 3.1, 180, 0.4 x 0.4

14. 1964RC1...C...0000d
Re:NGC 4382
= Messier 085
= Holm 397a
Extremely bright, diffuse nucleus. Weak, smooth whorls in a lens. Very faint
diametric distortion toward the south.
Pair with NGC 4394 at 7.8 arcmin.
Anonymous companion at 3.0 arcmin.
B.A.N., 16, 1, 1961.
Ap. J., 135, 6, 1962.
Ap. J., 71, 231, 1930.
B.A.N., 16, 1, 1961.
HII Regions:
Zeits. fur Ap., 50, 168, 1960.
SN 1960
H.A.C., 1521, 1960.
Mem. Soc. Astr. Ital., III, 74, 1962.
Ann. Guebhard, 39, 263, 1963.

15. 1918PLicO..13....9C
Re:NGC 4382
Very bright oval; 4' x 2'; very slight traces of spiral structure. M.85. 14 s.n.

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