Date and Time of the Query: 2019-05-22 T11:22:27 PDT
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Notes for object NGC 4550

14 note(s) found in NED.

1. 2006MNRAS.369..497K
Re:NGC 4550
This S0 galaxy has two counter-rotating stellar discs of similar mass (Rix et
al. 1992). There is evidence for the Mg b contours being flatter than the
isophotes. The H{beta} map shows a mildly elevated level in the central region
along the major axis.

2. 2006MNRAS.366.1151S
Re:NGC 4550
Known for hosting two counter-rotating stellar discs (Rix et al. 1992; Rubin,
Graham & Kenney 1992), the ionized-gas distribution and kinematics of this
peculiar object, together with the observed dust morphology, are consistent with
gas moving in a fairly inclined and dynamically cold disc. A spiral arm
extending to the south is evident in the EW maps. Wiklind & Henkel (2001) note a
similarly lopsided distribution for the molecular gas they detect. Consistent
with the measurements of Rubin et al. and Rix et al., the ionized gas rotates
against the stars in the disc dominating the stellar kinematics along the major
axis beyond 10 arcsec. However, the gas rotates in the same sense as the stars
in the main body of the galaxy. Because this implies that the gas does not
necessarily have an external origin, we decided to adopt a value of zero for the
kinematic misalignment between gas and stars in NGC 4550 for the purpose of the
analysis of Section 5. Independently derived maps for the [O III] distribution
and kinematics were presented by Afanasiev & Sil'chenko (2002).

3. 2006ApJS..164..334F
Re:VCC 1619
VCC 1619 (NGC 4550),This galaxy is intermediate, as far as dust morphology is
concerned, between the "dust filaments" types (e.g., M87 and NGC 4472) and the
"large-scale dust disk" types (e.g., VCC 1154). Dust filaments radiate outward
from the center, but they have larger optical depth compared to the ones seen in
M87 or VCC 355, for instance. Although the filaments form a disk structure, this
is not quite as organized as the disks seen in VCC 1154 or VCC 1532. The main
dust filaments/lanes are confined within a 10" from the center, but dust patches
can be seen further out, up to a distance of 25". The dust correction performs
well, indicating that the galaxy's color within the dust region is similar to
that of the neighboring areas. The surface brightness profile indicates the
presence of a large nucleus.

4. 2004MNRAS.352..721E
Re:NGC 4550
NGC 4550: This object has two counter-rotating stellar discs of similar
mass (Rix et al. 1992) which, at the spectral resolution of SAURON,
produce a large region with a near zero mean velocity V and a dispersion
increasing outwards along the major axis. Note the extraordinary
decoupling revealed by SAURON, the outer disc being counter-rotating
with respect to the main body of the galaxy further away from the
equatorial plane, also noticed by Afanasiev & Sil'chenko (2002). h_4_ is
significantly lower outside 5 arcsec along the major axis.

5. 2003ApJ...583..145T
Re:NGC 4550
NGC 4550 (L2). This source is not detected with the present Chandra
observation. A detection with the ROSAT PSPC is reported by Halderson
et al. (2001). The observed ROSAT flux in the 0.1-2.4 keV band is 1.65
x 10^-13^ ergs s^-1^ cm^-2^. This ROSAT source is offset from the
optical nucleus by 10''. If this source is indeed the nucleus, our
nondetection by Chandra (F0.1-2.4 keV < 6 x 10^-15^ ergs s^-1^ cm^-2^)
indicates time variability.

6. 2000ApJ...542..186N
Re:NGC 4550
NGC 4550.-The 2 cm source we detect is offset 9.3" west and 5.5" north
of the optical position determined by Cotton et al. (1999) from digital
sky survey plates. The 1 {sigma} error of the optical position
determination is estimated to be 2.3" in both right ascension and
declination. The galaxy does not show any obvious sign of a peculiar
morphology, and the east-west galaxy extent is ~1', so the radio-optical
offset does appear significant. A ~3" resolution 11 cm map (Haynes &
Sramek 1980) shows an unresolved radio core at a position between our
radio detection and the optical nucleus. Wrobel & Heeschen (1991) find
that the 6 cm emission over the central 5" is less than 1 mJy. We
measure a 2 cm peak flux density of 0.7 mJy beam^-1^, so the source is
probably flat spectrum, {alpha}_2_^6^ >= -0.3.

7. 1996ApJ...459..110F
Re:NGC 4550
NGC 4550
NGC 4550 is a member of the edge-on subsample. Although this S0 contains two
cospatial, counterrotating stellar disks (Rubin, Graham, & Kenney 1992; Rix et
al. 1992), the line strength profiles appear unremarkable. The line strengths
within the two disks are similar. Emission features throughout our spectra
prevent an accurate determination of the stellar H{beta} strength.

8. 1996AJ....112..937D
Re:NGC 4550
7: NGC 4550/1 (S0/E). Arecibo reported less than 1 Jy km s^-1^ while Green
Bank reported 9.03 Jy km s^-1^ for NGC 4550. Arecibo reported 0.13 Jy km s^-1^
for NGC 4551. We detect nothing for either galaxy down to a flux density of
<~1.5 mJy.

9. 1994CAG1..B...0000S
Re:NGC 4550
VCC 1619
Feb 4/5, 1979
103aO + Wr2c
60 min
This Virgo Cluster galaxy has a three-zone
S0 appearance albeit subtle enough that NGC
4550 is not classed as a pure S0 but rather as a
mixed E/S0 type. The galaxy is not a pure S0
because of the absence of a disk, which, at the
evidently nearly edge on viewing angle, would be
expected to be similar to the disk so evident in
NGC 3115 (panel 50).

10. 1994AJ....108.1579v
Re:NGC 4550
NGC 4550, is classified SB0 in the RC2 and E7/S01(7) in the RSA. It
has two remarkably similar, co-spatial, counter-rotating stellar disks
(Rubin et al. 1992; Rix et al. 1992). Filamentary dust in the inner
region (see Paper I), distorts the isophotes at a<~9". Outside this
radius the isophotes are disky, consistent with Bender et al. (1988), and
with the presence of the two disks.

11. 1994A&AS..105..481M
Re:NGC 4550
NGC 4550: An exceptional strongly inclined S0, which becomes more and
more disky farther than l= 50 arcsec. The bar implied by the RC2
classification has not been seen.

12. 1976RC2...C...0000d
Re:NGC 4550
= Holm 422a
Non-interacting pair with NGC 4551 at 3 arcmin
Ap. J., 146, 28, 1966.
Ap. J. Suppl., 26, No. 230, 1973.
Observatory, 88, 239, 1968.

13. 1973UGC...C...0000N
Re:UGC 07757
Paired with UGC 07759 at 3.2, 35
S0 (de Vaucouleurs)

14. 1964RC1...C...0000d
Re:NGC 4550
= Holm 422a
Non-interacting pair with NGC 4551 at 3 arcmin.
Lund 9 dimensions (0.9 arcmin x 0.3 arcmin) rejected, lens only.

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