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Notes for object MESSIER 090

28 note(s) found in NED.


1. 2012ApJ...754...67F
Re:NGC 4569
NGC 4569 .SXT2..-A nuclear spiral extends all the way to the center. The bulge
is classified as a pseudobulge by Fisher & Drory (2010). The major axis
rotational velocity rises with increasing radius to a local maximum of about 80
km s^-1^ at +/-3". The bulge radius is r_b_ = 9.6". The velocity then drops to
about 50 km s^-1^ at the maximum radius covered by our data. The velocity
dispersion rises with decreasing radius to about 100 km s^-1^ at a radius of 6"
and then drops and reaches a local minimum at around 3", roughly coinciding with
the locations of the local maxima in the velocity profile. The h_3_ moments are
anti-correlated with velocity inside the bulge. Their absolute values reach up
to 0.15. The h_4_ moments show a strong double peak feature at about 3" and fall
off to zero at the bulge radius. The minor axis profile shows rotation in the
bulge region. While somewhat asymmetric, the minor axis dispersion profile does
not show the same complicated structure of the major axis profile. The h_3_ mom
ents on the minor axis are mostly compatible with zero. The h_3_ moments on the
minor axis are mostly slightly positive with a mean value of 0.03. The h_4_
moments are generally noisy but the double peak feature of the major axis is
reproduced.

2. 2009A&A...503..409H
Re:NGC 4569
NGC 4569 (M90): In this moderately inclined spiral galaxy, polarized emission is
detected in the central disk region on either side of the minor axis. Polarized
intensity declines more slowly to the southwest and more rapidly to the
northeast (where the receding major axis is located (PA = 23^deg^, as
tabulated in Table 1). Moreover, the spectacular double lobe extension which is
oriented roughly along the minor axis is also detected in polarization,
particularly along its edges. Even more interesting is the continuum bridge
connecting the galaxy to its small companion, IC 3583 (located about 6 arcmin to
the northwest, and visible in both Figs. 4 and 5), which also has a polarized
counterpart. The large-scale structures in our map have already been observed at
lower spatial resolution and analyzed by Chyzy et al. (2006), who observed this
system with the Effelsberg telescope. The polarized bridge and the lobe
extensions have rather high polarized fractions. The bridge is polarized at the
20-30% level, the lobes at the 10-20% level, with localized hot-spots of higher
polarized fraction, of about 40%. The disk itself has polarized fractions of
only about 1-2%. As for the magnetic field orientations, the situation is
confused in the disk due to the modest angular resolution, but there seems to be
a slight tendency for field lines to follow the optical spiral arms. In the
radio lobes, the field lines appear to trace the edges of apparent cavities.
Finally, in the extension toward IC 3583, the magnetic field lines run roughly
along the direction of the extension. The brighter lobe of a background double
source provides an estimate of the Galactic foreground RM in this direction of
+18 +/- 2 rad m^-2^.

3. 2008MNRAS.388..500E
Re:UGC 07786
UGC 7766 (NGC 4559). The bar of this galaxy is almost aligned with the
major-axis; its signature can be seen on the velocity field as well as on the
rotation curve within the first 30 arcsec. Meyssonnier (1984) obtained a
rotation curve from slit spectroscopy which is in agreement, although it has a
much higher dispersion than our H{alpha} rotation curve. Our rotation curve is
more extended since our velocity field reaches more outer regions although our
field-of-view is limited by the size of the interference filter. Krumm &
Salpeter (1979) found a flat H I rotation curve from 2 to 7 arcmin. It has been
observed more recently by WHISP (website), their position-velocity diagram
confirms the flat behaviour of the rotation curve up to 9 arcmin together with
the amplitude determined by the previous authors. The width of the H I profile
at 20 per cent (254 km s^-1^, Springob et al. 2005) is in agreement with our
H{alpha} velocity field amplitude.

4. 2006MNRAS.366.1265B
Re:NGC 4569
This galaxy is located in the Virgo cluster. An off-plane structure to the west
of the disc of NGC 4569 has been seen through deep H{alpha} imaging (Tschoke et
al. 2001) and in H I data (Vollmer et al. 2004). It is observed here as a string
of H II regions whose kinematics follow the rotation of the disc, although it is
slightly more redshifted than inside the disc at equal azimuth angles (Chemin et
al. 2005).

5. 2006MNRAS.366..812C
Re:NGC 4569
The velocity field of the galaxy is perturbed, showing gas streamings along the
arm-like structures in the H{alpha} (severely) truncated disc. An off-plane
string of H II regions is observed to the West of the disc. It exhibits a
velocity gradient that follows the rotation of the disc. This gaseous structure
has already been seen in deep H{alpha} image (Tschoke et al. 2001) and in H I
data (Vollmer et al. 2004). The giant diffuse gaseous region to the West of the
disc (Tschoke et al. 2001) is not detected in the FP observation, which is
probably due to a too low S/N or to a likely cut-off in the transmission of the
interference filter. Vollmer et al. (2004) proposed an RPS model to explain the
H i asymmetry.

6. 2003PASJ...55...59S
Re:NGC 4569
4.10 NGC 4569 CO gas is distributed in an elliptical ring of radius 500
pc (Nakanishi et al. 2003), and the velocity field is complex, having
anomalously high non-circular rotation. The PVD is complicated with two
bright ridges having forbidden velocities. Our iteration program
averaged the observed PVD, and obtained an RC, which gives only
averaged rotation velocities. The SMD shows a bulge component and disk,
while its detail in the central 1 kpc is not reliable because of the
uncertainty in the RC determination.

7. 2003PASJ...55...17S
Re:NGC 4569
6.11 NGC 4569 The molecular gas is highly concentrated within ~1 kpc
radius. The CO intensity distribution is elongated in the same
direction as the optical major axis, and has two peaks with depression
at the nucleus, consistent with the earlier CO map (Sakamoto et al.
1999a). Thus, the central molecular morphology of this galaxy may be
classified in twin peaks at the present resolution. However, a higher
resolution CO map reveals that the apparent two peaks coincide with
both ends of an elliptical molecular ring, while they are not
associated with so called offset ridges (Nakanishi et al. 2003). The
velocity field is strongly disturbed from circular rotation, and the PV
diagram indicates significant 'forbidden' velocities. Nakanishi et al.
(2003) discuss the kinematics of this galaxy in detail, and tried to
explain these features using two models of non-circular motion and
warping of the inner disk. And they conclude that it is natural that
disturbed velocity field and forbidden velocities of the PV diagram are
due to non-circular motion. Helfer et al. (2001) have reported an
extended CO emission from their wide-field mosaic image. Jogee et al.
(2001) have also presented a high resolution CO image of this galaxy.

8. 2003ApJS..146..353M
Re:NGC 4569
NGC 4569 (C)
There are clear dust structures present, yet no obvious spiral
structure, and this may be due to the moderate inclination of the
galaxy. Pogge et al. (2000) also noted the chaotic circumnuclear dust
in their V-I color map. The round feature to the upper right in the
NIR image and color map is due to the NIC2 coronagraph.

9. 2002ApJS..142..223F
Re:NGC 4569
NGC 4569. NVSS reports a 73 mJy source, while FIRST detected a 14.3 mJy
source. 1.4 GHz, 48" resolution observations (Condon 1987; Condon et al.
1990, 1998b) detect an 83 mJy source. High-resolution 2.4 GHz
observations show an uncertain 3 mJy core detection (Turner, Helou, &
Terzian 1988), while the 0.2" resolution observations of Nagar et al.
(2000) give an upper limit of 1.1 mJy to any radio emission at 15 GHz.

10. 2002ApJS..139....1T
Re:NGC 4569
NGC 4569 (T2).-Detailed analysis of an ASCA observation is presented
in Terashima et al. (2000c). The ASCA image in the hard band (2-7 keV)
is clearly extended compared to the PSF. This implies that the
luminosity of the nucleus (before correction for absorption) is much
lower than the observed luminosity. The recent Chandra observation of
Ho et al. (2001) shows that the nucleus is surrounded by other sources
of comparable brightness; for a power-law spectrum with {GAMMA} = 1.8
and N_H_ = 2 x 10^20^ cm^-2^, the X-ray luminosity of the nucleus is
2.6 x 10^39^ ergs s^-1^ in the 2-10 keV band. This luminosity is about
a factor of 4 smaller than the ASCA luminosity in the same energy band.

11. 2001MNRAS.324..737R
Re:NGC 4569
A4 NGC 4569
NGC 4569 (M90) is in the Virgo cluster. It has a very bright nucleus,
probably the result of a recent star formation episode (Stauffer,
Kenney & Young 1996). Optical and IUE studies (Keel 1996) have demonstrated
that the nucleus is the host to a young star cluster, dominated optically
by A-type supergiants. HST UV imaging showed the nucleus to be a bright,
point-like, UV source (Maoz et al. 1995), although more recent observations
indicate that the UV source is clearly extended (Barth et al. 1998).
UV spectroscopy reveals that the dominant continuum source is a cluster of
massive stars and that there is no evidence in the UV for a LLAGN
(Maoz et al. 1998). Narrow-band ([O III]{lambda}5007 and H{alpha}+[N II])
HST optical imaging on the other hand, shows the nucleus to be bright and
unresolved on a subarcsec scale (Pogge et al. 2000).
A ROSAT PSPC observation reveals extended X-ray emission in the bulge
and disc of NGC 4569, with the emission peaking at the nucleus (Junkes &
Hensler 1996). The HRI observation, however, shows a luminous, unresolved
point source coincident with the nucleus (Colbert & Mushotzky 1999;
Roberts & Warwick 2000). ASCA observations of NGC 4569 confirm that the
X-ray emission is extended on scales of several kpc in both the soft
(0.5-2 keV) and hard (2-7 keV) ASCA bands (Terashima et al. 2000a). The
ASCA spectra are best described by a Raymond-Smith plus power-law (or
thermal bremsstrahlung) model, with parameters kT ~ 0.67 and {GAMMA} ~ 2.2
respectively; an additional column density of 1.7 x 10^21^ atom cm^-2^
applies to the second component. Terashima et al. (2000a) postulate that
there is no evidence for the presence of an AGN in NGC 4569; the soft
component could originate in star formation, whereas the hard component
could easily be the sum of a discrete (non-AGN) source contribution. In
combination with the other measurements summarized above, Terashima et al.
(2000a) conclude that the LINER spectrum of NGC 4569 is the probably the
result of the presence of hot stars in its nucleus.

12. 2000ApJ...534..670T
Re:NGC 4569
NGC 4569.-The M/L in the disk region increases by 2.4 times from r = 2
to 5 kpc. In the bulge region it appears to decrease inward and then
turns to increase toward the center. However, the spatial resolution is
not sufficient to confirm the central increase.

13. 2000ApJ...530..688A
Re:NGC 4569
NGC 4569 (M90).-The optical line ratios of this galaxy given in
Stauffer (1982) comply with Heckman definition of LINERs, however, it is
classified as a transition object in Ho et al. (1997a) based on both its
location in the diagnostic diagrams and the nondetection of a broad
component of H{alpha} (Ho et al. 1997c). The HST/UV spectrum of this
galaxy (as in NGC 404) shows absorption-line signatures indicative of a
continuum dominated by light from massive stars (Maoz et al. 1998), and
the HST/UV imaging shows extended emission (Barth et al. 1998). Keel
(1996) in a detailed study of the UV and optical properties reaches the
conclusion that a population of young stars is responsible for the
properties of NGC 4569, although an extra component associated with
either an AGN or a population of older stars is still necessary. Our J
and H-band spectra show that the emission is strongly dominated by the
underlying stellar continuum. The Pa{beta} line is clearly detected in
emission. All this evidence leads to a classification of
starburst-dominated LINER.

14. 1999ApJS..124..403S
Re:NGC 4569
5.11. NGC 4569
NGC 4569 is called an "anemic spiral" because of its small H I
extent compared to its optical size, presumably owing to gas stripping
in the Virgo Cluster (van den Bergh 1976; Cayatte et al. 1990). At the
nucleus of this barred galaxy is a compact (r <= 2 pc) UV source,
interpreted by Keel (1996) as a supergiant-dominated starburst. CO
emission is concentrated in a compact barlike region, 30" x 10"
(=2.4 x 0.8 kpc) in extent, elongated in the north-south direction
(p.a. ~ 20^deg^). The two peaks in the bar are separated by ~ 8"
(0.7 kpc). Strong noncircular motions are seen near the nucleus,
suggesting streaming motions in the bar.

15. 1999ApJ...519...89C
Re:NGC 4569
NGC 4569 (M90).-This spiral galaxy is in the Virgo cluster. HFS95
label it as having a transition (LINER/H II) type nucleus. We find a
compact X-ray source coincident with the nucleus.

16. 1998PASJ...50..427S
Re:NGC 4569
NGC 4569: The [N II] line is stronger than H{alpha} in the nuclear PV
component, which shows a steep rise of rotation within ~ 1", though the
details are not resolved in the present data. The rotation velocity then
attains a minimum at ~ 15", and increases to a flat part beyond R ~ 30".

17. 1998ApJ...496..133B
Re:NGC 4569
NGC 4569.--Maoz et al. (1995) found the UV source in NGC 4569 to be pointlike,
whereas in our image it is clearly extended even at the smallest radii, as
illustrated in Figure 4. The most likely explanation for this discrepancy is
that the FOC image of NGC 4569 was taken prior to the first HST refurbishment
mission and hence suffered from the aberrated HST PSF; it was also very heavily
saturated, making profile measurements at small radii extremely difficult.
Spacecraft jitter cannot be the cause of the spatial extent of the WFPC2 image,
as the spatial profile is identical in the two UV exposures. The maximum
possible contribution from a single point source in the WFPC2 image is 23% of
the total flux, but the fluxes measured in the WFPC2 and FOC images differ by
only 10%. The F547M image of NGC 4569 is saturated, and we are unable to
measure the optical nuclear sharpness parameter for this object. The UV
source has S(7x7) = 0.0489, compared with S(7x7) = 0.1531 for the synthetic
F218W PSF, another indication that the UV profile of NGC 4569 is significantly
more extended than a point source. The IUE and optical study by Keel (1996)
demonstrated that the nucleus of this galaxy is a young star cluster 6 mag more
luminous than the core of 30 Doradus and that the optical light from the cluster
is dominated by A-type supergiants. HST data presented by Maoz et al. (1998)
show that the UV spectrum is nearly an exact match to that of the young
starburst cluster NGC 1741-B, which has a likely age of 4-5 Myr (Conti,
Leitherer, & Vacca 1996).

18. 1998AJ....116.2682C
Re:IRAS 12343+1326
NGC 4569. LINER, Seyfert.

19. 1997ApJS..111..143B
Re:FAUST V129
V129 = NGC 4569 = M90 = UGC 7786.--An Sab galaxy. It was observed during a
FOC-HST program (Maoz et al. 1995) to have a nuclear UV source at 2300A whose
size is FWHM<=0.22"=2.2 h^-1^ pc (h is the Hubble constant in units of 100
km s^-1^). Spectroscopy of the source indicates it to be a transition between
an H II nucleus and a LINER. There is residual UV emission from an extended
source 0.65" south of the bright nuclear region. The flux density measured for
the nuclear source is 10^-14^ erg s^-1^ cm^-2^ A^-1^, or a monochromatic
magnitude at 2270 A of 13.82. The difference from the integrated UV flux
measured by FAUST is due to emission at much larger nucleocentric distances
than sampled by the FOC.

20. 1997AJ....114.2428S
Re:NGC 4569
NGC 4569: This Sab type galaxy shows also a high concentration of CO intensity
near the center. The velocity increases very sharply within the central 5" (300
pc) to about 200 km s^-1^.

21. 1995ApJS...98..477H
Re:NGC 4569
The UV morphology of the nucleus of NGC 4569 is best represented by a
bright, unresolved point source plus fainter extended emission (Maoz et
al. 1995). The emission-line spectrum resembles those of ``transition
objects'' (LINER/H II), most likely reflecting the composite source of
photoionization suggested by the UV imaging.

22. 1994CAG1..B...0000S
Re:NGC 4569
M90
VCC 1690
Hubble Atlas, p. 13
Sab(s)I-II
PH-12-Baum
Jan31/Feb 1, 1952
103aO + WG2
30 min
NGC 4569 is among the earliest of the Sab types. The outer arms
are smooth, similar to the early-type smooth-armed Sa prototypes (NGC
1302, panel 70; NGC 2811, panel 65), but the massive thick dust lanes
in the outer region of the bulge require a later
classification. Incipient star formation in the dust is evident. Small
knots, presumed to be small HII regions, exist in the dusty inner
arms. The combination of smooth outer arms devoid of much current star
formation and the active, very dusty inner region is moderately
unusual.
The galaxy is in the direction of the Virgo Cluster, about 1.5
deg northeast of the center of Virgo subcluster A (Binggeli, Tammann,
and Sandage 1987) associated with NGC 4486. The large angular size of
NGC 4569 and its negative velocity of v_o = -241 km/s were at one time
cited by some to place NGC 4569 in the foreground. However, no
galaxies in the RSA outside the Local Group have negative v_o
velocities except six galaxies in the direction of the Virgo Cluster,
a circumstance that shows that the negative velocity must reflect the
large velocity dispersion of Virgo Cluster members. Furthermore,
other Sb and Sc galaxies in the Virgo Cluster are as large in angular
size as NGC 4569 (van der Kruit 1986). There seems little question but
that NGC 4569 is a Cluster member.

23. 1993ApJS...86....5K
Re:NGC 4569
NGC 4569 (M90); SABab, LINER.
M90 belongs to the Virgo Cluster and, from properties of the optical
emission lines, is classified as a LINER (Stauffer 1982; Keel 1983b). It
is a strong emitter at 10 microns (Scoville et al. 1983), and its
emission in the range 1-20 microns is dominated by dust and starlight,
properties typical of normal galaxies (Willner et al. 1985). This object
has Fe II absorption and unusually strong Mg II absorption.

24. 1976RC2...C...0000d
Re:NGC 4569
= M90
In Arp 076
Non-interacting pair with dwarf IC 3583 at 6.0 arcmin north.
Possibly interacting.
Photometry (10 microns):
Ap. J.Let 176, L95, 1972.
Isodensitometry:
Ap. J. Suppl., 26, No. 230, 1973.
Spectrum:
Mt.Wilson velocity (Source B) rejected. See Ap. J., 159, 405, 1970.
Ap. J., 166, 1, 1971.
Ap. J. (Letters), 161, L109, 1970.
Astr. Ap., 27, 433, 1973.
Spectrophotometry:
Observatory, 88, 239, 1968.
Astr. Ap., 19, 405, 1972. Astr.
Ap., 27, 433, 1973.
Rotation Curve:
Ap. J., 166, 1, 1971.
HII Regions:
Ap. J. Suppl., 27, No. 1974.

25. 1973UGC...C...0000N
Re:UGC 07786
Arp 76
SAB(rs)ab (de Vaucouleurs)
Sb+ (Holmberg)
See UGC 07784
In Arp's class "spiral galaxies with small high surface brightness companions
on arms"; "apparent gap between arm and companion" (Arp)

26. 1964RC1...C...0000d
Re:NGC 4569
= Messier 090
Possibly interacting. Very small, extremely bright nucleus in a bright diffuse
bar with much dark material. Smooth regular arms or whorls.
Early Mt. Wilson velocity (MWC 531) was for the star superposed near the
nucleus; see A.J., 61, 110, 1956.
Yerkes 1 color classification: or g
Non-interacting pair with IC 3583 at 6.0 arcmin.
Photograph:
Ap. J., 135, 7, 1962.

27. 1961Hubbl.B...0000S
Re:NGC 4569
Messier 090
Sb
PH-12-Bm
Jan. 31/Feb. 1, 1952
103aO + WG2
30 min
Enlarged 2.0X
The soft texture of the spiral arms and the heavy dust
lanes near the center of this galaxy are similar to these
features in NGC 4826 (left). Spiral arms of this type were
described as "massive" by Reynolds and by Hubble. Dust
lanes can be traced almost to the nucleus, which is of high
surface brightness and about 2 mm in diameter on the
scale of this illustration. There is partial resolution of one
of the inner dust lanes into knots, which are presumed to
be HII regions.

28. 1957HPh....53..275d
Re:NGC 4569
SA(s)ab
(Plate 17)
(= Messier 090)
A large central bulge from which emerge two smooth and
massive regular arms which are closely wound, and separated
by dark lanes.
Faint outer spiral extensions showing a tendency to
return toward the central lens.
Compare with NGC 2855 (Plate 4) and NGC 4736 (Plate 21), and
NGC 4594 (Plate 39).


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