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Notes for object MESSIER 063

28 note(s) found in NED.

1. 2012ApJ...754...67F
Re:NGC 5055
NGC 5055 .SAT4..-The HST F606W image shows that the outer disk flocculent spiral
extends into the very center. Consequently this galaxy is classified as
pseudobulge by Fisher & Drory (2010). The velocity dispersion profile remains
flat inside the bulge radius of 18.3". The h_3_ moments are anti-correlated with
velocity inside the bulge and reach absolute values of up to 0.1 at the bulge
radius. The h_4_ moments are compatible with zero inward of 10". They become
noisy further out but show a weak tendency toward more positive values toward
the bulge radius. The minor axis velocities appear somewhat irregular but small
(<20 km s^-1^). The minor axis h_3_ moments are noisy but mostly scatter close
to zero. Again the h_4_ moments are mostly compatible with zero inward of 10".
but show a weak increase further out but only on the east side.

2. 2009A&A...503..409H
Re:NGC 5055
NGC 5055 (M63): Diffuse polarized emission is detected from the disk of this
inclined galaxy on both sides of the minor axis. The highest brightnesses are
associated with the zone of strong warping of the gaseous disk in the southwest
at the edge of the star-forming disk. A fainter counterpart is seen in the
northeast. The minimum in polarized intensity occurs at the PA of the receding
major axis (PA = 102^deg^, as tabulated in Table 1). The polarized fraction of
the brightest feature is mainly in the range of 5-10%, but at the southernmost
end (where the contribution from the bright inner disk is significantly fainter)
the fraction increases to 15-25%. The magnetic field lines closely follow the
spiral arm structure observed in the optical image. Two background double
sources yield an estimate of the background RM in this field of about -8 +/- 3
rad m^-2^.

3. 2008MNRAS.388..500E
Re:UGC 08334
UGC 8334 (NGC 5055, M 63). M 63 is a very well studied flocculent spiral galaxy.
Our observations are fully compatible with the H{alpha} Fabry-Perot data
observed with the 1.6-m Mont Megantic Telescope (Daigle et al. 2006a). Their
rotation curve is more extended, due to a larger field-of-view, but does not
reach the optical radius (~6 arcmin). It possesses a huge H I disc (~36 arcmin
diameter) strongly warped beyond the optical disc (Battaglia et al. 2006). The
agreement between our H{alpha} rotation curve and their H I rotation curve is
very good but we find a better symmetry for receding and approaching sides from
2 to 10 kpc radius. The position-velocity diagram shows that the velocities
steeply rise in the inner 10 arcsec.

4. 2008ApJ...677..926S
Re:NGC 5055
NGC 5055 is an Sbc spiral galaxy (de Vaucouleurs et al. 1976) at a distance of
7.2 Mpc (Pierce 1994). At this distance, the aperture from which the [Ne v] 14.3
micron line was detected corresponds to a projected size of ~170 x 380 pc. This
galaxy is optically classified as a transition object with no broad lines
detected (H97). Hence, there is no firm evidence for an AGN based solely on its
optical spectrum. The evidence for AGN activity at other wavelengths is
inconclusive. The nucleus is not detected at a number of radio frequencies, but
it is detected at 57.5 MHz with a flux density of 2.1 Jy (Israel & Mahoney
1990), implying that the source is radio-quiet. A central UV source is detected;
however, high-resolution HST observations show that it is resolved with a radius
of ~7 pc (Maoz et al. 1995) and shows no variability (Maoz et al. 2005). The UV
emission from this galaxy is therefore most likely dominated by a nuclear star
cluster. Chandra observations reveal the presence of numerous point sources
scattered across the nuclear region and a bright, hard point source coincident
with the optical and infrared nucleus (Flohic et al. 2006; Luo et al. 2007).
Flohic et al. (2006) argue that the spectrum of this source is well-fitted by a
two-temperature plasma model suggesting that the X-ray emission is powered by
stellar processes. Conversely, Luo et al. (2007) report that the central source
is well-fitted by an absorbed power law with a spectral index typical of an AGN.
The [Ne v] detection reported in this work provides firm confirmation of an AGN
in this galaxy. The central stellar velocity dispersion associated with the
bulge in this galaxy is 103 +/- 6 km s^-1^ (Heraudeau & Simien 1998.)

5. 2008AJ....136.2648D
Re:NGC 5055
4.14. NGC 5055 is an Sbc galaxy with an extended and warped tenuous outer H I
disk. Its H I distribution and kinematics were recently analyzed by Battaglia et
al. (2006). For V_sys_, Battaglia et al. (2006) find a value of 497.6 +/- 4.8 km
s^-1^, which is in close agreement with our value of 496.8 +/- 0.7 km s^-1^.
Their distributions of i and P.A. are also in agreement, and they note a similar
difference between the models for approaching and receding sides. We compare the
two rotation curves in Figure 17. The first inner maximum at R ~ 2 kpc is more
pronounced in our data set. This is likely due to a combination of increased
resolution and the use of Hermite polynomials as opposed to the Gaussian
functions that Battaglia et al. (2006) used. This is also the most likely
explanation for the higher rotation velocities we find in the outer parts.

6. 2008AJ....136.2648D
Re:NGC 5055
6.12. NGC 5055 The surface brightness profiles of NGC 5055 are shown in Figure
47. The 2MASS J, H, and K profiles can be traced out to ~350", and the 3.6 {mu}m
profile out to 450". There is clear evidence for a compact central component
which we model as an exponential disk with parameters {mu}_0_ = 13.4 mag
arcsec^-2^ and h = 0.35 kpc. For the outer disk, we simply used the observed
profile with the inner component subtracted, as indicated in Figure 47. Small
residuals are present, notably around R ~ 50", but these are of minor
importance. An exponential disk fit to radii 350" < R < 450" was used to extend
the outer disk profile. NGC 5055 has a significantly redder center, with a
well-defined color gradient at larger radii. For the central component we assume
a constant {GAMMA}^3.6^_*_ = 1.3, whereas for the outer disk we find values from
an inner {GAMMA}^3.6^_*_ ~= 1 to an outer {GAMMA}^3.6^_*_ ~ 0.5. Beyond the
radii where the 2MASS colors could be reliably determined, we assume a constant
valu e of {GAMMA}^3.6^_*_ = 0.5. In the very inner parts, we assumed an
extrapolated {GAMMA}^3.6^_*_ = 1.0 for the outer disk. The rotation curve fits
are presented in Figure 48. In the case of fixed {GAMMA}^3.6^_*_ the inner disk
overpredicts the curve by a large factor (not shown here), and we kept it as a
free parameter, yielding values of {GAMMA}^3.6^_*_ ~ 0.2 for the inner disk. The
NFW model seems to have particular difficulties fitting this galaxy. With
{GAMMA}^3.6^_*_ as a free parameter, the fit demands a negative value for the
outer disk. In the fits presented here, we have therefore set {GAMMA}^3.6^_*_ =
0 for this component.

7. 2007MNRAS.379.1249D
Re:NGC 5055
NGC 5055 is a spiral non-active galaxy, and the control for NGC 5194. Previous
radio and optical studies show an overall remarkable regularity and symmetry in
its morphology and kinematics (Thornley & Mundy 1997; Battaglia et al. 2006).
There is evidence of a tidal interaction with a companion (UGC 8313), and the
outer disc of NGC 5055 is warped. Blais-Ouellette et al. (2004) studied the
H{alpha} emission of NGC 5055 with a Fabry-Perot etalon installed on the Multi
Object Spectrograph focal reducer on the CFHT. They found two velocity
components in the inner 8 arcsec of this galaxy. One component is consistent
with the global disc kinematics while the second exhibits a pattern compatible
with a bipolar outflow or a counter-rotating disc.
Our SAURON stellar continuum map presents an asymmetry towards the north-west
(Fig. 4g). The stellar velocity field shows a very regular rotation pattern with
the kinematic major-axis aligned with the photometric major-axis at a PA of
100{degree}. The velocity dispersion rises in the very centre (r < 2 arcsec).
The ionized gas H{beta} and [O III] are mainly concentrated in the inner 5
arcsec. The [O III] distribution shows a V-shaped structure towards the north,
while the H{beta} intensity map shows a number of hotspots broadly distributed
over the FOV. The [O III] and H{beta} velocity fields are very regular and
similar to the stellar velocity field (except for their higher amplitudes). The
[O iii] velocity dispersion map is featureless but the H{beta} velocity
dispersion map shows an elongated structure of high dispersion, roughly aligned
with the kinematic major-axis. Finally, the [O III]/H{beta} line ratio reaches
its highest values in the region of high [O III] emission-line flux.

8. 2007ApJS..173..538T
Re:NGC 5055
NGC 5055 [M63] (Fig. 16.25).-This is an SA(rs)bc H II /LINER galaxy with a very
large warped H I disk (Battaglia et al. 2006). GALEX shows that the outer H I
disk has recently formed massive stars, principally along ridges in the gas
distribution. One particular region of UV emission to the southwest of the
galaxy is possibly a TDG (namely UGCA 342; Bremnes et al. [1999] suggest it is a
"condensation" in the outer gas disk). NGC 5055 is a member of the M51 group (7
members). NGC 5055 appears to be interacting with UGC 08313, found to the
northwest and connected by a filament of H I containing UV-bright complexes.
SDSS imaging recovers UGCA 342 and a few other XUV-clumps.

9. 2006MNRAS.366.1265B
Re:NGC 5055
This galaxy shows several arm patterns that are well visible in H{alpha}. It
harbours a very strong velocity gradient in its centre and a flat rotation
curve. No bar structure is visible. It has been studied in H I by Bosma (1981)
and in CO by Nishiyama et al. (2001). This galaxy has also been studied in
H{alpha} by Blais-Ouellette et al. (2004), which showed two velocity components
in its central region. The H{alpha} images presented in this paper have weaker
response on the receding side of the galaxy than on the approaching side due to
the wide span in the galaxy's velocities which made the receding emission fall
on the wing of the interference filter.

10. 2006ApJ...647..140F
Re:NGC 5055
This galaxy (T2, Sb/c) has five point sources in its nucleus, clustered close to
the center, and a bright hard source at the very center. The spectrum of this
source is well fitted by a two-temperature plasma model, but a power-law plus
plasma model gives a very poor fit. We did not attempt more complex models due
to the small number of degrees of freedom. Maoz et al. (1995) resolved the
central point source in the UV and obtained a radius of 7 pc (at the distance
assumed in this paper). Maoz et al. (2005) did not observe any variation of the
UV flux of this source. All of these pieces of evidence indicate that this
source is more likely a compact star cluster. This source is not detected at
various radio frequencies except at 57.5 MHz with S{nu}_ = 2.1 Jy (Israel &
Mahoney 1990), which means that this source is radio-quiet (R_X_ = -6) and not
likely to be an AGN. The stellar population of NGC 5055 has a range of ages from
1 Myr to 10 Gyr with most of the population of intermediate and old age
(Gonzalez Delgado et al. 2004; Cid Fernandes et al. 2004). Thus, the X-ray
emission of this LINER is powered by stellar processes.

11. 2006A&A...460...45G
Re:NGC 5055
NGC 5055 (M 63, UGC 8334). This galaxy shows a clearly unresolved nuclear source
coincident with the 2MASS position for the nucleus (Fig. 5). No previous Chandra
data have been reported. The only data available were ROSAT PSPC and HRI
observations (Read et al. 1997; Roberts & Warwick 2000) pointing to the
nucleated nature of this source within the low spatial resolution, 10" at best.
Recently, in the course of an investigation of ULX over a sample of 313 nearby
galaxies, Liu & Bregman (2005) found 10 ULX in this galaxy, one of which is
close to the nucleus with a variable luminosity between 0.96 and 1.59 x 10^39^
erg s^-1^ in 1.6 days.

12. 2005ApJS..160...76B
Re:NGC 5055
Low discordance and excellent S/N. Constant curve of growth and clear,
well-defined rotation. Patchy {sigma}_*_ field. See Figures 29 and 30d.

13. 2005ApJS..157...59L
Re:NGC 5055
This Sbc spiral galaxy at a distance of 8.5 Mpc show flocculent spiral arms in
the DSS image. ULX1 is close to but not the nucleus. ULX2 and ULX3 are on the
spiral arms. ULX4 (IXO 74) is on the outer edge of the galaxy. ULX4 showed a
luminosity drop from 9 * 10^39^ to 5 * 10^39^ ergs s^-1^ between two
observations separated by 3 years.

14. 2003AJ....126..742H
Re:NGC 5055
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."
3.32. NGC 5055
Figure 15 (bottom).
Spectra: Very strong continuum, which almost swamps the emission
lines. However, these faint emission lines show clear rotation.

15. 2002ApJS..142..223F
Re:NGC 5055
NGC 5055. NVSS detected a 265 mJy, the Green Bank survey a 124 mJy, and
FIRST a 20.2 mJy source. 1.4 GHz, 54" resolution observations (Condon
1987) detect an uncertain 22 mJy source. Moderate to high-resolution
observations at various frequencies either fail to detect or detect
uncertain, weak emission from this object, denoting that it is mainly
low surface brightness, arcsecond-scale emission (Condon & Broderick
1988; Condon et al. 1991a). The 0.2" resolution observations of Nagar
et al. (2000) give an upper limit of 1.1 mJy to any small-scale radio
emission at 15 GHz.

16. 2002ApJS..140..303L
Re:NGC 5055
NGC 5055 (Fig. 46).-NGC 5055 is similar to NGC 1097 in that the LINER
nucleus is surrounded by luminous young star clusters. The long-slit
HUT spectrum apparently includes some of these clusters. The spectrum
is too noisy for a rigorous analysis, but the broad C IV suggests an OB
population with a characteristic age of tens of Myr.

17. 2000ApJ...542..186N
Re:NGC 5055
NGC 5055.-The 20 cm FIRST map has peak flux density 1.5 mJy beam^-1^
and shows extended emission in P.A. 42^deg^ did not detect this galaxy
at 2 cm.

18. 2000ApJ...534..670T
Re:NGC 5055
NGC 5055.-The M/L in the disk region increases slowly by 3.0 times from
r = 5 to 15 kpc. In the bulge region its variation is difficult to
evaluate because of the insufficient resolution as well as because of
the large error in the luminosity profile caused by spiral arms. It
looks flat in the outer bulge and increases inward in the inner bulge

19. 1999ApJS..124..403S
Re:NGC 5055
5.15. NGC 5055
The extended gas distribution sharply peaks at the galactic center.
The velocity field is close to circular. Several gas clumps (GMAs) of
diameters about 10" (350 pc) and masses 1-3 x 10^7^ M_sun_ are seen in
the disk. There are two chains of GMAs to the south of the galactic
center, forming concentric arcs at radii of about 20" and 30".
Systematic velocity distortion is not evident on the arcs, though there
are random wiggles of velocity contours. A pair of gas spiral arms has
been identified in the disk of this galaxy by Kuno et al. (1997) and
Thornley & Mundy (1997a, hereafter TM97a). The latter group called the
arms "east" and "west" spiral arms. The outer arc in our map corresponds
to the west spiral arm, and the two GMAs on the arc are the GMAs 12 and
13 in TM97a. The inner string of GMAs, in which we identify four GMAs,
was not detected in the 7" resolution data of TM97a; the inner arc falls
on low CO intensity regions or voids in their maps. The inner string of
GMAs corresponds to the arc of H{alpha} and to the arc of excess K'-band
emission in the maps of TM97a. If the string is a part of the east
spiral arm, then the arm continues more than previously thought, as long
as 360^deg^. It is also possible that the inner arc does not connect to
the outer spiral arms. High-sensitivity observations of wider field of
view are necessary to obtain the complete picture of the spiral
features. In any case, the small radial separation between the arcs
helps to create the flocculent appearance of this galaxy.

20. 1997AJ....114.2428S
Re:NGC 5055
NGC 5055: The PV diagram shows a very steep rise within ~6" (210 pc) to a
velocity of V_i_~200 km s^-1^. Then, the rotation velocity is almost constant
till +/-40" (1.4 kpc).

21. 1996ApJ...469L..45T
Re:NGC 5055
NGC 5055.--The Sbc galaxy NGC 5055 (d = 7.2 Mpc) is one of the prototypes for
an Arm Class 3 flocculent galaxy (Elmegreen & Elmegreen 1987), but it shows
clearly a symmetric, two-arm spiral structure in the NIR (Fig. 3d). Each arm
extends over 150^deg^ in azimuth to a radius of 2.0' (4.0 kpc, 0.3 R_25_)
before decreasing in brightness. A ring of excess K' emission at a radius of
40" is coincident with a slight enhancement of H II regions seen in H{alpha}
images (Thornley et al. 1996). The bulge axial ratio indicated by inner
isophotes is 0.67, while the axial ratio of the disk at larger radii is 0.57,
which suggests that the bulge is triaxial.

22. 1995ApJS...98..477H
Re:NGC 5055
The emission-line spectrum is very weak and difficult to measure. After
removing the dominant stellar absorption spectrum, the emission-line
intensity ratios indicate a composite source of photoionization, although
the presence of a spatially resolved UV source (Maoz et al. 1995)
suggests that most of the ionizing radiation originates from young stars.

23. 1994CAG1..B...0000S
Re:NGC 5055
Hubble Atlas, p. 15
March 9/10, 1910
Seed 23 (blue)
300 min
NGC 5055 insert
May 14/15, 1926
180 min
The original plate used here as the main
print was taken by Ritchey in 1910 with the
newly completed Mount Wilson 60-inch reflector,
which many astronomers believe was the most
productive telescope of all time. The insert
negative print is made from the plate used for the
reproduction in the Hubble Atlas, taken by John
Duncan with the Mount Wilson 100-inch reflector
in 1926.
The quality of the images shows the superior
nature of both the 60-inch and the 100-inch
telescope optics in their ability to resolve to the
seeing limit of the Mount Wilson site (better than
0.4" under the best conditions).
The spiral pattern of NGC 5055 is similar
to those in four of the six galaxies on the preceding
panel. The inner region has very-high-surface-brightness
arms which thread throughout the disk.
These filamentary arms can be traced
as fragments almost to the center of the galaxy.
The surface brightness of the multiple-armed
pattern decreases abruptly at radius 50"
(2.7 kpc) from the center. The outer,
lower-surface-brightness multiple arm fragments,
together with their associated dust lanes, wind outward
and cover the extended disk, similar to the pattern
in the earlier Sb prototype NGC 2841
(panels 142, S4, S12).
Many small, generally unresolved HII
regions exist, the largest of which are less than
1.5" in diameter. The redshift of NGC 5055 is
small at v_o = 550 km/s.

24. 1976RC2...C...0000d
Re:NGC 5055
= M63
Ap. J., 148, 231, 1967.
L'Astronomie, 86, 137, 1972.
Astr. Ap., 29, 231, 1973.
Mem. S.A. Ital., 44, 65, 1973 = Cont. Asiago No. 284.
Photometry (5 Color):
A.J., 73, 313, 1968.
Photometry (UBV):
Ap. J., 143, 187, 1966.
Photometry (I.R. 1-3 microns):
Ap. J., 143, 187, 1966.
Ap. J. (Letters), 161, L203, 1970.
Ap. J., 163, 249, 1971.
Rotation Curve and Mass Determination:
Astr. Ap., 8, 364, 1970.
Ap. J., 184, 735, 1973.
HI 21cm:
Ap. J., 150, 8, 1967.
IAU Circ. No. 2330, 1971.
IAU Circ. No. 2332, 1971.
IAU Circ. No. 2333, 1971.
IAU Circ. No. 2334, 1971.
IAU Circ. No. 2336, 1971.
IAU Circ. No. 2338, 1971.
IAU Circ. No. 2341, 1971.
IAU Circ. No. 2347, 1971.
Ast. Tsirk. No. 630, 1971.
Ast. Tsirk. No. 648, 1971.
Yamamoto Circ. No. 1739, 1971.
Yamamoto Circ. No. 1740, 1971.
Publ.A.S.Japan, 23, 593, 1971.
Astr. Ap., 17, 146, 1972.
Astr. Ap., 22, 317, 1973.
L'Astronomie, 86, 137, 1972.
P.A.S.P., 85, 321, 1973.
Ap. J., 185, 303, 1973.
Mem. S.A. Ital., 44, 65, 1973.
Bull. A.A.S., 4, 320, 1972.
Radio Observations:
Ap. J., 144, 553, 1966.
Ap. J., 183, 791, 1973.
A.J., 78, 18, 1973.
Astr. Ap., 29, 231, 1973.
Astr. Ap., 31, 447, 1974.

25. 1973UGC...C...0000N
Re:UGC 08334
SA(rs)bc (de Vaucouleurs), Sb+ (Holmberg)
SN 1971i

26. 1964RC1...C...0000d
Re:NGC 5055
= Messier 063
Very small, very bright, stellar nucleus in a bright inner lens: 1.7 arcmin x
0.95 arcmin. Many filamentary, partially resolved arms. (r): 1.35 arcmin x
0.6 arcmin.
Lund 9 dimensions are much too small (rejected).
(B-V) is constant with log A/D(0); interpolated value.
Ap. J., 131, 282, 1960.
Ap. J., 134, 883, 1961.
Stockholm Ann., 15, No.9, 1949.
A.J., 66, 283, 1961.
Ap. J., 134, 880, 1961.
Lick Obs. Bull. 497, 1939.
Ap. J., 135, 698, 1962.
Ap. J., 135, 735, 1962.
Stockholm Ann., 17, No.4, 1951.
Orientation, Rotation, Mass:
Ap. J., 127, 487, 1958.
Ap. J., 131, 282, 1960.
Ap. J., 136, 352, 1962.
HII Regions:
Zeit. fur Ap., 50, 168, 1960.

27. 1961Hubbl.B...0000S
Re:NGC 5055
Messier 063
A-93 (100")
May 14/15, 1926
Enlarged 3.6X
The smooth-textured central region of this galaxy is only
6 sec of arc in diameter. Spiral arms can be traced to the
periphery of this central nucleus (6 sec of arc corresponds
to 1.4 mm on this illustration). The curious and significant
feature of this galaxy and all others that follow on
this and on the next page (NGC 3521, NGC 4699, NGC 1068, NGC 4736,
and NGC 4800) is the sharp discontinuity of surface brightness
of the spiral pattern between the inner and the outer regions.
The spiral structure is as pronounced and well
defined in the bright region as in the outer parts. The
important point here is that, if the inner arms were to
coalesce and to lose their identity as arms, the region would
look amorphous, would have a high surface brightness,
and would resemble the central regions of NGC 2841 and
NGC 0488, of the Sb galaxies, NGC 2775 (pg. 10), NGC 2811 (pg. 11), and
finally NGC 1302 (pg. 9) of the Sa galaxies, and all members of
the E and S0 classes. From the geometrical forms alone
we can place these closely coiled multiple-arm galaxies in
a sequence from Sc to Sa in the order NGC 3810 (pg. 30),
NGC 1232 (pg. 32), M101 (pg. 27), NGC 628 (pg. 29), NGC 1068 (pg. 16),
NGC 4699 (pg. 16), NGC 3521 (pg. 15), NGC 5055 (pg. 15), NGC 7217
(pg. 15), NGC 0488 (pg. 15), NGC 2841 (pg. 14),
NGC 2775 (pg. 10), NGC 3898 (pg. 10), NGC 2811
(pg. 11), NGC 6340, and NGC 1302 (pg. 9). In this order, the arms,
starting tangent to the central amorphous bulge, become
more tightly coiled, thinner, and more regular, and the
nuclear region grows at the expense of the arms. The
surface brightness of the central region appears to be
nearly constant whether it contains arms or amorphous

28. 1918PLicO..13....9C
Re:NGC 5055
Vol. VIII, Plate 46. A bright, beautiful spiral 8' x 3' in p.a. 98^deg^. Has an
almost stellar nucleus. The whorls are narrow, very compactly arranged, and show
numerous almost stellar condensations. See Abs. Eff. 33 s.n.

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