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Notes for object NGC 2903

29 note(s) found in NED.

1. 2009A&A...503..409H
Re:NGC 2903
In this galaxy, one of the Starburst supplement to the basic SINGS sample,
bright polarized arcs are detected along both sides of the minor axis trailing
away in brightness slowly to the northeast and more rapidly to the southwest.
The lowest brightness of polarized emission occurs on the receding major axis
(PA = 204^deg^, as tabulated in Table 1). The polarized fraction increases from
about 1% in the inner parts to about 5-15% at intermediate radii, to as high as
40%. The magnetic field vectors are roughly parallel to optical spiral arm
structures for the minor axis features, although generally with a slightly
larger radial component. Field lines run almost perpendicular to the linear
major axis feature. The Faraday depth distribution shows a small systematic
variation with PA in the minor axis features which we will comment on in Paper
III, together with a large systematic offset of these (by 60 rad m^-2^) relative
to the major axis feature. Very good consistency is found for the RMs toward
both lobe s of a double source in the field, suggesting a value of +3 +/- 1 rad
m^-2^ for the Galaxy in this direction.

2. 2008AJ....136.2648D
Re:NGC 2903
4.5. NGC 2903 was previously observed in H I by Begeman (1987). Figure 9
compares the two rotation curves. The Begeman (1987) value of V_sys_ = 557.3 +/-
1.3 km s^-1^ agrees well with our value of 555.6 +/- 1.3 km s^-1^. The outer
declining parts of the rotation curves also agree well with each other. There
are, however, significant differences in the inner, rising parts of the rotation
curve, where the curve by Begeman (1987) rises much more steeply. His data did
not allow a full tilted-ring model in the inner part of the galaxy, and the
sudden changes in P.A. and i are therefore also not detected in his analysis.
Rather, the innermost data points of the Begeman (1987) curve were derived from
a major axis position-velocity diagram. The higher spatial and velocity
resolution of our data and the different methods used to extract the velocities
both contribute to this large difference.

3. 2008AJ....136.2648D
Re:NGC 2903
6.4. NGC 2903 The surface brightness profiles of NGC 2903 are shown in Figure
29. The 2MASS J, H, and K profiles can be traced out to ~240", and the IRAC 3.6
{mu}m profile out to ~400". The break in the profile around 230" is due to the
sudden change in inclination at this radius. The profile can be decomposed into
two components: the inner one is modeled using an exponential disk with {mu}_0_
= 13.6 mag arcsec^-2^ and h = 0.17 kpc. For the outer disk, we used the observed
profile with the inner disk profile subtracted. At radii larger than 400" we
used an exponential extrapolation of the main disk. NGC 2903 shows a
well-defined color gradient. For the inner disk, we assumed {GAMMA}^3.6^_*_ =
1.3, which is the average value of {GAMMA}^3.6^_*_ within 20". For the outer
disk, we assumed {GAMMA}^3.6^_*_ = 0.75 in the innermost parts and
{GAMMA}^3.6^_*_ = 0.4 in the outermost parts. Between 20" and 150" we adopted
the observed {GAMMA}^3.6^_*_ profile. The rotation curve models for NGC 2903 are
shown in Figure 30. It is immediately obvious that the inner part of NGC 2903 is
not well fitted by the models. The models with {GAMMA}^3.6^_*_ fixed severely
overpredict the data independent of IMF. Models with {GAMMA}^3.6^_*_ as a free
parameter can only approximately fit the data by setting {GAMMA}^3.6^_*_ = 0 for
the inner disk. This large discrepancy is most likely due to the bar. A harmonic
decomposition of the velocity field shows significant noncircular motions in the
inner 1 kpc (Trachternach et al. 2008). Because of the low quality of the fits,
we do not list them in Tables 3-6. An additional source of uncertainty could be
the presence of a very dense inner molecular disk, with significant amounts of
associated star formation (Planesas et al. 1997). We performed an extra set of
fits to those parts of the rotation curve that are unaffected by the central
noncircular motions (the flat part of the curve at R>3.3 kpc). These are shown
in Figure 31. We find that with {GAMMA}^3.6^_*_ as a free parameter, the
resulting disk is dynamically more significant than predicted by population
synthesis models and (J - K) colors. The ISO model prefers a dynamically
insignificant central component, whereas the NFW model prefers a central
{GAMMA}^3.6^_*_ value close to the predicted one. Here also, the main disk is
found to be more massive than predicted by the colors. The NFW model fits better
than the ISO model but due to the presence of the noncircular motions, it is not
clear whether this can be generalized to the entire rotation curve. For fixed
{GAMMA}^3.6^_*_, the ISO model demands an extremely small core radius R_C_ and a
very large central density {rho}_0_ in order to produce the flat halo rotation
curve shown in Figure 31.

4. 2005MNRAS.360.1201H
Re:NGC 2903
NGC 2903. This starburst galaxy shows several peaks of star formation in the
circumnuclear region. These peculiar 'hotspots' have been identified and
described in different ways by various authors in H{alpha} (Marcelin, Boulesteix
& Georgelin 1983), in radio and in the IR by Wynn-Williams & Becklin (1985). A
strong velocity gradient can be seen along the bar in the velocity map. The PV
diagram shows a clear step in the RC. This step-like structure could be related
to its strong bar. The molecular gas, visible in CO observations (Helfer et al.
2003), follows the bar.

5. 2005MNRAS.357..361S
Re:NGC 2903
NGC 2903. The bar of this spectacular spiral is clearly seen at both 450 and 850
{mu}m. The ~125-arcsec submillimetre bar corresponds to 5.5 kpc at the
assumed distance of NGC 2903. Knots of bright submillimetre emission are seen
along the length of the bar as well as along the spiral arms attached to the bar
ends. There is a very high submillimetre contrast between the bar/arm regions
and the inter-arm regions and a bright unresolved galactic core is seen in the
submillimetre. There is some danger that we may have chopped some weak extended
emission out of this image.

6. 2005ApJS..160...76B
Re:NGC 2903
High level of discordance but S/N is good. Clear rotation and an irregular
{sigma}_*_ field. MPL did not converge in the central aperture. A known
starburst with a circumnuclear ring (Alonso-Herrero, Ryder, & Knapen 2001). See
Figures 9 and 10d.

7. 2005ApJS..157...59L
Re:NGC 2903
This barred Sbc spiral is a starburst galaxy at a distance of 7.4 Mpc. ULX1 is
on the edge of a spiral arm.

8. 2003ApJS..146..353M
Re:NGC 2903
NGC 2903 (C)
The well-known "hot spot" galaxy has a large number of resolved
circumnuclear star clusters, although there is only one dust lane with
sufficient curvature to suggest spiral structure. Because there are no
other, similar features, this is not classified as a nuclear dust

9. 2003AJ....126..742H
Re:NGC 2903
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."
3.8. NGC 2903 (C) (C-mp)
Figure 4 (top).
Spectra: They show strong emission, although the continuum is strong
only in the NUC spectrum. Rotation is clear on large scale. There is
secondary continuum in the OFF 1 spectrum.
Images: A hotspot galaxy; Alonso-Herrero, Ryder, & Knapen (2001) find
a circumnuclear star formation ring of diameter 625 pc in their
HST/NICMOS images. This ring would appear just outside of our images.

10. 2002MNRAS.337..808K
Re:NGC 2903
A3 NGC 2903
NGC 2903 is a 'hotspot' galaxy with a circumnuclear starburst. The B-I
colour map reveals a beautiful and complex multi-armed dust structure, but
no clear pair of dust lanes in the bar (Fig. 1c). In the H{alpha} images we
see SF along the bar and in the arms, mostly in the southern arm, and in
the CNR. Very luminous HII regions delineate the bar and arms in this
galaxy. The H{alpha} profile drops smoothly, outlining continuous and
strong HII emission all the way from the centre to the ends of the bar, and
further out into the disc. The profiles show a lot of structure throughout
the CNR and disc, caused by the combined effects of dust extinction and SF
activity. Blue dips in the B-I profile are accompanied by enhancements in
the H{alpha} and in some cases the B profiles. No NIR PA and ellipticity
profiles are given because these could not be fitted in Paper I.
The H{alpha} emitting regions do not all correspond in position and
intensity to the NIR hotspots (Fig. 2c). Our H{alpha} image shows just
three of them, whereas our ground-based NIR images, and especially the HST
NIR image (Paper I), show a plethora of individual emitting regions. A
detailed study of the SF properties of the CNR in this galaxy, using HST
archival H{alpha} and Pa{alpha} imaging and NIR spectroscopy, in
combination with stellar population synthesis modelling, has recently been
published by Alonso-Herrero, Ryder & Knapen (2001).

11. 2002ApJS..140..303L
Re:NGC 2903
NGC 2903 (Fig. 43).-Both the continuum and the line profiles are well
reproduced by a model of age 50 Myr. The fit is as good as those to the
10 galaxies that we used to derive the obscuration curve. NGC 2903 was
excluded, since the longer wavelength IUE data suggest late-type stars.
These stars are not seen in the HUT data. The apparent flattening
longward of 1600 {Angstrom} could be explained in principle by
blanketing effects due to OB stars. In the absence of information from
longer wavelengths, however, we cannot exclude a contribution from an
older population.

12. 2002AJ....124.2581S
Re:NGC 2903
NGC 2903 (Fig. 1): The stellar bar in NGC 2903 is
oriented at a position angle (P.A.) of 24^deg^ east
of north. The molecular gas is distributed toward
the leading side of the stellar bar, with a P.A.
of ~30^deg^. The H{alpha} emission is offset even
farther toward the leading side of the CO emission.
In the northern half of the bar, the CO emission
is brightest in a large complex labeled "C1." A bright
H{alpha} complex, H1, coincides with part of the
C1 complex. South of C1 by 3"-4" is a narrow ridge
of CO, labeled "C2," which bridges C1 with the bright
circumnuclear gas. Several discrete H{alpha} features
(H2, H3, H4, and H5) are seen on the leading side of
the CO. These structures are connected by a diffuse,
concave ridge of H{alpha} emission. On the trailing
(upstream) side some diffuse H{alpha} emission is
present, but there is a conspicuous lack of H II
regions; this is not an artifact of dust extinction.
In the dust lanes the dust extinction is usually
insufficient to hide H II regions (e.g., Regan &
Vogel 1995). Also, the gas density is expected to be
dramatically lower on the trailing side of the dust
lane as the gas piles up in the bar dust lane
(e.g., see model density distributions in Combes &
Gerin 1985; Athanassoula 1992b; Piner, Stone, &
Teuben 1995).
In the southern half of the bar, there are two
bright CO complexes, C3 and C4. As in the northern
half, H{alpha} complexes (H6, H7, and H8) are all on
the leading side of the CO emission. A diffuse ridge
of H{alpha} emission extends south of H7, with a
P.A. of ~5^deg^, on the leading edge of the CO
emission. In this half of the bar we also see a weak
CO spur, labeled "C5," east of C4 on the trailing
side of the dust lane. Diffuse H{alpha} emission is
present at the trailing edge of C5. In two places,
near H7 and north of H6, there is weak CO emission
on the leading side of the dust lane.

13. 2002AJ....124..675C
Re:UGC 05079
Very extended NVSS source.

14. 2000MNRAS.317..234P
Re:NGC 2903
3.3 NGC 2903
Fig. 2(c) shows several peaks of SF in the CNR of the starburst galaxy
NGC 2903, which, as expected, are resolved in much more detail in the
HST NICMOS image we obtained from the HST archive (Fig. 1). These
peculiar 'hotspots' in the nuclear region have been identified and
described in different ways by various authors. Marcelin, Boulesteix &
Georgelin (1983) found six 'hotspots' forming a linear structure that
crosses the central region. A later study in infrared and radio by
Wynn-Williams & Becklin (1985) showed that bursts of SF were not
confined to the visible hotspots. Simons et al. (1988) noticed the
presence of organized dust structure in the CNR using NIR and optical
imaging. We see patches of dust in our images, but no coherent
Regan & Elmegreen (1997) found, using a K-band image of the inner bar
region, that this galaxy has an isophotal twist, although the results
from an earlier study by Elmegreen et al. (1996) were ambiguous. Similar
twists have been interpreted as nuclear bars or triaxial structures
(e.g. Friedli & Martinet 1993; Shaw et al. 1995; Wozniak et al. 1995).
However, our images show such an abundance of structure that it is hard
to imagine that the measured changes in the radial behaviour of
ellipticity or PA would have any significance in this respect. For that
reason, we set the ellipticity and the PA to fixed values corresponding
to the parameters of the isophotes on the outskirts of our images when
we fit our radial colour profiles.
As in e.g. NGC 1300, the circumnuclear ring-like region of enhanced
SF shows up in the surface brightness profile as a change of slope, and
in the colour profiles as a significant red bump at the same radius.
Our colour index maps suggest that the nuclear hotspots may be part
of a pseudo-ring. We can identify more than six clumps in the broad-band
images, and even more in the colour index map. This is in good agreement
with the idea that obscuration by dust is the reason for a previous
underestimate of the extent of this SF region (cf. Jackson et al. 1991).
As in NGC 1530, we see significant emission from SF regions in the NIR,
including the K band, which must at least in part be due to red
supergiant emission. The red J-K and H-K colours of these regions make
them stand out clearly in the colour index maps.

15. 2000ApJ...534..670T
Re:NGC 2903
NGC 2903.-Both the SMD profile and {mu}(r) have a remarkable bump at
r ~ 2 kpc. Since the shape of the RC is also peculiar, we may not
neglect the effect of a nonaxisymmetric component such as caused by a
spiral arm. Interestingly, however, there appears no corresponding bump
in the M/L. The M/L in the disk region increases slowly by 5.5 times
from r = 4 to 9 kpc. This Sc galaxy has a compact bulge, and we cannot
evaluate the M/L of the inner bulge because of the insufficient spatial

16. 2000A&AS..142..425D
Re:NGC 2903
3.3 NGC 2903 = UGC 5079 = KIG 347 = PGC 27077 = IRAS 09292+2143
This large (12.6' x 6.0') bright (B_T_ = 9.68) spiral galaxy similar to
M 81 still remained unresolved into stars. In its wide vicinity there is
no other bright galaxy. This is why Karachentseva (1973) included
NGC 2903 in her Catalog of isolated galaxies (KIG). Within 3^deg^ around
NGC 2903 there are two dwarf galaxies: UGC 5086 and F565-v1 imaged by
Makarova & Karachentsev (1998). An image of NGC 2903 from the Digital
Sky Survey is shown in Fig. 6. Our two CCD frames indicated by the boxes
cover the basic part of its spiral pattern except the faint outer arms.
Reproductions of the northern and southern CCD images are presented in
Fig. 7 after subtracting frames smoothed with a median filter of
10x FWHM window. The results of the photometry of 273 brightest stars
are shown in V proportional to V-I diagram (Fig. 8). As in the case of
NGC 2683, slightly diffuse objects prevail amongst the brightest blue
ones. They are probably compact H II regions and multiple stars. As blue
supergiant candidates, we pick three stars. Their mean apparent
magnitude, 20.27, yields with galactic extinction of 0.07^m^ a distance
modulus of 29.74 or D = 8.9 Mpc. Being located in the same Leo spur
cloud as NGC 2683, the spiral galaxy NGC 2903 has also a low
radial-velocity to distance ratio: H= V_0_/D= 50 km s^-1^/Mpc (line 14
in Table 2).

17. 1999ApJS..124..403S
Re:NGC 2903
5.3. NGC 2903
The data of NGC 2903 are taken from Ishizuki (1993). The gas
distribution in NGC 2903 is not well resolved in the integrated
intensity map. However, there is a dip in the position-velocity map
around the systemic velocity, and the high- and low-velocity gases in
the channel maps are associated with radio continuum peaks to the north
and south of the nucleus respectively, implying twin peaks or ring
structure. This barred galaxy has circumnuclear star-forming regions
(hot spots) within a diameter about 10" or 300 pc (Wynn-Williams &
Becklin 1985). Radio continuum peaks are aligned on an ellipse with twin
prominent peaks on the opposite side of the major axis. If the
star-forming ring is associated with a molecular ring, as hinted from
the position-velocity map, it may be due to the ILR of this barred

18. 1998PASJ...50..427S
Re:NGC 2903
NGC 2903: The H{alpha} and [N II] lines show an almost identical
behavior both in the PV and intensity plots. The HNR is also normal, as
for in the H II regions. The nuclear component shows tilted double peaks
in the PV diagram, indicating a rotating ring of radius 4" comprising
H II regions. After decreasing to a minimum at R ~ 25", the disk
rotation gradually increases until R ~ 50"; it then increases suddenly,
with a step, to a maximum at R ~ 70", followed by flat rotation. This
step-like rotation may be related to its barred structure.

19. 1997AJ....114.2428S
Re:NGC 2903
NGC 2903: The PV diagram shows a steep rise within the central 7" (280 pc) to
V_rot_~160 km s^-1^. and has a maximum at ~15" (600 pc) at V_rot_~250 km s^-1^.
The main ridge of the PV diagram in the southern part has a peculiar step at 1'
(2.4 kpc) radius, with a flat part of about 170 km s^-1^ till 1', and, then,
steps up to a flat part at 200 km s^-1^. The outer rotation from H I, however,
is very flat until the edge.

20. 1994CAG1..B...0000S
Re:NGC 2903
Hubble Atlas, p. 35
Feb 15/16, 1950
30 min
NGC 2903 is nearby, as judged by the
degree of resolution into individual stars beginning
at about B = 22 in the two very-low-surface-brightness
outer spiral arms. Resolution is not as
easy as in M101, but is much easier than in any
of the Virgo Cluster spirals such as M100. The
redshift of NGC 2903 is v_o = 472 km/s.
The surface brightness of the inner spiral
pattern is exceptionally high. The arm pattern is
thick. In addition to the two main arms, well seen
in the print at the right, the outer arm pattern is
multiple, filling the disk. On the short exposure
on the right, the central pattern is a weak bar
from which one of the two principal arms springs.
The opposite arm forms part of the slightly
curved bar on that side.
The dust lanes throughout the disk are
spiral fragments. Their opening (pitch) angles
near the edges of the bar are very steep (the lanes
begin almost perpendicularly to the bar), flattening
to the pitch angles of an ordinary non-barred
spiral in the outer pattern. These dust lanes
undoubtedly trace the flow pattern of the
interstellar medium as its hydrodynamic response to
the gravitational potential of the rotating bar,
including shocks near the leading edges of the bar
(e.g., Huntley 1978, 1980, and references therein).

21. 1994CAG1..B...0000S
Re:NGC 2903
Hubble Atlas, p. 35
Feb 5/6, 1962
103aE + H{alpha} interference
90 min
The weak bar pattern is seen well in this H{alpha}
interference filter photograph taken with the
Palomar 200-inch Hale Telescope. The bar is not
well defined but is definite. It can also be seen as
an intensity enhancement across the disk in the
continuum photograph on the left.
The dust lanes along the bar on either side,
situated as usual on the leading edges of the bar
relative to the direction of rotation, are characteristic
of dusty barred spirals. They are thought
to be the result of shocks in the vicinity of the bar
caused by the bar's rotation (Prendergast 1962,
1983; Peterson and Huntley 1980; Huntley
1978, 1980).
The largest HII-region complexes seen here
have core + halo diameters of about 6". The
redshift of NGC 2903 is small, at v_o = 472 km/s.
Note the difference in the enlargement of
this image compared with that at the left.

22. 1993ApJS...86....5K
Re:NGC 2903
NGC 2903; Sbc, hot spot.
NGC 2903 contains active star formation within its hot spot knots and
also throughout its entire nucleus (Bonatto, Bica, & Alloin 1989). The UV
spectrum has deep, complex absorption features of a starburst galaxy, but
with a slope increasing toward long wavelength. This slope, as well as
the complex absorption features across the entire IUE wave band,
indicates the presence of a mixture of early and late-type stars, which
is consistent with the conclusions of Oka et al. (1974) based on optical
observations. Simons et al. (1988) note that the "patchy" appearance of
the central regions in the V band is due to a variation of internal
extinction. The Mg II absorption feature is too strong to be due to
Galactic absorption alone (see Table 4).

23. 1976RC2...C...0000d
Re:NGC 2903
Description and Classification:
P.A.S.P., 79, 152, 1967.
P.A.S.P., 81, 51, 1969.
IAU Symp. No. 38, 29, 1970.
Small interacting group 33 arcmin west-south-west (V = 10,200 km/sec):
Ap. J., 183, 791, 1973.
Ann. Ap., 28, 698, 1965 = Publ. O.H.P., 7, No. 50.
IAU Symp. No. 29, 434, 1968.
P.A.S.P., 81, 51, 1969.
Astr. Ap., 29, 231, 1973.
Ap. J., 194, 559, 1974.
Publ. A.S. Japan, 26, 289, 1974.
A.J., 73, 313, 1968.
A.J., 74, 344, 1969.
Publ. A.S. Japan, 26, 289, 1974.
Photometry: (I.R.: 10, 21 microns)
Ap. J. (Letters), 176, L95, 1972.
Spectrum and Systemic Velocity Field:
Ap. J., 159, 405, 1970.
Bull. A.A.S., 3, 352, 1971.
Bull. A.A.S., 6, 321, 1974.
Publ. A.S. Japan, 26, 289, 1974.
Ap. J., 163, 249, 1971.
Ap. J. (Letters), 193, L49, 1974.
Astr. Ap., 19, 405, 1972.
Astr. Ap., 27, 433, 1973.
Sov. A.J., 13, 593, 1970.
Astrofizika, 7, 417, 1971.
Rotation Curve and Mass Determination:
Astr. Ap., 8, 364, 1970.
Ap. J., 184, 735, 1973.
HII Regions:
Ann. Ap., 28, 698, 1965 = Publ. O.H.P., 7, No. 50.
"Atlas and Catalogue", Univ. Washington, Seattle, 1966.
Ap. J., 155, 417, 1969.
Ap. J., 194, 559, 1974.
Bull. A.A.S., 5, 349, 1973.
Distance Modulus:
Ap. J., 194, 559, 1974.
Radio Observations:
Austral. J. Phys., 16, 360, 1963.
Ap. J., 144, 553, 1966.
Ap. J., 150, 413, 1967.
Ap. J., 183, 791, 1973.
A.J., 78, 18, 1973.
Astr. Ap., 29, 231, 1973.

24. 1973UGC...C...0000N
Re:UGC 05079
SAB(rs)bc (de Vaucouleurs), Sc- (Holmberg)
UGC 05086 at 9.6, 105

25. 1964RC1...C...0000d
Re:NGC 2903
Very bright nucleus in a short bright bar. Complex pattern of bright,
partially resolved arms. Pseudo (r): 2.5 arcmin x 1.4 arcmin. Weak,
partially resolved outer arms.
NGC 2905 is a detail.
Unusual (B-V) relation in nucleus (emission?).
Ap. J., 132, 640, 1960
P.A.S.P., 75, 222, 1963.
Ap. J., 50, 384, 1919.
IAU Symp. 5, 1958 = Lick Cont., II, No 81, 1958.
Ap. J., 135, 698, 1962.
Rotation and Mass:
Ap. J., 132, 640, 1960.
HI Emission:
A.J., 66, 294, 1961.
A.J., 67, 437, 1962.

26. 1961Hubbl.B...0000S
Re:NGC 2903
Feb. 15/16, 1950
30 min
Enlarged 1.3X
The internal pattern of dust is almost as intricate in NGC 2903
as it is in NGC 0253. The galaxy is seen more nearly
face on, and is more distant than NGC 0253, so that the delicate
dust filaments threading across luminous regions are lost
in NGC 2903, but there is no question that these patterns are
present. The nucleus is composed of about eight intense
knots, presumed to be giant HII regions. The repro-
duction is overexposed in the central regions and does
not do justice to the intricate pattern. Two thin, regular
spiral arms are present in the outer regions of NGC 2903.

27. 1956AJ.....61...97H
Re:NGC 2903
HMS Note No. 061
Hydrogen absorption lines wide and strong.
Faint condensation 78 arcmin [south-west] of nucleus on the major axis
shows no emission lines on a plate taken 1950 Mar 13.3, 6h, IIa-0,
slit 4 arcsec x 2 arcmin in position angle 130 deg.

28. 1918PLicO..13....9C
Re:NGC 2903
Vol. VIII, Plate 20. A beautiful, bright spiral 12' x 5' in p.a. 18^deg^. Large,
confused nuclear portion containing five rather nebulous condensations.
Whorls rather open, showing numerous condensations. Traces of the {phi}-type
formation. See Abs. Eff. 7 s.n.

29. 1918PLicO..13....9C
Re:NGC 2905
Vol. VIII, Plate 20. A beautiful, bright spiral 12' x 5' in p.a. 18^deg^. Large,
confused nuclear portion containing five rather nebulous condensations.
Whorls rather open, showing numerous condensations. Traces of the {phi}-type
formation. See Abs. Eff. 7 s.n.

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