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Notes for object NGC 5248

19 note(s) found in NED.


1. 2012ApJ...754...67F
Re:NGC 5248
NGC 5248 .SXT4..-Has a prominent nuclear spiral clearly visible in HST F814W.
SAURON maps show the presence of a nuclear ring in H{beta} and [O III] emission.
A lowered [O III]/H{beta} shows that the ring is star-forming. The bulge was
classified as a pseudobulge by Fisher & Drory (2010). The rotational velocity
starts to flatten at about 6"-well inside the bulge radius of 15.4". The
velocity profile shows a shelf between ~=10" and ~=40". The velocity dispersion
profile is mostly flat at about 80 km s^-1^ with two small peaks at r ~= +/- 4".
The h_3_ moments are anti-correlated with velocity and reach values of up to
+/-0.1. The h_4_ moments scatter around values of 0.05.

2. 2009ApJ...697.1870E
Re:NGC 5248
NGC 5248 We were able to measure 13 offsets at r = 4.2-9 kpc (0.6'-1.4'), which
were found to be almost zero, while two spiral arms were clearly traced. Three
possible reasons for no observed offsets in NGC 4321 are also applicable to this
galaxy. In addition to a small bar with size of 0.4', Jogee et al. (2002) found
a large-scale stellar bar with a semimajor axis of 1.6', indicating that the
spiral structure seen in CO and H{alpha} could be inside the larger bar. They
also estimated R_CR_ ~ 1.9' from the assumed ratio of the corotation radius to
the bar semimajor axis (1.2), while Elmegreen et al. (1992) derived a comparable
value. Following the concept of the larger bar, Yuan & Yang (2006) developed a
nonlinear model for the spiral density waves excited by a bar potential, and
succeeded in explaining the observational features of this galaxy. Their orbits
show strong inward streaming motions along the spiral arm at r <~ 0.8', or 5.8
kpc using our distance. As we found that offsets of up to 1.4' in radius were
almost zero, this noncircular orbit can partially explain this feature.

3. 2008ApJS..174..337M
Re:NGC 5248
NGC 5248 (Fig. 5j).-Nineteen H II regions define the full, elliptically shaped
ring. The youngest H II region is located 4^deg^ away from of one of the bar
contact points (PA = 47^deg^).

4. 2007MNRAS.379.1249D
Re:NGC 5248
NGC 5248 is a nearby inactive spiral galaxy, and the control for both NGC 4051
and 6951. It harbours two prominent circumnuclear rings (Laine et al. 2001) and
an inner molecular spiral within 1.5 kpc driven by the large scale bar (Jogee et
al. 2002b). The arms of the spiral connect with the inner circumnuclear ring.
Jogee et al. (2002b) also mention the presence of streaming motions in this
galaxy.
The stellar continuum shows an elongated structure along the global disc
orientation at PA ~ 150{degrees} (Fig. 4d). The velocity field presents a
regular rotation pattern, the major-axis of which is oriented at a PA of
115{degrees}, aligned with the photometric major-axis (PA = 105{degrees}; Jogee
et al. 2002b). A {sigma}-drop is revealed by our velocity dispersion map in the
inner 3 arcsec with an amplitude of ~60 km s^-1^.
The H{beta} emission-line distribution shows a ring-like structure with a
radius of ~5 arcsec. The [O III] distribution is concentrated within the central
few arcsec, and in the two brightest peaks of the ring. This ring-like structure
corresponds to the known ring of the H II region described by Laine et al.
(2001). The [O III]/H{beta} emission-line ratio is lower inside the ring (0.15),
consistently with the presence of star formation, and rises slightly towards the
very centre (0.7). The ionized gas velocity field is dominated by rotation with
its major-axis aligned with the stellar kinematic one. The H{beta} velocity
dispersion map shows a depression in the star formation ring (50 km s^-1^), and
slightly rises towards the very centre (80 km s^-1^; Fig. B1). The [O III]
velocity dispersion map shows no specific features, with roughly constant values
around 50 km s^-1^.

5. 2003AJ....126..742H
Re:NGC 5248
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."
.
3.33. NGC 5248: A Stellar Nuclear Spiral Arm (GD?)
Figure 16 (top).
Spectra: The spectra show patchy H{alpha} and [N II] emission.
Continua are weak. A secondary continuum is present in OFF 2.
Classified in NED as either H II or Seyfert, but our spectra show no
evidence for broad lines.
Images: One of the clearest nuclear spirals in the sample. Laine et
al. (2001) have previously investigated the two-dimensional velocity
field of NGC 5248. They conclude that the pattern speed of the nuclear
spiral is the same as for the large-scale spiral structure, implying
that they are coupled. In the images shown here, only one spiral arm
is clearly present. The R-H color map shows it to be a blue feature,
probably a site of star formation.

6. 2002MNRAS.337..808K
Re:NGC 5248
A11 NGC 5248
Laine et al. (1999) used some of the optical data presented here, in
combination with our NIR data from Paper I and adaptive optics NIR imaging,
to describe the spiral structure in this galaxy at various scales,
including at scales of tens of pc, where it manifests itself in the form of
a nuclear grand-design spiral. We refer the reader to Laine et al. for a
description of the general disc morphology of NGC 5248, as well as of the
CNR. Further detailed studies of the CNR and host galaxy can be found in
Laine et al. (2001) and Jogee et al. (2002a,b). Our B-I colour index map
(Fig. 1k ) shows a pair of curved dust lanes emerging from the nuclear
region, more prominent southwest than northeast of the nucleus. Massive SF,
as measured by H{alpha} emission, is very strong in the CNR and in the
(non-active) nucleus, and is located mainly along the spiral arms in the
bar (see Jogee et al. 2002a ). The H{alpha} profile outlines the central
region with its peak in intensity, followed by a second maximum that
corresponds to the region of the arms where the SF is found. In the region
of the second maximum a small bump in the B - I colour profile is also
visible. The ellipticity and PA profiles are remarkably flat.
NGC 5248 (Fig. 2k) also exhibits massive SF sites mainly situated in the
nuclear ring, seen in H{alpha} and in the HST H-band image (Paper I). The
massive SF activity seems not to extend to the spiral arms and is confined
to the nuclear ring and the region immediately surrounding it.

7. 2002ApJS..143...73E
Re:NGC 5248
NGC 5248.---Sb: Nuclear point source embedded in a short, wide nuclear
bar. Nucleus/bar structure is further embedded in a luminous
elliptical bulge with a P.A. skewed ~45deg from that of the bar. Two
well-defined, asymmetric spiral arms appear in the inner disk. The
arms are rich in knots. The north arm turns through ~90deg and then
terminates abruptly. The surface brightness of the south arm drops
after ~90deg also, but the south arm can be traced beyond this point
for another ~90deg before fading from view. There are wispy, very LSB
features in the outer disk, mainly on the west side.

8. 2002AJ....124..675C
Re:UGC 08616
The S(1.4 GHz) = 128 mJy background radio source at
RA = 13 37 29.42, DEC = +08 55 01.5 has been excluded from the listed
flux density. See the 1.465 GHz C-array image in Hummel et al.
(1985).

9. 2001A&A...368...16M
Re:NGC 5248
38. NGC 5248 is an Sbc spiral of medium inclination. The outer arms have
very low surface brightness and are outside our field of view. NGC 5248
has a central ring of star formation of ~12" diameter
(Storchi-Bergmann et al. 1996). Inside this ring a tiny nuclear spiral
was discovered (Laine et al. 1999). These nuclear structures produce a
corresponding residuum pattern as result of our disk-bulge fit
(Fig. 6 in on-line version).

10. 2000MNRAS.317..234P
Re:NGC 5248
3.11 NGC 5248
NGC 5248 is a galaxy with an H II nucleus and a lot of SF activity in
the CNR. Elmegreen et al. (1997) found very conspicuous central spiral
arms, and several hotspots that form a ring-like spiral pattern. Buta &
Crocker (1993) detected a nuclear ring with a diameter of 10-17 arcsec.
This activity shows up clearly in our broad-band NIR images, as well as
in our colour index maps (Fig. 2k). Spiral structure with star-forming
arms, accompanied by dust lanes, is the dominant feature. The western
spiral arm has colours which are redder by about 0.1 mag in J-K than its
counterpart in the east. Our J-K image has been published earlier by
Laine et al. (1999). They compared it with the images obtained using
adaptive optics, which show a nuclear grand-design spiral structure.
This nuclear spiral, at scales of tens of parsecs, is not expected to
show up in a single broad-band NIR image, even at HST resolution, and in
fact does not show up (Fig. 1). The HST H-band image does show a wealth
of structure in the CNR, again in the form of emitting regions
distributed along spiral arm fragments, and accompanied by less luminous
regions which may well be dusty.
As in other galaxies, we can see the signature of the ring as a peak
at a radius of ~ 7 arcsec in all radial profiles. There is no evidence
for nested bars.

11. 1999ApJS..124..403S
Re:NGC 5248
5.17. NGC 5248
This galaxy shows a bisymmetric pair of gas spiral arms in the
central 4 kpc. Streaming motions on the arms are evident in the mean
velocity map and in the position-velocity diagram. Comparison with
optical and near-IR images in Laine et al. (1999) suggests that the gas
spiral features are a continuation of dust lanes associated with the
outer spiral features. Although NGC 5248 is thought to have a weak bar
(classified as SAB), it is hard to determine from optical images whether
the galaxy really has a bar or whether it just has a pair of open spiral
arms that looks like a bar with dust lanes at its leading edge. In the
former case the central molecular spirals may be the pseudoring at the
ILR of the stellar bar, while in the latter case the gas feature may be
a part of open spiral arms.
NGC 5248 is one of the hot-spot galaxies that have several bright
H II regions surrounding the nucleus (Morgan 1958; Kennicutt, Keel, &
Blaha 1989; Maoz et al. 1996). The H{alpha} hot spots in the image by
Pogge (1989) are located inside the gas spiral arms. Similar inside
offsets have been seen in the inner spiral feature at the ILR of another
hot-spot galaxy NGC 4321 (Sakamoto et al. 1995). The gas clumps on the
arms have sizes about 0.5-1 kpc, comparable to our resolution, and
masses ~ 3 x 10^8^ M_sun_.

12. 1998MNRAS.297..579C
Re:NGC 5248
NGC 5248. Both Ws and continuum ratios show the presence of aringat |r|=10
arcsec from the nucleus (Fig. 42). The values of Ca K and the G band are
typical of an S5 template at the nucleus, S6 at the ring and S4 at 15 arcsec
from the nucleus, decreasing to values typical of S6-S7 templates farther
out. Mg and continuum ratio values indicate redder templates, S4 at the nucleus,
S5 at the ring and S2-S3 at 15 arcsec, decreasing to S5-S6 farther out. Our
result for the nuclear stellar population is similar to that one obtained by
Bonatto et al. (1989).

13. 1994CAG1..B...0000S
Re:NGC 5248
Hubble Atlas, p. 33
Sbc(s)I-II
PH-209-MH
May 15/16, 1950
103aO
30 min
The two major spiral arms dominating the
inner disk of NGC 5248 have high surface
brightness, similar to the pattern in NGC 1566
(panel 171) and M51 (panel 172). The spiral
pattern breaks into three fragments of very low
surface brightness beyond the rim of the inner
disk. The two main spiral fragments of this outer
pattern are well defined and can be traced
outward for another half revolution.
Resolution into individual stars occurs at
apparent magnitude of about B = 22, which is
about 1 mag above the plate limit. The largest of
the numerous HII regions resolve at the 3" level.
The redshift of NGC 5248 is v_o = 1049 km/s.

14. 1976RC2...C...0000d
Re:NGC 5248
Description and Structure:
P.A.S.P., 77, 287, 1965.
P.A.S.P., 79, 152, 1967.
IAU Symp. No.38, 29, 1970.
Spectrophotometry:
Ap. J., 163, 249, 1971.
HII Regions and Distance Modulus:
Ap. J., 194, 559, 1974.
Dynamics and Mass Determination:
Ap. J., 184, 735, 1973.
Radio Observations:
Australian J. Phys., 21, 193, 1968.

15. 1973UGC...C...0000N
Re:UGC 08616
SAB(rs)be (de Vaucouleurs), Sc- (Holmberg)

16. 1964RC1...C...0000d
Re:NGC 5248
Extremely bright nucleus in a very bright lens with many dark lanes. Pseudo
(r): 2.4 arcmin x 1.1 arcmin. Bright part or lens: 3.6 arcmin x 2.1 arcmin.
Faint partially resolved outer arms form a pseudo (R): 6.6 arcmin x 4.5 arcmin.
Photograph, Rotation and Mass:
Ap. J., 136, 128, 1962.
HII Regions:
Zeit. fur Ap., 50, 168, 1960.

17. 1961Hubbl.B...0000S
Re:NGC 5248
Sc
PH-209-MH
May 15/16, 1950
103aO
30 min
Enlarged 5.0X
This magnificent Sc galaxy shows a high degree of symmetry.
The two principal inner spiral arms are of high
surface brightness. Both arms contain conspicuous dust
lanes on their inner edge. There is considerable dust
silhouetted against the central lens. It forms multiple spiral
lanes starting near the small nuclear region.
Five outer spiral arms of low surface brightness open
wide from the central regions. They can be seen in the
insert. The outer arms are branched. Two of the five hug
the bright central region on the west side; they are stubby
arms, of higher surface brightness than the remaining
three. Two other of the outer arms start from the end of
the bright inner arm at the northwest end of the major
axis and can be traced for about 180 degrees from the junction.
The remaining outer arm begins at the southeast end of
the major axis and spirals north through west. It is
branched at its northwest end.

18. 1956AJ.....61...97H
Re:NGC 5248
HMS Note No. 168
Broad absorption lines, fainter ones of poor visibility.

19. 1918PLicO..13....9C
Re:NGC 5248
A fine bright spiral 3.2' x 1.4' in p.a. 140^deg^. Very bright, elongated
nuclear portion 0.3' in length, a confused mass of bright nebulosity involving
numerous closely packed stellar condensations. Numerous almost stellar
condensations in the two bright, open whorls.


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