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Notes for object NGC 3504

23 note(s) found in NED.


1. 2008MNRAS.388..500E
Re:UGC 06118
UGC 6118 (NGC 3504). This early-type galaxy presents an almost circular outer
ring, and a thin bar (more visible in JHK band from NED) embedded in a rather
oval structure (axial ratio ~0.5). A bulge is visible in the near infrared
images. The agreement between our H{alpha} map and the one from Hameed &
Devereux (2005) is very good. The main bar has a size ~1.2 arcmin. A secondary
bar may be suspected in the first ~20 arcsec around the very bright H{alpha}
nuclei. An H{alpha} spiral structure is observed within the oval structure
starting at the end of the inner bar. We find the major kinematical axis to be
almost parallel to the bar and the oval structure. Our H{alpha} velocity field
is almost limited to the central oval structure and the bar, with only a few
points in the outer ring. A steep inner rise of the velocities is observed in
the galaxy core, otherwise the H{alpha} velocities remain roughly constant
before 45 arcsec, radius beyond which they begin to increase slightly. This is
not observed in th e H I position-velocity diagram from WHISP (Noordermeer et
al. 2005), and the H I rotation curve slightly increases all along the first
arcminute. Their H I velocity field perfectly covers the outer ring and leads to
an inclination of 39^deg^. The morphological inclination deduced from the outer
ring is ~27^deg^,, while the inclination of the oval structure is ~45^deg^. The
kinematical inclination of 52^deg^ deduced from our H{alpha} velocity field is
consistent with the inclination of the oval distortion. Nevertheless, we
computed the rotation curve using the H I inclination because our kinematical
inclination mainly relies on velocities measured within the central oval
structure. The central region of the velocity field within the bar displays an
S-shape pattern encircling two symmetric velocity peaks leading to two strong
bumps on the rotation curve (at ~0.5-1 kpc). Our H{alpha} rotation curve is in
good agreement with the long-slit observations of Usui, Saito & Tomita (2001).

2. 2005MNRAS.364..283E
Re:NGC 3504
NGC 3504. Bar measurements are from a BARS Project I-band image from the NOT (no
R-band images are available). Outer disc orientation is from Grosbol (1985) and
Kenney, Carlstrom & Young (1993). Although the inclination is uncertain,
deprojection is not a major issue given that the bar is almost aligned with the
outer-disc major axis.

3. 2005A&A...442..137N
Re:UGC 06118
The central hole in the disk of UGC 6118 (NGC 3504) is not due to a true absence
of gas, but rather an artefact caused by H I absorption against a central
continuum source (see also UGC 2487).

4. 2004MNRAS.355.1251L
Re:NGC 3504
NGC 3504 (Fig. 8e, available in the online version; see also Fig. 2).
This is another example of a bar/ring system with prominent spiral
arms, which are forining a ring. This is a good example of galaxies
showing a bar with two blobs at the ends of the bar, manifesting also
some spiral-like characteristics. The amplitude profile also has two
peaks in the bar region. In this case, the tiny spiral arm segments are
not related to the outer spiral arm structure, being rather part of the
bar/inner ring system. The Q_T_ profile is asymmetric, but in the
opposite direction than in NGC 5101. The outer pseudo-ring of NGC 3504
is type R'_1_ (appendix 3 of RC3).

5. 2004A&A...415..941E
Re:NGC 3504
NGC 3504: Perez-Ramirez et al. (2000) noted a possible inner bar in this SBb
galaxy, but also an apparent double nucleus. This latter feature makes it
difficult to be certain about the inner bar.

6. 2003ApJS..146....1W
Re:NGC 3504
NGC 3504.-Although the S/N ratio in this spectrum is low (3.3 per
resolution element), the Galactic O VI line clearly is very weak. The 3
{sigma} limit for the -70 to 70 km s^-1^ velocity range is
190 m{angstrom} [log N(O VI) < 14.19]. Just 1deg away lies Mrk 36, toward
which W(O VI) = 232 +- 57m{angstrom}. The intrinsic Ly{beta} line in
NGC 3504 is clearly visible and centered at about 1370 km s^-1^. The
galaxy's spectrum further shows a depression in the region between 1030
and 1040 {angstrom}. This makes the flux near the Galactic O VI
absorption rather low, and the resulting upper limit rather high.

7. 2002MNRAS.337..808K
Re:NGC 3504
A5 NGC 3504
NGC 3504 is an inclined barred galaxy with a nuclear starburst. The double
nuclear peak seen in the NIR (Paper I) does not show up in our optical
images owing to the limited spatial resolution. The B-I colour map shows
two curved dust lanes in the bar region, but very little organized dust in
the disc region (Fig. 1e). In our H{alpha} image, we see an elliptical
region around the nucleus, where SF activity is intense. Outside the CNR,
the most luminous HII regions are found near the ends of the bar, but SF is
also prominent in the rest of the surrounding disc structure. The radial
H{alpha} profile shows a decrease from the nucleus to the radius
corresponding to the end of the bar, where enhanced SF activity causes a
local maximum in the profile. The B-I radial profile shows a blue peak at
the same radius, of about 50 arcsec. The values for the B-I colour are
between 1.5 and 2. The central H{alpha} emission in NGC 3504 (Fig. 2e) is
elongated in the direction of the double nucleus, as discussed in Paper I.

8. 2002ApJS..143...73E
Re:NGC 3504
NGC 3504.---(R)SB(r)a: Bright nuclear point source in a small slightly
elliptical bulge. Bulge is threaded by a thin, well-defined bar. Ansae
at the ends of the bar form the base of the spiral arms. The arms wrap
into an inner ring and then peel off to form a broken outer
pseudoring. There are a few knots in the ansae, but little other
evidence of ongoing star formation.

9. 2001AJ....121.2483U
Re:NGC 3504
NGC 3504. - The major axis almost coincides with the direction of a bar.
The H{alpha} emission is strong at the nucleus and the ends of the bar. The
rotation curve rises steeply, and there are bumps around 0.5 kpc. The
similar feature is also seen in some galaxies observed by Rubin, Kenney,
& Young (1997). The H{alpha} emission is the weakest, and both the
[N II]/H{alpha} and [S II]/H{alpha} are the highest between the nucleus and
the ends of the bar. These regions may be shock-excited, induced by the
bar. While the [S II]/H{alpha} of other regions is typical of H II regions,
the [N II]/H{alpha} is enhanced also in the nuclear region. HFS97
classified the nucleus of this galaxy as H II region based on the weak
[O I] emission, consistent with our observation.

10. 2000MNRAS.317..234P
Re:NGC 3504
3.5 NGC 3504
Our NIR imaging of this barred galaxy reveals a lot of structure,
including a double peak in the central part of the NIR broad-band images
(Fig. 2e). Recent adaptive optics images obtained with the CFHT (by
F. Combes & J. H. Knapen, private communication) confirm this double
peak, but spectroscopic follow-up observations are needed to confirm
whether these peaks are in fact two nuclei. No HST NIR imaging is
available.
The colour index images show a pair of long and straight dust lanes
that come into the CNR through the main bar, and intricate dust lane
structure in the central region. The nuclear double peak is very obvious
in the colour index maps. Elmegreen et al. (1997) showed a ring in J-K
with five discrete clumps of SF. The signal-to-noise ratio in our images
is too low to reveal these SF clumps.
The previously reported isophote twist (e.g. Pompea & Rieke 1990) is
obvious from our imaging, as well as from the PA and ellipticity
profiles. The double bar, outlined by the two separate peaks in the
ellipticity profile, is most probably not exclusively due to the nuclear
double peak, because the accompanying isophote twist in fact starts
somewhat outside the region of influence of the double peak. The surface
brightness and colour profiles show the hump at the CNR radius that is
seen in many similar galaxies presented in this paper.

11. 2000ApJ...530..688A
Re:NGC 3504
NGC 3504.-This galaxy has been classified as a weak-[O I] LINER (Ho
et al. 1993) and as a H II region (Ho et al. 1997a). In Alonso-Herrero
et al. (1997) we presented H and K-band spectroscopy of this galaxy and
concluded that the LINER characteristics of NGC 3504 could be easily
explained with the presence of a recent starburst. The age of the burst,
based on the [Fe II] 1.257 micron/Pa{beta} line ratio would be very
similar to that of NGC 253. From Table 7 and Figure 8 it is clear that
the optical line ratios of this galaxy are well reproduced with an H II
region photoionized with stars with temperature T = 38,000 K without the
presence of very hot stars.

12. 1999ApJ...524..684G
Re:NGC 3504
NGC 3504 is a barred starburst nucleus originally included on Sersic's
list of peculiar nuclei (Sersic 1973). The nuclear radio emission
comprises a compact, unresolved core surrounded by a ~10" diffuse halo
(e.g., Saikia et al. 1994). The halo probably traces synchrotron
emission from a 12" diameter starburst ring, revealed in near-infrared
color maps (Elmegreen et al. 1997). Dickey (1986) reported a tentative
detection of H I absorption. We clearly detect an absorption line
toward the unresolved radio nucleus of this galaxy.

13. 1999A&AS..135..437G
Re:NGC 3504
NGC 3504. This Sb galaxy (Sandage & Bedke 1994) has a "composite"
nucleus showing both non-thermal activity and recent star formation, the
optical spectrum being dominated by the regions of stellar activity
(Keel 1984). Ho et al. (1993a), who published line ratios for this
object, suggested that it could be a "transition" between a H II region
and a Liner, but Ho et al. (1997a) called it a H II region. Fitting our
red spectrum with a single set of Gaussians does not give a satisfactory
fit and indicates the presence of weak broad wings in the [N II] lines;
two sets of Gaussians are needed, revealing the presence of a weak
Seyfert-like nebulosity with {lambda}6583/H{alpha} = 1.87. The blue
spectrum was also fitted by two sets of Gaussians satisfying,
respectively, {lambda}5007/H{beta} = 0.1 and {lambda} 5007/H{beta} = 10.
The NGC 3504 spectrum is therefore "composite" and dominated by a
starburst; a weak Seyfert feature is also present. No component showing
Liner characteristics was detected in this object.

14. 1998AJ....116.2166U
Re:NGC 3504
The H{alpha} emission is strong in the galactic center and also in the
inner ring. The brightest part in the ring coincides with the southern
end of the bar. There is a companion galaxy, NGC 3512, at 12' east of
this galaxy. This galaxy is extensively studied by Kenney, Carlstrom, &
Young (1993).

15. 1997A&A...326..449M
Re:NGC 3504
NGC 3504. This is a typical case of SF distribution in the bar of an early-type
spiral. A few "chains" of faint HII regions are observed next to the dust lanes
and tremendous SF is present in the galaxy centre. An enhancement of SF is
observed at the SE tip of the bar. There are no clear signs of SF in the
northern part of the stellar bar. An extensive study of the nuclear starburst
in NGC 3504 has been presented by Kenney et a. (1993); they concluded that the
nuclear starburst is reccnt (<100 Myr). The presence of HII regions along the
bar suggests that some gas is still falling toward the nucleus. The galaxy is a
member of a small group but shows no obvious sign of interaction. Kenney et al.
(1993) found two ILRs in this galaxy.

16. 1995ApJS...98..477H
Re:NGC 3504
HFS identified NGC 3504 as a ``transition object,'' based on its
emission-line intensity ratios, which are intermediate between those of
LINERs and H II nuclei. Such objects may owe their ionization to a
composite source which is both stellar and nonstellar.

17. 1994CAG1..B...0000S
Re:NGC 3504
Hubble Atlas, p. 46
Sb(s)/SBb(s)I-II
PH-1169-S
Dec 14/15, 1955
103aO
30 min
NGC 3504 is similar in its general features
to NGC 7552 on the preceding panel.
The oval is the weak bar from which the two
major luminous arms begin at opposite rim edges.
The two characteristic dust lanes beginning at the
nucleus can be identified in the low-contrast
print, where the detail in the interior of the oval
is well seen. One of the lanes is straight for its
entire length to the edge of the oval; the other is
straight over about half the size of the oval after
which it curves into a spiral dust fragment.
Two main low-surface-brightness arms begin
at opposite ends of the oval, nearly overlapping
after each reaches about half a revolution. Very
little current star formation is occurring in the
smooth outer arms. The places having the highest
current star-formation rates are at the ends of
the oval where the two outer spiral arms begin.
The largest HII regions resolve into disks at
about the 2" level. The redshift of NGC 3504 is
v_o = 1480 km/s.

18. 1993ApJS...86....5K
Re:NGC 3504
NGC 3504; SABab, starburst.
Optical and radio data suggest that the galaxy has a composite nucleus,
which shows both nonthermal activity and recent star formation (Keel
1984). The radio emission is due to the presence of a strong nuclear
radio source in a region of about 1 kpc (Condon et al. 1982). The
optical spectrum is dominated by the regions of active star formation
(Keel 1984), which are possibly triggered by the companion NGC 3512, 50
kpc distant from the main galaxy (van Moorsel 1983).
The UV spectrum is rich in absorption lines, with the presence of a
P Cygni profile for C IV, indicative of an evolved population of massive
supergiants. The flat continuum and the rich absorption features resemble
the spectrum of the prototype starburst galaxy NGC 7714.

19. 1976RC2...C...0000d
Re:NGC 3504
Pair with NGC 3512 at 12 arcmin
Bologna radio source = B2 1100+28
Photometry (5,10,21 microns):
Ap. J. (Letters), 176, L95, 1972.
Photometry (7 Color):
Izv. Spets. Ast. Obs., 6, 27, 1974.
Spectrophotometry:
Astrophys. Lett., 15, 35, 1973.
Dynamics and Mass Determination:
Ap. J., 184, 735, 1973.
HII Regions:
"Atlas and Catalogue", Univ. Washington, Saettle, 1966.
Ap. J., 155, 417, 1969.
Radio Observations:
A.J., 73, 876, 1968.

20. 1973UGC...C...0000N
Re:UGC 06118
(R)SAB(s)ab (de Vaucouleurs)
Paired with UGC 06128 at 12.0, 72
Companion 4.0, 55, 0.4 x 0.1

21. 1964RC1...C...0000d
Re:NGC 3504
Extremely bright nucleus in a bright lens: 1.4 arcmin x 0.8 arcmin with dark
lanes. Faint smooth outer whorls form (R): 2.05 arcmin x 1.9 arcmin.
Non-interacting pair with NGC 3512 at 12 arcmin.
Photograph, Rotation and Mass:
Ap. J., 132, 661, 1960.
Spectrum:
Ap. J., 135, 697, 1962.

22. 1961Hubbl.B...0000S
Re:NGC 3504
SBb(s)/Sb
PH-1169-S
Dec. 14/15, 1955
103aO
30 min
Enlarged 5.9X
The dust lanes are not well shown in this illustration.
The lane starting from the nucleus in the upper left is
quite straight, as in all normal SBb(s). The lower right
lane is slightly curved into a spiral pattern. The dust
lanes spiral into the nucleus similarly to those in M100
(pg. 31 of the Hubble Atlas) and NGC 1097 (top right).
NGC 3504 is a transition type between SBb and Sb.

23. 1918PLicO..13....9C
Re:NGC 3504
2' long, somewhat oval; a {phi}-type spiral with a very bright, round nucleus.
9 s.n.


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