Date and Time of the Query: 2019-05-22 T14:10:35 PDT
Help | Comment | NED Home

Notes for object NGC 4725

18 note(s) found in NED.

1. 2009A&A...503..409H
Re:NGC 4725
Extremely faint polarized emission is detected in this moderately inclined
barred spiral galaxy, with the polarized emission originating at both ends of
the minor axis. The polarized emission avoids the bar, which is at a position
angle of about 45 degrees, and is mostly found on the outer periphery of the
ring-like structure. The polarized emission is too faint to allow investigation
of its detailed properties; deeper observations would be required. It is not
possible to say anything about the magnetic field orientation, as too little
signal is available. The foreground RM from the Galaxy in this direction can be
estimated from the double radio source in the field at +4 +/- 4 rad m^-2^; a
value consistent with several other unresolved sources in the field.

2. 2007AJ....134..648M
Re:NGC 4725
NGC 4725 (Figs. 7.52, 9.52, 20.52): The nuclear morphology of this early-type
spiral shows not many features apart from the bright, resolved nucleus
surrounded by extended emission with a clear exponential profile.

3. 2006MNRAS.366.1265B
Re:NGC 4725
This barred ringed Sab lenticular galaxy is catalogued as a double barred galaxy
by Erwin (2004) and H i rich by Rosenberg & Schneider (2003). No kinematical
data are available for this galaxy. The kinematics in the centre of the galaxy
are hard to resolve given its early type.

4. 2005MNRAS.364..283E
Re:NGC 4725
NGC 4725. The large-scale bar in this galaxy is peculiar and somewhat difficult
to measure, because it twists sharply with radius (it is similar to NGC 3185 and
5377 in this respect). None the less, there is a clear ellipticity maximum very
close to the inner ring (which itself defines L_bar_); this agrees fairly well
with the measurements of Martin (1995) and Chapelon et al. (1999). Although the
galaxy is somewhat dusty, the R-band bar measurements agree very well with
measurements made with a K-band image kindly provided by Johan Knapen. The outer
disc scalelength is from the r-band image of Frei et al. (1996); distance is
from HST Cepheid measurements (Freedman et al. 2001). The ellipticity of the
outer disc is uncertain, due to the presence of two strong spiral arms, so the
inclination is based on inverting the Tully-Fisher relation using the H-band
magnitude of Gavazzi & Boselli (1996), the H I width W_20_ from RC3, the Cepheid
distance and the H-band Tully-Fisher relation as given in (Binney & Merri field
1998, p. 425).

5. 2005A&A...442..137N
Re:UGC 07989
No H I gas is detected in the bulge of UGC 7989 (NGC 4725), nor in the giant
bar. It is rather concentrated in narrow spiral arms, which coincide with the
stellar arms. The outer arm on the east side is particularly prominent, whereas
the arms on the northwest side seem to be truncated, causing marked asymmetries
in the H I surface density map and global profile.

6. 2004A&A...415..941E
Re:NGC 4725
NGC 4725: Laine et al. (2002). Outer-bar measurements are from the
r-band image of Frei et al. (1996) and a K-band image kindly provided by
Johan Knapen, with L_bar_ from the inner ring; the outer bar is rather
peculiar (similar to those of NGC 1808 and ESO 443-39), and its position
angle is not well defined. Inner-bar measurements are from a NICMOS2
F160W image. See Erwin (2004a) for a discussion of the outer-disk
orientation; the distance is from Cepheid measurements (Freedman
et al. 2001).

7. 2003ApJS..146..353M
Re:NGC 4725
NGC 4725 (C)
The nuclear dust structures are very low contrast in this galaxy, and
those visible do not form any obvious spiral pattern.

8. 2002AJ....124..675C
Re:UGC 07989
Diffuse radio source. F12478+2545 is probably the correct
identification despite the very large optical/FSC offset; it lies
near the NVSS peak.

9. 2001ApJS..133...77H
Re:NGC 4725
NGC 4725 (S2:). - Not detected. No previous high-resolution radio

10. 2001A&A...368...16M
Re:NGC 4725
36. NGC 4725 is an Sb/SBb spiral of medium inclination. The neglect of the
small bar in our fit resulted in a corresponding residual feature (Fig. 6).
In the HST key project the Cepheid distance of NGC 4725 was determined to
13.0 Mpc (Gibson et al. 1999; Sakai et al. 2000).

11. 1999AJ....118.2331V
Re:NGC 4725
This galaxy was observed for the HST Extragalactic Distance Scale
Key Project, and the archive contains a large number of F555W images and
a lesser number of F439W and F814W images. Many more images in these
bands were planned, but we have used only those available before our
cutoff date. We combined the individual images into a single image in
each band. This galaxy has been host to two SNe: SN Ia 1969H, which is
not in these images, and SN II 1940B, whose environment is shown in
Figure 1. The position of this SN is not accurate (based on the nuclear
offset, 95" east and 118" north), and we show the 10" error circle
around the nominal position. The SN occurred near the edge of what
appears to be two associations of bright, blue stars (also see Zwicky
1965, his Plate IV). We performed PSF-fitting photometry on the combined
images in all three bands, although we also analyzed the individual
images as a check on our results.
We show in Figure 2 the color-magnitude diagrams (CMDs) for the
measured objects within the error circle; most of them are in the bright
associations. Also shown are unreddened isochrones from B94 for various
ages, corrected by the distance modulus m - M = 30.50 to NGC 4725
(Gibson et al. 1999). The object at m_F555W_ ~ 21.2, F439W - F555W ~
0.3, F555W - F814W ~ 0.6 mag, in particular, is too bright to be a
single star and is probably a compact star cluster. (Although we have
left the isochrones unreddened, examination of the CMDs shows that
reddening may be appropriate for some stars; SN 1940B itself may have
been somewhat reddened; see Minkowski 1964, de Vaucouleurs 1974, and
Patat et al. 1993.)
The environment of SN 1940B contains many bright, young, blue
stars, particularly in the large OB associations. Several red stars,
presumably red supergiants, with possible ages of about 8 to 20 Myr, are
also seen on the CMDs. The detected stars generally have ages, depending
on the actual reddening, in the range from 6 to 30 Myr. SN 1940B may
have been associated with the populations of young stars; if the SN
progenitor was a red supergiant, it may have had an age similar to the
detected red supergiants, but could have been as young as 6 Myr. The
lack of a precise SN position, in particular, prevents us from being
more restrictive about the nature of the progenitor.

12. 1995ApJ...450..137B
Re:NGC 4725
NGP-79.-Source 79 is identified as NGC 4725, an Sb/SBb galaxy.

13. 1994CAG1..B...0000S
Re:NGC 4725
Hubble Atlas, p. 21
Jan 2/3, 1941
80 min
The bar is not well defined in NGC 4725. It
is a region of enhanced luminosity but still of low
surface brightness, elongated across the central
lens. (See the print in the Hubble Atlas for good
detail of this region.)
The inner, high-surface-brightness spiral
pattern forms one of the most complete near-rings
of any galaxy in the RSA. Star formation is
high in this near-ring. Many bright HII regions
exist, as well as a number of faint small ones. A
few of these in the outer faint-surface-brightness
arms resolve into disks at the 3" level. The
redshift of NGC 4725 is v_o = 1167 km/s.
Very-faint-surface-brightness outer arms
are branched. The principal one of these arms is
an extension of a bright inner arm that forms
part of the nearly complete inner ring. This arm
branches into two, which then travel together for
another 200^deg^ of unwind.

14. 1976RC2...C...0000d
Re:NGC 4725
= Holm 468a
Pair with NGC 4712 at 12 arcmin.
Note correction to Dec. in Astr. Ap. Suppl., 3, 325, 1971.
"Stellar Structure", Stars and Stellar Systems, Vol. 8, 396, 1965.
Photometry (5 Color):
A.J., 73, 313, 1968.
Ap. J. Suppl., 26, No. 230, 1973.
Ann. Rev. Ap., Vol. 2, 249, 1964.
"Supernovae & SN Remnants", Ap. & Space Sc. Lib., Vol. 45, p.207, 1974.
IAU Circ. No. 2155, 1969.
P.A.S.P., 82, 736, 1970 (with photograph).
Ap. J., 185, 303, 1973.

15. 1973UGC...C...0000N
Re:UGC 07989
SAB(r)ab pec (de Vaucouleurs), Sb+ (Holmberg)
SN 1940b
See UGC 07977

16. 1964RC1...C...0000d
Re:NGC 4725
= Holm 468a
Very small, extremely bright nucleus in a faint, smooth, broad bar with dark
lanes. Strong, partially resolved (r): 4.3 arcmin x 2.5 arcmin. One main arm
forms an incomplete pseudo (R): 10.0 arcmin x - .
Lick 13 dimensions are for the bright part only.
Pair with NGC 4712 at 12 arcmin.
Ap. J., 46, 206, 1917.
Ap. J., 50, 384, 1919.
SN 1940
H.A.C., 522, 1940.
P.A.S.P., 52, 206, 1940.

17. 1961Hubbl.B...0000S
Re:NGC 4725
Jan. 2/3, 1941
80 min
Enlarged 2.2X
This is a transition galaxy between a normal Sb and an
SBb. The region of enhanced luminosity across the central
lens is not a well defined bar as in NGC 1398 (pg. 47). The
basic nebular type is closer to Sb than SBb. The internal
"ring" is not complete but resembles that in NGC 4580.
It begins abruptly at the edge of the amorphous central
region and breaks into multiple, tightly wound spiral arms
in the southeast quadrant. The dust lanes are seen
silhouetted against the background light especially well in
this quadrant. The inner arms are resolved into knots.
Two faint external arms are present, which can be traced
in the insert. These arms are smooth in texture with no
hint of resolution into knots. The external arms are not
on opposite sides of the nucleus but travel together, one
lapped on the inside of the other. Careful inspection of
the insert picture will separate the two, although on small-
scale plates they will appear as a single arm.
A supernova was discovered in NGC 4725 on May 5, 1940, by
J. J. Johnson at Palomar (Harv. Ann. Card 522). Two
photographs of NGC 4725 which show the supernova appear
on the back cover of The Sky, February 1941. The
supernova can still be seen on this plate taken by Hubble
in January 1941, some 9 months after outburst.

18. 1918PLicO..13....9C
Re:NGC 4725
Vol. VIII, Plate 42. A beautiful spiral 5' x 4' in p.a. 38^deg^. Nucleus very
bright; the whorls are on the periphery of the nebula, there being none near the
center. A wide faint band of matter lies along the major axis of the nebula; an
excellent exemplar of the {phi}-type spiral. Whorls show a.number of almost
stellar condensations. 19 s.n.

Back to NED Home