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Notes for object NGC 4278

31 note(s) found in NED.


1. 2006MNRAS.369..497K
Re:NGC 4278
This LINER (Ho, Filippenko & Sargent 1997) and radio source (e.g. Capetti et al.
2000) show some central dust features (e.g. Peng et al. 2002). There is some
evidence that the Mg b contours are more flattened than the isophotes. There is
a well-defined depression in the H{beta} line strength within the central 5
arcsec (see also Davies et al. 1993) which we partly ascribe to imperfect
removal of strong H{beta} emission.

2. 2006MNRAS.366.1151S
Re:NGC 4278
This galaxy shows the strongest emission, in terms of the EW of the lines, in
our sample, allowing us to appreciate in detail the peculiar distribution and
kinematics of the gas. As in previous objects, the ionized gas displays an
integral-sign pattern, a twisted Vgas field, and an asymmetric ?gas central peak
and distribution of the [O III]/H{beta} ratio. Dust absorption features are
visible only on the north-western side of the galaxy. Their morphology suggests
an orientation similar to that of the integral-sign pattern. The gaseous and
stellar kinematics are misaligned by increasingly wider angles, as the stellar
and gaseous velocity fields twist in opposite directions towards the outer parts
of the field. This object also hosts an outer H I ring (Raimond et al. 1981)
that may be physically connected with the ionized gas, given the similar
orientation of the two gaseous systems (Goudfrooij et al. 1994).

3. 2006A&A...447...97B
Re:UGC 07386
UGC 7386: a total of 310 nuclear counts in 0.2-8 keV band were extracted from a
2" diameter circle without background subtraction and converted to X-ray
luminosity (2-10 keV) assuming an intrinsic power-law spectrum with photon index
{GAMMA} = 1.8 and a column density N_H_ = 2 x 10^20^ cm^-2^ (Ho et al. 2001).

4. 2005ApJ...622..235T
Re:NGC 4278
Large rotating H I + dust disk; strong nuclear LINER
emission lines; core-halo radio source with compact core; optically
visible dust patches

5. 2004MNRAS.352..721E
Re:NGC 4278
NGC 4278: This galaxy shows fairly regular kinematics, with the mean
velocity decreasing at radii larger than 10 arcsec along the major axis
(Schechter & Gunn 1979; Davies & Birkinshaw 1988). The central
dispersion peak is elongated along the major axis. The h_4_ map reveals
relatively high positive values everywhere except inside 6 arcsec, where
it drops significantly, consistent with the long-slit data published by
van der Marel & Franx (1993), but not with Bender et al. (1994).

6. 2004MNRAS.352..673A
Re:1217+295
1217+295 (NGC 4278). This is a well-known radio galaxy. The
broad-band spectrum between 5 and 43 GHz is relatively steep, and
the submillimetre emission is likely to be thermal, something that is
consistent with the detection of large-scale dusty regions reported
by Carollo et al. (1997).

7. 2004MNRAS.352..112B
Re:TXS 1217+295
3.1.14 1217+295 This source is identified with the nearby type 1
Seyfert galaxy NGC 4278 at z= 0.002 (1 mas ~= 0.04 pc). On the
kiloparsec scale the radio source is slightly resolved showing a short
jet pointing to the south (Wrobel & Heeschen 1984). On the parsec-scale
the source shows an extended core and a jet elongated to the
south-east. Some patchy diffuse emission is detected on the
north-western side (Falcke et al. 2000; Giovannini et al. 2001; Ly,
Walker & Wrobel 2004). The overall morphology is very reminiscent of
that of 0902+468. We do not detect polarization on the parsec scale,
and our limit is consistent with the integrated value found at 8.4 GHz
with the VLA (Bower, Falcke & Mellon 2002).

8. 2004A&A...416...41X
Re:NGC 4278
NGC 4278. This elliptical galaxy shows a complex dust structure in its
core (van Dokkum & Franx 1995). We do not detect any excess at 6.7
micron but we detect a 15 micron excess indicating the presence of warm
dust in this galaxy.

9. 2003ApJ...583..145T
Re:NGC 4278
NGC 4278 (L1.9). A result on the same data set is presented by
Ho et al. (2001).
.
We analyzed archival ASCA data observed on 1998 May 24. The effective
exposure times after standard data screening were 19.6 ks for each SIS
and 23.9 ks for each GIS. The ASCA spectrum is well fitted with a
power law with a photon index of 1.85 (1.77-1.94). The best-fit
absorption column is N_H_ = 0, with an upper limit of 5.4 x 10^20^
cm^-2^. The observed flux in the 2-10 keV band is 2.0 x 10^-12^ ergs
s^-1^ cm^-2^.
.
Our Chandra image in the hard band is dominated by the nucleus, and no
bright source is seen in the field. Therefore, the hard X-ray
measurement with ASCA seems reliable. The Chandra flux in the 2-10 keV
band (7.1 x 10^-13^ ergs s^-1^ cm^-2^) is about one-third of the ASCA
flux, indicating variability.

10. 2002AJ....124.3465S
Re:KISSR 0029
There are only two LINERs in the ROSAT-KISS sample
(the other example being KISSR 2059). KISSR 29 (NGC 4278)
is remarkable in that it is one of the optically brightest
sources in KISS (m_B_ = 11.53); this galaxy is extremely
nearby (only 8 Mpc distant). KISSR 29 is the only
ROSAT-KISS object for which archival HRI images are
available. However, in the interests of uniformity, we
have not made use of the pointed data in our calculations.
Halderson et al. (2001) used pointed PSPC observations of
KISSR 29 to derive an estimate of the total soft X-ray
flux (0.1-2.4 keV) of 5.92 x 10^-13^ ergs s^-1^ cm^-2^,
assuming a photon index of {GAMMA} = 2.5 and column density
NH = Galactic + (2.0 x 10^20^) cm^-2^. Using the same
spectral parameters, we find that the 0.1-2.4 keV flux for
this object is 2.49 x 10^-13^ ergs s^-1^ cm^-2^ using the
RASS detection.

11. 2001ApJ...552..508G
Re:NGC 4278
1217+29 (NGC 4278). - This nearby (z = 0.0021; distance modulus = 30.61,
corresponding to 13.2 Mpc) elliptical galaxy shows strong nuclear optical
emission lines and a large amount of neutral hydrogen (see
Schilizzi et al. 1983 and references therein). At arcsecond resolution it
shows an unresolved emission, while an extended structure is visible at
milliarcsecond resolution (Schilizzi et al. 1983).
We observed this source with the VLBA+single VLA antenna on 1995 July at
5 GHz. Our image (see Fig. 12) shows a complex structure with a central
emission with a peak flux density of 95 mJy beam^-1^ and an extended halo,
which in the north shows a large bend, being oriented east-west in the
external regions. A distorted jetlike structure could be present in the
southern region; however, because of the extended structure also in the
northern region, no information on the jet velocity and orientation may be
derived from present data. Our image is in good agreement with the map
presented by Schilizzi et al. (1983) at a lower angular resolution and
with the image given by Falcke et al. (2000), where only the southern
jetlike structure is visible because of their lower sensitivity to extended
structures (they do not have the short baseline VLA-VLBA Pie Town).
A comparison with unpublished images at 8.4 GHz by us confirms the core
identification with the central region where the highest brightness is
measured. The VLBI total flux density is ~400 mJy, in agreement with
arcsecond-scale observations; therefore we are confident that we have
mapped the whole structure of this small-size source. We note that because
of the nearness of this source, the linear resolution of our image is very
good (the half-power beamwidth [HPBW] is 2.5 mas, corresponding to
0.15 pc).

12. 2001AJ....122..653R
Re:NGC 4278
NGC 4278: The irregular dust patches of the optical images
(van Dokkum & Franx 1995; Carollo et al. 1997; Tomita et al. 2000) are
barely visible in the NIR residual map. The central point source is
slightly mismatched by the PSF.

13. 2001AJ....122..637H
Re:NGC 4278
NGC 4278. - Koratkar et al. (1995) fitted the spectrum with an absorbed
power-law model. They report an unabsorbed 0.2-2.2 keV flux of
2.56 x 10^-12^ ergs cm^-2^ s^-1^. Note that this is corrected not only for
Galactic absorption, but also for the total best-fit column density, which
exceeds the Galactic value. If we adopt the same waveband and correct for
the same column density, we obtain about half their flux. Their measured
count rate is not listed, but since we used spectral parameters very
similar to theirs, they presumably extracted counts from a bigger region
than we did.

14. 2000ApJ...542..186N
Re:NGC 4278
NGC 4278.-Jones (1984) have observed this object using VLBI and find
the core flux density is 180 and 190 mJy at 18 and 6 cm, on size scales
less than 5 and less than 1 mas, respectively. Wilkinson et al. (1998)
find a 3.6 cm peak flux density of 153 mJy beam^-1^ at 200 mas
resolution, and we find a 2 cm peak flux density of 88.3 mJy beam^-1^ at
150 mas resolution, so the core may be flat between 18 and 6 cm and then
steeper down to 2 cm. Alternatively, the lower flux density at 2 cm may
be a result of source variability. The 20 cm emission detected in FIRST
is extended in P.A. 166^deg^, but the UGC and RC3 do not list a host
galaxy P.A., as the galaxy is almost round.

15. 2000A&AS..144...53K
Re:NGC 4278
For this galaxy we used the SB-profile of Goudfrooij et al. (1994); this
was oversmoothed compared to the GCV estimation (see Sect. 4) and
extrapolated towards the center; the fitted central slope is -0.50.

16. 2000A&A...362..871C
Re:NGC 4278
1217+29 (NGC 4278): This source is associated with the nearby galaxy
NGC 4278. It shows a regular structure only slightly modified by diffuse
dust absorption to its NW side. The nucleus is unresolved. The radio
source is very compact, ~ 1 pc (see, e.g., Schilizzi et al. 1983). The
galaxy is known to have strong nuclear emission lines (Osterbrock 1960).
It contains a large amount of neutral hydrogen (Raimond et al. 1981)
rotating around an axis at -45^deg^.

17. 1999MNRAS.310...30C
Re:B2 1217+29
B2 1217+29
PSPC and HRI analyses of this source are consistent. A {beta} + point
model fits the data better than a {beta} model alone (see Table 2).

18. 1999ApJ...519...89C
Re:NGC 4278
NGC 4278.-This is a nearby elliptical galaxy with large-scale radio
emission (Wrobel & Heeschen 1984). NED lists its classification as a
Seyfert 1 galaxy and HFS95 classify its nucleus as having a LINER
spectrum. We find a compact X-ray source coincident with the galaxy
nucleus.

19. 1998AJ....116.2682C
Re:IRAS 12175+2933
NGC 4278. LINER, Seyfert 1, elliptical. Optical position from Argyle &
Eldridge (1990). Compact flat-spectrum radio source (Condon, Frayer, &
Broderick 1991a).

20. 1997ApJS..112..391H
Re:NGC 4278
NGC 4278.--As illustrated in Figure 2, a relatively weak, broad H{alpha} line
can be extracted from NGC 4278, an elliptical radio galaxy with a LINER
nucleus. Rotational broadening contributes to the large width (FWHM=480
km s^-1^) of the narrow lines, each of which is well modeled by the sum of two
Gaussians.

21. 1997ApJ...481..710C
Re:NGC 4278
One side of the galaxy is heavily obscured by large-scale dust located
north-northwest of the nucleus. The dust distribution is far from settled
and seems to spiral down into the nucleus. Its distribution shows several
dense knots, interconnected by filaments. The filaments are roughly
perpendicular to the extended radio emission. The densest and largest of
the knots appears about 5.4" north of the nucleus and is ~12 pc in size.
The large amount of dust dominates the higher order terms of the Fourier
expansion. These are reduced to zero in the fit to the dust-improved I
frame, which demonstrates the effectiveness of this procedure. The color
profiles rise from the very center to ~1" and decrease toward bluer
values outside this radius. A central point source has been found
(V ~ 19.7, M_V_ ~ -9.6, V - I ~ 0.9). It is bluer than the surrounding
stellar population (see the V - I profile). In addition, there is a weak
indication from the V - I color map that the stellar population
surrounding the central point source is also bluer than the surrounding
galactic regions (note the slow increase in Fig. 1 in V - I to a radius
of ~1").

22. 1994CAG1..B...0000S
Re:NGC 4278
Pair
Hubble Atlas, p. 1
E1
PH-676-S
Feb 7/8, 1954
103aD + GG11
45 min
NGC 4278 (redshift v_o = 584 km/s) forms a pair with the dE,N/Im
mixed-morphology dwarf companion NGC 4286 (redshift v_o = 600 km/s)
and is in the field of NGC 4283 (panels 2, 20) which, at v_o = 1053
km/s, is probably in the background.
The very many globular clusters over the face of NGC 4278 are
well seen in the negative print here. The specific globular cluster
frequency listed by Harris (1988) is high at S = 8.3; this value
compares with the average for all globular clusters in the list by
Harris of S = 5.0. Note again that S = 15 for the unusual case of NGC
4486 (M87).
NGC 4278 was one of the first E galaxies in which HI 21-cm
radiation was detected (Gallagher et al. 1977). The origin of the
neutral hydrogen may be the long-sought gas shed from evolving stars
by the normal processes of stellar evolution (Sandage 1957, Faber and
Gallagher 1976). Emission lines in the spectra of the center were
discussed by Osterbrock (1960), following their discovery by Humason
in a number of E galaxies.

23. 1994CAG1..B...0000S
Re:NGC 4278
E1
PH-676-S
Feb 7/8, 1954
103aD + GG11
45 min
The projected spatial configuration of the three galaxies is
shown here from the same plate used for the print of NGC 4278 at the
left. NGC 4278 is the brightest galaxy in the frame at the lower left,
NGC 4283 is in the middle, and the dE,N/Im mixed-morphology dwarf NGC
4286 is at the upper right. The orientation of this print and the one
on the right is north to the right, east at the top.

24. 1994A&AS..105..481M
Re:NGC 4278
NGC 4278: For this roundish galaxy, our data does not agree well with
BDM88. Indeed e_4_ fluctuates around zero, but it is mostly positive
farther than l = 20 arcsec, so that the diE class is adopted.

25. 1994A&AS..105..341G
Re:NGC 4278
Elliptical galaxy with large HI ring, inclined by ~45^deg^ to the line of
sight (Raimond et al. 1981). The outer contours of the ionized gas
distribution in our H{alpha}+[NII] image have an axis ratio of ~0.74
which indicates an inclination of ~48^deg^ to the line of sight if the
contours are intrinsically circular in space. The ionized gas may thus be
physically associated with the neutral gas which is located further out.
The B-I image reveals prominent patchy dust out to ~25" (see also Ebneter
et al. 1988), most prominently on the northern side of the nucleus.
Although the extinction in the dust patches N of the nucleus amounts to
E_[B-I]_~0.12 mag, no sign of obscuration is seen in the H{alpha}+[NII]
image. This suggests that the dust patches are located (at least
partially) behind the ionized gas.

26. 1994A&AS..104..179G
Re:NGC 4278
Elliptical galaxy with large HI disk (Raimond et al 1981). Residual
images reveal prominent patchy dust in the inner 15" (see also Ebneter et
al 1988). S4 and C4 ~ -0.01 at r = 40".

27. 1976RC2...C...0000d
Re:NGC 4278
= Holm 369a
= B2 1217+29
Pair with NGC 4283 at 3.5 arcmin
Photometry (UBVRIJKL):
Ap. J., 143, 187, 1966.
Photometry (5 Color):
A.J., 73, 313, 1968. .
Photometry (10 Color):
Ap. J., 179, 731, 1973.
Spectrum:
Ap J. (Letters), 164, L35, 1971.
Spectrophotometry:
"Nuclei of Galaxies", 151, 1971.
Polarization:
Ap. J. (Letters), 179, L93, 1973.
Dynamics and Mass Determination:
Ap. J., 139, 284, 1964.
Radio Observations:
Ap. J. (Letters), 151, L135, 1968.
Ap. J. (Letters), 152, L63, 1968.
Ap. J., 157, 481, 1969.
Ap. J., 189, 379, 1974.
Astrophys. Lett., 2, 187, 1968.
Astrophys. Lett., 6, 49, 1970.
A.J., 75, 523, 1970.
A.J., 77, 568, 1972.
Sov. A.J., 13, 881, 1970.
Ast. Tsirk., No. 545, 1970.
IAU Symp. No.44, 222, 1972.

28. 1973UGC...C...0000N
Re:UGC 07386
E1-2 (de Vaucouleurs), E (Holmberg)
In a triple chain with UGC 07390 at 3.6, 58, and UGC 07398 at 8.8, 62

29. 1964RC1...C...0000d
Re:NGC 4278
= Holm 369a
Very bright center. Smooth structure. Many globular clusters.
Pair with NGC 4283 at 3.5 arcmin.
Photometry:
Ap. J., 50, 384, 1919.
Ap. J., 71, 231, 1930.
Spectrum:
Ap. J., 116, 66, 1952.
Ap. J., 132, 325, 1960.
Rotation, Mass and M/L Ratio:
Ap. J., 132, 325, 1960.
Ap. J., 134, 910, 1961.

30. 1961Hubbl.B...0000S
Re:NGC 4278
E1
PH-676-S
Feb. 7/8, 1954
103aD + GG11
45 min
Enlarged 4.0X
NGC 4278 is a typical E1 galaxy. There is a smooth intensity
gradient from the center to the outside where the
luminosity of the galaxy fades far below the surface
brightness of the background sky. There is no outer
envelope like that in S01 systems.
The many condensations in the atmosphere of NGC 4278
are undoubtedly globular clusters. There are not so many
of them here as in NGC 4486 (M87), but about 50 exist. NGC
4278 is north of the Virgo Cluster, in the south wing of
the Ursa Major Cloud.

31. 1918PLicO..13....9C
Re:NGC 4278
Nearly round, 1' in diameter; central part very bright; no spiral structure
discernible. .


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