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Notes for object NGC 2748

12 note(s) found in NED.


1. 2009MNRAS.397.2148G
Re:NGC 2748
The apparent nuclear star cluster is due to dust (Seigar et al. 2002; Hughes et
al. 2005).

2. 2008MNRAS.386.2242H
Re:NGC 2748
NGC 1300 and NGC 2748 - NGC 1300 has spiral-like dust lanes down to the
centre, wrapping around the nucleus (Scarlata et al. 2004) and
connecting to the leading edge of a strong kpc-scale bar (Martini et al.
2003), which suggests gas inflow in both large and small scale. The
bulge of NGC 1300 is disc-like with Sersic index n= 1.3 (Laurikainen et
al. 2004), and identified as a pseudo-bulge by Kormendy & Fisher (2005).
The nuclei of N2748 are not well defined in HST observations due to
dust-lane obscuration (Scarlata et al. 2004). The masses of SMBHs in NGC
1300 (6.6^+6.3^_-3.2_ x 10^7^ M_sun_) and NGC 2748 (4.4^+3.5^_-3.6_ x
10^7^ M_sun_) are measured by nuclear gas kinematics (Atkinson et al.
2005). The authors neglected the effect of extinction by dust in the
analysis of the gaseous rotation curves. The extinction in the H band
which was used to measure the black hole masses yields an
underestimation in luminosity of ~20 per cent for NGC 1300 and ?58 per
cent for NGC 2748 in their central 50 pc regions. Furthermor e, the
extinction is probably uneven due to the complex dust structures.
Therefore, the M_bh_ in two galaxies is not well estimated. Their
results are much higher than the prediction of M_bh_-{sigma}* or M_bh_-L
relations ( 7 x 10^6^ or 2 x 10^7^ M_sun_ for NGC 1300; 6 x 10^6^ or 7 x
10^6^ M_sun_ for NGC 2748). In fact, the HST can only barely resolved
the sphere of influence of SMBHs with the mass predicted by the
M_bh_-{sigma}* or M_bh_-L relations ( rbh= 0.04 ~ 0.1 arcsec for NGC
1300; r_bh_ = 0.03 arcsec for NGC 2748).

3. 2005ApJS..160...76B
Re:NGC 2748
Typical S/N and discordance. Clear rotation and patchy {sigma}_*_. NGC 2748 has
an inclination of ~70{degree}, which could account for LOSVD obscuration
especially in the presence of dust lanes (Hughes et al. 2003). These are the
first measures of {sigma}_*_ in NGC 2748 and are constant with aperture radius.
See Figures 8 and 10c.

4. 2003AJ....126..742H
Re:NGC 2748
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."
.
3.7. NGC 2748 (C)
Figure 3 (bottom).
Spectra: Very patchy emission. There is some large-scale rotation, but
it is not obvious for central regions.
Images: STIS image shows spider-like dust lanes, which are not seen in
the NICMOS image.

5. 2002AJ....123..159C
Re:NGC 2748
Dust throughout central region

6. 2000A&AS..141..385V
Re:NGC 2748
C-28 = NGC 2748. (E,G,J,N,W) Exhibits a faint structure perpendicular to
the stellar disc, and appears to be a spiral galaxy surrounded by a
polar ring. It may be in the process of forming a ring through accretion
(Reshetnikov & Combes 1994). Flat H{alpha} major axis rotation curve,
H II-type nuclear spectrum (Reshetnikov & Combes 1994; Ho et al. 1997).
Its optical kinematics were studied by Hagen-Thorn et al. (1996) and
Courteau (1997). Deep r-band CCD surface photometry: see Courteau (1996)
and Heraudeau & Simien (1996). Radial luminosity profile fit shows no
evidence for a bulge (Baggett et al. 1998). The only possible other
galaxy within the Nancay search area might the 16.9 mag object
IRAS F09075+7631, of unknown redshift, at a distance of 10'. The FWHM of
the Nancay profile (313 km s^-1^) is consistent with the 5 other
literature values (see Table 3), and much broader than the 140 km s^-1^
measured at Effelsberg.

7. 1997MNRAS.284..773G
Re:NGC 2748
3.7 NGC 2748 (C-28)
NGC 2748 has a systemic velocity of 1476 km s^-1^, and exhibits a faint
structure perpendicular to the stellar disc. A detailed kinematical and
photometrical study of this object indicates that it is a spiral galaxy
surrounded by a polar ring (Bettoni et al. 1996), perhaps similar to NGC 660,
although of a later type. The area around it contains many galaxies of unknown
redshifts and one faint object, PGC 26654, at the same redshift and 38 arcmin
distant, which corresponds to a projected distance of 261 kpc.
A double-horn-like CO signal appears in the nucleus, with maxima at 1400 and
1550 km s^-1^. Moving along the galaxy major axis, there is CO emission at 28
arcsec north-east (peak at 1395 km s^-1^) and at 28 arcsec south-west of the
nucleus, with the latter being broader and stronger for velocities ~1500
km s^-1^. The faint optical ring also presents a clear CO signal, centred at
~1500 km s^-1^, at 28 arcsec south-east. The spectra are noisy and the signal
fades out at 42 arcsec south-east, and on the other side of the ring at 28
arcsec north-west. The CO emission seems asymmetric, with the southern part
receding. The molecular hydrogen mass was determined by simply adding the
observed integrated intensities, with the exception of the (-20 arcsec, 20
arcsec) position. Assuming that the centre position we used is correct, ~25 per
cent of the molecular mass is in the ring.

8. 1994CAG1..B...0000S
Re:NGC 2748
Sc(s)II
PH-7930-S
Nov 7/8, 1980
103aO
12 min
The morphology of NGC 7361 is similar to
that of NGC 253. The HII regions are unresolved
at 1". The redshift is v_o = 1634 km/s.

9. 1994A&A...291...57R
Re:UGC 04825
NGC 2748 (UGC 4825)
The rotation curve along the major axis of NGC 2748 is very symmetric -
it rises to about 135 km/s at 40" and stays at that level up to 93" (10.0
kpc) from the nucleus. Radial velocities along the minor axis in a first
approximation follow a straight line (gradient 1.15 km/s/arcsec = 11
km/s, kpc) with {sigma} = 12.3 km/s. Assuming a spherical mass
distribution, we find M/L_B_ = 2.6f_sun_.

10. 1976RC2...C...0000d
Re:NGC 2748
Rotation Curve:
Astr. Ap., 8, 364, 1970.
Systemic Velocity:
Astr. Ap., 8, 364, 1970.

11. 1973UGC...C...0000N
Re:UGC 04825
SAbc (de Vaucouleurs)
Companion 3.0, 340, 0.7: x 0.1, very faint

12. 1964RC1...C...0000d
Re:NGC 2748
Very bright center with a small nucleus. Several knotty arms with dark lanes.
Poorly resolved.
Magnitude:
Ap. J., 82, 62, 1935.
Ap. J., 85, 325, 1937.
Spectrum:
IAU Symp., No. 5, 1958 = Lick Cont. II, No.81, 1958.


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