Date and Time of the Query: 2019-03-26 T09:13:31 PDT
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Notes for object NGC 4748

9 note(s) found in NED.

1. 2009ApJ...705..199B
Re:NGC 4748
Examination of Figure 14 shows that there could be evidence for an outflow in
the BLR of NGC 4748. The extremely broad shape of the CCFs for the H{beta} flux
in this object (see Figure 1) combined with the relatively low-level flux
variations results in rather large uncertainties for the measured lag times in
this object. Each of the four velocity bins has a lag time that is consistent
within ~1.5{sigma} of the lag times measured for the other bins, and so the
significance of the velocity-resolved structure for NGC 4748 is not clear.

2. 2006A&A...457...61R
Re:NGC 4748
NGC 4748. Classified as NLS1 by Goodrich (1989), this object had been
previously cataloged as a Seyfert 1/1.5 (see for example, Osterbrock &
de Roberties 1985). It resides in an interacting pair, in contact, as
evidenced by the H{alpha} +[N II] image of Mulchaey et al. (1996). It
displays considerable soft X-ray emission (Rush et al. 1996). The
L-band spectroscopy of Imanishi & Wada (2004) shows 3.3 microns PAH
emission in this object, confirming the presence of circumnuclear star
formation. Our NIR spectrum reveals conspicuous emission lines, where
[S III] 9531 Angstrom and He I 10830 Angstrom are the strongest ones
observed. From the width of the permitted lines, we confirm the NLS1
classification of this object: O I 11287 Angstrom and Pa{beta} show
FWHM of approx 1740 km s^-1^ and 1950 km s^-1^, respectively. The
spectrum is dominated by BLR features, including fluorescent lines of
Fe II. The continuum emission is composite by a power-law-like form and
absorption lines of CO both in H and K. Molecular emission lines of H2
were also detected.

3. 2001A&A...372..730V
Re:NGC 4748
NGC 4748 (1249-13) is an NLS1 with strong Fe II emission (Osterbrock &
de Robertis 1985; Moran et al. 1996). The H{beta} FWHM is in the range
1100-1500 km s^-1^ (Osterbrock & de Robertis 1985; Maza & Ruiz 1989;
Winkler 1992). Rodriguez-Ardila et al. (2000b) measured ~2350 km s^-1^ for
the FWHM of the broad Balmer components. Our own measurements show that
they have a FWHM of ~1500 km s^-1^.

4. 1998MNRAS.297..579C
Re:MCG -02-33-034
MCG-02-33-034. This galaxy was classified as Seyfert 1 by Osterbrock & De
Robertis (1985), based on the appearence of permitted lines broader than the
forbidden ones and strong Fe II emission. Mulchaey et al. (1996) show that it
presents evidence of two nuclei, both emitting in [O III] and H{alpha}. We can
see the dilution of Ws and colour changes due to a blue FC in the nuclear region
(Fig. 7). The Ws change to values of an S3 template at 4 arcsec and farther out,
while the continuum ratios have values similar to an S4 at 4 arcsec and farther
out. As noted in Section 3, although dilution clearly occurs, the complex
nuclear spectrum (Fig. 2d) prevents an accurate determination of both Ws and
continuum at r=0 for this galaxy.

5. 1998AJ....116.2682C
Re:IRAS 12495-1308
NGC 4748. Seyfert 1.

6. 1996ApJS..102..309M
Re:MCG -02-33-034
MCG-2-33-34 shows evidence for two nuclei in our green continuum image. Both
nuclei are detected in [O III] and H{alpha}.

7. 1993ApJS...86....5K
Re:MCG -02-33-034
NGC 4748; Seyfert 1.
IRAS 1249-131 is classified as a Seyfert 1 galaxy from its optical
spectrum by Osterbrock & De Robertis(1985), de Grijp et al. (1985), and
Carter(1984). It has been alternatively classified as a Seyfert 1.5 by
Dahari & De Robertis (1988), on the basis of the scheme by Veilleux &
Osterbrock (1987), and as a "narrow-line" Seyfert 1 by Goodrich (1989).
Goodrich concluded that NGC 4748 is a Seyfert 1 with a small
line-of-sight velocity dispersion in its BLR. The UV spectrum does indeed
show emission lines (most notably C IV {lambda}1550) narrower than those
of a typical Seyfert 1 (Kinney et al. 1991b).

8. 1971CGPGX.C...0000Z
Re:NGC 4748
12 49.5 -13 07. [No. 2 of] Pair of interconnected neutral spherical compacts
surrounded by spherical haloes. 15" S[W]S of no. 1. m_p = 16.5 [No. 1 is
2MASXi J1252129-132438.]

9. 1968MCG4..C...0000V
Re:MCG -02-33-034
Interacting pair, in contact.
{rho} = 0.3 arcmin.
The disk is perturbed.

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