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Date and Time of the Query: 2019-05-20 T08:47:25 PDT
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Notes for object NGC 5141

13 note(s) found in NED.


1. 2003ApJS..148..419N
Re:NGC 5141
NGC 5141 (UGC 8433).-This S0 galaxy has a nuclear dust lane (width :
length = 0.25). It has a core-jet radio morphology on VLBA scales and a
twin-jet morphology on VLA scales. The STIS slits were aligned parallel
to the galaxy major axis. The central kinematic and flux properties are
listed in Table 22; the gas exhibits a regular rotation profile. The fit
to the central spectrum is improved by the addition of a broad
component. Data for this galaxy are shown in Figure 18 (see key in
Fig. 1 for an explanation of these plots).

2. 2001ApJ...552..508G
Re:NGC 5141
1322+36 (NGC 5141). - We observed this small-size FR I radio galaxy for
6 hr at 5 GHz in 1993 September. The final image shows a one-sided jet
emission extended ~10 mas in the same direction as the main large-scale
jet (Fig. 14). We derive a jet/counterjet ratio greater than 20, which
gives a value of {beta} cos {theta} > 0.54, implying a jet velocity
{beta} >~ 0.54 and an orientation angle {theta} >~ 58^deg^.

3. 2001A&A...378..370V
Re:NGC 5141
NGC 5141 and NGC 5142: two S0 galaxies, not detected in our survey
(estimated I_HI_ < 2.3 and < 2.2 Jy km s^-1^, and M_HI_/L_B_ < 0.11 and
< 0.16 M_sun_/L_sun,B_, respectively).

4. 2000AJ....120.2950X
Re:UGC 08433
UGC 08433 (NGC 5141)-Core-jet structure is detected, with the
milliarsecond jet pointing to the southern and slightly stronger VLA
jet.

5. 2000A&A...362..871C
Re:NGC 5141
1322+36 (NGC 5141): There is a wide dust band in the center of this
galaxy, at P.A. ~ 85^deg^. See also Verdoes Klein et al. (1999).

6. 1999AJ....118.2592V
Re:NGC 5141
NGC 5141 is part of a group of six galaxies (Ramella, Geller, &
Huchra 1989) and has a companion galaxy, NGC 5142, at 2.3' (47 kpc). It
has a central slightly wedge-shaped dust lane with a size of 800 pc
(2.3"). The H{alpha} + [N II] emission peaks at the center, and
low-level emission is detected in the dust lane. NGC 5141 has two-sided
radio jets with broad lobes (Xu et al. 1999a). Our isophotal analysis is
consistent with a ground-based study by Gonzalez-Serrano et al. (1993).
In contrast to our results, however, they report a sharper decrease in
ellipticity inward of 3". This difference might be caused by their
larger seeing and/or a distortion of the inner isophotes by the central
dust distribution.

7. 1998A&AS..128..153M
Re:GB2 1322+366
NGC5141; UGC8433. WSRT 5-GHz map in
Fanti et al. (1977A&AS...29..279F). Physical parameters in
Condon & Broderick (1988AJ.....87.1064C)

8. 1997A&AS..126..335M
Re:B2 1322+36B
1322+36 The difference in polarization rotation angle between the two lobes is
46^deg^+/-8^deg^.

9. 1993AJ....105.1710G
Re:UGC 08433
1322+36 (NGC 5141, 4C36.24)
The V image shows two bright galaxies separated by 2.3' (47 kpc), the
Southwestern one containing the radio source. The Northeast companion,
NGC 5142, is clearly distorted and shows boxy and disklike isophotes. The
radial velocities of the galaxies differ only by 53 km s^-1^ (Soares
1989). The radio source presents a two-sided jet in P.A. 12^deg^,
although both jets bend by ~45^deg^, showing S symmetry.
The brightness profile is well represented by an r^1/4^ law and the
isophotes are nonelliptical in shape. Positive (r<~ 10") and negative
(r >~ 10") B_4_ isophotes are present (see Fig. 2). NGC 5141 is a clear
example of an interacting galaxy with distorted jet morphology. Emission
in the H{alpha} line has been observed in the nuclear region (Morganti et
al. 1992).

10. 1993A&AS...99..407C
Re:B2 1322+36B
1322+36
The brighter jet points to the more polarized lobe.

11. 1976RC2...C...0000d
Re:NGC 5141
= 4C 36.24
= B2 1322+36
= Kara[72] 373a
Pair with NGC 5142 at 2.3 arcmin
Spectrum:
Ap. J. (Letters), 182, L13, 1973.
M.N.R.A.S., 158, 277, 1972.

12. 1973UGC...C...0000N
Re:UGC 08433
Paired with UGC 08435 at 2.3, 57

13. 1970AJ.....75..764O
Re:4C +36.24
The identification is NGC 5141. Caswell and Wills (1967, M. N. R. A. S.,
135, 231) also identified this source.


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