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Notes for object UGC 11130

21 note(s) found in NED.


1. 2006ApJS..164..307M
Re:3C 371
This object is often classified as a BL Lac in the literature. In our image it
appears as a round and smooth galaxy with a very bright nucleus that causes
marked diffraction spikes.

2. 2004ApJS..155...33S
Re:VSOP J1806+6949
(3C 371) A GOT image can be found in VSOPPR.

3. 2004ApJ...613..752G
Re:UGC 11130
1807+698. This is a well-known source (3C 371), with a jet detected in
the optical with HST (Scarpa et al. 1999) and in the X-rays with Chandra
(Pesce et al. 2001). This jet does not bend significantly and is well
aligned (at P.A. ~ 100deg) with the parsec-scale jet imaged with
the Space VLBI by Gomez & Marscher (2000). The orientation is in good
agreement with the P.A. of the jet visible in our C-array image
({DELTA}P.A. consistent with 0) and of the main lobe detected in the deep
B-array image at 5 GHz by Wrobel & Lind (1990); see also the 5 and 15
GHz VLA observations of O'Dea et al. (1988). Thanks to the lower
frequency and more compact configuration, we also detect a diffuse halo
of about 340 mJy, surrounding both lobes and extending over 200"
(see also Cassaro et al. 1999).

4. 2003ApJS..149...29G
Re:RX J1806.8+6949
This is a BL Lac in a cluster of galaxies. Redshift comes from Falco
et al. (1999PASP..111..438F).

5. 2003A&A...407..503D
Re:3C 371
3C 371: The Western elongation of the soft X-ray emission in Fig. 1 is
due to the X-ray jet (Pesce et al. 2001). Seven X-ray sources are
detected in the Chandra field but only two sources, B and G, have an
optical counterpart.

6. 2003A&A...400...95N
Re:RGB J1806+698
1806+698: Nilsson et al. (1997) discovered the optical jet roughly SW of
the nucleus. This jet has also been imaged with HST (Martel et al. 1999;
Scarpa et al. 1999b). There is a bridge of emission connecting the host
galaxy of 1806+698 to a pair of companion galaxies SW of the BL Lac. The
radio structure of 1806+698 is atypical, resembling more an FR II radio
galaxy than an FR I radio galaxy (Wrobel & Lind 1990).

7. 2002MNRAS.329..877C
Re:GB6 J1806+6949
222-redshift and spectrum in Marcha et al. (1996).

8. 2000A&AS..143..357K
Re:3C 371
3C 371 (S4 1807+69) is a BL Lac object in a large elliptical galaxy
whose emission is dominated by the flux from the nucleus. Earlier it was
classified as an N galaxy. Observations by Sandage (1967) showed that
3C 371 was optically variable. The brightness in the V-band was between
14.6 and 15.0 mag in autumn 1996 (Fig. 19). In spring 1997
(JD^bar^ 50520) the brightness was rising towards mag 14.3. The minimum
brightness was 15.02 (JD^bar^ 50360) and the maximum 14.23
(JD^bar^ 50554).

9. 1999ApJS..122...81M
Re:3C 371
3C 371. - An optical synchrotron jet was recently confirmed in this
BL Lac object by Nilsson et al. (1997) from ground-based imaging. The
main knot of the jet is weakly visible on our WFPC2 image at a
projected radius of 3" (3 kpc) to the southwest of the nucleus. The
host galaxy itself is very circular and smooth. The nucleus is a bright,
unresolved point source (the diffraction spikes are clearly visible on
our image).

10. 1999ApJS..121..131F
Re:3C 371
The N galaxy 3C 371.0 (z_em_ =0.0506; Miller 1975) is related to BL Lac
objects because of its optical variability ({DELTA}m~2.0 mag) and
polarization (P~12%; Shaffer 1978; Kinman 1976; CH84). Miller (1975)
suggests that the polarization increases significantly in the UV band if
the visual polarization is diluted by starlight. Capps & Knacke (1978)
reported an expected lower-than-optical infrared polarization
(P_IR_ =5.3+/-1.5%) if the starlight heavily dilutes the infrared. There
are only 7 nights of infrared data in the literature, giving
f_J_ =13.8 mJy, f_H_ = 16.0 mJy, and f_K_ =19.6 mJy (Heckman et al.
1983), which show a variation of 1 mag in K (from 10.86 to 11.88 mag).

11. 1999A&AS..139..601C
Re:[HB89] 1807+698
1807+698: Kollgaard et al. (1996) find the radio structure of this
source, at arcsecond resolution, consisting of a ~ 30" long jet
extending from the core to the west direction. Wrobel & Lind (1990) find
a double lobed structure of total extension of ~ 60", at 4.88 GHz (VLA,
B configuration). Our image from A+B+D configuration (Fig. 27) shows a
diffuse halo of ~ 220" of extension surrounding the core-jet structure
in agreement with the morphology seen by Wrobel & Lind (1990). The jet
is clearly visible in our A array image at 1.36 GHz (Fig. 28) and in the
B array 4.88 GHz image (Fig. 29).

12. 1996ApJS..107..541L
Re:3C 371
1807+698.--The sharp drop at the blue end below the power law is almost
certainly not real, as it is not seen in other spectra of this object
(M. Cohen, private communication). The cause remains unidentified.

13. 1995ApJS..100...37G
Re:3C 371
3C 371 is an optically violent variable object (Angel & Stockman 1980;
Webb et al. 1988; Stickel et al. 1991; Burbidge & Hewitt 1992) and is
also a superluminal source (Mutel 1989) which has been classified as a
RBL (Giommi et al. 1990; Hewitt & Burbidge 1993). EXOSAT observations of
this blazar were carried out on 1984 September 11 and 29 (Staubert,
Brunner, & Worrall 1986b), but only the spectrum of September 11 has
signal significance above 4 {sigma}. In the present analysis we have used
only this spectrum, which can be best fitted with a power-law plus fixed
absorption model. Best-fitting parameters are listed in Table 3. Results
of our analysis are in agreement with that of Staubert et al. (1986b).
Using the simultaneous observations at radio, NIR, optical, and UV
wavelengths during 1981 May (Worrall et al. 1984a), radio and millimeter
wavelengths during 1983 March-April (Landau et al. 1986), and UV and x-
rays during September 29 and 30 1984, we have constructed the
multifrequency spectrum of this blazar (Fig. 3k), and it can be well
represented by two parabolic spectral components.

14. 1995A&A...303....8H
Re:3C 371
3C 371 (z = 0.050) This object (Miller 1975) is a weak lined galaxy with
BL Lac properties. A spectrum of the object can be found in de Grijp et
al. (1992).

15. 1994ApJS...91..491G
Re:3C 371
1807+698 (3C 371) - A high-resolution radio image is given by Pearson et
al. (1985).

16. 1994A&AS..105..247A
Re:3C 371
1807+697, 3C371, galaxy/BL Lac: Our map of this source shows a bright
core and a one-sided jet extending out to ~3 arcsec from the core. A high
dynamic range VLA map (Wrobel & Lind 1990) shows faint extension of the
jet out to 25 arcsec, and a faint twin-lobes straddling the core-jet
structure. Wrobel & Lind interpret the structure as an edge-brightened
double viewed at a large enough angle that the radio lobes only
marginally overlap. The associated low brightness emission detected by
Wrobel and Lind could account for about 40% of the source flux density
(Kuhr et a1. 1978) missed in our map.

17. 1994A&A...289..673T
Re:3C 371
1807+698(3C371)
1807+698 is a source with only moderate flux changes ({DELTA}S_max_ ~ 1
Jy) in the flux levels in the low frequency flux curves, and the number
of data points at 90 GHz is too low for any analyses. No correlations
between the different radio frequencies nor between optical and radio
frequencies could be detected. Pomphrey et al. (1979) reported a possible
radio-optical connection mainly dominated by one strong event in both
regimes, but Balonek's analysis of data streams after this event showed
no correlations.

18. 1993A&AS...98..393S
Re:3C 371
1807+698
3C 371 is the only BL Lac object of the 1 Jy sample, which also appears
in the low-frequency selected 3C catalogue (Spinrad et al. 1985). The
direct image shows that 1807+698 is an interacting system with tidal
tails towards the neighbouring galaxy 75" to the southwest and possibly
also towards another galaxy 50" to the east. The tidal interaction of
1807+698 with these two nearest neighbouring galaxies has already been
noted by Arp (1970), who also has drawn attention to the small group of
galaxies surrounding 1807+698, which is not covered by our CCD frame. It
is remarkable that two imaging studies aimed at the investigation of the
frequency of interacting galaxies among radio sources (Colina & Perez-
Fournon 1990; Smith & Heckmann 1989a,b) did not detect the interacting
nature of 1807+698. Nevertheless, the brightness distribution of the host
galaxy can be modeled very well by a de Vaucouleurs law (see Table 5).
The optical spectrum of the BL Lac object shows absorption features of
the stellar population as well as narrow [O II] {lambda}3727,
[O III] {lambda}{lambda}4959,5007, [O I] {lambda}6300, [N II]
{lambda}6584 and [S II] {lambda}6717,6731 emission lines, while H{alpha}
is badly blended with the atmospheric B band. Interestingly, the
[O III] {lambda}4959,5007 emission region extends farther out from the
nucleus in the southwest direction towards the interacting companion
compared to the northeast direction, which may be taken as evidence that
this line emission is connected to the tidal interaction rather than to
the presence of the active BL Lac nucleus.
The radio structure resembles a Fanaroff-Riley type II radio galaxy
with relatively low radio power (Wrobel & Lind 1990) seen at a small
angle to the jet direction.

19. 1988ApJ...328..114P
Re:3C 371
1807+698 (3C 371).-This nearby N galaxy or BL Lac object has been
intensively studied in the radio, optical and X-ray bands. A high
dynamic range VLA map at 1.7 GHz by Ulvestad and Johnston (1984) reveals
that the compact radio source is embedded in an elliptical halo 2' x
1.5' in extent with the major axis in the east-west direction. Higher
resolution VLA observations by Perley, Fomalont, and Johnston (1980) and
MERLIN observations by Browne et al. (1982b) reveal a one-sided jet
structure, similar to that seen in 3C 120, extending at least 3" in
P.A. 240deg. The object is highly variable on time scales of a few
months (Seielstad, Pearson, and Readhead 1983), and Perley's
observations (1982) reveal that it is polarized at the 1evel of 2.7% at
5 GHz.
Numerous VLBI observations have been made of the nuc1eus of 3C 371.
Our first-epoch map, shown here in Figure 1, has a1ready been published
(Pearson and Readhead 1981). The map reveals an asymmetric core-jet
structure extending 14 mas in P.A. -97deg We obtained a good fit to the
data with the four-component model given in Table 4. Our second-epoch
map (Readhead, Pearson, and Unwin 1984) has been reanalyzed, together
with third-epoch data, by Lind (1987). The source has a complex,
variable, core-jet structure, but no clear evidence has been found for
superluminal motion. There is, however, evidence for bulk relativistic
motion from X-ray and radio variability arguments (Worrall et al. 1984).
Where necessary, we have assumed H_0_ = 100h km s^-1^ Mpc^-1^ and
q_0_ = 0.5 to convert angles to projected distances.

20. 1973UGC...C...0000N
Re:UGC 11130
VII Zw 768, 3C 371
"large blue spherical compact... variable, interconnected with several
elliptical galaxies of about the same redshift" (CGPG)

21. 1971CGPG..C...0000Z
Re:CGPG 1807.2+6949
VII Zw 768
3C 371
Large blue spherical compact.
Variable, interconnected with several elliptical galaxies of
about the same redsh1ft.
Spectrum: Emission: Strong cont. weak [OII], [NeIII].
= 15,300 km/sec. (Zwicky 1965)
See also H. C. Arp, Ap. J. Letters 5, 73 (1970).
m(pg) = 14.4 [CGCG]


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