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Notes for object [HB89] 1418+546

15 note(s) found in NED.


1. 2007A&A...472..763B
Re:[HB89] 1418+546
The whole source is fading in flux density, which complicates the jet component
identification.

2. 2003AJ....126.2237D
Re:OQ +530
.
4.8. Blazars
.
Blazars are common in the radio-excess sample; PKS 0235+164
(F02358+1623), PKS 0338-214 (F03384-2129), PKS 0420-014 (F04207-0127),
PKS 0537-441 (F05373-4406), PKS 0735+17 (F07352+1749), PKS 0754+100
(F07543+1004), PKS 0829+046 (F08291+0439), OJ 287 (F08519+2017),
PKS 1144-379 (F11445-3755), 3C 273 (F12265+0219), 3C 279
(F12535-0530), B2 1308+32 (F13080+3237), OQ 208 (F14047+2841), OQ 530
(F14180+5437), B2 1732+389 (F17326+3859), Q2005-489 (F20057-4858),
BL Lac (F22006+4202), and 3C 446 (F22231-0512). These BL Lac objects
are optically variable, flat radio spectrum quasars, or "transition
objects" between traditional BL Lac objects and (strong emission-line)
quasars. Many of the blazars have extremely high radio powers
[L_{nu}_(4.8 GHz) > 10^27^ W Hz-1] and FIR luminosities
[{nu}L_{nu}_(60 micron) > 10^13^L_solar_] and are at relatively large
redshifts (z > 0.9). Blazars also occur in the sample at lower
redshifts and powers, as low as z ~ 0.05 and L_{nu}_(4.8 GHz) ~ 10^25^
W Hz-1. All the known blazars in the radio-excess sample have large
radio excesses (u < -0.2), several with extreme values of u ~ -1.0.
CAB comment that the blazars in their full sample all have u < -0.15
and spectral indices between 1.4 and 4.8 GHz of less than 0.5. This
makes them flat spectrum objects with large radio excesses.

3. 2003A&A...400...95N
Re:RGB J1419+543
1419+543: This is one of the two objects in the sample for which a
formally better fit is obtained when using a disk model ({beta} = 1.0)
than when using the de Vaucouleurs model ({beta} = 0.25). It has also
the highest fitted {beta} (0.57) of the sample. Previous authors have
alternatively described 1419+543 as a disk galaxy (Abraham et al. 1991;
Wurtz et al. 1996) or an elliptical galaxy (SUOO, P02). Stickel et al.
(1993) noted that the outer parts of the host (r > 5 arcsec) follow
{beta} = 0.25 closely, whereas in the inner part there is an additional
component that showed up after subtraction of the elliptical model. This
object is discussed in more detail in Sect. 6.

4. 2002MNRAS.329..877C
Re:GB6 J1419+5423
139-redshift, classification and spectrum in Stickel et al. (1993b).

5. 2000ApJS..127...11G
Re:OQ +530
3.11. PG 1418+546 (OQ 530)
The OQ 530 blazar is a member of the 1 Jy BL Lac sample
(Kuhr et al. 1981) and is a highly polarized quasar (Mead et al. 1990).
The multifrequency (radio through {gamma}-ray) spectrum of this source
suggests that it is an LBL object (Fossati et al. 1998 and references
therein). This intraday optically variable blazar (Heidt & Wagner 1996)
has also displayed rapid optical variability (Miller & Carini 1991). We
observed this blazar on four nights during 1998 June-July (Table 3),
and the results are plotted in Figure 9. This figure shows weak
variations of this source on timescales of weeks.

6. 1999MNRAS.307..725G
Re:[HB89] 1418+546
3.8 1418+546
This BL Lacertae object is in the centre of a relatively nearby
galaxy; the surface brightness profile resembles that of an S0 galaxy,
giving rise to speculation that 1418+546 could be one of a minority of
BL Lacertae objects with spiral host galaxies (Wurtz, Stocke & Yee
1996). The redshift of z = 0.152 reported by Stickel et al. (1993) was
based on absorption features of the galaxy, as well as
[O II] {lambda}3727 and [O III] {lambda}{lambda}4959, 5007 emission
lines, and confirms the tentative value reported by Stickel, Fried &
Kuhr (1989). The 6-cm VLBI image of Xu et al. (1995) showed this source
to have a VLBI jet extending toward the southeast.
Our observations clearly show the VLBI jet in structural position
angle ~130^deg^ (Fig. 6). The jet structure is initially very compact,
and then broadens: the outermost component, at a distance of about
4 mas, is heavily resolved. We detected polarization from the core and
all three jet components we identified. The polarization position
angles {chi} in the core and the innermost knot K3 are roughly aligned
with the jet direction, {chi} for the middle knot K2 is roughly
transverse to the jet direction, and {chi} in the outermost, very
extended feature K1 bears no obvious relation to the jet direction. It
is interesting that the plane of the optical polarization measured
nearly simultaneously with the VLBI data was {chi}_opt_ = 154^deg^,
which is aligned with {chi} in the jet component K3 to within less than
10^deg^ (Gabuzda, Sitko, & Smith 1996).

7. 1999ApJS..121..131F
Re:[HB89] 1418+546
1418+546 shows a large optical variation of 4.8 mag, ranging from 11.3
to 16.1 mag in the Miller (1978a) study; its optical polarization of
5%-24% (Marchenko 1980) is greater than the infrared polarization,
P_IR_ =19% (Impey et al. 1984). In the infrared, some properties have
been shown in the papers of O'Dell et al. (1978a, 1978b) and Puschell &
Stein (1980). No correlation was found between the spectral index and
the brightness, but the flux variations are found to be larger at lower
frequencies by Massaro et al. (1995) and Takalo et al. (1992). For the
spectral shape and the brightness of the source, the long-term data show
(see Fig. 16) (J-K)=-0.08H+2.65 with r=-0.40 and p=2.6% and
(J-H)=-0.08K+1.75 with r=-0.41 and p=2.2%, indicating that the spectrum
steepens when the source brightens. No similar correlation has been
found in the visual band (Worrall et al. 1984b). The infrared light
curves show two bursts separated by about 8 yr and the variation at
lower frequency to be greater. The infrared variations are smaller than
those in the optical band. (J-K) is found to be related with (J-H) and
(H-K) (see Fig. 16): (J-K)=1.56(J-H)+0.43 with r=0.856 and p=1.6x10^-8^,
and (J-K)=1.98(H-K)+0.03 with r=0.61 and p=7.0x10^-4^.

8. 1999A&AS..139..601C
Re:[HB89] 1418+546
1418+546: Murphy et al. (1993) found a component to the West of the
compact core also present in the image from the FIRST survey (Fig. 18).
Our WSRT observations (Fig. 19) show that this component is elongated to
the south, with an extended flux density higher than reported by
Murphy et al. or revealed by the FIRST image. The low resolution D array
image (Fig. 20) is dominated by a point-like component; however extended
and diffuse emission is detected all around, suggesting the presence of
a halo with a total size of 4.5 arcmin similar to that observed in
1807+698 (see below).

9. 1997ApJ...480..547W
Re:[HB89] 1418+546
1413+135 and 1418+546.-These two BL Lacs were the only ones in the CFHT
Survey to be found in spiral host galaxies in Paper I. The low B_gb_
values for these fields are consistent with late-type galaxy environs.

10. 1996ApJS..103..109W
Re:[HB89] 1418+546
1 Jy 1418+546 (OQ 530).--Previous studies classified this galaxy as an
elliptical (Stickel et al. 1993b) and a spiral (AMC). Our profile fit supports
the AMC result that the host galaxy is better fit by a spiral surface
brightness profile, and we find no reasons to distrust this interpretation
(i.e., no close companions, no evidence for sky brightness gradients across
our images, etc.). The surface brightness profile resembles an S0 type galaxy.
Because the other two BL Lac objects with spiral host galaxies are both quite
unusual, this object should be scrutinized further for peculiarities in all
wave bands.

11. 1996AJ....112.1877G
Re:[HB89] 1418+546
3.2 1418+546
1418+546 was discovered to be a BL Lacertae object during an optical
polarization search of the Ohio State radio sources by Craine et al. (1978). It
has since been extensively observed both photometrically and polarimetrically.
Marchenko (1985) has suggested that this source might have a preferred
direction of polarization near {chi}=120^deg^ when the polarization is high.
The VLBI jet extends to the southeast in structural position angle
{theta}=+130^deg^ (Fig. 2). Radio polarization was detected in the VLBI core
and in two VLBI jet components: a compact component barely resolved from the
VLBI core and a rather extended component further from the core. The
polarization in the VLBI core is aligned with {theta}, the polarization in the
inner knot is somewhat less well aligned with {theta}. The polarization in the
outer part of the jet does not bear any obvious relationship to the jet
direction. {chi}_opt_ is roughly aligned with {chi}_jet_ in the inner knot,
roughly perpendicular to {chi}_jet_ in the outer jet, and bears no obvious
relation to {chi}_core_.

12. 1994A&AS..105..211S
Re:[KWP81] 1418+54
The optical spectrum and redshift is given in Stickel et al. (1993b)

13. 1994A&AS..103..349S
Re:S4 1418+54
1418+546: The optical spectrum and redshift are given in Stickel et al.
(1993b).

14. 1994A&A...289..673T
Re:OQ +530
1418+546 (OQ 530)
As usual, the 22 and 37 GHz events correlate with each other well and
simultaneously, but because of the small number of temporally overlapping
observations at other frequencies it is somewhat difficult to draw
further conclusions. The light curves show however that the one event
observed well at 90 GHz, the flare in 1987.4-1988.0, appeared
simultaneously at 37 and 22 GHz. The optical data is undersampled but
there seem to be rather smooth rising and falling patterns in the total
flux, and none of them clearly correlates with the radio data.

15. 1993A&AS...98..393S
Re:OQ +530
1418+546
This is the only BL Lac object of the 1 Jy sample, which was found in the
center of a previously undetected relatively nearby galaxy. The redshift
of z = 0.152 is derived from absorption features of the galaxy as well as
[O II] {lambda}3727 and [O III] {lambda}{lambda}4959,5007 emission lines
and confirms the tentative value reported in Stickel et al. (1989a).
The spectroscopic redshift agrees well with the redshift estimated by
Hagen-Thorn & Marchenko (1989) using a two-color method to separate the
host galaxy from the central point source. This method relies mainly on
the assumption, that the host galaxy is a bright elliptical with
M_V_ ~ -23.
Since Abraham et al. (1991) proposed that (in contrast to the results
given in Paper I) the brightness profile of the host galaxy of 1418+546
is more closely represented by an exponential law characteristic for disk
type galaxies, the direct imaging data for this BL Lac object are
discussed in some detail in Sect. 3.4.
There is an apparent group of galaxies surrounding 1418+546 and
redshifts have been measured for eight members of this group.
Surprisingly, three different redshift systems have been found for these
eight galaxies. The second brightest galaxy ~40" to the southwest has the
same redshift as the BL Lac object while the nearest neighbouring galaxy
only ~10" northwest is a background object, viewed through the outskirts
of the BL Lac host galaxy.


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