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Date and Time of the Query: 2022-01-18 T02:05:41 PST
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Notes for object [HB89] 0317+185

6 note(s) found in NED.


1. 1999A&A...352...85F
Re:MS 0317.0+1834
MS 0317.0+1834: WSY96 could not distinguish between elliptical and disk
host for this source, for which they derived M(R) = -23.0 and
R(e) = 5.1 kpc. After masking out the close companion, we clearly prefer
an elliptical host with M(R) = -23.7 and R(e) = 4.7 kpc, a somewhat
brighter host.

2. 1998MNRAS.296..961W
Re:[HB89] 0317+185
1E 0317+185
The BL Lac object 1E 0317+185 has a redshift of 0.190 (Morris et at. 1991) as
measured from stellar absorption feature in its spectrum. The only previous
study of the host galaxy of this object was carried out by WSY, who found that a
disc morphololgy was the best representation of their data, and derived an
absolute magnitude for the host of M_r_=-22.52+/-0.20. However, they noted that
the presence of a companion ~1-2 arcsec from the object may have hampered the
profile extraction so the morphological class attributed is somewhat uncertain.

3. 1998MNRAS.296..961W
Re:[HB89] 0317+185
5.1.3 1E 0317+185
The host galaxy of the BL Lac 1E 0317+185 (z=0.19) is just resolved in both of
the IRCAM K-band images (Figs Id and e). From our elliptical galaxy model fits
we derive absolute host galaxy magnitudes of =-25.50+/-0.40 and
-24.97+/-0.40 for the first and second image respectively. Assuming a disc
galaxy model, we derive =-25.21+/-0.30 and -24.69+/-0.30. The host galaxy
was previously resolved by WSY, who found a disc galaxy host with an absolute
magnitude of M_r_=-22.52+/-0.20. We estimate the rest frame colour of the host
galaxy to be R-K~2.5+/-0.4 for the elliptical model, and R-K~2.2+/-0.4 for the
disc model. For comparison, typical elliptical and spiral galaxies have rest
frame AX colours of approximately 3.5 and 3.0 respectively (Steidel & Dickinson
1995).
The contour plot of the underlying galaxy, in Fig. 4(b), shows a slightly
distorted structure. We derive a scalelength of r_1/2_=3.8 arcsec (elliptical
model) or 2.7 arcsec (disc model), which correspond to 15.5 and 11.0 kpc
respectively, and note that the host is detectable out to a radius of ~7.0
arcsec (28.5 kpc). The structure observed in this host may be related to the
interaction with a companion, which was noted by WSY, but could also arise from
inaccuracies in the PSF subtracted.

4. 1996ApJS..103..109W
Re:[HB89] 0317+185
MS 0317+185.--This EMSS object has a companion within 1"-2" of the core,
making host galaxy profile extraction very difficult. The excess light that is
likely present in this companion causes the profile to be better fit by an
exponential rather than an r^1/4^ law at intermediate radii. On this basis, we
see no compelling evidence that this BL Lac object is in a spiral host despite
the lower {chi}^2^ value for the S fit (see Table 5).

5. 1995ApJS..100...37G
Re:[HB89] 0317+185
1E 0317+18 is a BL Lac object (Stocke et a1. 1989, 1990; Burbidge &
Hewitt 1992) which has also been classified as an XBL (Giommi et al.
1990; Hewitt & Burbidge 1993). X-ray spectra of this source can be best
fitted with the power-law plus absorption model. It is a steep X-ray
spectrum source ({GAMMA} ~2.4+0.60; Table 3 and Giommi et al. 1987), and
it did not vary during EXOSAT observations (1985 January 14 and February
9). Derived values of N_H_ are consistent with the Galactic N_H_ value.
No rapid X-ray variability on the timescales of hours was detected in
this source. The radio to X-ray spectrum of this blazar can be represented
by a single parabolic curve (Fig. 4a).

6. 1993ApJS...85..265J
Re:MS 0317.0+1834
MS 0317.0+1834
This object is a confirmed BL Lac object. The largest observed polarization
was 5.2%. Star A in this field has detectable interstellar polarization at a
position angle consistent with some of our measurements of the polarization.
The variability of the position angle of the polarization from the XSBL
confirms that it has intrinsic variable polarized emission.


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