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Notes for object [HB89] 0414+009

9 note(s) found in NED.

1. 2003AJ....125.1060R
Re:1ES 0414+009
The VLBA map (Fig. 6) resolves a jet that initially extends to the
east-northeast (P.A. = +68^degrees^) of the core. There is also weak,
extended (~3-4 s) emission to the southeast of the jet, which suggests
either that the jet is collimated and bends to the south ~10 pc from the
core, or that the projected jet opening angle is wide (~60^degrees^). If
the jet does indeed bend to the southeast, the misalignment angle could be
as large as {DELTA}P.A. =~ 60^degrees^; however, the inner portion of the
jet is well aligned ({DELTA}P.A. = 5^degrees^) to the kpc-scale jet shown
in Figure 3 of Laurent-Muehleisen et al. (1993).

2. 2003A&A...400...95N
Re:RGB J0416+010
0416+010: This BL Lac has been previously imaged extensively (see
Table 3). The host galaxy parameters have been determined by 7 studies
with the host magnitude and effective radius ranging from 17.45 to 17.80
and from 0.8 to 6.1 arcsec, respectively. Our values (17.73 and 2.9
arcsec) lie within this range.

3. 1999A&A...352...85F
Re:1ES 0414+009
1ES 0414+009: This BL Lac was resolved into an elliptical galaxy with
M(R) = -24.8 by the HST (U99b). It was also studied by Falomo (1996) who
derived for the host M(R) = -24.3 and R(e) = 5 kpc. We derive for the
elliptical host at z = 0.287 M(R) = -24.7 and R(e) = 5.8 kpc, in good
agreement with the other measurements. This source was also studied by
WSY96, who could not distinguish between elliptical and disk morphology.
They derived for the host M(R) = -24.4 and R(e) = 30.8 kpc. While the
host luminosity is in agreement, the scale length from WSY96 is clearly
too large. Note that 1ES 0414+009 is the dominant member of a moderately
rich cluster at z = 0.287 (Abell class 0; McHardy et al. 1992;
Falomo et al. 1993).

4. 1998ApJS..117..319A
Re:[ATZ98] A158
Already listed as a BL Lac object in NED. Our spectrum shows a
featureless blue continuum supporting this classification. The object is
near the center of a conspicuous distant cluster.

5. 1997ApJ...480..547W
Re:[HB89] 0414+009
0414+009.-The cluster around this BL Lac (z = 0.287) has been previously
studied by McHardy et al. (1992) and Falomo et al. (1993a), who confirmed
cluster membership for five galaxies. WESY93 found a B_gb_ value consistent
with an Abell richness class 1 cluster (class 0 using the new Yee
& Lopez-Cruz 1997 calibration) and presented a color-magnitude diagram,
which confirmed a z ~ 0.3 cluster.

6. 1996MNRAS.283..241F
Re:[HB89] 0414+009
0414+009 This is a moderately distant (z=0.287) object that is found in a
cluster of galaxies of Abell richness class 0 (McHardy et al. 1992; Falomo,
Pesce & Treves 1993, hereafter FPT93). The host galaxy is a luminous
elliptical that is the dominant member of the associated cluster (Falomo &
Tanzi 1991; McHardy et al. 1992). The new images presented here essentially
confirm the previous findings, and, thanks to the better resolution (seeing
~0.65 arcsec), it is possible to obtain more reliable values for host
parameters. The luminosity profile (see Fig. 2) can be well fitted by an
elliptical model (plus point source) with effective radius of 5 arcsec (29 kpc
at z=0.287). This effective radius is substantially larger than that reported
previously (about 1 arcsec). The discrepancy is mainly due to the reliability
of points close to the nucleus (around ~2 arcsec) that allow us to better
constrain the model. With worse seeing, only the farthest (and faintest) part
of the profile has a significant fraction of the light from the host galaxy.
In the latter case, the net effect would be to underestimate the effective
radius. In spite of a large difference of effective radius, the total
magnitude is consistent with previous findings (cf. also Abraham et al. 1995).
The excellent resolution of these images permits us to clarify a number of
points about the associated group of galaxies. For a number of galaxies in
this field, spectroscopy was obtained that confirmed that the galaxies form a
physical group, with the galaxy hosting H0414+004 being the dominant member
(FPT93). The object labelled B1 by FPT93 is composed of a star (late spectral
type) and a fainter galaxy ~1 arcsec to the south-west. Also, the galaxy B2 is
actually an elliptical and has a fainter companion galaxy at 1 arcsec to the
north. Galaxies C1 and C2 have early spiral and irregular barred
Magellanic-like morphology, respectively. Finally, the galaxy pair Al and A2
is composed of an elliptical (A2) and a late barred spiral (A1). The presence
of the bar in A1, together with a faint emission which appears to connect
these two galaxies (that have the same redshift), supports the interaction

7. 1995ApJS..100...37G
Re:[HB89] 0414+009
1H 0414+009 is a BL Lac object (Impey & Tapia 1988; Mead et al. 1990;
Maccagni et al. 1989; Halpern et al. 1991) and has been classified as an
XBL (Giommi et al. 1990; Hewitt & Burbidge 1993). It was observed with
EXOSAT on four occasions during 1984 September 9-30 (Sambruna et al.
1993). No variations of the LE flux were noticed in this source, but the
ME flux varied by a factor of 2 within 16 days(1984 days 258-274). Rapid
(on the timescales of hours) variability of the ME flux of this blazar
was found on 1984 September 9, which was also noted by Giommi et al.
1990. We have used the power-law plus absorption model and other models
mentioned in Section 4.1 to fit the spectra of this XBL. We find that the
power-law plus absorption model fits the spectra best, and other models
do not differ significantly (i.e., with significance at less than the 5%
level) from the power-law model. The best-fit parameters of the spectral
analysis are given in Table 3. From the results of the spectral analysis
of 1H 0414+009, we find that the spectral slope steepened when the source
intensity (2-10 keV) decreased (see Table 3). The multifrequency spectrum
of this source can be represented by a single parabolic component, except
for the infrared fluxes, which are much stronger than the radio and
optical fluxes (Fig. 4 c).

8. 1994ApJS...93..125F
Re:[HB89] 0414+009
0414+009.-We obtained six spectra of this X-ray selected source,
classified as a BL Lac object by Ulmer et al. (1983). We found that the
contribution of the stellar emission due to the host galaxy is, on
average, P_g_ = 0.08, corresponding to an absolute magnitude
M_V_ = -22.2 +/-0.5.

9. 1993AJ....106...11F
Re:1H 0414+009
An x-ray selected object of M_V_ ~ 16 located in a group of galaxies
(Ulmer et al. 1983) at z = 0.287 (Halpern et al. 1991). The spectral flux
distribution indicates the presence of a thermal component. Our
decomposition gives a thermal contribution P_g_ ~ 01 and {alpha} ~ 0.4.
The absolute magnitude of the host galaxy is M_V_ ~ -22.5.

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