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Date and Time of the Query: 2022-01-16 T20:32:11 PST
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Notes for object WISE J172504.34+115215.5

6 note(s) found in NED.


1. 1996ApJS..103..109W
Re:4U 1722+11
4U 1722+119.--While we list this source as unresolved, there is some slight
evidence for counts in excess of the scaled PSF at >4" (see Fig. 5). The upper
limit on host galaxy magnitude quoted in Table 5 is consistent with this
slight excess and is not inconsistent with a luminous host galaxy for this
object similar to others in this sample.

2. 1995ApJS..100...37G
Re:4U 1722+11
4U 1722+119 is an X-ray-selected BL Lac object (Griffiths et al. 1989;
Brissenden et al. 1990; Burbidge & Hewitt 1992; Hewitt & Burbidge 1993;
Giommi et al. 1990). The X-ray spectrum of this blazar, observed with
EXOSAT can be best fitted with the power-law plus absorption model. The
fit parameters are listed in Table 3, and it can be seen from this table
that 4U 1722+119 is a steep-spectrum source with no intrinsic absorption.
Using the fluxes from nonsimultaneous observations, we have constructed
the multifrequency spectrum of this blazar, which can be fitted with a
single parabolic curve (Fig. 4k).

3. 1994ApJS...93..125F
Re:H 1722+119
1722+119.-The optical continuum of this X-ray selected object recently
discovered by Brissenden et al. (1990), is well described by a power-law
model with stable spectral index {DELTA}{alpha} <~ 0.27). We have
observed this source 4 times in 4 consecutive nights finding a variation
of 0.3 magnitudes.

4. 1993ApJS...85..265J
Re:H 1722+119
H 1722+119
This object is also known as 4U 1722+119. Of all XSBLs, it has reached the
highest levels of percent polarization (U band P = 18.04 +/- 1.40%). The
first polarimetry of this object was presented by Brissenden et al. (1990).
Although the object appears extended, no redshift is available.

5. 1993AJ....106...11F
Re:H 1722+119
1722+119
This is a highly polarized x-ray selected BL Lac recently discovered
by (Brissenden et al. 1990). A tentative redshift of 0.018 was proposed
by Griffiths et al. (1989) but not confirmed (Veron-Cetty & Veron 1992).
Our spectral flux distribution shows a marked curvature between IR and
optical also after the reddening correction (A_V_ = 0.51). This suggests
the presence of a thermal component at z = 0.2 with {alpha} ~ 0.5 and
P_g_ ~ 0.15, corresponding to a host galaxy of M_V_ ~ -23.6.

6. 1993A&AS..100..521V
Re:H 1722+119
H 1722+119 (Brissenden et al. 1990), 4U 1722+11 (Forman et al. 1978) or
1H 1720+117 (Wood et al. 1984) is an X-ray source which has been
identified with a 16.6 mag. starlike object with a strong UV excess
(U - B = -0.50) (Griffiths et al. 1989; Brissenden et al. 1990); this
object has a featureless spectrum according to Brissenden et al.; however
Griffiths et al. have observed an absorption feature near 6000 A which
could be redshifted Na I D {lambda}5892 A in the host galaxy in which
case the redshift would be 0.018. It shows a high degree of optical
polarization (Griffiths et al.; Brissenden et al.). It is associated with
a weak (S ~ 0.1 Jy) flat spectrum radiosource (Brissenden et al.;
Griffiths et al.; Gregory & Condon, 1991). A companion with m_B_ = 20.6
has been detected at 2.6" (Falomo et al. 1990).
Our spectrum is continuous with no trace of an absorption feature near
6000 A. A weak absorption line is detected at 5892 A which could be Na I
D in our galaxy (the galactic latitude of the source is b = 24^deg^);
this line has also been seen by Griffiths et al.; weak galactic Ca II H
and K are also seen.


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