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Date and Time of the Query: 2019-06-25 T03:51:03 PDT
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Notes for object PG 1216+069

9 note(s) found in NED.


1. 2009ApJ...705..962C
Re:PG 1216+069
This sight line shows strong positive high-velocity Si III absorption spread out
over at least two components. This feature is detected in C IV over the same
velocity extent, and in Si II {lambda}1260.42 over a slightly narrower velocity
range. Although not included by S03, owing to IGM Ly{beta} contamination, the
feature seems present in O VI as well. Based on comparisons of absorption
profiles, we analyze the feature as two components separated at V_LSR_ = 234 km
s^-1^.

2. 2008ApJS..179...37T
Re:PG 1216+069
3.9. PG 1216+069 The STIS data for PG 1216+069 (z_qso_ = 0.3313) allow us to
search for O VI doublets in the range 0.1309 < z_abs_ < 0.3078. We detect only a
single intervening O VI absorber, at z_abs_ = 0.28232. z_abs_ = 0.28232 (Fig.
16; Table 11).-The only O VI system we detect toward PG 1216+069, this absorber
has very weak O VI absorption, along with very strong, saturated, multicomponent
H I, allowing us to set only a lower limit on log N(H I). We also detect
saturated C III {lambda}977, and strong Si III {lambda}1206. In the C III
region, we fit only the zero velocity component. Other components may be bona
fide C III associated with the blue H I component, but this is not clear.
Precise knowledge of the H I component positions would be valuable for
determining this.

3. 2008ApJS..179...37T
Re:PG 1216+069
4.4. PG 1216+069 [IMAGE] .-O VI {lambda}1037 blends with the heavily saturated
Ly{beta} line from the absorber at z = 0.28232, and hence this system cannot
meet our criteria for a doublet search.

4. 2003ApJS..146....1W
Re:PG 1216+069
PG 1216+069.-There is a Lyman series at v = 1880 km s^-1^ in this
spectrum, associated with the Virgo Cluster. The Ly{alpha} line can be
seen in the FOS spectrum (Savage et al. 2000). The Ly{beta} line in this
series overlaps the Galactic O VI component. This makes it impossible
to measure the Galactic O VI {lambda}1031.926 absorption. The Galactic
O VI {lambda}1037.617 is not clearly seen either. It is still possible to
discern a high-velocity O VI component in the O VI {lambda}1031.926 and
O VI {lambda}1037.617 lines (near 290 km s^-1^), whose presence would be
consistent with other similar components seen in neighboring directions
(3C 273.0, HE 1228+013 1, PG 1116+215, and Mrk 734).

5. 2002ApJS..143..257K
Re:PG 1216+069
1219+0638ra.---Blue end of the G190H spectrum is noisy and was ignored
below 1605 {Angstrom} before merging; note that this region lies on
Ly{alpha}.

6. 2002ApJS..140..143B
Re:PG 1216+069
q1216+0655, z = 0.334.-J98 suggest a metal line absorber at z = 0.1247,
but there are not strong arguments supporting it. G270, G190, G130.

7. 2000ApJS..129..563S
Re:PG 1216+069
PG 1216+069 (z_em_ = 0.334). - This QSO was observed with the
G130H, G190H, and G270H gratings (see Table 4). The modest Mg II average
velocity equivalent width of 112 km s^-1^ is considerably larger than
the 21 cm emission width of 82 km s^-1^. The possible structure seen in
the wings of the Mg II lines has low statistical significance. The
modest Mg II width is consistent with the absence of known H I HVCs in
this direction. Seven Galactic ISM lines in the incomplete sample of
absorption lines for this QSO are found in Table 7 of CAT3.

8. 1998MNRAS.298..121B
Re:PG 1216+069
This radio-quiet object was imaged by Hutchings, Crampton & Campbell
(l984) who described it as having a halo. Kellerman et. al. (1994)
presented 5-GHz D and A-configuration VLA maps of the source. These show
an unresolved core coincident with the optical quasar plus a second
elongated component stretching from the core with a PA~25^deg^. The
total size of the radio source is 0.85 arcsec. The PC image of this
object is severely contaminated by scattered light from a nearby bright
star. None the less, We managed to obtained a reasonable fit to the data
using the cross-correlation technique by only fitting to the pixels to
the south of the image (away from the scattered light). The image is
better fit by a GdV model than an exponential disc. The best-fitting
model gives a derived M_Host_(V)= -20.9, about 1 mag brighter than L*.
There are two close apparent companion objects, one at a projected
separation of 1.8 arcsec (13.6 kpc), the other at 2.7 arcsec (20.4
kpc).

9. 1996AJ....111..645F
Re:[HB89] 1216+069
1216+069
nearby object to southwest.


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