Q0906 6930: The Highest Redshift Blazar

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Q09066930 The Highest Redshift Blazar

• GLAST for Lunch 11.18.04
• David Sowards-Emmerd

Quiz from previous talk Whats wrong with this
slide????
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How did we find it?

• Serendipity! J09066930 was part of a
  radio/X-ray selected
• survey of EGRET-like blazar candidates.
• Very faint optical counterpart at precise radio
  position
• Color faint radio as a possible method for
• selecting hi-z radio bright quasars.

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Survey Selection

• Motivation GLAST should detect thousands of
  blazars,
• the current samples contain only hundreds of
  blazars.
• Coordinated observing campaigns are much easier
  if theres
• a source list to work from.
• Selected 710 sources (northern hemisphere) using
  our
• Figure of Merit ranking technique.
• Significant correlation of these candidate
  blazar source
• positions with residual/background EGRET
  photons.

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J09066930
Very significant detection of the Lyman break
along with several other lines. Exact redshift
is a bit uncertain due to absorption of Lya To
be re-observed with a different setup at HET
instrument issues
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Spectroscopy Issues

• Wavelength range dependent on setup
• Resolution vs. S/N
• Order overlap worse with HET
• Blocking filters
• Sky subtraction
• Near-IR flux calibration
• Fringing

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Properties of J09066930
Radio S1.4 91 mJy S8.4 188 mJy S15 115
mJy S43 42 mJy a1.4-8.4 -0.4 Optical I
23 X-ray Not detected by RASS ?-ray EGRET
upper limit only lies in the overlap between
two 3EG sources So why do we believe its a
blazar?
? Implications for SZ/CMB experiments
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Broadband SED
Fun with SSC models!
Redshifted 3C279 SED for comparison.
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VLBA Follow-up
? JET!
(multi-epoch obs. would be nice!)
15 GHz
43 GHz
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X-ray Follow-up
CHANDRA Observations to search for CMB photons
Compton upscattered by the jet. Similar
observations have been performed for other high-z
quasars, but few X-ray jets (non-core components)
have been seen.
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Black Hole Mass Estimates
Follow-up optical spectroscopy is needed to
place better constraints on the mass of the
central black hole The SiIV/OIV line is not
ideal for this, but its the only line weve got
at the moment.
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Related Future Lunch Talk Ideas

• EBL attenuation
• CMB upscatter in jets
• Black hole mass estimates
• AGN classification (unrelated)