The SEXSI Survey: Recent Progress
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Transcript of The SEXSI Survey: Recent Progress
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November 2006 1
Megan E. Eckart
Caltechwith Fiona Harrison, David Helfand,
Daniel Stern, Luke Kotredes
The SEXSI Survey: Recent Progress
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Overview
• Introduction to the SEXSI sample and optical followup
• Highlights of the optical/X-ray sample composition
• Spitzer data – high-z type 2 quasar candidates– SED’s of spectroscopically ID’d sources
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SEXSI Survey
• Study dominant contributors to XRB
• 1034 2-10 keVsources from 27 Chandra pointings; (2 deg2)
• R-band imaging
• 438 spectroscopic redshifts from Keck
Harrison et al. 2003, ApJ, 596, 944-956 (Paper 1)
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4Harrison et al. 2003, ApJ, 596, 944-956 (Paper 1)
SEXSI Survey
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Redshift Distribution
• Peak: z ~ 0.7
• 34 narrow-lined Lx>1044 sources(type-2 quasar candidates)
• nine z > 2, obscured type-2 quasar candidates
Eckart et al. 2006, ApJS, 165, 19-56 (Paper 3)
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Fraction Obscured
• SEXSI - excellent statistics over flux range
~50% obscuredindependent of luminosity
log (Unobscured 2-10 keV Luminosity [erg s-1])
Fra
ctio
n w
ith lo
g(N
H)
> 2
2
Eckart et al. 2006, ApJS, 165, 19-56 (Paper 3)
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Spitzer Data
• Spitzer data over five SEXSI fields
(IRAC & MIPS)
• 250 SEXSI X-ray sources covered
• 140 with spectroscopic ID
•62% of total X-ray sources are in “wedge”
• 86% of BLAGN
• 67% of NLAGN
• 28% of ELG
• 15% of sources with Lx<10 43.5 erg s-1
- wedge from Stern et al. (2005)
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High-z QSO 2
- quadrant split from Martinez-Sansigre, Lacy et al. (2005)
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High-z QSO 2
- quadrant split from Martinez-Sansigre, Lacy et al. (2005)
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BLAGN SED’s
• Many BLAGN fit a typical quasar SED (Elvis et al. 1994)
•BUT, there are many that fit a star forming template better in mid-IR/optical (Devriendt et al. 1999 template plotted above)
log ( [Hz]) log ( [Hz])
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NLAGN SED’s
• Fits star forming template in IR • Bad match to both templates
•(would match an absorbedAGN spectrum …)
log ( [Hz]) log ( [Hz])
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ELG SED’s
• Overwhelming majority (but not all) of ELG fit starforming template
log ( [Hz])
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In Progress…
Synthesis of spectrally identified and unidentified SED’s
X-ray stacking of Spitzer sources with Chandra nondetections
Acknowledgements: Fiona Harrison, David Helfand, Dan Stern, Luke Kotredes
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