the x-ray properties of spitzer-selected type-2 quasars mark lacy (ssc), nick seymour, anna sajina,...
Post on 19-Dec-2015
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The X-ray properties of Spitzer-selected type-2
quasars
Mark Lacy (SSC),
Nick Seymour, Anna Sajina, Lisa Storrie-Lombardi, Lee Armus (SSC)
Andreea Petric (Columbia), Gabriela Canalizo (Riverside), Susan Ridgway (NOAO), Elinor
Gates (Lick Obs)
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Surveys for dust-obscured AGN
• Chandra surveys vs Spitzer surveys– Spitzer finds objects on basis of hot dust emission.– Finds preferentially high accretion-rate objects
(“dirty accretors”).– Chandra misses the most heavily obscured
objects, but can find low accretion rate objects that Spitzer misses (e.g. some LINERS/XBONGs/low-luminosity radio galaxies - the “clean” accretors).
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Spitzer selection of AGN• Use “wedge” in IRAC color-color plot to select
objects with hot dust continua, or require red power-law in mid-IR.
• At bright (24mu flux ~5mJy) levels, <z>~0.6, median (bolometric) luminosity about x10
QSO/Seyfert divide.• Optically, our IR-wedge selected AGN sample
is 33% normal type-1, 44% type-2, 14% reddened type-1 and 9% low-ionization in the optical (Lacy et al. 2006).
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What about the X-ray?
• Some of our type-2 quasars overlap 20-50ks XMM pointings.
• Most fluxes from 2XMM.
• About half the type-2s are detected.
• All the detected type-2 objects have high hardness ratios where available.
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X-ray survey strategies
• Areal density of bright AGN low ~ 6/deg^2 to ~5mJy at 24mu.
• Shallow X-ray survey will find the ~1/3 unobscured objects.
• Deep pointed observations (~30ks) required for the obscured objects.
• Contrast with GOODS-type surveys - finds these objects, but only at z>>1.
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ADIOS (Richards et al)
• Wide area (~200deg^2) survey in SDSS equatorial field• Field is repeated when northern fields are unavailable• Limit ~25 mag• Applying for Spitzer/IRAC time, principally for quasar survey.
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Summary
• Making sense of the AGN population requires both Spitzer and Chandra.
• Host galaxy absorption/extinction probably plays an important role at the highest columns, but more study of heavily absorbed objects required.
• May have to abandon the “pyramid scheme” to study luminous heavily absorbed quasars at z<1 (and other rare objects).
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The Compton thick elephant…
(with apologies to Banksy (and the elephant))