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Lens-Aided Multi-Angle Spectroscopy ( LAMAS )

Lens-Aided Multi-Angle Spectroscopy ( LAMAS ). How spectral differences between lensed quasar images may reveal important new information about outflows in AGN ApJ, in press (astro-ph/0603033) Paul Green (CfA). Z qso =1.74 z cl =0.68. Inada et al. 2003. SDSS J1004+4112.

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Lens-Aided Multi-Angle Spectroscopy ( LAMAS )

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  1. Lens-Aided Multi-Angle Spectroscopy (LAMAS) How spectral differences between lensed quasar images may reveal important new information about outflows in AGN ApJ, in press (astro-ph/0603033) Paul Green (CfA)

  2. Zqso =1.74 zcl =0.68 Inada et al. 2003

  3. SDSS J1004+4112 HST ACS image (Inada et al. 2005) HST ACS

  4. Spectroscopic Differences in Lensed Quasar Images Bona fide lensed quasars show significant differences between image components in • Optical/UV spectra • HE2149--2745; SBS1520+530 (Burud et al. 2002) • SDSSJ1004+4112 (Inada et al. 2003) • SDSSJ1206+4332 (Oguri 2005) • Absorber properties in BALQSO lenses • APM0829+5255 (Lewis et al. 2002) • H1413+117 (Angonin et al. 1990)

  5. Hypothesis 1: Microlensing • Integral field spectroscopy from [Wisotski et al. 2004] shows that A/B continuua are identical while CIV difference persist • Microlensing unlikely to amplify part of the BELR but not the continuum region • CIV blue wing enhancement disappears and reappears • Strong profile differences persist in CIII] and MgII [Richards et al. 2004], which originate from larger regions.

  6. Hypothesis 2:Intrinsic Variability • The asymmetry (rA-rB)/(rA+rB) of the A and B images wrt the lens means the maximum delay between them is <30d [Oguri et al. 2004] • B never showed a bluewing bump, although it persisted in A for >>1 month. [Richards et al. 2004]

  7. Differential Absorption?

  8. Differential Absorption?

  9. SDSS BAL and non-BAL QSO Composites Reichard et al. 2003

  10. Skimming the Spinning Dented Bugle Bell? Elvis (2000)

  11. Geometry LAMAS and variability in SDSSJ1004+4112 provide complementary constraints on absorber size From rotation speed; variability timescale (a<300AU) θFrom absorber distance; image splitting  No match for ~RBELR (~100 lt-d or 1017cm), but OK within recent BALR distance estimates of 5 – 700pc (deKool et al 2001, Everett et al. 2002)  30<a<3000 AU

  12. Variability in X-ray Absorbers Ubiquitous! Risaliti, Elvis & Nicastro (2002) Fast! Elvis et al. 2004 (NGC 4388)

  13. Ubiquitous Warm Broad Absorbers? Sobolewska & Done 2005

  14. LAMAS • The A image of SDSS J1004+4112 shows variable spectral differences not easily explained by microlensing or variability+time delay. • SDSS J1004 and other lenses may illustrate that small angle changes to the nuclear region can strongly affect spectral details. • The spectral differences mimic differential absorption from a high column, highly ionized wind.

  15. Further Implications • Quasars have high column, highly ionized winds. • All quasar spectra may be self-absorbed by their smoothly outflowing winds. • In a large sample of lenses, spectral difference should correlate with θ and be independent of proximity to a bright galaxy of high microlensing optical depth. • X-ray measurements during a similar UV blue emission line asymmetry event should show lower absorption in that component.

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