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)
Inad
a et
al.
2003
Zqso =1.74zcl =0.68
HS
T A
CS
imag
e (I
nada
et a
l. 20
05)
SDSS J1004+4112
Spectroscopic Differences in Lensed Spectroscopic Differences in Lensed Quasar ImagesQuasar 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)
Hypothesis 1: MicrolensingHypothesis 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.
Hypothesis 2:Intrinsic VariabilityHypothesis 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]
Differential Absorption?
Differential Absorption?
SDSS BAL and non-BAL QSO Composites
Rei
char
d et
al.
2003
Skimming the Spinning Dented Bugle Bell?
Elvis (2000)
GeometryGeometry
LAMAS and variability in SDSSJ1004+4112 provide complementary constraints on absorber size
tVa transV
θ From absorber distance; image splittingaRa
From rotation speed; variability timescale (a<300AU)
aR (~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
No match for ~RBELR
Variability in X-ray Absorbers
Ubiquitous!Risaliti, Elvis & Nicastro (2002)
Fast!Elvis et al. 2004 (NGC 4388)
Ubiquitous Warm Broad Absorbers?
Sob
olew
ska
& D
one
2005
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.
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.