Variable X-ray absorption in the mini-bal QSO PG
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1 Variable X-ray absorption in the mini-bal QSO PG Margherita Giustini Massimo Cappi, George Chartas, Mauro Dadina, Mike Eracleous, Gabriele Ponti, Daniel Proga, Francesco Tombesi, Cristian Vignali, and Giorgio G.C. Palumbo A&A in press, arxiv : AGN Winds in Charleston - Saturday, October 15, 2011
2 A Intro AGN accretion disk winds BAL and mini-bal QSOs X-ray observations B The 2008/09 XMM-Newton campaign on PG The AGN structure Wind kinetic efficiency Future perspectives So what? C
3 AGN accretion disk winds There are strong evidences that outflowing matter is a key ingredient of the inner regions of AGN observational Saturday and Sunday sessions theoretical Monday session relevant to: AGN structure and Cosmic feedback Monday and Tuesday sessions
4 BAL and mini-bal QSOs Powerful outflows from the inner regions of AGN Broad (FWHM > 2000 km/s) ) and mini-broad (FWHM < 2000 km/s) ) Absorption Line Quasars Arav et al Misawa et al log ξ ~ 0 erg cm s -1 logn H ~ cm -2 υ out ~ c Observed fraction: ~16% among optically selected QSOs Intrinsic fraction: ~40% Ganguly & Brotherton 2008; Allen et al Hewett & Foltz 2003: Knigge et al. 2008; Gibson et al. 2009; Rodriguez Hidalgo 2009
5 Green et al ApJ 450, 51 X-ray obser vat io ns RASS x LBQS Fi rst syst em at ic survey BAL QSOs are X-ray weak : 1/37 BAL QSO detected ( ) ( ) < %2 optical to X-ray spectral index " ox = log f 2keV / f 2500# log $ 2keV /$ 2500# Mar gher it a Gi us t ini - AGN winds in Char les ton - Sat ur day, Oct ober 15, 2011
6 Green et al ApJ 450, 51 X-ray obser vat io ns BAL QSOs are X-ray weak : 1/37 BAL QSO detected ( ) ( ) < %2 optical to X-ray spectral index " ox = log f 2keV / f 2500# log $ 2keV /$ 2500# Brandt et al ApJ 528, 637 RASS x LBQS Fi rst syst em at ic survey BAL QSOs X-ray weakness correlates with EW(C IV) and is thus consistent with being due to absorption Mar gher it a Gi us t ini - AGN winds in Char les ton - Sat ur day, Oct ober 15, 2011
7 Green et al ApJ 450, 51 X-ray observations BAL QSOs are X-ray weak : 1/37 BAL QSO detected ( ) ( ) < %2 optical to X-ray spectral index " ox = log f 2keV / f 2500# log $ 2keV /$ 2500# Brandt et al ApJ 528, 637 RASS x LBQS First syst emat ic survey BAL QSOs X-ray weakness correlates with EW(C IV) and is thus consistent with being due to absorption Gallagher et al ApJ 546, 795 Gallagher et al ApJ 603, 425 ASCA Chandra First spectra of BAL and mini-bal QSOs Complex absorption and a typical underlying intrinsic continuum
8 The new XMM-Newton observational campaign PG z=0.062 M BH ~1.2 x 10 8 M r g ~1.8 x cm t L ~ 600 s L BOL ~ L M acc ~ 0.7 M /yr L/L Edd ~ 0.26
9 The new XMM-Newton observational campaign PG z=0.062 M BH ~1.2 x 10 8 M Wang et al r g ~1.8 x cm t L ~ 600 s L BOL ~ L M acc ~ 0.7 M /yr L/L Edd ~ 0.26 υ UV ~ 5,000 km/s IUE: mini-bals in C VI, Si IV, N V
10 The new XMM-Newton observational campaign PG z=0.062 M BH ~1.2 x 10 8 M r g ~1.8 x cm t L ~ 600 s L BOL ~ L M acc ~ 0.7 M /yr L/L Edd ~ 0.26 υ UV ~ 5,000 km/s
11 The new XMM-Newton observational campaign PG z=0.062 M BH ~1.2 x 10 8 M Wang et al r g ~1.8 x cm t L ~ 600 s L BOL ~ L M acc ~ 0.7 M /yr L/L Edd ~ 0.26 υ UV ~ 5,000 km/s
12 The new XMM-Newton observational campaign PG z=0.062 Wang et al M BH ~1.2 x 10 8 M r g ~1.8 x cm t L ~ 600 s L BOL ~ L M acc ~ 0.7 M /yr L/L Edd ~ 0.26 υ UV ~ 5,000 km/s ROSAT: Soft X-ray absorption
13 The new XMM-Newton observational campaign PG z=0.062 XMM Archive, December 2004 : 33 (28) ks M BH ~1.2 x 10 8 M r g ~1.8 x cm t L ~ 600 s L BOL ~ L M acc ~ 0.7 M /yr L/L Edd ~ 0.26 υ UV ~ 5,000 km/s
14 The new XMM-Newton observational campaign PG z=0.062 XMM Archive, December 2004 : 33 (28) ks M BH ~1.2 x 10 8 M r g ~1.8 x cm t L ~ 600 s L BOL ~ L M acc ~ 0.7 M /yr L/L Edd ~ 0.26 υ UV ~ 5,000 km/s
15 The new XMM-Newton observational campaign PG z=0.062 M BH ~1.2 x 10 8 M r g ~1.8 x cm t L ~ 600 s L BOL ~ L XMM Archive, December 2004 : 33 (28) ks A NEW OBSERVATIONAL CAMPAIGN M acc ~ 0.7 M /yr L/L Edd ~ 0.26 υ UV ~ 5,000 km/s
16 The new XMM-Newton observational campaign PG z=0.062 M BH ~1.2 x 10 8 M r g ~1.8 x cm t L ~ 600 s XMM Archive, December 2004 : 33 (28) ks XMM AO-7, June 2008 : 31 (4) ks XMM AO-7, December 2008 : 12 (4) ks XMM AO-8, June 2009 : 134 (92) ks L BOL ~ L M acc ~ 0.7 M /yr L/L Edd ~ 0.26 υ UV ~ 5,000 km/s The longest X-ray look ever at a mini-bal QSO
17 The new XMM-Newton observational campaign Li ght Cu r v es December 2004 : 28 ks Spect ra
18 The new XMM-Newton observational campaign Li ght Cu r v es December 2004 : 28 ks June 2008 : 4 ks Spect ra
19 The new XMM-Newton observational campaign Li ght Cu r v es December 2004 : 28 ks June 2008 : 4 ks December 2008 : 4 ks Spect ra
20 The new XMM-Newton observational campaign Li ght Cu r v es December 2004 : 28 ks June 2008 : 4 ks December 2008 : 4 ks June 2009 : 92 ks Spect ra
21 The new XMM-Newton observational campaign Li ght Cu r v es December 2004 : 28 ks June 2008 : 4 ks December 2008 : 4 ks June 2009 : 92 ks Spect ra Strong X-ray variability on time scales of months on time scales of hours
22 Spectral analysis: the average spectra Fit to a power law
23 Spectral analysis: the average spectra Fit to a power law Γ ~ 0.6 χ 2 /ν=8801/1591
24 Spectral analysis: the average spectra Fit to a power law A moderately-ionized absorber ionization parameter log ξ ~1.5 erg cm s -1 column density logn W ~23.1 cm -2 logn W ~22.5 cm -2 logn W ~22.8 cm -2 logn W ~23.1 cm -2 Γ ~ 0.6 χ 2 /ν=8801/1591 Γ ~ 2.1 χ 2 /ν=2234/1583
25 Spectral analysis: the average spectra Fit to a power law A moderately-ionized absorber ionization parameter log ξ ~1.5 erg cm s -1 column density logn W ~23.1 cm -2 logn W ~22.5 cm -2 logn W ~22.8 cm -2 logn W ~23.1 cm -2 Γ ~ 0.6 χ 2 /ν=8801/1591 Γ ~ 2.1 χ 2 /ν=2234/1583
26 Spectral analysis: the average spectra Spect ral residuals power law moderately ionized absorber
27 Spectral analysis: the average spectra Spect ral residuals power law moderately ionized absorber c EW 1 =80 ± 20 ev EW 2 =125 ± 25 ev Δχ 2 /Δν =60/4
28 Spectral analysis: the average spectra Spect ral residuals A highly-ionized absorber power law log N W ~ cgs log ξ W ~1.5 cgs moderately ionized absorber Γ~2.1 F scatt ~2-3% logn H ~23.8 cgs log ξ H ~3.5 cgs υ out ~16,500 km/s c logn H <22.8 cgs logn H <22.8 cgs logn H ~23.3 cgs log ξ H ~3.7 cgs EW 1 =80 ± 20 ev EW 2 =125 ± 25 ev Δχ 2 /Δν =60/4 Δχ 2 /Δν =122/9
29 Spectral analysis: the average spectra α ox is variable DEC 2004 JUN 2008 DEC 2008 JUN 2009
30 Spectral analysis: the average spectra α ox is variable DEC 2004 JUN 2008 DEC 2008 JUN 2009
31 Time-resolved spectral analysis Strong variability on time scales of months and hours
32 Time-resolved spectral analysis Strong variability on time scales of months and hours kev kev Mar ghe r it a Gi us t ini - AGN winds in Char les ton - Satur day, October 15, 2011
33 Time-resolved spectral analysis E < 6 kev Strong variability on time scales of months and hours Two distinct spectral components kev E > 1.5 kev kev Mar ghe r it a Gi us t ini - AGN winds in Char les ton - Satur day, October 15, 2011
34 Time-resolved spectral analysis Li ght Cu r v e
35 Time-resolved spectral analysis Li ght Cu r v e Spect ra
36 Time-resolved spectral analysis Li ght Cu r v e Fe K band residuals 68%,90% lev els Spect ra
37 Time-resolved spectral analysis Li ght Cu r v e Fe K band residuals 68%,90% lev els Spect ra
38 Time-resolved spectral analysis Li ght Cu r v e Fe K band residuals 68%,90% lev els Spect ra
39 Time-resolved spectral analysis Li ght Cu r v e Fe K band residuals 68%,90% lev els Spect ra
40 Time-resolved spectral analysis Li ght Cu r v e Fe K band residuals 68%,90% lev els Spect ra The highly-ionized absorber is variable over time scales of hours
41 So What - the AGN structure Strong X-ray variability on time scales of months and hours Two distinct spectral components: one emerging at E < 6 kev (months), the other at E > 1.5 kev (hours). A moderately ionized absorber is varying on time scales of months. A highly ionized absorber is varying on time scales of hours. WE ARE STARTING TO PROBE THE DYNAMICS OF THE INNER ACCRETION/EJECTION FLOW IN AGN The observed α ox is varying as well. Is the wind seeing the variations at E ~ 6-10 kev or at E ~ 2 kev? Margherita r a Giustini t ini - AGN winds in Charleston - Satur urday, October r 15, 2011
42 What about the feedback? kinetic efficiency " w # M 2 out$ out L acc mass outflow rate " A(r)#(r)$ out (r) So What - the wind kinetic efficiency
43 What about the feedback? So What - the wind kinetic efficiency kinetic efficiency " w # M 2 out$ out L acc Assuming spherical symmetry, isotropy, constant velocity: = 4"m H nr 2 # out C f F V mass outflow rate " A(r)#(r)$ out (r)
44 What about the feedback? So What - the wind kinetic efficiency kinetic efficiency " w # M 2 out$ out L acc mass outflow rate " A(r)#(r)$ out (r) Assuming spherical symmetry, isotropy, constant velocity: = 4"m H nr 2 # out C f F V Assuming photoionization equilibrium, and the absorber as a thin shell: = 4"m H L ion # $ outc f F V
45 What about the feedback? So What - the wind kinetic efficiency kinetic efficiency " w # M 2 out$ out L acc mass outflow rate Assuming spherical symmetry, isotropy, constant velocity: = 4"m H nr 2 # out C f F V Assuming photoionization equilibrium, and the absorber as a thin shell: " M acc # w " up to a few % For the highly ionized, high velocity phases. " A(r)#(r)$ out (r) = 4"m H L ion # $ outc f F V BUT All the assumptions are highly uncertain!
46 What about the feedback? So What - the wind kinetic efficiency kinetic efficiency " w # M 2 out$ out L acc mass outflow rate " A(r)#(r)$ out (r) Assuming spherical symmetry, isotropy, constant velocity: = 4"m H nr 2 # out C f F V Assuming photoionization equilibrium, and the absorber as a thin shell: = 4"m H L ion # $ outc f F V " M acc # w " up to a few % For the highly ionized, high velocity phases. BUT All the assumptions are highly uncertain! ΔR ~ N H /n R
47 What about the feedback? So What - the wind kinetic efficiency kinetic efficiency " w # M 2 out$ out L acc mass outflow rate " A(r)#(r)$ out (r) Assuming spherical symmetry, isotropy, constant velocity: = 4"m H nr 2 # out C f F V Assuming photoionization equilibrium, and the absorber as a thin shell: = 4"m H L ion # $ outc f F V " M acc # w " up to a few % For the highly ionized, high velocity phases. BUT All the assumptions are highly uncertain! ΔR ~ N H /n R
48 What about the feedback? So What - the wind kinetic efficiency kinetic efficiency " w # M 2 out$ out L acc mass outflow rate Assuming spherical symmetry, isotropy, constant velocity: = 4"m H nr 2 # out C f F V Assuming photoionization equilibrium, and the absorber as a thin shell: " M acc # w " up to a few % For the highly ionized, high velocity phases. " A(r)#(r)$ out (r) = 4"m H L ion # $ outc f F V BUT All the assumptions are highly uncertain! Large systematic uncertainty also on ξ
49 What about the feedback? So What - the wind kinetic efficiency kinetic efficiency " w # M 2 out$ out L acc mass outflow rate " A(r)#(r)$ out (r) Assuming spherical symmetry, isotropy, constant velocity: = 4"m H nr 2 # out C f F V Assuming photoionization equilibrium, and the absorber as a thin shell: = 4"m H L ion # $ outc f F V " M acc # w " up to a few % For the highly ionized, high velocity phases. BUT All the assumptions are highly uncertain! Large systematic uncertainty also on ξ
50 What about the feedback? So What - the wind kinetic efficiency kinetic efficiency " w # M 2 out$ out L acc mass outflow rate " A(r)#(r)$ out (r) Assuming spherical symmetry, isotropy, constant velocity: = 4"m H nr 2 # out C f F V Assuming photoionization equilibrium, and the absorber as a thin shell: = 4"m H L ion # $ outc f F V " M acc # w " up to a few % For the highly ionized, high velocity phases. BUT All the assumptions are highly uncertain! Large systematic uncertainty also on ξ
51 What about the feedback? So What - the wind kinetic efficiency kinetic efficiency " w # M 2 out$ out L acc mass outflow rate " A(r)#(r)$ out (r) Assuming spherical symmetry, isotropy, constant velocity: = 4"m H nr 2 # out C f F V Assuming photoionization equilibrium, and the absorber as a thin shell: = 4"m H L ion # $ outc f F V " M acc # w " up to a few % For the highly ionized, high velocity phases. BUT All the assumptions are highly uncertain! BE CAREFUL WITH MASS OUTFLOW RATE ESTIMATES! Large systematic uncertainty also on ξ
52 So What - fut ure perspect iv es Enlarge the numbers: SDSS and XMM/Chandra data to be comp are d with AGN accretion dis k winds th eoretical predictions Re fine the studies: deep observational campaigns on the most pr omising sources: unv eiling the dyna mics of the in ner accr etion/ejectio n flow The future: is now called ATHENA, se e Massimo Cappi s talk: PN 5 ks XMS 5 ks Mar gher it a Gi us t ini - AGN winds in Char les ton - Sat ur day, Oct ober 15, 2011
53 So What? THANKS FOR YOUR ATTENTION! Mar gher it a Gi us t ini - AGN winds in Char les ton - Sat ur day, Oct ober 15, 2011
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arxiv: v1 [astro-ph.co] 16 Dec 2011
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**Volume Title** ASP Conference Series, Vol. **Volume Number** **Author** c **Copyright Year** Astronomical Society of the Pacific arxiv:1112.3750v1 [astro-ph.co] 16 Dec 2011 Variable X-ray absorption
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