Probing quasar outflows with intrinsic narrow absorption lines 1/15 The Central Engine of AGN in Xi’an (Oct. 17, 2006) T. Misawa, M. Eracleous, J. C. Charlton (PSU), R. Ganguly (University of Wyoming), D. Tytler, D. Kirkman, N. Suzuki, D. Lubin (UCSD) QAL group

Background A fraction of narrow quasar absorption lines (NALs) have been thought to be produced by gas ejected from the quasar central engines rather than by the intervening structures. These lines (intrinsic absorption lines) are believed to arise in a wind from the accretion disk around the super-massive black hole. Quasar absorption lines are historically classified into three categories by their line widths: categoryNALMini-BALBAL FWHM (km/s) < ,000> 2,000 Intrinsic ??YY 2/15

Outline Introduction: How to separate intrinsic NALs from intervening NALs - Covering factor analysis - Time variability analysis PART I --- Statistical analysis: search for intrinsic absorption lines in spectra of 37 quasars (at z = 2-4) obtained with Keck to investigate global properties of wind material around the quasars (submitted to ApJ). → see a poster Ganguly et al. (P-ID088) for low-z targets PART II --- Monitoring project: monitoring the variability of an intrinsic NAL in the quasar HS with the Subaru telescope, which enables us to investigate the detailed structure of absorbers (1AJ, 1ApJ, and 1ApJ submitted). 3/15

observer disk intergalactic gas halo gas gas around quasar quasar Redshift gas in our galaxy What produces NALs? Absorption lines in the spectra of quasars are produced whenever the line of sight to the quasars pass through clouds of gas. (3) → e.g., Lyα forest Lyα forest (2) → e.g., DLA, LLS, metal lines DLA metal lines (2) (4) BAL profile → e.g., BAL profile (1) → e.g., ISM, HVC in MW MW There are several types of absorbers: (1) absorbers in our Galaxy (2) disk/halo-gas in intervening galaxies (3) the intergalactic gas (4) gas physically associated with the quasars intervening intrinsic Introduction 4/15

How to identify intrinsic absorption lines With high-dispersion spectroscopy, individual intrinsic NALs have been resolved into narrower multiple components. R~3000 R~45000 Introduction Time variability analysis Covering factor analysis QSO absorber (A) Change of ionization condition in absorbing gas (B) Gas motion across the line of sight Time variability of line profiles: e.g., depth, equivalent width, and line centroid, C f within a few years in the absorber’s rest frame. (e.g., Hamann et al. 1997) (e.g., Wampler et al. 1995) 5/15

Class A (reliable intrinsic) Class B (possible intrinsic) Class C (intervening/unclassified) Census 28 class-A 11 class-B 111 class-C 150 NAL systems in 37 Keck/HIRES quasar spectra RESULTS: PART 1 - Census of intrinsic NALs - 6/15

Fraction of intervening NALs associated (v ej <5,000 km/s) Total C IV N V Si IV N/A non-associated (v ej >5,000 km/s) C IV: 11-19% of all C IV NALs have partial coverage. Among “associated” NALs (AALs; within 5,000 km/s of the quasar emission redshift), 33% show partial coverage. N V: Because of the Ly  forest, we were unable to study N V doublets with v ej < -5,000 km/s. Of the associated N V NALs, 75% show partial coverage. Si IV: 14-18% of all Si IV NALs have partial coverage. None of them are associated NALs. Census 7/15

Fraction of Quasars that have Intrinsic NALs Number of quasars that have 0-4 intrinsic NAL systems - If we assume that NAL absorbers are in the region with opening angle of 60 degree from the axis, then they cover 50% of the total solid angle. Census Proga et al. (1998,1999,2000) BAL (~10-15%) NAL (~50%) /15 At least half of all quasars have one or more intrinsic NAL systems. - The model of Proga et al. (2000) shows that the column density of this region is too low (and IP is too high) to produce C IV NALs. Therefore, the NAL gas would be denser filaments embedded in the higher ionization gas.

Ionization Conditions of Intrinsic NALs (1) Strong C IV system Strong N V system 28 C IV systems Strong (sometimes saturated) C IV and Lyα with weak/no N V Strong N V and weak C IV and Lyα(less than twice the N V EW) Census 11 N V systems 9/15

Ionization Conditions of Intrinsic NALs (2) Lo-NAL Hi-NAL d e t e c t e d d e t e c t e d d e t e c t e d N o t d e t e c t e d N o t d e t e c e t d N o t d e t e c t e d N o t d e t e c t e d d e t e c t e d d e t e c t e d d e t e c t e d d e t e c t e d 16 NALs23 NALs IP ~25% of quasars are LoNAL quasars Census About 2% of quasars are LoBAL quasar (Sprayberry & Foltz 1992; Reichard et al. 2003). 10/15

ABC DEFGH System B System A C f ~ 1.0C f < 1.0C f ~ 1.0 ABC DEFGH Monitoring RESULTS: PART 2 11/15 Monitoring a quasar HS

Time Variability Analysis C IV lines in HS Monitoring 12/15

Monitoring Model Fittings 13/15

Monitoring No clear correlations are seen between fit parameters → inhomogeneous internal structure Variable screening by another absorber. All absorption components changed in concert → change of ionization condition 14/15

VLT+UVES archive data we are now proposing to get additional spectra with Subaru and VLT. Chandra and XMM-Newton archive data Extend sample size and study of NAL demographics based on quasar properties (e.g., radio-loudness) Investigate inner regions of the accretion disks, and compare our optical results. monitor other NAL systems with more than one transition, and apply photoionization model to monitor ionization conditions. 15/15 Future Plans