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High Velocity Outflows in Quasars

High Velocity Outflows in Quasars. Paola Rodriguez Hidalgo Advisor: Fred Hamann University of Florida Collaborators: Daniel Nestor, Joseph Shields. Classification of Absorption Lines. Based on similar redshift to the quasar: Associated Non-associated

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High Velocity Outflows in Quasars

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  1. High Velocity Outflows in Quasars Paola Rodriguez Hidalgo Advisor: Fred Hamann University of Florida Collaborators: Daniel Nestor, Joseph Shields

  2. Classification of Absorption Lines • Based on similar redshift to the quasar: Associated Non-associated • Based on the absorber is ejected from the quasar: Intrinsic Non-intrinsic • Based on the width of the line: BAL NAL miniBAL

  3. Classification of Absorption Lines • Based on similar redshift to the quasar: Associated Non-associated • Based on the absorber is ejected from the quasar: Intrinsic Non-intrinsic • Based on the width of the line: BAL: form in winds NAL: origin? Most AALs are intrinsic (see Leah Simon, Daniel Nestor and Rajib Ganguly posters), how many at High Velocity (HV) are intrinsic? (36% ? - Richards et al. 1999, 2001) miniBAL: barely studied: how common are they?, how often do they appear at HV? HighVelocity Outflows

  4. Example of a High Velocity Outflow Ly+NV PG 0935+417 v ~ 51,000 km/s SiIV+OIV CIV CIV!

  5. Goals • Account for types of outflows to input information into physical/geometrical models. • Understand miniBAL-BAL relationship: distinct or same thing with different sightline? • Confirm intrinsic nature of large number of systems for follow-up and, hopefully, get information about location, densities, … and to explain wind structure and dynamics.

  6. Searching for High Velocity Outflows: the Sample • SDSS Quasar spectra: • R ~ 150 km/s • Spectral coverage 3820-9200 A; to see CIV 1548,1550 absorbers: zem > 1.8 to see velocities up to 0.2c: zem > 2.1 • Choose the n(t) spectra with best S/N • Look for every blue-shifted CIV absorber - zabs, v, FWHM, REW, BI, AI

  7. Searching for High Velocity Outflows: the Sample • SDSS Quasar spectra: • R ~ 150 km/s • Spectral coverage 3820-9200 A; to see CIV 1548,1550 absorbers: zem > 1.8 to see velocities up to 0.2c: zem > 2.1 • Choose the 2,200 spectra with best S/N -> 1,846 • Look for every blue-shifted CIV absorber - zabs, v, FWHM, REW, BI, AI - 5320 absorption systems measured

  8. Searching for High Velocity Outflows: the results

  9. CIV absorbers found BAL miniBAL NAL Restframe wavelength (A)

  10. CIV absorbers found • Number of miniBALs = 423 • Number of quasars with miniBALs = 284 • Number of quasars with miniBALs at v > 10,000 km s-1 = 175 • Number of quasars with miniBALs at v > 25,000 km s-1 = 51

  11. CIV absorbers found 14% 2.5%

  12. Some questions: • What sorts of structures and what lines of sight through the outflow produce miniBALs? • How often should we see miniBALs vs BALs and NALs if we view these outflows along random sightlines? • How fast do miniBALs evolve or cross the line of sight? Should we see acceleration /decceleration? • Should HV miniBALs come with more/less Xray abs than BALs?

  13. Variability study Ly+NV PG 0935+417 v ~ 51,000 km/s SiIV+OIV CIV CIV!

  14. Variability study Flux HV CIV Observed wavelength (A)

  15. Searching for Variability: Data • KPNO 2.1m : R~200 km s-1, ~3600-6200 A • MDM 2.4m : R~230 km s-1 , ~3600-5200 A (collaboration with Joe Shields) • Lick3.0m : (collaboration with Jason Prochaska) • Literature: LBQS survey (Hewitt et al. 1994), etc…

  16. Variability study: some results

  17. Variability study: some results • 18 well-measured quasars in 3 observing campaigns • 5 quasars show clear variability in miniBALs (5/18~30%): If changes are due to ionization: tobs=0.7-1.9 yrs = high (?) upper limit for tvar ne= 6000-16200 cm-3 : lower limit Rmax=1700-4900 pc : upper limit • So far, no variability in NALs • Most systems vary only in strength, but some show shift in velocities

  18. Current & Future work • Continue Variability study ->looking for more intrinsic systems and monitoring campaign to study flow properties of confirmed ones • High resolution observations of best/interesting candidates to obtain more accurate properties • Compare to absorption in Xray data to explore UV-Xray correlations and the relationship miniBALs-BALs • Input results in current theoretical models to help constrain parameters

  19. Summary • We have searched the SDSS database looking for CIV absorbers to compile, for the first time, a catalog of CIV absorption lines in high-redshift quasars: 2,200 quasars, 5320 CIV absorption systems found • We did and continue to follow up some of these systems with new observations (KPNO 2.1m, MDM 2.4m, Lick 3.0m) to confirm intrinsic nature based on variability and characterize it. • We will follow up with Xray observations to study the relationship UV-Xray absorbers and miniBALs-BALs. • We will input the results into theoretical models to help constrain model parameters. Xiexie

  20. Questionable/Interesting HV candidates

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