1 / 20

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

felix
Télécharger la présentation

High Velocity Outflows in Quasars

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related