RL -- RQ QUASAR DICHOTOMY in 4D Eigenvector 1 CONTEXT

1. J. Sulentic Instituto de Astrofisica de Andalucia P. Marziani Osservatorio Astronomico di Padova S. Zamfir University of Alabama RL -- RQ QUASAR DICHOTOMY in 4D Eigenvector 1 CONTEXT

3. BEFORE AVERAGING SPECTRA • A CONTEXT THAT UNIFIES SPECTROSCOPIC DIVERSITY • MULTI-WAVELENGTH • MULTI-DIMENSIONAL • TO REMOVE DEGENERACY BETWEEN PHYSICS AND ORIENTATION

5. EIGENVECTOR 1 PARAMETER SPACE FWHM H velocity dispersion of LIL EW (FeII Optical) / EW (Broad H) (RFeII) ratio of LIL with opposite density dependences Soft X-ray Photon Index (soft) thermal emission signature CIV 1549 Broad Line Shift systematic motions of HIL Precursors: Boroson & Green (1992); Boller et al. (1996); Marziani et al. (1996); Wang et al. (1996);Laor et al. (1997)

6. Another motivation for a spectroscopic investigation: BLR radius  1 light-month  at z = 0.01, angular size  0.1 mas HST resolution 46 mas VLBI (radio) resolution of ~ 1 mas IR-interferometry – several mas

7. Brightest ~400 SDSS DR5 • Only ~~400! Why? • Because the other 59000 are noisy! • Can we average them?

8. SPECTRAL DIVERSITY • Indiscriminate averaging of spectra—no matter how many—is of little use • Averaging must be done in some context—4DE1

9. The Brightest ~400 SDSS DR5

10. OUTLIERS FWHM H RFeII

11. B FWHM H FWHM HBC 4000 km/s A RFeII

13. DICHOTOMY • Population A: strong/moderate FeII, HIL blueshift/asymmetry, soft X-ray excess, radio quiet • Population B: weak/moderate FeII, no HIL blueshift or soft X-ray excess, mixed RL-RQ

15. PHYSICAL TRENDS  - Ionization parameter m - Dimensionless accretion rate M - BH mass ne - Electron density m ne FWHM H  M RFeII

19. Hypothesis 1 • Parent population of RL quasars show lobe dominated (LD) FRII radio morphology (very few sources with FRI morphology show optical or UV broad emission lines)

21. Hypothesis 2 • All RL core (CD) sources are beamed/boosted FRII sources • All RL CD sources in a radio flux-limited sample will be more radio luminous (higher R_K) than the faintest LD source • Radio luminosity is a more robust parameter for evaluating RLoudness than R_K

24. R_K • Standard RL cutoff -- R_K=10 • Weakest FRII -- R_K~ 70 • Our RL cutoff -- R_K~ 70 • All sources with R_K<70 are RQ

25. 1.4GHz Radio Luminosity • Better discriminator than R_K • RL cutoff Log L_1.4GHz~~31.5 • All sources log R<31.5 are RQ? • Sources between log R~30.5 - 31.5 Are RI? • All RI show core or core-jet morphology.

28. SDSS J075407.96+431610.6 z=0.3476

29. SDSS J232721.97+152437.3 z=0.0457 Not covered by FIRST

30. Objects that show extended radio emission, yet FIRST fails to identify multiple radio components SDSS J082439.00+405707.8 z=0.6125 SDSS J115324.47+493108.8 z=0.3339

31. SDSS J110538.99+020257.4 z=0.1066

32. 4DE1 and Radio Loudness • Compare 4DE1 domain occupation for RL, RI and RQ sources • Therefore RI same as RQ • RI can be??? 1) Radio brightest RQ quasars 2) Some boosted if they have jets 3) RL precursors

35. Conclusions • RL are either a distinct quasar population • Or part of our population B which also includes ~25% of the RQ quasars • RI are not a distinct class • Radio emission from the majority of RQ quasars is orders of magnitude weaker than the weakest RL source (and shows radio-FIR correlation).

36. Thanks

37. Netzer et al. 2007

38. Glikman et al. 2006

39. From vanden Berk et al. 2001, AJ, 122, 549 based on ~2200 SDSS spectra

44. Kaspi relation

45. Kellermann et al. 1989, AJ, 98, 1195 Boundary RL/RQ Stocke et al. 1992, ApJ, 396, 487 Balmaverde & Capetti 2006, A&A, 447, 97 Terashima & Wilson 2003, ApJ, 583, 145 Boundary RL/RQ Jester et al. 2005, AJ, 130, 873

46. White et al. 2007, ApJ, 654, 99