1 / 29

Local ULIRGs and Quasars

Real. Local ULIRGs and Quasars. S. Veilleux (U. Maryland). AGN activity Host Properties Environments Galactic Winds. Observed. Three Pagodas, Dali, China (8/15/05). Ground-based Optical Spectroscopy. log(L IR /L Sun ) < 11 11 – 11.99 12 – 12.29 12.3 – 12.8

temple
Download Presentation

Local ULIRGs and 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. Real Local ULIRGs and Quasars S. Veilleux (U. Maryland) • AGN activity • Host Properties • Environments • Galactic Winds Observed Three Pagodas, Dali, China (8/15/05)

  2. Ground-based Optical Spectroscopy log(LIR/LSun) < 11 11 – 11.99 12 – 12.29 12.3 – 12.8 Total = 29 68 77 31 (SV et al. 1995; Kim, SV, & Sanders 1998; SV, Kim, & Sanders 1999; also Kewley, Dopita et al.) • Fraction of Seyfert nuclei: • ~ 5 % @ log[LIR/LSun] = 10 – 11 • ~ 50% @ log[LIR/LSun] > 12.3

  3. Ground-based vs HST/STIS (Farrah, Surace, SV, Sanders, & Vacca 2005) Ground: H II S2 S2 H II HST: S2 S1 S2 mini-BALQSO

  4. F05189-2524 red F05189-2524 blue F05189-2524 UV Very Highly Ionized!

  5. Search for Obscured QSOs with CXO/XMM (Teng, Wilson, SV, Young, Sanders, & Nagar 2005) AGN ULIRGs L2 – 10 keV/LFIR • Trends with IRASf25/f60 color • Evidence for hidden QSOs in a few sources (also: Ptak et al. 2003; Franceschini et al. 2003) *burst “cool”f25/f60 “warm”

  6. NIR Spectroscopy (SV, Sanders, & Kim 1997, 1999) • NIR signatures of AGN in most Seyfert ULIRGs, but not in LINER or HII ULIRGs (also Goldader+95, Murphy+01a, Lutz+02, and spectropolarimetry…) • L(BLR) / L(BOL): most ULIRGs with BLR are AGN-dominated

  7. ISO Spectroscopy (Tran et al. 2001) • Excellent agreement between optical/NIR and ISO classifications(e.g., Genzel et al. 1998; Lutz et al. 1999; Rigopoulou et al. 1999; Lutz, SV, & Genzel 1999; Tran et al. 2001) AGN *burst

  8. QUEST:Quasar/ULIRG Evolutionary STudy • Medium-size Cycle-1 Spitzer program (95.3 hrs) • Maryland: S. Veilleux (PI), D.-C. Kim, D. Rupke, A. Baker • MPE: R. Genzel (co-PI), E. Sturm (Project Scientist), D. Lutz, …….. L. Tacconi, M. Lehnert, A. Contursi, K. Dasyra, M. Schweitzer • Hawaii: D. Sanders, J. Barnes, R. Joseph, A. Stockton, O. Guyon • IPAC: J. Mazzarella, S. Lord • Tel Aviv U.: H. Netzer,A. Sternberg • CWRU: C. Mihos

  9. QUEST:Quasar/ULIRG Evolutionary STudy • Sample: • 29 1-Jy ULIRGs + 25 PG QSOs • Z < 0.3 • This set of objects samples the full range of infrared luminosity and colors, merger state, and AGN/starburst fraction • SST Data • Infrared Spectrograph (IRS) • Low-resolution spectra: 5 – 14 m (SL2, SL1) • High-resolution spectra: 10 – 37 m (SH, LH) • High S/N

  10. QUEST:Quasar/ULIRG Evolutionary STudy • Ancillary Data • Optical & NIR ground-based imaging (Veilleux, Kim, Guyon, Sanders) • NIR HST/NICMOS imaging (PI: Veilleux) • NIR VLT spectroscopy (PI: Tacconi) • Evolutionary stage of the merger • Structure and dynamics of ULIRG progenitors • Structure and dynamics of ULIRG and QSO hosts • Locations of ULIRGs and QSOs in the fundamental plane of ellipticals • SST/IRS spectra of optically- and infrared-selected LINERs (PI: Sturm)

  11. Silicate Emissions in AGN: From LINERs to QSOs (Sturm et al. 2005; see also Hao et al. 2005; Siebenmorgen et al. 2005) • Signature of dust “obscuring torus” viewed face-on? • But: • Tdust ~ 200 K << T(torus walls) • Not all Type 1 objects show silicate emission features • QSOs vs LINERs: dust composition? Grain size? Crystallization? AGN *burst

  12. R K′ Hosts of Local ULIRGs • R and K´ images of 118 ULIRGs in 1-Jy sample (SV, Kim, & Sanders 2002) • Most of the 1-Jy sources are in the late stages of a merger • Remnants are often elliptical-like 1-Jy Sample

  13. Data n=1 n = 4 Deep HST H-band Imaging .27 1-Jy ULIRGs .  6 PG QSOs U U Q Q Low Surface Brightness Features (SV, Kim, Peng, Ho, et al. 2005) • Signs of mergers visible in all ULIRGs and PG QSOs • Large-scale stellar disks visible in some systems

  14. GALFIT Analysis: PSF + Sérsic component (SV, Kim, Peng, Ho, et al. 2005) n = 3.96 n = 1.0 n = 4.0

  15. Low Surface Brightness Disks in ULIRGs and PG QSOs • Bulge + Disk in 3 objects • Lobsided or tidally-shredded “disks” in possibly 5 additional objects Data Residuals Disk Bulge Data Residuals Disk Bulge (SV, et al. 2005) Data Residuals Disk Bulge

  16. Unsuspected Binaries (SV, et al. 2005) • M….

  17. Trends between Dominant Morphological Types, Spectral Types, and Infrared Colors (SV, et al. 2005) • M….

  18. Strength of tidal features (SV, et al. 2005) Tidal features are weaker among warm, AGN-like, early-type systems Strength of tidal features 

  19. Sizes and Magnitudes of ULIRG & PG QSO Hosts (SV, et al. 2005) <re> ~ 2.7 kpc <LH> ~ (1.5 ± 1) LH*

  20. Photometric Fundamental Plane ULIRG & PG QSOs: Intermediate-mass ( ~ 1-2 m*) elliptical / lenticular galaxies .(consistent with Genzel et al. 2001; Tacconi et al. 2002; Dasyra et al. 2005) (SV, et al. 2005)

  21. Environments of 1Jy ULIRGs (Zauderer, SV, & Yee 2005 in prep) ARC 3 • Bgc Cluster-Galaxy correlation amplitude (e.g., Longair & Seldner 1979; Yee & López-Cruz 1999) • <BGC> = 95 ± 16 Mpc1.77 • No obvious dependence on spectral type 2 1 0 * Starbursts ∙ LINERs ▲Seyfert 2s ∙ Seyfert 1s

  22. Environments of 1Jy ULIRGs (Zauderer, SV, & Yee 2005) • Red = 1Jy ULIRGs • Blue = RQ QSOs + RL QSOs + RGs (McLure & Dunlop 2001) (cf. Tacconi et al. 2002) 4 3 2 1 0

  23. Environments of 1Jy ULIRGs (Zauderer, SV, & Yee 2005) • Red = 1-Jy ULIRGs • Black = Seyferts (de Robertis et al. 1998)

  24. NGC 1482 [N II] / H Galactic Winds (SV, Cecil, & Bland-Hawthorn 2005, ARAA; astro-ph/0504435) Blueshifted Na ID absorption lines (78 starbursts) (SV & Rupke 2002) NGC 3079 HST + CXO % (Rupke, SV, & Sanders ‘02, ’05ab; also Martin 05) (Cecil, Bland-Hawthorn, & SV 2002)

  25. NGC 1482 [N II] / H Galactic Winds (SV, Cecil, & Bland-Hawthorn 2005, ARAA; astro-ph/0504435) Blueshifted Na ID absorption lines (78 starbursts) (SV & Rupke 2002) NGC 3079 HST + CXO (Rupke, SV, & Sanders ‘02, ’05ab) Na ID (Cecil, Bland-Hawthorn, & SV 2002)

  26. Neutral Winds in Nearby LIRGs 80% Starburst99 30% Starburst99 Starbursts Seyfert 2s Seyfert 1s Dwarfs (SM04) (Rupke, SV, & Sanders 2005abc) log (LIR) ~

  27. Neutral Winds in Nearby LIRGs 80% Starburst99 30% Starburst99 Starbursts Seyfert 2s Seyfert 1s Dwarfs (SM04) (Rupke, SV, & Sanders 2005abc) log (LIR) ~

  28. Summary • AGN activity is present (and often dominant) in: • > 30% of all local ULIRGs • >50% of local ULIRGs with log[LIR/Lsun] > 12.3 • Stay tuned for upcoming SST results… • Hosts: • Warm AGN-like systems have • prominent spheroids • weaker tidal features and stronger nuclei than cool LINER / HII systems • They are in the final phase of a merger • The luminosities, sizes, and stellar masses of PG QSO hostscoincidewith those of E-like 1-Jy ULIRGs • Environments: (preliminary) • 1-Jy ULIRGs live in low-density environments although there are exceptions • Good but not perfect overlap with environments of local Seyferts and QSOs • Galactic Winds: • Winds are present in virtually all ULIRGs • <Vout >, <dM/dt>, and <dE/dt> are very significant and probably affect evolution

  29. (SV, 08/15/05) Summary • AGN activity is present (and often dominant) in: • > 30% of all local ULIRGs • > 50% of local ULIRGs with log[LIR/Lsun] > 12.3 • Stay tuned for upcoming SST results… • Hosts: • Warm AGN-like systems have • prominent spheroids • weaker tidal features and stronger nuclei than cool LINER / HII systems • They are in the final phase of a merger • The luminosities, sizes, and stellar masses of PG QSO hostscoincidewith those of E-like 1-Jy ULIRGs • Environments: (preliminary) • 1-Jy ULIRGs live in low-density environments although there are exceptions • Good but not perfect overlap with environments of local Seyferts and QSOs • Galactic Winds: • Winds are present in virtually all ULIRGs • <Vout >, <dM/dt>, and <dE/dt> are very significant and probably affect evolution

More Related