Local ULIRGs and QuasarsS. Veilleux (U. Maryland)

AGN activity

Host Properties

Environments

Galactic Winds

Three Pagodas, Dali, China (8/15/05)

Real

Observed

Ground-based Optical Spectroscopy

Fraction of Seyfert nuclei:

• ~ 5 % @ log[LIR/LSun] = 10 – 11

• ~ 50% @ log[LIR/LSun] > 12.3

(SV et al. 1995; Kim, SV, & Sanders 1998; SV, Kim, & Sanders 1999; also Kewley, Dopita et al.)

log(LIR/LSun) < 11 11 – 11.99 12 – 12.29 12.3 – 12.8

Total = 29 68 77 31

Ground-based vs HST/STIS

(Farrah, Surace, SV, Sanders, & Vacca 2005)

Ground: H II S2 S2 H II

HST: S2 S1 S2 mini-BALQSO

F05189-2524 red

Very

Highly

Ionized!

F05189-2524 blueF05189-2524 UV

Search for Obscured QSOs with CXO/XMM

Trends with IRAS f25/f60 color

Evidence for hidden QSOs in a few sources

(also: Ptak et al. 2003; Franceschini et al. 2003)

(Teng, Wilson, SV, Young, Sanders, & Nagar 2005)

“cool” f25/f60 “warm”

L

2 –

10 k

eV/L

FIR

*burst

AGN

ULIRGs

NIR Spectroscopy

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

(SV, Sanders, & Kim 1997, 1999)

ISO Spectroscopy

(Tran et al. 2001)

AG

N

*

burs

t

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)

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

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

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)

Silicate Emissions in AGN: From LINERs to QSOs

(Sturm et al. 2005; see also Hao et al. 2005; Siebenmorgen et al. 2005)

AG

N

*

burs

t

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?

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

R K′

1-Jy Sample

Low Surface Brightness Features

Signs of mergers visible in all ULIRGs and PG QSOs

Large-scale stellar disks visible in some systems

(SV, Kim, Peng, Ho, et al. 2005)

Data n=1 n = 4

U

U

Q

Q

Deep HST H-band Imaging

. 27 1-Jy ULIRGs . 6 PG QSOs

GALFIT Analysis: PSF + Sérsic component(SV, Kim, Peng, Ho, et al. 2005)

n = 3.96 n = 1.0 n = 4.0

Low Surface Brightness Disks in ULIRGs and PG QSOs

Bulge + Disk in 3 objects

Lobsided or tidally-shredded “disks” in possibly 5 additional objects

(SV, et al. 2005)

Data Residuals Disk Bulge

Data Residuals Disk Bulge

Data Residuals Disk Bulge

Unsuspected Binaries

M….

(SV, et al. 2005)

Trends between Dominant Morphological Types, Spectral Types, and Infrared Colors

M….

(SV, et al. 2005)

Strength of tidal features

Strength of tidal features

Tidal features are weaker among warm, AGN-like, early-type systems

(SV, et al. 2005)

Sizes and Magnitudes of ULIRG & PG QSO Hosts

<re> ~ 2.7 kpc <LH> ~ (1.5 ± 1) LH*

(SV, et al. 2005)

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)

Environments of 1Jy ULIRGs

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

(Zauderer, SV, & Yee 2005 in prep)

0

1

2

ARC 3

* Starbursts

∙ LINERs

▲ Seyfert 2s

∙ Seyfert 1s

Environments of 1Jy ULIRGs

Red = 1Jy ULIRGs Blue = RQ QSOs + RL

QSOs + RGs (McLure & Dunlop 2001)

(cf. Tacconi et al. 2002)

(Zauderer, SV, & Yee 2005)

0

1

2

4

3

Environments of 1Jy ULIRGs

Red = 1-Jy ULIRGs

Black = Seyferts

(de Robertis et al. 1998)

(Zauderer, SV, & Yee 2005)

Galactic Winds

(Rupke, SV, & Sanders ‘02, ’05ab; also Martin 05)

NGC 3079 HST + CXO

%

NGC 1482 [N II] / H

(Cecil, Bland-Hawthorn, & SV 2002)

(SV & Rupke 2002)

Blueshifted Na ID absorption lines (78 starbursts)

(SV, Cecil, & Bland-Hawthorn 2005, ARAA; astro-ph/0504435)

Galactic Winds

(Rupke, SV, & Sanders ‘02, ’05ab)

NGC 3079 HST + CXO

NGC 1482 [N II] / H

(Cecil, Bland-Hawthorn, & SV 2002)

(SV & Rupke 2002)

Blueshifted Na ID absorption lines (78 starbursts)

(SV, Cecil, & Bland-Hawthorn 2005, ARAA; astro-ph/0504435)

Na ID

Neutral Winds in Nearby LIRGs

log (LIR) ~

Starbursts Seyfert 2s Seyfert 1s Dwarfs (SM04)

(Rupke, SV, & Sanders 2005abc)

80% Starburst

99

30% Starburst

99

Neutral Winds in Nearby LIRGs

log (LIR) ~

StarburstsSeyfert 2sSeyfert 1sDwarfs (SM04)

(Rupke, SV, & Sanders 2005abc)

80% Starburst99

30% Starburst99

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 hosts coincide with 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

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 haveprominent spheroidsweaker 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 hosts coincide with 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

(SV, 08/15/05)