local ulirgs and quasars
DESCRIPTION
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 - PowerPoint PPT PresentationTRANSCRIPT
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Local ULIRGs and QuasarsS. Veilleux (U. Maryland)
AGN activity
Host Properties
Environments
Galactic Winds
Three Pagodas, Dali, China (8/15/05)
Real
Observed
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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
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Ground-based vs HST/STIS
(Farrah, Surace, SV, Sanders, & Vacca 2005)
Ground: H II S2 S2 H II
HST: S2 S1 S2 mini-BALQSO
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F05189-2524 red
Very
Highly
Ionized!
F05189-2524 blueF05189-2524 UV
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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
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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)
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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)
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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
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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
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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)
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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?
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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
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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
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GALFIT Analysis: PSF + Sérsic component(SV, Kim, Peng, Ho, et al. 2005)
n = 3.96 n = 1.0 n = 4.0
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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
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Unsuspected Binaries
M….
(SV, et al. 2005)
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Trends between Dominant Morphological Types, Spectral Types, and Infrared Colors
M….
(SV, et al. 2005)
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Strength of tidal features
Strength of tidal features
Tidal features are weaker among warm, AGN-like, early-type systems
(SV, et al. 2005)
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Sizes and Magnitudes of ULIRG & PG QSO Hosts
<re> ~ 2.7 kpc <LH> ~ (1.5 ± 1) LH*
(SV, et al. 2005)
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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)
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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
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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
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Environments of 1Jy ULIRGs
Red = 1-Jy ULIRGs
Black = Seyferts
(de Robertis et al. 1998)
(Zauderer, SV, & Yee 2005)
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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)
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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
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Neutral Winds in Nearby LIRGs
log (LIR) ~
Starbursts Seyfert 2s Seyfert 1s Dwarfs (SM04)
(Rupke, SV, & Sanders 2005abc)
80% Starburst
99
30% Starburst
99
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Neutral Winds in Nearby LIRGs
log (LIR) ~
StarburstsSeyfert 2sSeyfert 1sDwarfs (SM04)
(Rupke, SV, & Sanders 2005abc)
80% Starburst99
30% Starburst99
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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
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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)