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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
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
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
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
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)
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)