desika narayanan evla conference the formation and evolution of smgs: a (mostly) panchromatic view...
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![Page 1: Desika Narayanan EVLA Conference The Formation and Evolution of SMGs: A (mostly) Panchromatic View Desika Narayanan Harvard-Smithsonian Center for Astrophysics](https://reader035.vdocuments.us/reader035/viewer/2022062421/56649ccf5503460f9499abc7/html5/thumbnails/1.jpg)
Desika Narayanan EVLA Conference
The Formation and Evolution of SMGs:A (mostly) Panchromatic View
Desika Narayanan Harvard-Smithsonian Center for Astrophysics
The Team:
T.J. CoxLars HernquistPatrik Jonsson
Chris HaywardJosh Younger
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Desika Narayanan EVLA Conference
Discovery History
Barger et al., Hughes et al.
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Desika Narayanan EVLA Conference
The Incredible Fluxes of SMGs:
• Median Redshift z~2.4 (Chapman et al 2004)
• Selected at S850 > 5 mJy, seen up to S850 ~ 20 mJy
z~2.4~mJy source
(NED; Benford 1999)
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Desika Narayanan EVLA Conference
Where We’re at with SMGs:
• Median Redshift z~2.4 (peak of cosmic BH and SFR activity)
Chapman et al 2004 - though see recent z>4 detections by J. Younger et al.
• LIR > 1013 L
• SFR ~ 1000-3000 M/yr
• Huge Masses:– DM: 5x1012 M (Blain et al. 2004) – H2: Gas rich ~1010 M(Greve et al., Tacconi et al.)
– Stellar: ~1011 M (Swinbank et al., Lonsdale et al.)
Similar to z~2 QSOs
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Desika Narayanan EVLA Conference
Where We’re at with SMGs:
• Median Redshift z~2.4 (Chapman et al 2004)
• Selected at S850 > 5 mJy, seen up to S850 ~ 20 mJy
• Huge Masses:– DM: 5x1012 M (Blain et al. 2004) – H2: Gas rich ~1010 M(Greve et al., Tacconi et al.)
– Stellar: ~1011 M (Swinbank et al., Lonsdale et al.)
– SFR~ 2000 M/yr
SMGs are the most luminous,
heavily star forming galaxies at
the epoch of peak galaxy
formation
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Desika Narayanan EVLA Conference
The Theoretical Challenge (how do we catch up to the observers?):
• What is a physical model for SMGs (how do we form them)?
• How do they fit in an evolutionary scenario for hierarchical galaxy formation? (aka, how do we connect
them to quasars?)
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Desika Narayanan EVLA Conference
Clues for the Modelers: Physical Parameters
Merger? Disks?
+
massive galaxies (~few x 1011 M in stars)
= 5-20 mJy SMGs?
Lonsdale et al. 2008
Tacconi et al. 2008
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Desika Narayanan EVLA Conference
Clues for the Modelers:
• Huge CO Line Widths:
(800 km/s : (maybe) ~ twice z~2 QSOs) (Greve et al. 2004, Carilli & Wang 2006)
•Off MBH-M* Relation?(Alexander et al. 2008)
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Desika Narayanan EVLA Conference
The Theoretical Challenge (how do we catch up to the observers?):
• What is a physical model for SMGs (how do we form them)?
• How do they fit in an evolutionary scenario for hierarchical galaxy formation?
![Page 10: Desika Narayanan EVLA Conference The Formation and Evolution of SMGs: A (mostly) Panchromatic View Desika Narayanan Harvard-Smithsonian Center for Astrophysics](https://reader035.vdocuments.us/reader035/viewer/2022062421/56649ccf5503460f9499abc7/html5/thumbnails/10.jpg)
Desika Narayanan EVLA Conference
The Theoretical Challenge: Forming SMGs
• What is a physical model for SMGs (how do we form them)?
SAMs:Flat IMF: dn/dln(m) ~ m
(Baugh et al. 2004, Swinbank et al. 2008)
Numerical Models:Merger models, diffuse ISM
(Chakrabarti et al. 2006)
S850--->
S85
0---
>Time--->
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Desika Narayanan EVLA Conference
GADGET (SPH) + SUNRISE (IR)+ Turtlebeach (Molecular Line)
Physics Included in Hydrodynamics:-Full numerics: DM, Gas, Stars and BHs-Multi-phase McKee-Ostriker ISM-Star formation follows KS relations-BH growth and associated AGN feedback-Supernovae pressurization of ISM
-Virial Properties of Galaxy disks scaled to z~3-Mergers and Isolated disks simulated-Halo Masses: 1-5 x 1012 M
Go to http://www.cfa.harvard.edu/~dnarayan/Movies/ for the movies in the presentation
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Desika Narayanan EVLA Conference
Narayanan et al. 2008
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Desika Narayanan EVLA Conference
GADGET (SPH) + SUNRISE (IR) + Turtlebeach (Molecular Line)
GMC
Diffuse ISM
Physics Included in Monte Carlo IR RT:-IR transfer of stellar and AGN spectrum(starburst 99 for stars and Hopkins+ 07 for AGN)
-dust radiative equilibrium
-Kroupa IMF, MW Dust to Metals (0.4)
-Stellar Clusters surrounded by placental GMCs (covering fraction is free parameter; fcover=0.3-1 measured in ULIRGs)
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Desika Narayanan EVLA Conference
GADGET (SPH) + SUNRISE (IR) + Turtlebeach (Molecular Line)
Narayanan et al. (2008)
Physics Included in Monte Carlo CO RT
-Mass spectrum of GMCs included as SISs
-Molecular statistical equilibrium (collisions and radiation)
-Pressure-driven H2 formation/destruction (Blitz & Rosolowsky 2006)
-Milky Way Abundances for CO
coco
co
co
co
co
co
co
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Desika Narayanan EVLA Conference
SMGs are Major Mergers at z~2
Narayanan, Hayward, Cox et al. in prep.Narayanan, Hayward, Cox, Younger et al. submitted
Opacity dominated by
birth clouds during
starburst
Opacity dominated by
diffuse dust during inspiral
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Desika Narayanan EVLA Conference
SMGs are Major Mergers at z~2
Narayanan, Hayward, Cox et al. in prep.Narayanan, Hayward, Cox, Younger et al. submitted.
Opacity dominated by
birth clouds during
starburst
Opacity dominated by
diffuse dust during inspiral
1. Low luminosity (~5 mJy) SMGs are smaller scale (~100-200 M/yr)starbursts.
2. The most luminous (~20 mJy) SMGs are “maximal” high mass starbursts duringfinal coalesence.
3. Individual Spirals will have trouble reproducing anything except very low luminosity SMGs.
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Desika Narayanan EVLA Conference
Model SED at z=2: Matching Observations
Pope et al. (2006) Kovacs et al. (2006)
Narayanan, Hayward, Cox, Younger et al. submitted
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Desika Narayanan EVLA Conference
The Theoretical Challenge:
• What is a physical model for SMGs (how do we form them)?
• How do they fit in an evolutionary scenario for hierarchical galaxy formation? Are SMGs and quasars related?
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Desika Narayanan EVLA Conference
The life of an SMG: Sub-mm, CO and B-band evolution
Narayanan, Hayward, Cox et al. in prep.
√2
Coppin et al. 2008
virial
= 225 km/s * 2.354 =
530 km/s FWHM
Sub-mm Flux
B-band Flux
Narayanan, Cox, Hayward, Younger et al. in prep.
escape
~ 225 km/s * 2.354 * √2 =
750 km/s FWHM
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Desika Narayanan EVLA Conference
The Connection between SMGs and QSOs
Narayanan, Hayward, Cox et al. in prep.
Sub-mm Flux
B-band Flux
Time Scale between
peak SMG phase and
peak QSO phase: ~50 Myr -
though note tons of overlap
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Desika Narayanan EVLA Conference
The MBH-M* Relation in SMGs and Quasars: Observed
SMGs
Alexander et al.
Quasars
Shileds et al.
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Desika Narayanan EVLA Conference
The MBH-M* Relation in SMGs and Quasars: Modeled
Time
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Desika Narayanan EVLA Conference
The Trip Toward the Magorrian Relation: SMGs
Observations (Alexander
et al.)
Models
(DN, Hayward, Cox, Younger et al.)
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Desika Narayanan EVLA Conference
Are High-z QSOs on the MBH-M* relation ?
Quasars at z~2
Shields et al. 2006
Quasars at z~6
Walter, Carilli et al.
~120 km/s
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Desika Narayanan EVLA Conference
CO FWHM-QSO Luminosity Relation
Optically Luminous LOSs have small CO FWHMs because of molecular disk formation
Narayanan, Li et al. (2008)
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Desika Narayanan EVLA Conference
Line widths of lower luminosity z~6 quasars Are observed to be broader (~600 km/s), consistent with large halo mases
Carilli et al. (2007)Maiolino et al. (2007)
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Desika Narayanan EVLA Conference
Potential Contribution from the eVLA: Morphologies of SMGs(does our merger-driven scenario work in real life?)
Sub-mm flux
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Desika Narayanan EVLA Conference
Contribution from the EVLA: True Line Width Distribution of QSOs
Sub-mm flux
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Desika Narayanan EVLA Conference
Conclusions• Merger-driven model can reproduce S850 5-20 mJy using only
observationally motivated physical parameters
• Sub-mm duty cycles, SEDs, CO fluxes and line widths naturally reproduced in a merger-driven model
• SMGs evolve naturally into QSOs and then onto Magorrian Relation
• Quasars may be selected to have face-on molecular disks
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Desika Narayanan EVLA Conference
QSOs may have preferentially face-on disks
Narayanan, Hayward, Cox et al. in prep.
Sub-mm Flux
Coppin et al. 2008
Narayanan et al. 2008
QSOs
SMGs
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Desika Narayanan EVLA Conference
GADGET (SPH) + SUNRISE (IR) + Turtlebeach (Molecular Line)
GMC
Diffuse ISM
Physics Included in Monte Carlo IR RT:-IR transfer of stellar and AGN spectrum(starburst 99 for stars and Hopkins+ 07 for AGN)
-dust radiative equilibrium
-Kroupa iMF, MW Dust to Gas
-Stellar Clusters surrounded by placental GMCs (covering fraction is free parameter)
z = 2.5 SED input