desika narayanan evla conference the formation and evolution of smgs: a (mostly) panchromatic view...

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

Desika Narayanan EVLA Conference

Discovery History

Barger et al., Hughes et al.

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)

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

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

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?)

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

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)

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?

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--->

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

Desika Narayanan EVLA Conference

Narayanan et al. 2008

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)

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

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

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.

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

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?

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

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

Desika Narayanan EVLA Conference

The MBH-M* Relation in SMGs and Quasars: Observed

SMGs

Alexander et al.

Quasars

Shileds et al.

Desika Narayanan EVLA Conference

The MBH-M* Relation in SMGs and Quasars: Modeled

Time

Desika Narayanan EVLA Conference

The Trip Toward the Magorrian Relation: SMGs

Observations (Alexander

et al.)

Models

(DN, Hayward, Cox, Younger et al.)

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

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)

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)

Desika Narayanan EVLA Conference

Potential Contribution from the eVLA: Morphologies of SMGs(does our merger-driven scenario work in real life?)

Sub-mm flux

Desika Narayanan EVLA Conference

Contribution from the EVLA: True Line Width Distribution of QSOs

Sub-mm flux

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

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

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