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


Discovery History

Barger et al., Hughes et al.


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)


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


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


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?)


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


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)


The Theoretical Challenge (how do we catch up to the observers?):


• How do they fit in an evolutionary scenario for hierarchical galaxy formation?


The Theoretical Challenge: Forming SMGs


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--->


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

http://www.cfa.harvard.edu/~dnarayan/


Narayanan et al. 2008


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)



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


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


diffuse dust during inspiral


SMGs are Major Mergers at z~2

Narayanan, Hayward, Cox et al. in prep.Narayanan, Hayward, Cox, Younger et al. submitted.


birth clouds during

starburst


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.


Model SED at z=2: Matching Observations

Pope et al. (2006) Kovacs et al. (2006)

Narayanan, Hayward, Cox, Younger et al. submitted


The Theoretical Challenge:


• How do they fit in an evolutionary scenario for hierarchical galaxy formation? Are SMGs and quasars related?


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


The Connection between SMGs and QSOs


Sub-mm Flux

B-band Flux

Time Scale between

peak SMG phase and

peak QSO phase: ~50 Myr -

though note tons of overlap


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

SMGs

Alexander et al.

Quasars

Shileds et al.


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

Time


The Trip Toward the Magorrian Relation: SMGs

Observations (Alexander

et al.)

Models

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


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


CO FWHM-QSO Luminosity Relation

Optically Luminous LOSs have small CO FWHMs because of molecular disk formation

Narayanan, Li et al. (2008)


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)


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

Sub-mm flux


Contribution from the EVLA: True Line Width Distribution of QSOs

Sub-mm flux


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


QSOs may have preferentially face-on disks


Sub-mm Flux

Coppin et al. 2008

Narayanan et al. 2008

QSOs

SMGs



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

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

Documents

mjy smgs

qsos slide

yr smgs

evolution of smgs

median redshift z

incredible fluxes of

mjy huge masses

hierarchical galaxy