Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Counts Of Submillimeter Galaxies At

High Redshift With Variable IMF

Alejandra MunozProf. Nelson Padilla

June 25, 2009

Cosmology Project 2009Departamento de Astronomıa y Astrofısica

Facultad de FısicaPontificia Universidad Catolica de Chile

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Outline

Initial Mass Function

Submillimeter Galaxies

The Model With Variable IMF

Results

Conclusions And Future Work

References

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Outline

Initial Mass Function

Submillimeter Galaxies

The Model With Variable IMF

Results

Conclusions And Future Work

References

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

IMF ξ(m)

I Specifies the relative number of stars formed at each mass

I ξ(m)dm: number of stars that have been born with masses betweenm and m + dm

ξ(m) ∝ m−(α+1)

0.01

0.1

1

10

1 10

ξ(m

/M⊙

)

m/M⊙

SalpeterKennicutt

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

I Dwarf dominated (steeper) or remnant dominated (top-heavy)I (α + 1) = 2.35: SalpeterI (α + 1) = 0.4 (m < 1M¯), (α + 1) = 1.5 (m > 1M¯): Kennicutt

I Galaxy properties that depend on the IMF:I Star formation rate (SFR)I Feedback and metal enrichmentI Rate of luminosity evolution of a simple stellar population (SSP)

IMF dictates the evolution and fate of galaxies and star clusters!!!

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Outline

Initial Mass Function

Submillimeter Galaxies

The Model With Variable IMF

Results

Conclusions And Future Work

References

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

SMGs

I SCUBA: emission at 850[µm]I Dust-enshrouded starburstsI SFR=659[M¯yr−1]I M=3.5·1011M¯I z ≈ 4− 2

I Source of emission: dustreprocessed emission fromyoung stars, active galacticnuclei (AGN)

Figure: A source of submillimeter radiation, available athttp://www.astronomy.com/asy/objects/images/brightgalaxy 900.jpg

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

An Important Question

Contribution of SMGs to cosmic stellar mass assembly?Counts of submillimeter sources!!!

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

A Previous Work In This Spirit

I Baugh et al. (2005): a modelthat predicts the abundance ofSMGs in the ΛCDMcosmology

I GRASIL codeI Silva et al. (1998)I Uses predicted star

formation and metalenrichment histories

I Output: galaxy spectralenergy distributions (SED)

I A top-heavy IMF in bursts

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Outline

Initial Mass Function

Submillimeter Galaxies

The Model With Variable IMF

Results

Conclusions And Future Work

References

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Where And How

I Lagos et al. (2008)I Semy-analytic model of galaxy formationI Processes of gas cooling, star formation, feedback from core-collapse

supernovae (SNe CC) explosions and AGN, galaxy mergers, chemicalenrichment of baryons

I Salpeter IMF

I NewI Weidner & Kroupa (2006)I Set of 6 values of α: 1.40 to 2.10, step 0.14I A corresponding SFR and ηCC (number of SNe CC per solar mass)

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Outline

Initial Mass Function

Submillimeter Galaxies

The Model With Variable IMF

Results

Conclusions And Future Work

References

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Luminosity Functions (LF), Stellar Mass Function (SMF)

-26 -24 -22 -20 -18 -16 -14Mbj - 5log10(h)

10-5

10-4

10-3

10-2

10-1

φ [h

3 /Mpc

3 /mag

] Norberg (2002)

-30 -28 -26 -24 -22 -20 -18MK - 5log10(h)

10-5

10-4

10-3

10-2

10-1

φ [h

3 /Mpc

3 /mag

]

Cole (2001)

Huang (2003)

10-6

10-5

10-4

10-3

10-2

10-1

100

dN/d

log 1

0 M

Ste

llar [

h3 /Mpc

3 dex

-1]

z=4.5

z=2

Drory et al. (2005)

8 9 10 11 12 13log10(MStellar [h

-2 Mo])

10-6

10-5

10-4

10-3

10-2

10-1

100

dN/d

log 1

0 M

Ste

llar [

h3 /Mpc

3 dex

-1]

z=1

8 9 10 11 12 13log10(MStellar [h

-2 Mo])

z=0.5

Drory et al. (2004)

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Mean IMF And Weighted Mean IMF

〈IMF〉 =P

i IMF(gi )Pi gi

〈IMF〉w =P

i 10−MbJ

(gi )IMF(gi )Pi 10

−MbJ(gi )

Requires further revision...

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Outline

Initial Mass Function

Submillimeter Galaxies

The Model With Variable IMF

Results

Conclusions And Future Work

References

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

I Small changes in the galaxy LFs in the bJ and K bands, and in theSMF at several redshifts

I At high redshifs both mean values of IMF tend to decrease

Still there are situations interesting to analyze...

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Dust And Neighbors

I Connect this model with GRASIL: review implementation of F.Navarrete (2007)

I Number of neighbors a galaxy has within a beam: may change theshape of the predicted counts

I N = nR

cone(1 + Γ(s ′))d3s ′ = 2πn

R r/d

0sin(θ)dθ

R r

0(1 + Γ(s, θ, φ))s2ds

I Γ(r) = (r/r0)−γ two-point correlation function

I γ ' 1.8, r0 ' 5.4h−1 [Mpc]

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

The Challenge

Nature of SMGs is still largely unknown... Decoding their star formationhistories and sources of emission may allow us to learn about our

Universe when this was less than 20% of its current age!!!

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Outline

Initial Mass Function

Submillimeter Galaxies

The Model With Variable IMF

Results

Conclusions And Future Work

References

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

I L. S. Sparke & J. S. Gallagher, Galaxies in the Universe: AnIntroduction, Cambridge University Press, Cambridge, UK (2007).

I P. Schneider, Extragalactic Astronomy and Cosmology, Springer(2006).

I A. Renzini, arXiv:astro-ph/0410295v2.

I C. M. Baugh et al., Mon. Not. R. Astron. Soc. 356 (2005), 1191.

I M. J. Michalowski et al., arXiv:astro-ph.CO/0905.4499v1.

I L. Silva et al., Astrophys. J. 509 (1998) 103.

I G. L. Granato et al., Astrophys. & Space Science 276 (2001), 973.

I C. Weidner & P. Kroupa, Mon. Not. R. Astron. Soc. 365 (2006),1333.

I P. Kroupa, arXiv:astro-ph/0201098v1.

I C. Lagos et al., Mon. Not. R. Astron. Soc. 388 (2008), 587.

I F. Navarrete, Bachelor Practice Report (2007).

I V. J. Martınez & E. Saar, arXiv:astro-ph/0203251v1.

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF

Initial Mass Function Submillimeter Galaxies The Model With Variable IMF Results Conclusions And Future Work References

Thanks.

Figure: Artistic image of a cluster of ”monster galaxies”, available athttp://www.nao.ac.jp/E/Outreach/pr-rl/2009/img/topics090507big.jpg

Alejandra Munoz Prof. Nelson Padilla

Counts Of Submillimeter Galaxies At High Redshift With Variable IMF