What do we know about the evolution with redshift of dust ... · What do we know about the evolution with redshift of dust attenuation in galaxies? ! JWST@ROE,!Edinburgh,!july2016

What do we know about the evolution with redshift of dust attenuation in

galaxies?

JWST@ROE, Edinburgh, july 2016

Véronique Buat With the contribution of Barbara Lo Faro

LAM, Marseille, France

Madau & Dickinson, 2014

Wavelength

Selec-ve a.enua-on A(λ) measured with an a.enua-on curve A(λ)/AV or k(λ)/EB-‐V

To define the framework

F(λ)

λ1 λ2 JWST@ROE, Edinburgh, july 2016

Amount of a.enua-on In the UV (AUV) well constrained by dust (IR) emission IRX:LIR/LUV

emi@ed

observed

Outline

•  The a.enua-on law from the local to the distant universe:

  Formalisms and shapes of the laws  A@enuaLon laws for UV/opLcally selected galaxies  A@enuaLon laws for Dusty IR selected galaxies •  The measure of the amount of dust a.enua-on   Using the UV slope ß   Using opLcal/NIR colors   Using stellar masses


Outline


  Formalisms and shapes of the laws  A@enuaLon laws for UV/opLcally selected galaxies

 A@enuaLon laws for Dusty IR selected galaxies •  The measure of the amount of dust a.enua-on   Using ß, colors   Using stellar masses



The shapes of some popular a.enua-on/ex-nc-on curves

5000 10000 15000 20000wavelength

0

1

2

3

4

5

A=A

V

SMC

MW

LMC2

Charlot;Fall00(n = ¡0:7)

Calzetti + 00

Buat + 11

ExLncLon curves


Charlot & Fall 2000: power laws CalzeS and CalzeS modified laws

The formalisms of the attenuation laws currently used

€

k(λ) =A(λ)

E(B−V )+

Ebλ2γ 2

(λ2 − λ02 )+λ2γ 2

⎛

⎝ ⎜

⎞

⎠ ⎟

λλV

⎛

⎝ ⎜

⎞

⎠ ⎟

δ

δ=-‐0.13

nBC & nISM may be different and/or not fixed (Magphys code (da Cunha+08), , Wild+11 Chevallard+13…)

CalzeD+00, Cigale code (Noll+09), Buat+11,12 Kriek&Conroy13, Zeimann+15, Salmon+15… with or without faP

€

ˆ τ λBC = (1−µ) ˆ τ V (λ /λV )n

BC

ˆ τ λISM =µ ˆ τ V (λ /λV )n

ISM

€ €

(Calzetti+00 + UV bump) X power law

CIGALE code’s recipe (Noll+09) E(B-‐V)young for young stars E(B-‐V)old = faP E(B-‐V)young old stars

0<faP<1

€

ˆ τ λ (t) = ˆ τ λISM + ˆ τ λ

BC for t ≤107 yearsˆ τ λ (t) = ˆ τ λ

ISM for t >107 years


Charlot & Fall 2000 Double power law Solid lines

CalzeS+00 & modified Dashed lines

The formalisms of the a.enua-on laws currently used induce different shapes in the op-cal-‐NIR

δ=-‐0.13

Courtesy of Barbara Lo Faro

n= € €

nISM=nBC= n

Outline


  Formalisms and shapes of the laws  A@enuaLon laws for UV/opLcally selected galaxies  A@enuaLon laws for Dusty IR selected galaxies •  The measure of the amount of dust a.enua-on   Using ß, colors   Using stellar masses



Kriek & Conroy 13 Newfirm composite SEDs 0.5<z<2

C00

LMC

SMC

C00: Starburst law, Calzed.00

1<Z<2

Buat+11,12, Bump~LMC2, slightly steeper than C00

The variation of the attenuation curve in UV/optically (emission lines)

selected star-forming galaxies

‘Calzed modified’ formalism or method

AV

UV selected galaxies with IR detecLons

5000 10000 15000 20000wavelength

0

1

2

3

4

5

6

7

A/A

(V)

Calzetti+00Reddy+15, MOSDEF, Z~2SMCBattisti+16 Z ~0 ( Rv=4.05)

Calzed+94 method

E b

δ


Zeimann+15, emission line galaxies


Salmon+15, arXiv , CANDELS data, 1.5<z<3 galaxies detected in the UV rest-‐frame and with SPITZER

Tenta-ve conclusion?: A shallower a@enuaLon law for increasing a@enuaLon and mass(?) A@enuaLon laws which can be steeper than the Calzed one with a moderate bump

Outline



 A@enuaLon laws for Dusty IR selected galaxies •  The measure of the amount of dust a.enua-on   Using ß, colors   Using stellar masses



Herschel Extragalactic Legacy Project FP7/SPaCE P.I. Seb Oliver

A census of galaxy popula-ons and their star forma-on history from the local to the distant

universe

« UlLmate « source extracLon in all the cosmological Herschel fields (including HerMES and H-‐ATLAS surveys), UV to radio complementary data

photo-‐z, SFR, M* for all the sources


CalzeS& modified, Double Power law GRASIL cigale.lam.fr adlibitum.oats.inaf.it/silva/grasil/grasil.html

Physically-‐mo-vated SED modelling

UV-to-FIR SED fitting comparison with radiative transfer modelling

Lo Faro et al. to be submiPed

Radia-on transfer SED modelling

Z~1 LIRGs and Z~2 ULIRGs) (from Lo Faro+13,15) Nearby (U)LIRGs from the GOALS sample (Armus+09)


Grasil power law fixed power law free Calzed+00 Buat+11

nISM= -‐0.48 & nBC =-‐0.8


FlaPening of the aPenuaôn curve in high aPenuated objects  In agreement with Chevallard et al. 2013:

CompilaLon of RadiaLve Transfer modeling results, confirming GRASIL calculaLons All predict a grayer a@enuaLon for an increasing a@enuaLon

A larger amount of a.enua-on at longer wavelengths (NIR) than allowed by Calzed+00 a@. law. (Mitchell+13, Da Cunha+10)  Affects the determina-on of the stellar mass (Mitchell+13, Lo faro+13)

Calzed+00

How do these ``fla.er’’ a.enua-on curves affect the SED ?

a@enuaLon in NIR


nISM=nBC=-‐0.5

Outline



 A@enuaLon laws for Dusty IR selected galaxies •  The measure of the amount of dust a.enua-on   Using the UV slope ß   Using colors   Using stellar masses



GALEX+IRAS Cosmos field

Casey+14

0<Z<3.5 Z=0

Measuring dust attenuation without IR data : the slope of the UV continuum: β

Z=3

IRX-β : LBG selection at z~3 & stacking of Herschel data

Alvarez-‐Marquez et al. 2016


−2.0 −1.5 −1.0 −0.5 0.0 0.5

1

10

100

1000

−2.0 −1.5 −1.0 −0.5 0.0 0.5UV slope, b

1

10

100

1000

L IR/L

FU

V0.5

2.1

4.5

6.9

AF

UV

IRX−bUV relation (This work)Meurer+1999Takeuchi+2012

M*−bUV stack 1 (This work)M*−bUV stack 2 (This work)PACS−LBGs (Oteo+2013)


The IRX-β plot is very sensitive to the shape of the attenuation curve in the UV

ULIRGs at z~2 detected by Herschel: a fla@er curve in the UV

Lo Faro et al. To be submiPed, see also Salmon+15, Safarzadeh+16

nISM

Outline



 A@enuaLon laws for Dusty IR selected galaxies •  The measure of the amount of dust a.enua-on   Using the UV slope ß   Using rest-‐frame NIR opLcal colors   Using stellar masses



Arnouts+13 NUV-‐R, R-‐K colors Forrest+13, U-‐V, V-‐J colors

Using rest-frame colors to infer dust attenuation corrections

0<z<1 1<z<3

Needs to be calibrated to be used at higher/different redshits


Attenuation-stellar mass relation on a large range of z UV selected and star forming galaxies (Stacking of Spitzer/Herschel data)

Z=1.5, 3, 4

Heinis+14, UV rest frame selecôn

Whitaker+14, CANDELS , UVJ selecôn, MIPS stacking

See also Oteo+14, Panella+15, Dunlop+16….

Dust a@enuaLon in IR and UV selected samples: a difference in stellar mass

0 0:2 0:4 0:6 0:8 1:0 1:2 1:4 1:6 1:8 2:0redshift

0

1

2

3

4

5

AU

V(m

ag)

Fiducial

att¡ curve : Calzetti

att¡ curve : SMC

Burgarella + 13¡ ¯t

Burgarella + 13¡ data

Cucciati + 12

Heinis + 14

Heinis + 14(Mstar ' 1010:9M¯)

Ibar + 13

Ibar + 13(Mstar ' 1010:9M¯)

Reddy + 08

Buat + 07

Choi + 06

Oi + 15

Bernhard + 14

Buat+15

IR selected samples: IRAS/Spitzer/AKARI

UV rest-‐frame selecLons

IRX-‐M* relaLon assumed, Bernhard+14



At higher redshij: ALMA observa-ons Either an evolu-on of the IRX-‐M* rela-on or an increase of T(dust) with z

HUDF-‐ASPECS, Bouwens+16 arXiv


An evoluLon of the IRX-‐M* relaLon is needed to understand the variaLon of IR to UV luminosity density raLo

Burgarella et al. in prep

Burgarella+13

To conclude

  Confirma-on of the varia-on of the a.enua-on curve among galaxies: shape in UV/NIR, UV bump: as a funcLon of the amount of a@enuaLon, stellar mass, sSFR… sample selecLon)

  Fortunately, some recipes seem reliable to measure the total amount of a.enua-on: colors, stellar mass, but need to be well calibrated, at different redshits

  The IRX-‐ß diagnosLc is very sensiLve to the a@enuaLon curve and very likely to the stellar mass of galaxies


WiP & Gordon 00

(IRX)

Documents

What do we know about the evolution with redshift of dust ... · What do we know about the evolution with redshift of dust attenuation in galaxies? ! JWST@ROE,!Edinburgh,!july2016