Whichdustattenuationcurve(s) for star forminggalaxies? · Véronique Buat 1 David Corre1, Médéric Boquien2, KasiaMalek3,1 & the HELP/Herschel team 1 LAM, Aix-Marseille Université,

Which dust attenuation curve(s)forstarforming galaxies?

VéroniqueBuat1DavidCorre1,MédéricBoquien2,Kasia Malek3,1

&theHELP/Herschelteam1LAM,Aix-MarseilleUniversité,France

2 CITEVA,Universidad ofAntofagasta,Chile3NCNR,Warzawa,Poland

DustingtheUniverse,Tucson,2019

Dusting theUniverse,Tucson,2019

Theshape oftheattenuation law is found tovary atlow andhighz,fromdataandsimulations….only fewexamples

From numerical simulationsNarayanan+18Cousin+19Z=0,SDSS,Salim+18

ULIRGs atz=2LoFaro+171.5

Thederived quantities SFR&Mstar aremodified


Theios +19SMC(UVsteep)andCalzetti (UVflat)curves

(nodust emission)

Maleketal.2018,HELPprojectCharlot&Fall recipe (NIRflat)andCalzetti (NIRsteep)attenuation lawsLoFaroetal.2017Very flatattenuation curves forULIRGs atz=2

9.0 9.5 10.0 10.5 11.0 11.5 12.0log(Mstar) [M�]

0.0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

Nor

mal

ized

coun

ts

CF00

Calzetti2000

LoFaro2017

Charlot&Fall 00recipe

Outline of the talk

• Formalisms fortheattenuation laws &flexiblerecipes• Thestudy ofaHerschel+3D-HSTsample intheCOSMOSfield• Extinction/attenuation:galaxieshosting Gamma-raysbursts (GRBHs)

**Comparison with RadiationTransfermodeling**


𝐴"#$ = 𝐴$ 𝜆 0.55+

,-.

𝐴"/01 = 𝐴&/01 𝜆 0.55+

,234

Charlot&Fall 2000(CF00)à freeISMslope

Calzetti+2000(C00)à freeslope

Themost usual formalisms fortheattenuation laws &flexiblerecipes

(daCunha+08,,Wild+11,Chevallard+13,LoFaro+17,Malek+18)

(Buat+11,12,Kriek&Conroy 13,Salmon+15,Zeimann+15,Seon &Draine2016,Corre+18,Wang+18)

nosingleattenuation lawage dependent attenuation forstars

t~107 yrs (BC),

CF00:nBC=nISM=-0.7,µ=0.3

Asingleattenuation law forallthestellar continuumMWextinction+screen fornebular lines

C00:δ =0,EBV-factor=0.44

EBV-factor=E(B-V)star/E(B-V)lines


𝑘 𝜆 = 𝐴(𝜆)

𝐸(𝐵 − 𝑉) ×

𝜆𝜆&

>

𝜇 = 𝐴&/01 𝐴&/01 + 𝐴$+

• OriginalCF00recipe fortheISM:𝜆-0.7 ,Rv ~5.8

• Calzetti lawRV=4.05

0:2 0:3 0:4 0:5 1 2

wavelength[¹m]

0:05

0:1

0:2

0:5

1

2

5A

(¸)=

A(V

)

C00¡ ± = 0Calz¡mod¡ ± = ¡0:6Calz¡mod¡ ± = 0:2CF00¡ slope = ¡0:7CF¡ ISMfree¡ slope = ¡1:1CF¡ ISMfree¡ slope = ¡0:5

TheCalzetti law is steeper than theCharlot&Fall recipe at𝜆> 𝜆V


LoFaro+17,Buat+18

100 101 102 103

� [µm]

0.0

0.2

0.4

0.6

0.8

1.0

tran

smis

sion

GALEX NUV

CFHT MegaCam u

Subaru suprime B

Subaru suprime V

Subaru suprime r

Subaru suprime i

Subaru suprime z

Subaru suprime y

UKIRT WFCam J

CFHT wircam H

VISTA vircam Ks

Spitzer IRAC 3.6

Spitzer IRAC 4.5

Spitzer IRAC 5.8

Spitzer IRAC 8.0

Spitzer MIPS 24

Herchel PACS 100

Herchel PACS 160

Herchel SPIRE 250

Herchel SPIRE 350

Herchel SPIRE 500

21photometric bands+Hαfluxes


THECOSMOS3DHSTandHerschelsample

+Hα+[NII]fluxes

1e¡ 20 1e¡ 19 1e¡ 18FH®(3D¡ HST)[Wm¡2]

1e¡ 20

2e¡ 20

5e¡ 20

1e¡ 19

2e¡ 19

5e¡ 19

1e¡ 18

2e¡ 18

FH®(¯

ts)[

Wm¡

2]

Buat+18,A&A,619,A135

33SEDs,fits with CIGALEPhotometry

+Emissionlines (Cloudy)Boquien+19

NUV submm

0.6

0 0:2 0:4 0:6 0:8 1:0¹

0

0:2

0:4

0:6

0:8

1:0

E(B¡

V) s

tar=

E(B¡

V) l

ine

¡1:0 ¡0:8 ¡0:6nISM

¡0:6¡0:5¡0:4¡0:3¡0:2¡0:1

0

0:1

0:2

±

Parametersoftheflexibleattenuation recipes:• µ andEBV-factor correlate• nISM and 𝛿 correlate ,inaverage steeper valuesthan theoriginalones.

-->Nouniversal values

EBV-factor=0.44

µ=0.3

nISM =-0.7


=0.54± 0.19=0.60± 0.23

=-0.33± 0.18=-0.82± 0.19

𝛿 =0

EBV-factor

Buat+18

0 0:5 1:0 1:5 2:0 2:5 3:0

AV(mag)

¡3

¡2

¡1

0

pow

er¡

law¡

expon

ent[FU

V¡

V]

0 0:5 1:0 1:5 2:0 2:5 3:0

AV(mag)

¡3

¡2

¡1

0

pow

er¡

law¡

expon

ent[H¡

V]

Comparison with Radiationtransfer modeling ofspiralgalaxieswhich predicts aflattening ofattenuation laws with increasing

obscuration/inclination(e.g.Pierini+04,Tuffs+04,Law+18&Chevallard+13compilation)

FUV-VrangeV-Hrange


__Chevallard+13■.DBPL-free•Calzetti-like __Chevallard+13

■.DBPL-free•Calzetti-like

stee

per

CFfreerecipe

CFfreerecipe

Buat+18

D.Corre,PhDthesis.Corre,Buat,etal.Inprep

• 𝜆 < 𝜆V K(𝜆)mod =K(𝜆)C00*(𝜆 /𝜆V)𝛿• 𝜆 >𝜆V K(𝜆)mod =K(𝜆)C00*(𝜆 /𝜆V)𝛿+𝜀

CANDELS@UMASS,october2018

Modifying theflexibleCalzetti-like recipe intheNIR?

RTfrom Seon &Draine2016(various dust models andspatialdistributions)

D.Corre,PhDthesis.Corre,Buat,etal.Inprep

RTfrom Seon &Draine2016(various dust models andspatialdistributions)

• 𝜆 < 𝜆V K(𝜆)mod =K(𝜆)C00*(𝜆 /𝜆V)𝛿• 𝜆 >𝜆V K(𝜆)mod =K(𝜆)C00*(𝜆 /𝜆V)𝛿+𝜀

CANDELS@UMASS,october20180 1 2 3

AV(mag)[H¡ V]

¡3

¡2

¡1

0

pow

er¡

law¡

expon

ent

! =0

Average SD16relation

Modifying theflexibleCalzetti-like recipe intheNIR?

Aselection ofGRBhoststostudy dust extinction/attenuation


Corre,BuatInprep.

GRBhostgalaxieswith:• Atleast5photometric bands,1inFUVrest-frame• Hα,H𝛽 (Kruehler+15)

Dust attenuation andcomparison with Seon andDraine(2016)models

Among them:6GRBHs with anextinctioncurvemeasured along thelineofsight oftheGRBafterglow

à extinction/attenuation comparison

Corre+18,A&A,617,A141

D.Corre,2018,PhDthesis

Extinctioncurves forGRBHsmeasured with observationsoftheafterglow

Zafar+18

Theafterglow is modelled byasingleordoublepower-law:any deviationin theUV-NIRrangeis duetodust extinction

DustingtheUniverse,Tucson,2019Corre+18


MWlike curves observed

Attcurve flatterthan Extcurve

Attcurve similar toExtcurve

Attcurve flatterthan Extcurve Attcurve steeper than Extcurve

DustingtheUniverse,Tucson,2019Corre+18

variety of configurations

flexibility of models & recipes


Which dust attenuation curve(s)forstarforming galaxies?

ANSWER:alot……

Documents

Whichdustattenuationcurve(s) for star forminggalaxies? · Véronique Buat 1 David Corre1, Médéric Boquien2, KasiaMalek3,1 & the HELP/Herschel team 1 LAM, Aix-Marseille Université,