formation and evolution of high-z dust

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1 formation and evolution of high-z dust Raffaella Schneider INAF/Osservatorio Astronomico di Roma

Simone Bianchi, INAF/OAArcetri Benedetta Ciardi, MPA Munich Pratika Dayal, Kapteyn Groningen Leslie Hunt, INAF/OAArcetri

2 the FIRST team and collaborators Matteo Alparone, student Matteo de Bennassuti, PhD Michele Ginolfi, PhD Luca Graziani, Pdoc Mattia Mancini, PhD Stefania Marassi, Pdoc Edwige Pezzulli, PhD Rosa Valiante, Pdoc Marco Bocchio, INAF/OAArcetri Simone Bianchi, INAF/OAArcetri Benedetta Ciardi, MPA Munich Pratika Dayal, Kapteyn Groningen Leslie Hunt, INAF/OAArcetri Marco Limongi INAF/OAR Umberto Maio, AIP Potsdam Roberto Maiolino, Cambridge University

3 stellar sources of dust: SNe observations of SNe and SN remnants show signatures of the presence of dust associated with the ejecta Schneider+14 Crab 1987A N49 CasA Gall+11, Gomez+12, Dunne+09, Barlow+10, Matsuura+11, Otsuka+10 Kozasa & Hasegawa 1987; Todini & Ferrara 2001; Nozawa et al 2003; Schneider, Ferrara & Salvaterra 2004; Bianchi & Schneider 2007; Chercheneff & Dwek 2010; Fallest et al. 2011; Sarangi & Cherchneff 2013; Marassi+2014, 2015, 2016; Bocchio+2016

SN dust yields Kozasa & Hasegawa 1987; Todini & Ferrara 2001; Nozawa et al 2003, 2007; Schneider, Ferrara & Salvaterra 2004; Bianchi & Schneider 2007; Chercheneff & Dwek 2010; Fallest et al.

4 SN dust yields Kozasa & Hasegawa 1987; Todini & Ferrara 2001; Nozawa et al 2003, 2007; Schneider, Ferrara & Salvaterra 2004; Bianchi & Schneider 2007; Chercheneff & Dwek 2010; Fallest et al. 2011; Sarangi & Cherchneff 2013; Marassi+2014, 2015, 2016 fixed energy explosion models ( erg) and fully mixed ejecta dependence on mass and parameters dependence on the strength of the reverse shock Z = Z SUN N 2 α = 1 fallback 20% survive 7% 2% Bianchi & Schneider (2007)

5 SN dust yields: reverse shock destruction Nozawa et al 2006, 2007; Bianchi & Schneider 2007; Silvia et al. 2010, 2012; Marassi et al. 2014, 2015; Bocchio et al. 2016; Micelotta+2016 evolution of the SN forward and reverse shock reverse shock Different physical processes: Sputtering due to grain-gas interaction Sublimation due to collisional heating Shattering due to grain-grain collisions Vaporisation the passage of the reverse shock has a strong effect on the SN dust size distribution and mass

6 SN dust yields: reverse shock destruction Nozawa et al 2006, 2007; Bianchi & Schneider 2007; Silvia et al. 2010, 2012;.Marassi et al. 2014, 2015; Bocchio et al. 2016; Micelotta+2016 modification of grain size distribution SN dust mass surviving the reverse shock Z = 0 Z = Z sun 20% survives 7% 2% Marassi et al Bianchi & Schneider 2007

7 SN dust yields: comparison with observations Schneider+14 Bocchio+16 CasA 1987A N49 Bianchi & RS 07 no reverse shock 1987A Cas A Crab Bianchi & RS 07 with reverse shock Crab N49 Gall+11, Gomez+12 Dunne+09 Barlow+10 Matsuura+11 Otsuka+10 theoretical SN dust yields are in broad agreement with available data the mass of SN dust that will enrich the ISM << than observed in SN remnants with t age < 10 4 yr

8 SN dust yields: importance of fallback, metallicity and rotation Marassi, RS, Limongi, Chieffi, Graziani, Bianchi in preparation Grid of SN progenitor models with 13 M sun M star 120 M sun 10-3 Z/Z sun 1 and different v rot models with fixed explosion energy: E sn = erg calibrated explosion models FE set A [Fe/H]=0 (v=0 km/s) CE set A [Fe/H]=0 (v=0 km/s) 03dh 03lw 03dh 03lw 93J 94I 06aj 03bg 87A 08D 05bf 02ap 97ef 98bw 93J 94I 06aj 03bg 87A 08D 05bf 02ap 97ef 98bw 97D 97D 99br 99br data: Nomoto+2013

SN dust yields: importance of fallback, metallicity and rotation Marassi, RS, Limongi, Chieffi, Graziani, Bianchi in preparation Grid of SN progenitor

9 SN dust yields: importance of fallback, metallicity and rotation Marassi, RS, Limongi, Chieffi, Graziani, Bianchi in preparation Grid of SN progenitor models with 13 M sun M star 120 M sun 10-3 Z/Z sun 1 and different v rot models with fixed explosion energy: E sn = erg calibrated explosion models

10 stellar sources of dust: AGB their role in the early Universe depends on the mass- and metallicitydependence of the dust yields Ferrarotti & Gail 01; 02; 06; Zhukovska+08; Nanni+13; Ventura+12a,b; Di Criscienzo+13; Dell Agli+14; Ventura+14 stationary spherically symmetric wind grain growth (olivine, pyroxene, quartz, iron, corundum, silicon carbide, carbon) numerical integration of stellar models (ATON code, Ventura+98) - Third Dredge Up: surface C enrichment - Hot Bottom Burning: C (and O) surface depletion Grid of AGB/SAGB stars with 1 M sun M 8 M sun and 0.01 Z sun Z Z sun

11 dust yields from AGB stars Ferrarotti & Gail 01; 02; 06; Zhukovska+08; Nanni+13; Ventura+12a,b; Di Criscienzo+13; Dell Agli+14; Ventura+14 Grid of AGB/SAGB stars with 1 M sun M 8 M sun and 0.01 Z sun Z 1 Z sun ATON yields: Ventura+12a; Ventura+12b; Di Criscienzo+13; Ventura+13 modeling uncertainties due to treatment of mass loss and convective borders

12 the contribution of AGB and SN to early dust enrichment all stars are formed in a single burst at t = 0 with a Salpeter IMF: AGB dust yields from Ferrarotti & Gail (2006) SN yields from Bianchi & Schneider (2007) 0.05 Z sun 0.2 Z sun 0.4 Z sun 300 Myr 300 Myr 300 Myr 80% 80% 80% 40% 50% 40% AGB contribute to ~ 50% of the total dust budget in 300 Myr (Valiante et al. 2009)

13 the contribution of AGB and SN to early dust enrichment all stars are formed in a single burst at t = 0 with a Salpeter IMF: AGB dust yields from ATON code (Ventura+12,13) SN yields from Bianchi & Schneider (2007) 0.05 Z sun 0.2 Z sun 0.4 Z sun 300 Myr 300 Myr 300 Myr 70% 15% 20% 25% 35% 2% with ATON yields, AGB contribution to the total dust budget becomes > 30% only when the Z > 0.2 Z sun and becomes dominant in 500 Myr when Z 0.2 Z sun AGB dust is always sub-dominant wrt to SN dust

14 dust yields from AGB stars: metallicity dependence Ventura+12b; Di Criscienzo+13 Ventura+12b; Di Criscienzo+13 LMC softer HBB higher Si abundance ü Silicates are produced by > 3 M sun stars ü Silicate dust production increases with Z ü No silicates are produced when Z < ü Carbon dust is produced by < 3 M sun stars and does not depend on Z ü When Z < 10-4 HBB is present even at M < 2 M sun à no AGB dust

15 the dust mass in extreme galaxies at z ~ 6: quasar hosts are stellar sources enough to produce ~ 10 8 M sun of dust in < 1 Gyr? Valiante et al. 2009, 2011, 2014; Gall et al. 2010, 2011; Dwek & Cherchneff 2011; Mattsson 2011; Pipino et al 2011; Calura et al M dust does not correlate with M star M dust does correlate with M H2 stellar dust is not enough to reproduce the observed M dust the observed M dust require super-solar metallicities and very efficient grain growth in dense gas Valiante et al. 2014, 2015

16 0.01 Z/Z sun the dust mass in normal SF galaxies at z ~ 6 Shimizu+14; Mancini, RS+2015, 2016; Khakaleva-Li & Gnedin 2016; Zhukowska+ 2016; Grassi+ 2016; McKinnon Aoyama+ in prep; Graziani+ in prep the dust mass in normal galaxies at 5 < z < 7 compared to local galaxies Gas-to-dust mass ratios in local galaxies over a 2 dex metallicity range Remy-Ruyer+2014 Asano+2013; Hirashita+2014

the dust mass in z ~ 6 normal SF galaxies Ouchi+2013; Kanekar+2013; Ota+2014; Schaerer+2014; Maiolino+2015; Watson+2015, 2016 semi-numerical approach: SFR, metal and gas masses from a cosmological

17 the dust mass in z ~ 6 normal SF galaxies Ouchi+2013; Kanekar+2013; Ota+2014; Schaerer+2014; Maiolino+2015; Watson+2015, 2016 semi-numerical approach: SFR, metal and gas masses from a cosmological simulation dust mass evolution in post-processing dust vs stellar mass: simulation results vs observations dust evolution of the most massive galaxies grain growth 2 Myr stellar dust Mancini et al. (2015) see also Zhukovska et al. 2016

18 the dust mass in z ~ 6 normal SF galaxies Ouchi+2013; Kanekar+2013; Ota+2014; Schaerer+2014; Maiolino+2015; Watson+2015, 2016 semi-numerical approach: SFR, metal and gas masses from a cosmological simulation dust mass evolution in post-processing dust vs stellar mass: simulation results vs observations dust evolution of the most massive galaxies grain growth 0.2 Myr stellar dust Mancini et al. (2015) efficient grain growth is required to account for the observed dust mass

19 effects on the evolution of the UV colours at z ~ 5-10 Mancini, RS+2015, 2016; Khakaleva-Li & Gnedin 2016; Graziani+ in prep Mancini+2016 dust has an important effect on the UV LF at z < 7 and on galaxy colours Remy-Ruyer+2014

20 effects on the evolution of the UV colours at z ~ 5-10 Mancini, RS+2015, 2016; Khakaleva-Li & Gnedin 2016; Graziani+ in prep Mancini+2016 Mancini+2016 simulated galaxies are consistent with modest reddening at z > 7 SFRs at z > 5 may be over-estimated if dust-correction based on local relations (Meurer+99) are applied Remy-Ruyer+2014

21 simulating dust evolution in high-z galaxies Khakaleva-Li & Gnedin 2016; McKinnon+2016; Graziani+ in prep dustygadget: metallicity- and mass-dependent SN and AGB dust yields grain growth in the ISM destruction by astration, SN shocks and thermal sputtering in hot halo gas distribution of gas, stars, metals and dust in the most massive halo in a 30 h -1 cmpc box Mancini+2016 Remy-Ruyer+2014

simulating dust evolution in high-z galaxies Khakaleva-Li & Gnedin 2016; McKinnon+2016; Graziani+ in prep dustygadget: metallicity- and mass-dependent SN and AGB dust yields grain growth in the

22 simulating dust evolution in high-z galaxies Khakaleva-Li & Gnedin 2016; McKinnon+2016; Graziani+ in prep dustygadget: metallicity- and mass-dependent SN and AGB dust yields grain growth in the ISM destruction by astration, SN shocks and thermal sputtering in hot halo gas distribution of stars, metals and dust in the most massive halo in a 30 h -1 cmpc box Mancini+2016 Remy-Ruyer+2014

23 Summary comparison between models and data suggests that effective SN dust yields may be 1/10-1/100 than currently observed at high-z the relative importance of SN and AGB stars depends on the metallicity dependence of AGB yields (and SFH, IMF.) observed properties of z > 6 quasars hosts require efficient grain growth in the ISM dust enrichment in normal star forming galaxies affect the UV LF at z < 7 and galaxy colours à ALMA and JWST will be able to probe the emergence of dust-enriched galaxies at high-z TBD: including dust in numerical simulations of high-z galaxies (dustygadget Graziani et al. in prep)

from dust to galaxies: testing the evolution of the stellar IMF

First Galaxies Ringberg, 26 June 1 July 2011 from dust to galaxies: testing the evolution of the stellar IMF Raffaella Schneider INAF/Osservatorio Astronomico di Roma http://www.arcetri.astro.it/david