High-Velocity Outflows Without AGN Feedback

Collaborators: John Moustakas, Christy Tremonti, Alison Coil, Ryan Hickox, Aday Robaina, Greg Rudnick, Paul Sell

Aleks Diamond-StanicCGE Fellow, UC San Diego

see arXiv.1205.2368

Eddington-Limited Star Formation in Compact Massive Galaxies

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Papers on astro-ph by conference participants since April

Alberto Dominguez arXiv:1206.1867Amanda Ford arXiv:1206.1859Charlotte Christensen arXiv:1205.5567Gurtina Besla arXiv:1205.4724Jean-Rene Gauthier arXiv:1205.4037Anthony Gonzalez arXiv:1205.3788Fabrizio Arrigoni Battaia arXiv:1205.3095Aleks Diamond-Stanic arXiv:1205.2368Evan Kirby arXiv:1205.1057Kathy Kornei arXiv:1205.0812Christopher Churchill arXiv:1205.0595Naveen Reddy arXiv:1205.0555Sijing Shen arXiv:1205.0270Glenn Kacprzak arXiv:1205.0245Kurt Soto arXiv:1205.0082Joo Heon Yoon arXiv:1204.6316Sebastiano Cantalupo arXiv:1204.5753Kathy Cooksey arXiv:1204.2827Brice Menard arXiv:1204.1978

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Can star formation feedback launch >1000 km s-1 outflows?

Tremonti, Moustakas, Diamond-Stanic 2007

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Kereš, Katz, Davé et al. 2009

Oppenheimer, Davé, Kereš et al. 2010

Why do theorists need feedback?

suppress star formation in low- and high-mass halosFriday, June 15, 12

What does feedback look like?

radiation pressure supernovae AGN

Rosette Nebula

Crab Nebula

M82 in X-rays

Mrk 231

Perseus A

NGC 3603cartoon based on Rupke & Veilleux 2011

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How do you produce a high-velocity outflow?

radiation pressure supernovae AGN

massive, compact,

large dust opacityMurray, Menard, Thompson 2011

high SFR, small launch radius,

large hot wind velocityMurray, Quataert, Thompson 2005

need to couple AGN output to the ISM

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Rupke, Veilleux, Sanders 2005Martin 2005: v∝SFR0.35

How does outflow velocity scale with galaxy properties?

Weiner, Coil, Prochaska + 2009 Kornei, Shapley, Martin + 2012v∝ΣSFRsee also Rubin, Weiner + 2010; Chen, Tremonti + 2010

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Heckman, Borthakur, Overzier et al. 2011

a compact (r ~100 pc) starburst can accelerate clouds to 1000 km s-1

dominant central objects

Can star formation feedback launch high-velocity outflows?

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Heckman, Borthakur, Overzier et al. 2011

How do you produce a high-velocity outflow?

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HST reveals compact

morphologies,re ~ 100 pc

WISE reveals ongoing star formation

SFR ~ 300 M⊙ yr-1

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Compact starbursts revealed by HST and WISE

Diamond-Stanic et al. 2012, arXiv:1205.2368

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SFR surface density v. stellar mass

data from Wuyts et al. 2011

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SFR surface density v. stellar mass

threshold from Heckman 2002 limit from Meurer, Heckman, Lehnert + 1997

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SFR surface density v. stellar mass

data from Wuyts et al. 2011

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SFR surface density v. stellar mass

data from Law, Steidel, Shapley + 2012

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SFR surface density v. stellar mass

threshold from Heckman 2002 limit from Meurer, Heckman, Lehnert + 1997

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SFR surface density v. stellar mass

gas rich mergers from Veilleux, Kim, Peng + 2006, Overzier, Heckman, Tremonti + 2009

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SFR surface density v. stellar mass

Diamond-Stanic et al. 2012, arXiv:1205.2368

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Size v. mass

van Dokkum, Franx, Kriek et al. 2008

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Size v. mass

van Dokkum, Franx, Kriek et al. 2008

These galaxies are remarkably compact

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Summary

extremely large ΣSFR in galaxies with >1000 km s-1 outflows

substantial momentum input from radiation pressure and supernovae

no need to invoke AGN feedback

could this type of feedback help theorists at

the high-mass end?

see arXiv.1205.2368

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Size v. mass

Hopkins, Murray, Quataert, Thompson 2010

Wuyts, Cox, Hayward et al. 2010

Is the stellar mass as compact as the light?

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