High-Velocity Outflows Without AGN Feedback · Kathy Kornei arXiv:1205.0812 Christopher Churchill...
Transcript of High-Velocity Outflows Without AGN Feedback · Kathy Kornei arXiv:1205.0812 Christopher Churchill...
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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
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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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