Crystal Martin
Crystal Martin
Crystal Martin
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The Astrophysics of Galaxy Formation:<br />
Quantifying the Role of Starburst Winds<br />
<strong>Crystal</strong> <strong>Martin</strong>, Colleen Schwartz, Taro Sato, Victor<br />
Sciortino, Akimi Fujita (UC Santa Barbara)<br />
Collaborators: Tim Heckman, Chip Kobulnicky, Fabian<br />
Walter, Lee Armus, Eliot Quartaert, Todd Thompson, Norm<br />
Murray<br />
Dark Matter Density Field: 100 Mpc box at z=2 , Nagamine, Springel, & Hernquist `04
Hubble Ultra Deep Field<br />
Ω b = 0.04<br />
WHIM: 10 5 -10 7 K<br />
Cen & Ostriker 1999<br />
Ω *~ 0.1Ω b<br />
•Does Does Feedback Shape the<br />
Galaxy Luminosity Function?<br />
•How How Far do Winds Spread<br />
Heavy Elements?
Emission Line Observations Multiphase Winds<br />
Ott, <strong>Martin</strong>, &<br />
Walter 2003<br />
Suchkov 95,96<br />
<strong>Martin</strong>, Kobulnicky, &<br />
Heckman 2002<br />
Stevens et al. 2003<br />
Kobulnicky & <strong>Martin</strong> 2004
Metal-Enriched Winds<br />
<strong>Martin</strong>, Kobulnicky, & Heckman 2002<br />
Energy (keV)
Henize 2-10<br />
X-rays: Kobulnicky<br />
& <strong>Martin</strong> 2005<br />
UV: Schwartz &<br />
<strong>Martin</strong> 2005<br />
170 km/s
Absorption Lines Probe Outflows at all Epochs<br />
STIS Data: Schwartz et al. 2005<br />
Schwartz et al. 2005<br />
Shapley et al. 2003
Strickland<br />
Absorption Lines Are Sensitive to Diffuse Gas<br />
Keck ESI Spectra of Na I Doublet<br />
V = -435 km/s<br />
V = -96 km/s<br />
IRAS 17208-0014<br />
Doppler<br />
Shift =<br />
400 km/s Rest V<br />
IRAS 11506+1331
Slower Outflow Speeds in Dwarf Starburst Galaxies<br />
Schwartz & <strong>Martin</strong> 2004<br />
Keck HIRES Spectra near Na I Doublet<br />
34 km/s<br />
23 km/s<br />
SPEED<br />
LIMIT<br />
V MAX=1.7 C S<br />
650 km/s<br />
Why Don’t the Cool Clouds<br />
Reach the Speed of the Hot<br />
Wind?
Hot Gas Escapes from<br />
Dwarf Starbursts<br />
Rotation Speed <br />
C s = 380 km/s<br />
<strong>Martin</strong> 1999, Heckman et al 2000, <strong>Martin</strong> 2004<br />
Tremonti et al 2004<br />
<strong>Martin</strong> 2005
Na I Velocities<br />
AGN<br />
?<br />
V term = 650<br />
km/s<br />
<strong>Martin</strong> 2005
<strong>Martin</strong> 2004b
20<br />
kpc<br />
10<br />
kpc<br />
Na I Absorption Covers Large Angle<br />
….Suggests Wind Extends<br />
~20 kpc into Halo<br />
20<br />
kpc<br />
10<br />
kpc
M ~ 1.1e9 Msun
How Much Mass in<br />
Outflowing Cool Gas?<br />
IRAS1720-03: Can Supernovae Power the Outflow? YES<br />
Measure K.E. > 7e56 ergs<br />
SFR ==> E_SN (@10 Myr) ~ 30e56 ergs, or (@100 Myr) 1700e56 ergs
NaI Column Density vs Position along Slit<br />
M ~ 2.9e9 Msun<br />
M ~ 1.8e8 Msun<br />
M ~ 7.1e7 Msun<br />
320 Msun/yr<br />
450 Msun/yr<br />
250 Msun/yr
Halo/Wind Velocity Gradients
Angular Momentum Conservation?
Rotation+Orbit<br />
Summary of Halo<br />
Velocity Gradients<br />
1. Flat (Not-Rotatin)<br />
2. Break (Minor Axis?)<br />
3. Steep (Rotating?)<br />
Disk Rotation Orbital Motion
Merger-Driven Winds vs. vs.<br />
Starburst Winds<br />
• Shocks from Radial Encounters Generate Hot Gas Reservoir<br />
(Instead of SNe Shocks)<br />
• Large Variation in Energy/Mass with Impact Parameter<br />
(Instead of SFR)<br />
• Test with X-ray Observations and Shock-Like Emission-Line<br />
Diagnostics<br />
Cox et al 2004<br />
Continuous Starburst:<br />
e.g. IRAS1056+24<br />
10 Myr Ew = 3e57 ergs<br />
100 Myr Ew = 1.7e59<br />
ergs
Extended X-Ray Halos in ULIGS<br />
IRAS10565+2448 IRAS17208-0014<br />
Sciortino &<br />
<strong>Martin</strong> (2005)
Summary: Feedback in Different Mass Galaxies<br />
Reionization<br />
Hot Starburst Winds<br />
Galaxies<br />
Momentum-Driven<br />
Winds (SNe + Rad.)<br />
Number Density<br />
Luminosity<br />
AGN?<br />
Radio Galaxies?<br />
Halos<br />
Benson et al. 2003<br />
• Why Do Small Halos<br />
AND Large Halos Fail<br />
to Host Galaxies?<br />
1. Cooling Time<br />
2. Feedback<br />
a. SNe<br />
b. Merger Induced?
Toy Model #1:<br />
Angular Momentum Conservation<br />
i<br />
• Wind Launched from a ring at R0 with circular rotation speed V 0<br />
• Wind velocity is radial at angle theta_w<br />
• View at some inclination i
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