1 / 24

New Views of Outflows from Ultraluminous Starbursts

New Views of Outflows from Ultraluminous Starbursts. Crystal Martin, Colleen Schwartz, Taro Sato, Victor Sciortino (UC Santa Barbara). Collaborators: Akimi Fujita, Tim Heckman, Chip Kobulnicky, Fabian Walter, Lee Armus, Eliot Quartaert, Todd Thompson, Norm Murray.

davina
Download Presentation

New Views of Outflows from Ultraluminous Starbursts

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. New Views of Outflows from Ultraluminous Starbursts Crystal Martin, Colleen Schwartz, Taro Sato, Victor Sciortino (UC Santa Barbara) Collaborators: Akimi Fujita, Tim Heckman, Chip Kobulnicky, Fabian Walter, Lee Armus, Eliot Quartaert, Todd Thompson, Norm Murray Dark Matter Density Field: 100 Mpc box at z=2 , Nagamine, Springel, & Hernquist `04

  2. Hubble Ultra Deep Field Wb = 0.04 W*~ 0.1Wb • Does Feedback Shape the Galaxy Luminosity Function? • How Far do Winds Spread Heavy Elements? WHIM: 105 -107 K Cen & Ostriker 1999

  3. Measuring Supernova Feedback Keck I&II Chandra X-Ray Observatory • Radio 21 cm Line  Neutral Interstellar Gas at 102 - 103 K • Optical Emission Lines  Photoionized Gas at 104 K • X-Rays  Thermal Emission from 106 K Gas NOAO/AURA

  4. Emission Line Observations  Multiphase Winds Suchkov 95,96 Ott, Martin, & Walter 2003 Stevens et al. 2003 (i) Martin, Kobulnicky, & Heckman 2002 Kobulnicky & Martin 2004

  5. Martin, Kobulnicky, & Heckman 2002 Energy (keV) Metal-Enriched Winds

  6. SPEED LIMIT VMAX=1.7 CS 650 km/s Tremonti et al 2004 Hot Gas Escapes from Dwarf Starbursts Cs = 380 km/s Rotation Speed  Martin 1999, Heckman et al 2000, Martin 2004

  7. Henize 2-10 X-rays: Kobulnicky & Martin 2005 STIS UV: Schwartz & Martin 2005 170 km/s

  8. IRAS 17208-0014 Doppler Shift = 400 km/s Rest V IRAS 11506+1331 V = -435km/s V = -96 km/s Strickland Absorption Lines Are Sensitive to Diffuse Gas Keck ESI Spectra of Na I Doublet

  9. Slower Outflow Speeds in Dwarf Starburst Galaxies Keck HIRES Spectra near Na I Doublet  23 km/s Schwartz & Martin 2004 Slower Outflows in Dwarf Starbursts 34 km/s

  10. Vterm = 650 km/s AGN? Na I Velocities Martin 2005

  11. Martin 2005b

  12. M ~ 1.1e9 Msun

  13. Angular Momentum Conservation?

  14. How Much Mass in Outflowing Cool Gas? IRAS1720-03: Can Supernovae Power the Outflow? YES Measure K.E. > 7e56 ergs SFR ==> E_SN (@10 Myr) ~ 30e56 ergs, or (@100 Myr) 1700e56 ergs

  15. Significant Fraction of Disk Gas in Flow 10%

  16. Supernova Provide Sufficient Energy 10% SFR X 10 Myr

  17. NaI Column Density vs Position along Slit 320 Msun/yr M ~ 2.9e9 Msun 450 Msun/yr M ~ 1.8e8 Msun 250 Msun/yr M ~ 7.1e7 Msun

  18. Large Variations in Outflow Mass Surprise! N(NaI) not correlated with SFR. Ionization Effects? Dynamical Age Mass of Cold Outflow SFR

  19. Merger-Driven Winds vs. Starburst Winds • Outflow covers the entire disk. • Exhibits disk-like, or orbit-like, rotation • Variation in mass/energy linked to merger age Do Shocks from Encounters Generate Hot Gas Reservoir? Cox et al 2004 Continuous Starburst: e.g. IRAS1056+24 10 Myr Ew = 3e57 ergs 100 Myr Ew = 1.7e59 ergs

  20. With Winds Without Winds Theuns et al. 2002

  21. How Far do the Metals Go? dN/dz ~ n0 c / H0 • Dwarf Galaxies @ Present Epoch • Pressure confined at R ~ 130 kpc (SFR/0.1 M0/yr)1/3. • Intervening OVI ALS are 200 - 270 kpc from 0.1L* • galaxies (Danforth & Shull 2005; Stocke et al 2005) • Ultraluminous Starbursts(?) @ Higher Redshift • (vcirc = 250 km/s, SFR=100 Mo/yr, NH=5 x 1020 cm-2, L=1012)

  22. Feedback in Massive Galaxies -- Cool Outflows • SB/AGN Ram Pressure Decelerates at R ~ 19 kpc Turn around at very large R! • SB/AGN Radiation Pressure Decelerates at R ~ 4 kpc Turn around at R ~ 32 kpc • Merger-driven Outflow ==> ? ULIGs are rare ==> small dN/dz If all galaxies are briefly ULIGs, still need contribution from 0.01L* galaxies to match dN/dz of strong metal line systems.

  23. Summary: Feedback in Different Mass Halos Reionization Hot Starburst Winds Momentum-Driven Winds (SNe + Rad.) AGN? Galaxies Halos Radio Galaxies? Number Density • Why Do Small Halos AND Large Halos Fail to Host Galaxies? • Cooling Time • Feedback Luminosity Benson et al. 2003

More Related