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Large-Scale Winds in Starbursts and AGN

Large-Scale Winds in Starbursts and AGN. Rupke, Veilleux, & Sanders 2005a,b,c, submitted. David S. Rupke University of Maryland Collaborators: Sylvain Veilleux D. B. Sanders. v = - 1550 km s -1. Density. Temperature. Cooper, Bicknell, & Sutherland 2005, in prep., and . . .

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Large-Scale Winds in Starbursts and AGN

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  1. Large-Scale Winds in Starbursts and AGN Rupke, Veilleux, & Sanders 2005a,b,c, submitted David S. Rupke University of Maryland Collaborators: Sylvain Veilleux D. B. Sanders v = -1550 km s-1

  2. Density Temperature Cooper, Bicknell, & Sutherland 2005, in prep., and . . . Veilleux, Cecil, & Bland-Hawthorn 2005, ARAA, in press

  3. Sample • 78 starbursts • 50% luminous infrared galaxies (LIR > 1011 L) • 50% ultraluminous infrared galaxies (LIR > 1012 L) • 26 AGN • mostly Seyfert 2 ULIRGs • a few Seyfert 1s • 104 total galaxies!  the largest superwind survey to date at z < 3

  4. Method • Spectroscopy of the Na I D doublet • Moderate resolution 65-85 km s-1 • Data from Keck II (10m), MMT (6.5m), KPNO (4m) • Fit absorption lines • multiple velocity components • Gaussians in optical depth • yields velocity, Doppler parameter, optical depth, covering fraction • Compute • Mass, Momentum, Energy, and their outflow rates • *Simple model of constant-velocity, mass-conserving wind (* Model assumes thin shell, time-averaged outflow rates)

  5. Detection rates • Comparison of different subsamples • starburst LIRGs 45% (± 10%) • Seyfert 2 ULIRGs 45% (± 10%) • starburst ULIRGs 70 – 80% (± 10%) • Differences in detection rate appear to reflect GEOMETRY • wind opening angle for moderate starbursts and Seyfert 2s in local universe is CΏ ~ 0.4-0.5 there are winds in all starburst LIRGs and Seyfert 2 ULIRGs! • Same conclusion applies to ULIRGs

  6. Spectral Type V(H II) < V(LINER) < V(Sy2) 120 km/s < 230 km/s < 310 km/s Velocities } significant Star Formation rate / Nuclear Activity V(LIRG) < V(SB ULIRG) < V(Sy2 ULIRG) 100 km/s < 170 km/s < 220 km/s

  7. AGN- vs. Starburst-driven winds? • Can we demonstrate that AGNs help drive winds in Seyfert ULIRGs? • No! The statistics don’t convincingly indicate it. • But there are hints . . . • Seyfert 2 ULIRGs are statistically indistinguishable from SB ULIRGs • however, the SFRs and outflow detection rates are lower in Seyfert 2 ULIRGs than in SB ULIRGs • So differences between Sy2 ULIRGs and LIRGs may imply an AGN contribution.

  8. Outflow properties vs. Galaxy properties • = Starbursts  = Seyfert 2s isothermal escape speed Murray et al. 2004, Martin 2005 Outflow velocity Circular velocity Star formation rate dwarf galaxies from Schwartz & Martin 2004

  9. = Starbursts  = Seyfert 2s Starburst99 prediction (tSB > 40 Myr, Z = Z) Mass outflow rate Circular velocity Infrared luminosity

  10. = Starbursts  = Seyfert 2s Radiation pressure SB99 Momentum outflow rate Circular velocity Infrared luminosity

  11. = Starbursts  = Seyfert 2s SB99 Energy outflow rate Circular velocity Infrared luminosity

  12. Slopes of Correlations • Strong dependence on galactic mass • velocity, mass, momentum, and energy all increase sharply with circular velocity • Power-law slopes of 3-5! • Linear dependence of mass, momentum on SFR • but energy increases more sharply as SFR increases  increase in thermalization efficiency with SFR? • v  SFR0.2 • Metallicity effects • incorporating the K-band L–Z relationship (Salzer et al. 2005) does not change these conclusions significantly • I.e. metallicity is not driving these trends! (preliminary)

  13. Correlations at SFR  100 M yr-1 • We observe a statistically significant flattening in dependence of outflow properties on galaxy properties. • Possible explanations: • depletion of gas reservoirs • decrease in thermalization efficiency • velocity ceiling (Murray et al. 2004, Martin 2005) • saturation in star formation surface density (Strickland et al. 2004a,b)

  14. Na I D model [N II] [O III] Vmax(ionized)  Vmax(neutral)

  15. Neutral/Ionized Correlations All galaxies Galaxies with BELA FWHM [O III] 5007 Na I D velocity Na I D velocity

  16. Mrk 231 – AGN + Starburst winds? • A Seyfert 1 ULIRG • Small-scale AGN outflow observed in Na I D • broad, high-velocity (v = 4000 – 8000 km s-1) absorption (e.g., Boksenberg et al. 1977) • highest velocity component is variable • A large-scale outflow observed • blueshifted emission lines (Hamilton & Keel 1987) • blueshifted absorption lines (v  2000 km s-1) • Jet or wide-angle outflow? • disk geometry and measured velocities favor wide-angle outflow • however, jet could still inject energy . . .

  17. blueshifted Na I D 4 kpc Nuclear offset (kpc) 4 kpc vsys Heliocentric velocity

  18. Summary/Outlook • Winds occur in ~ all LIRGs and ULIRGs • Can’t yet convincingly demonstrate influence of AGNs on large-scale outflow • need more data on Seyfert 2s • there are hints • Outflow and galaxy properties are strongly correlated • flattening at high SFR, galaxy mass • Ionized and neutral gas is correlated • Vmax(ionized)  Vmax(neutral) • Mrk 231 is a good example of a galaxy with both a small- and a (spatially-resolved!) large-scale wind.

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