1. The Prevalence and Properties of Outflowing Galactic Winds at z = 1 Katherine A. Kornei (UCLA) Alice E. Shapley (UCLA) Crystal L. Martin (UCSB) Alison L. Coil (UCSD) STScI/JHU Galaxy Journal Club - November 18, 2011

2. Galaxies are not closed boxes. enrich the IGM in metals/dust …quench star formation …regulate black hole growth Outflows IGM 2

3. Outflows are seen in local starbursts. HST/ACS BVIHα (M. Westmoquette) M82 (z=0.0008)  3

4. Outflows can be inferred through line offsets. MgI MgII Given outflowing material between the observer and the galaxy: Weiner et al. 2009 [OII] 3727 Å Nebular line – at z sys z sys Velocity (km/sec) MgII 2796/2803 MgI 2852 Outflowing gas will be blueshifted with respect to nebular lines tracing star forming regions. 4

5. A variety of absorption lines are used to probe outflows. Na I D ≈ 5900 Å z 0.5 1.03.0 Fe II/Mg II ≈ 2600 ÅH I + others ≈ 1200 Å 5 Reddy et al. 2008 Redshift

6. 50,000 galaxies at z ≈ 1 in 3.5 deg 2 DEIMOS on Keck II (90 nights: ‘02-’05) DEEP2 survey (the origin of the sample). 6 Slitmasks with 120 targets R = 5000 (70 km s -1 ) BRI color cuts in 3/4 fields for z > 0.75 Galaxy environments, ages, colors at z ≈ 1 Clustering statistics Evolution of dark matter halos Close pairs/merger rates Resolved [OII] doublets ≈ 1 hour integration z < 0.75 z > 0.75 R-I

7. Extended Groth Strip – no color cuts and lots of ancillary data. 7 F606W HST imaging (F606W, F814W) 6” Spitzer imaging (IRAC, MIPS) GALEX imaging (FUV, NUV)

8. LRIS observations of DEEP2 objects at z = 1. LRIS: 3400-6700 Å LRIS: 7200-9000 Å DEIMOS: 6500-9100 Å [OII] (z sys ) CIV, FeII, MgII, MgI (z out ) 8 212 objects from the DEEP2 survey; B < 24.51.19 < z < 1.35 CIV 1549, MgI 2852 Rest Wavelength (angstroms) 12012777 z = 1.27 Si II, C IV Fe II Mg II Al II Mg I

9. Many analyses are possible. LRIS spectroscopy fit FeII absorption lines measure fine structure FeII* emission lines define z sys ([OII], Balmer series) characterize MgII emission 9 HST imaging, F606W & F814W morphologies colors galaxy areas inclinations SFRs, dust attenuation from GALEX

10. 10 Blue, star-forming galaxies at z = 1.

11. A physical model for fitting absorption lines. z sys z out Define a systemic reference frame, ideally from the LRIS spectra. Fit multiple emission lines ([OII], OIII, Balmer) using template spectra. Simultaneous fit to 5 resonant FeII absorption lines We use a single component fit with 4 free parameters: covering fraction op. depth at line center line center Doppler parameter (2 ½ σ) tilted OII lines (small fraction of sample) 11

12. Blueshifted FeII absorption features are not ubiquitous in the sample. 12 OutflowsInflows 12100420 z = 1.20 Inflow? Other outflow diagnostics: MgII, FeII*

13. The strength of outflows is correlated with various galaxy properties. SFR (M * /yr) dwarf starbursts ULIRGs Outflow velocity increases with increasing star formation rate. 13 Chen et al. 2010 Na D edge-on face-on Outflows not seen in edge-on systems. edge-on

14. No trend between outflow velocity and star- formation rate. 14 Martin 2005 1000 M sun yr -1 0.1 M sun yr -1

15. Are outflows correlated with star-formation rate surface densities? Σ UV, 24 μm, emission lines, etc. Half-light radius? Petrosian radius? A = πR 2 F606W 6” Clumpy objects at high z – need a better area estimate that traces luminous regions. 15

16. A new technique for estimating galaxy areas. Given “clumpy” galaxies: Include only those pixels brighter than a certain luminosity threshold, thereby flagging clumps. F606W Petrosian area Clump area 16

17. Higher star-formation rate surface density objects show larger blueshifts. 17 No trend seen: Rubin et al. 2010 (used half-light radius) Steidel et al. 2010 (ground-based imaging) Kornei et al., in prep.

18. 18 Composite spectra show same trends as individual objects. Kornei et al., in prep. High Low Star-formation rate surface density composites:: High: dV = -31 ± 7 km s -1 Low: dV = 44 ± 15 km s -1 High: dV = -300 km s -1 Mg II shows more kinematic variation than Fe II

19. 19 The geometry of outflowing winds at z = 1. Chen et al. 2010 Na D edge-on face-on edge-on Estimate inclination from axis ratios from HST imaging: i = cos -1 (b/a) b a

20. Face-on galaxies show stronger blueshifts than edge-on systems. 20 More edge-on: dV = 28 ± 11 km s -1 More face-on: dV = -19 ± 9 km s -1 Inclination composites:: Low High edge-on

21. Fine structure FeII* emission is associated with resonance absorption lines. z sys v = 0 v = +100 v = -100    21 2600 Å (resonance) 2626 Å (fine structure) Leitherer et al. 2010 Kornei et al., in prep. probing very different scales at z = 1 and z = 0 Does this emission come from star forming regions or from outflows? F606W 8400 pc/”16 pc/”

22. FeII* emission is prevalent. Kornei et al., in prep. Stacks of FeII* emitters/non-emitters FeII* emitters FeII* non-emitters 22 Kornei et al., in prep. The strongest FeII* emitters are bright and blue. FeII* emission appears to be ubiquitous FeII, FeII* MgII stronger FeII* = stronger MgII emission

23. Complexities of the MgII feature at ≈ 2800 Å. 23 Composite spectrum Individual spectra show MgII emission AGN? (Weiner et al. 2009) Scattered wind? (Rubin et al. 2010) MgII MgII and FeII absorption are kinematically distinct.

24. Summary. Reddy et al. 2008 Petrosian area Clump area 24 Kornei et al., in prep. LRIS: 3400-6700 Å LRIS: 7200-9000 Å DEIMOS: 6500-9100 Å CIV, FeII, MgII, MgI (z out ) [OII] (z sys ) Outflow velocity most strongly correlated with the concentration of star formation.

25. 25

26. 26 N E Hubble Space Telescope 1.6 μm Weiner et al. 2009 F160W F775W