The Prevalence and Properties of Outflowing Galactic Winds at z = 1
Katherine A. Kornei (UCLA) UC Riverside Astronomy Talk January 27, 2012
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Crystal Martin (UCSB)
Alice Shapley (UCLA)
Alison Coil (UCSD)
Several important people.
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Galaxies are not closed boxes.
enrich the IGM in metals/dust
…quench star formation
…regulate black hole growth
Outflowsoutfl
ows?
IGM
AGN feedback?
cold streams?
AGN feedback?
outfl
ows?
4
Outflows are seen in local starbursts.
HST/ACS BVIHα (M. Westmoquette)
M82 (z=0.0008)
6”
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Outflows can be inferred through line offsets.
MgI MgII
Given outflowing material between the observer and the galaxy:
Wei
ner e
t al.
2009
[OII] 3727 ÅNebular line – at zsys zsys
Velocity (km/sec)
DN/s
ec/p
ixel MgII 2796/2803
MgI 2852
Outflowing gas will be blueshifted with respect to nebular lines tracing star forming regions.
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Galaxies near and far show blueshifted absorption lines.
Rupk
e et
al.
2005
ULIRGz = 0.2
LBGsz = 3
Shap
ley
et a
l. 20
03
Interstellar Absorption
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A variety of absorption lines are used to probe outflows.
Na I D ≈ 5900 Å z z = 0.5 1.0 3.0
Fe II/Mg II ≈ 2600 Å H I + others ≈ 1200 Å
Reddy et al. 2008
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The necessary data set.
Spectroscopy of lines tracing outflowing gas
lines tracing the systemic redshift
+ Photometry for calculating stellar masses, etc.
+ Ancillary data for obtaining dust-corrected SFRs, morphologies, galaxy inclinations, etc.
The ideal data set.
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50,000 galaxies at z ≈ 1 in 3.5 deg2
DEIMOS on Keck II (90 nights: ‘02-’05)
DEEP2 survey (the origin of our sample).
Slitmasks with 120 targets
R = 5000 (70 km s-1)
Resolved [OII] doublets
≈ 1 hour integration
Color cuts in 3/4 fields for z > 0.75
DEEP
2 Te
am
z < 0.75z > 0.75
B-R
R-I
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Extended Groth Strip – no color cuts and lots of ancillary data.
http:
//ae
gis.
ucol
ick.
org/
F606W
HST imaging (F606W, F814W)
6”
Spitzer imaging (IRAC, MIPS)
GALEX imaging (FUV, NUV)
The ideal data set. Photometry, imaging
✓
The necessary data set. Lines tracing outflows & systemic z
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LRIS observations to cover lines tracing winds.
LRIS: 3400-6700 Å LRIS: 7200-9000 Å
DEIMOS: 6500-9100 Å
[OII] (zsys)CIV, FeII, MgII, MgI (zout)
212 objects; B < 24.5 1.19 < z < 1.35 = CIV 1549, MgI 2852 coverage
Rest Wavelength (angstroms)
Nor
mal
ized
Flux
Si II, C IV
Fe IIFe II
Mg II
Al II Mg I
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Many analyses are possible. LRIS spectroscopy
fit FeII absorption lines to determine zout
measure fine structure FeII* emission lines
define zsys ([OII], Balmer series)
characterize MgII emission
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72 LRIS objects are in the Extended Groth Strip.
EGS (72)
Other fields (140)
star-formation ratesdust attenuationsHST imaging
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More analyses are possible for EGS objects. LRIS spectroscopy
fit FeII absorption lines
measure fine structure FeII* emission lines
define zsys ([OII], Balmer series)
characterize MgII emission
HST imaging
morphologies
colors
galaxy areas
inclinations
SFRs, dust attenuations from GALEX
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Blue, star-forming galaxies at z = 1.
Korn
ei e
t al.,
in p
rep.
Korn
ei e
t al.,
in p
rep.
16
Defining systemic and outflow velocities.
zsyszout Define a systemic reference frame, ideally from the LRIS spectra. Fit multiple emission lines ([OII], OIII, Balmer) using template spectra.
tilted [OII] lines(small fraction of
sample)
resonance abs.
fine structureemission
2250, 2260 2344, 2374 2587 Å
FeII
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A physical model for fitting absorption lines.
A single component fit with 4 free parameters.
covering fraction
op. depth at line center
line center
Doppler parameter
Primary quantity of interest is λ0, from which we estimate an outflow velocity.
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Blueshifted FeII absorption features are not ubiquitous in the sample.
Korn
ei e
t al.,
in p
rep.
12100420 z = 1.20
Mar
tin e
t al.,
in p
rep.
Inflow?
Other outflow diagnostics: MgII, FeII*
Velocities from FeII
Outflows Inflows
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The strength of outflows is correlated with various galaxy properties.
Mar
tin 2
005
outfl
ow v
eloc
ity (k
m/s
)
SFR (M*/yr)
dwarf starbursts
ULIRGs
Outflow velocity increases with increasing star formation rate.
Chen et al. 2010
Na D
edge-on
face-on
Outflows not seen in edge-on systems.
face-on edge-on
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No trend between outflow velocity and star-formation rate.
Martin 2005 1000 Msun yr-10.1 Msun yr-1
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Are outflows correlated with star-formation rate surface densities?
Σ
SFR estimate area estimate
UV, 24 μm, emission lines, etc.
Half-light radius?Petrosian radius?
A = πR2F606W
6”
Clumpy objects at high z – need a better area estimate that traces luminous regions.
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A new technique for estimating galaxy areas.
Given “clumpy” galaxies:
Include only those pixels brighter than a certain surface brightness
threshold, thereby flagging clumps.
F606W
Petrosianarea
Clumparea
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Higher star-formation rate surface density objects show larger blueshifts.
No trend seen:
Rubin et al. 2010(used half-light radius)
Steidel et al. 2010(ground-based imaging)
Kornei et al., in prep.
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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
MgII
SN IIFeII FeII
MgII in supernova ejecta; FeII merely entrained?
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The geometry of outflowing winds at z = 1.
Chen et al. 2010
Na D
edge-on
face-on
face-on edge-on
Estimate inclination from axis ratios from HST imaging:
i = cos-1(b/a)b
a
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Face-on galaxies show stronger blueshifts than edge-on systems.
More edge-on: dV = 28 ± 11 km s-1More face-on: dV = -19 ± 9 km s-1
Inclination composites::
Low High
face-on edge-on
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Mergers are not required to drive outflows.
Korn
ei e
t al.,
in p
rep.
Gini (G) – measure of how light is distributed in a galaxy
Law
et a
l. 20
07
high G low G
M20 – second order moment of a galaxy’s 20% brightest pixels
Lotz
et a
l. 20
08
high M20low M20
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Fine structure FeII* emission.
zsysv = 0
v = +100v = -100
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/”
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FeII* emission is prevalent.
Kornei et al., in prep.
Stacks of FeII* emitters/non-emitters FeII* emitters FeII* non-emitters
The strongest FeII* emitters are bright and blue.
FeII* emission appears to be ubiquitous
FeII, FeII*
MgII
stronger FeII* = stronger MgII emission
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Complexities of the MgII feature at ≈ 2800 Å.
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.
Mar
tin e
t al.,
in p
rep.
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Measuring an outflow velocity from MgII
2796 Å (resonance)
A resonantly trapped transition.
MgII
Vmax
where 90% of the continuum is met.
No correlation:SFR and Vmax
Significant correlation:SFRSD and Vmax
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Summary.
Reddy et al. 2008
Petrosianarea
Clumparea
LRIS: 3400-6700 Å LRIS: 7200-9000 Å
DEIMOS: 6500-9100 Å
CIV, FeII, MgII, MgI (zout)[OII] (zsys)
Outflow velocity most strongly correlated with the concentration of star formation.
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