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AGN Feedback at z~2
in the Keck/MOSDEF Survey
Alison CoilUCSD
Collaborators: Gene Leung, Mojegan Azadi MOSDEF co-PIs: Alice Shapley, Mariska Kriek, Naveen
Reddy, Brian Siana, Bahram Mobasher
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MOSDEF surveyNew survey at 1.4 < z < 3.8 using MOSFIRE on Keck4 year survey, 48 nights total, started in 2013Full sample will have ~1500 galaxies + ~150 AGN
Targeting CANDELS fields, H-band selected (depth=24.5)Sample spans a wide range of stellar mass and SFR
Kriek et al. (2015)
stellar massH
mag
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Data from first 1/2 of the survey.
AGN separate well from galaxies, NII/Ha is crucial.
We are using the Melendez et al. (2014) line to identify
optical AGN- less contaminated than Kauffmann, much more complete than Kewley
MOSDEF BPT Diagram
Azadi in prep.
Galaxies + X-ray and IR-selected AGN
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Outflow Identification
Perform multiple-component Gaussian fits simultaneously to Hβ, [OIII], Hα and [NII]. Allow for an outflow component in all lines
and/or very broad component in Hα and Hβ.
outflow
broad line, no outflow
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Outflow vs Merger
Use HST imaging to remove potential mergers
potential mergers no indication of merger
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Outflow Host Galaxy Properties
All star-forming hosts, log M*~10-11.5, log SFR~0.5-3.5
outflows
potential mergers
MOSDEFSF galaxies at z~2
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Incidence of Detected Outflows
• 19 sources have a potential outflow component (ie, a 2nd kinematic component) with S/N>3 in [OIII] and/or Hα
• 12 of those do not appear to be potential mergers in HST
Out of initial sample of 66 AGN (X-ray/IR/optical):
• The detected outflow rate is >18% - this is a lower limit on actual AGN outflow rate, as need high S/N spectra and/or fast outflow to detect (and some mergers could have outflows).
Hα S/N
num
ber
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Outflow Kinematics
• velocity centroid of outflow component ~100-500 km/s• maximum velocity of outflow component ~300-1300 km/s• FWHM ~100-1300 km/s
[OIII] [NII] + Hα
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Outflow Sizes
Spatial extent from 2d spectra:
6 are resolved, FWHM of physical extent is ~3-10 kpc7 are spatially offset from narrow line, with a max. physical offset of ~7 kpc
NLoutflow
outflow
NL
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Interesting Source
COSMOS 11223: has 2 outflows, one is spatially offset
#1: velocity offset: 160 km/s, FWHM: 470 km/s, spatial offset: 0 kpc#2: velocity offset: 340 km/s, FWHM: 390 km/s, spatial offset: ~7 kpc
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Outflows on BPT Diagram
outflow component:
log ([NII]/Hα)
log
([O
III]/
Hβ)
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Outflow Energy Rate
Energy injection rate into ISM:assuming an energy conserving bubble into a uniform medium
• ~order of magnitude lower than ULIRGs at z~2 (Harrison et al. 2012) - r and v are a bit lower for our sample than in ULIRGs
• bolometric AGN luminosities for our sample ~1043 - 1045 erg/s
r10 is half extent of outflow in 10 kpcv1000 is velocity offset in 1000 km/s
dE/dt ~ 1042 - 1044 erg/s
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Conclusions
Have 12 AGN outflows in the current MOSDEF sample (first 1/2 of survey).
AGN-driven outflows occur in at least 18% of X-ray/IR/optical AGN at z~2 in “normal” star-forming galaxies.
Maximum velocities ~300-1200 km/s.
Outflows are often resolved and/or spatially offset. We detect physical sizes (FWHM) of ~3-10 kpc.
These are galaxy-wide outflows.