ir spectral diagnostics of z=2 dust obscured galaxies (dogs) jason melbourne (caltech) b.t. soifer,...
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![Page 1: IR Spectral Diagnostics of z=2 Dust Obscured Galaxies (DOGs) Jason Melbourne (Caltech) B.T. Soifer, Lee Armus, Keith Matthews, Vandana Desai, Arjun Dey,](https://reader035.vdocuments.us/reader035/viewer/2022062518/56649d575503460f94a3682e/html5/thumbnails/1.jpg)
IR SIR Spectral Diagnostics of z=2 pectral Diagnostics of z=2 Dust Obscured Galaxies (DOGs)Dust Obscured Galaxies (DOGs)
Jason Melbourne (Caltech)B.T. Soifer, Lee Armus, Keith Matthews, Vandana Desai, Arjun Dey, Shane
Bussmann
Melbourne et al. 2008
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DOGs are Defined by Very Red DOGs are Defined by Very Red Optical to Mid-IR Colors Optical to Mid-IR Colors
• R-[24] > 14 (Vega mag)
• F[24]/F[R] > 1000
• Significant amounts of warm dust.
• Total IR energy densities great than ULIRGs.
Dey et al. 2008
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Over 2000 DOGs Identified in the Over 2000 DOGs Identified in the NOAO Deep Wide Field Survey of NOAO Deep Wide Field Survey of
BootesBootes
• 10 square degrees• BRI ground based imaging
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
• Spitzer IRAC imaging • Spitzer MIPS imaging
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The Redshift Distribution of DOGs The Redshift Distribution of DOGs is Centered About z=2is Centered About z=2
• Median redshift of z = 1.99
z = 0.5
Dey et al. 2008
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Spectral Energy Distributions Vary Spectral Energy Distributions Vary
with 24 micron Fluxwith 24 micron Flux
• Brighter DOGs tend to show power-law SEDs.
• Fainter DOGs tend to show a “bump” in the observed mid-IR.
Dey et al. 2008
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IRS Spectra of Power-Law DOGs IRS Spectra of Power-Law DOGs Suggest AGN ActivitySuggest AGN Activity
Weedman et al. 2005
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IRS Spectra of “Bump” DOGs IRS Spectra of “Bump” DOGs Suggest Star FormationSuggest Star Formation
Desai et al. 2009
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TripleSpec: 5 Orders in the Near-TripleSpec: 5 Orders in the Near-IR, Including J, H, and K in One IR, Including J, H, and K in One
Spectrum Spectrum
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Spectra of Spectra of Power-LawPower-Law DOGs DOGs Reveal Reveal Broad HBroad H
Melbourne et al. in prep
H [nm]
z Line width [km/s]
2.282 2.477 1370
2.144 2.266 2350
1.761 1.684 2760
1.510 1.300 1550
1.260 0.919 1190
H
1
2
3
4
5
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Spectra of Spectra of “Bump”“Bump” DOGs DOGs Reveal Reveal Narrow HNarrow H
Melbourne et al. in prep
H [nm]
z Line width [km/s]
2.235 2.405 320
1.550 1.365 420
H
1
2
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Broad Ha from AGN dominates, Broad Ha from AGN dominates, but narrow Ha suggests star but narrow Ha suggests star
formation formation
Broad H
Narrow H
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OSIRIS Sample is AGN DominatedOSIRIS Sample is AGN Dominated
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These look different These look different
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SummarySummary
• A simple optical to mid-IR color selection identifies extreme z=2 ULIRGs.
• These Dust Obscured Galaxies (DOGs) may evolve into massive the ellipticals of today.
• DOGs are powered by a combination of SF and AGN activity.
• OSIRIS observations pinpoint the location of the AGN and constrain SFR.
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Spectra of Spectra of Power-LawPower-Law DOGs DOGs Reveal Reveal Broad HBroad H
Observed Wavelength (m)
Cou
nts
1.5 1.6 1.7 1.8