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AGN / Starbursts in the very dusty systems in Bootes

AGN / Starbursts in the very dusty systems in Bootes. Kate Brand + the Bootes team NOAO Lijiang, August 2005. The Importance of ULIRGS. ULIRGs have L bol >10 12 L o and contribute significantly to the total energy budget of the Universe.

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AGN / Starbursts in the very dusty systems in Bootes

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  1. AGN / Starbursts in the very dusty systems in Bootes Kate Brand + the Bootes team NOAO Lijiang, August 2005

  2. The Importance of ULIRGS • ULIRGs have Lbol>1012Lo and contribute significantly to the total energy budget of the Universe. • ULIRGS are an increasingly significant population at high redshifts. • They are difficult to study due to their extreme obscuration at most wavelengths. • - What is their dominant power source? AGN or starburst? • Crucial in determining the build-up of their galaxy bulges via star formation and SMBH growth via AGN activity. • - What is the contribution of AGN to the 24m background? • - What is the nature of the population with extreme 24m to optical ratios?

  3. The Data - The NDWFS Bootes field (9 deg2)

  4. 8 m @ z=1 24 m @ z=1 8 m @ z=1 24 m @ z=1 4 6 8 10 12 14 16 4 6 8 10 12 14 16 Rest Wavelength (m) Rest Wavelength (m) Using Log(f(24)/ f(8)) to divide AGN / starburst galaxies Starburst galaxies AGN Shallow dust continuum (+ possible silicate abs.) steep dust continuum + strong PAHs f(24:8)~0.0 f(24:8)~0.5 Templates copied from Laurent et al. 2000

  5. 8 m @ z=0.6 8 m @ z=0 4 6 8 10 12 14 16 Rest Wavelength (m) The low redshift star-forming contaminants • Normal star-forming galaxies at z < 0.6: • enhanced 8m emission. • f(24:8)~ -0.2.

  6. AGN AGN AGN High z Starbursts High z Starbursts High z Starbursts Low z star-forming galaxies Low z star-forming galaxies Low z star-forming galaxies Stars or z=0 galaxies Stars or z=0 galaxies Stars or z=0 galaxies Log(f(24)/ f(8)) distributions for different f(24) bins

  7. The fraction of AGN dominated ULIRGs as a function of f24 24m number counts from Papovich et al. 2004 -> AGN contribute to ~5-13% of the 24 m background.

  8. Summary • f(24:8) is a good discriminator for distinguishing AGN and starburst dominated ULIRGs. • The fraction of AGN dominated ULIRGs increases from ~20% at f24=0.3mJy to ~60% at higher f24. • AGN contribute to ~5-13% of the 24 m background. • Caveats - • Silicate absorption band - lower f(24:8) at z~1-2 • Strong PAH emission features - higher f(24:8) • Heavily embedded AGN - could the 24m emission still be dominated by an AGN?

  9. The extreme optically obscured ULIRGS • Arp 220 - a local starburst dominated ULIRG known to be heavily obscured. • R-[24]>15 (Log(f(24)/ f(R)) >1.8) sources - more extreme than Arp 220 out to high redshifts. • If at z~2 as IRS follow-up suggest, Lbol~ 10-100 x LArp220 but fainter than 0.1L* galaxy in the optical. • 859 (4% of the 24 m sources) have R-[24]>15 - a large population of extreme dusty obscured sources at high redshifts with no comparable examples in the local Universe.

  10. What are the R-[24]>15 sources? Interacting but optically invisible Optically extended / interacting X-ray loud but optically invisible Optically blank

  11. Log(f(24)/ f(8)) of R-[24]>15 sources

  12. What are the R-[24]>15 sources? • The f24 faint sources (intrinsically less luminous or higher redshift?) tend to be steep spectrum sources dominated by powerful but heavily obscured starbursts. • The less numerous (14%) f24 > 0.75mJy sources (intrinsically more luminous or lower redshift?) have a larger fraction of AGN dominated sources (as found in IRS follow-up observations).

  13. Summary • f(24:8) is a good discriminator for distinguishing AGN and starburst dominated ULIRGs. • The fraction of AGN dominated ULIRGs increases from ~20% at f24=0.3mJy to ~60% at higher f24. • AGN contribute to ~5-13% of the 24 m background. • There exists a large population of extreme dusty obscured sources at high redshifts with no comparable examples in the local Universe. The faintest f24 sources are dominated by powerful but heavily enshrouded starbursts whereas the brightest f24 sources have a larger contribution from AGN.

  14. Future Directions • f(24:8) diagnostic • Redshifts to investigate obscuration as a function of mid-IR luminosity. • More IRS spectroscopy to test and confirm f(24:8) diagnostic • R-[24]>15 sources • Keck spectra of optically brighter sources - z~1-2. • IRS spectroscopy of X-ray loud sources to investigate unified schemes of dust and gas distribution.

  15. The R-[24] color of the 24m population Fainter f(24) sources are more optically obscured.

  16. Rmag and f24 for AGN/starburst dominated sources STARBURSTS AGN STARBURSTS AGN

  17. Redshift distribution of R<21.5 sources

  18. f(24:8) vs. f(24:R)

  19. The Data - The NDWFS Bootes field • 20,000 sources detected by Spitzer/MIPS @ 24 m (f24 limit = 0.3mJy, survey area ~ 9 deg2). • 18,000 with Spitzer/IRAC @ 8 m (Spitzer shallow survey; Eisenhardt et al. 2004). • 18,000 sources with R<25.5 counterparts in NDWFS. • 1200 sources detected in 5-ks Chandra XBootes Survey (Kenter et al. 2005; Brand et al. 2005). • 20,000 optical spectra of galaxies down to I~20 and MIPS/IRAC/ Chandra sources down to I~21.5 from AGES (Kochanek et al. in prep). • 300 optical spectra from KECK/DEIMOS.

  20. R-[24] distribution for AGN/starburst dominated sources AGN STARBURSTS Un-obscured Obscured

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