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The IRAC/MIPS Survey in EGS

The IRAC/MIPS Survey in EGS. Jia-Sheng Huang /Giovanni Fazio and the EGS Consortium Harvard-Smithsonian Center for Astrophysics Cambridge, MA 02138, USA. Extended Groth Strip (EGS). Spitzer observation of EGS.

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The IRAC/MIPS Survey in EGS

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  1. The IRAC/MIPS Survey in EGS Jia-Sheng Huang /Giovanni Fazio and the EGS Consortium Harvard-Smithsonian Center for Astrophysics Cambridge, MA 02138, USA

  2. Extended Groth Strip (EGS)

  3. Spitzer observation of EGS • IRAC(3.6, 4.5, 5.8, 8.0um): Jan. 2004 (1.5h/p) , July 2004 (1.5h/p), total ~120h for all IRAC observation (3h/p). • MIPS(24, 70, and 160um): Jan. 2004 Spitzer safed, only 1/3 data were taken; June 2004, full depth data; total ~50-60h for MIPS observation. • Mosaic image: 3.6, 4.5, 5.8, 8.0, 24, 70um • Catalogs: 8um, 24um, 70um-selected samples.

  4. Extended Groth Strip (EGS) 5’x5’ 3h IRAC 3.6 µm IRAC 8.0 µm

  5. Q1700 deep field 5’x5’ 8h IRAC 3.6 µm IRAC 8.0 µm

  6. NOISE AS A FUNCTION OF TIME(Q1700 FIELD) • Noise in Channels 1 and 2 deviates from root time at ~ 3000 sec (onset of source confusion noise). • Noise in Channel 3 and 4 is still decreasing as root time at 20,000 sec.

  7. EGS

  8. Number Counts at 3.6 micron

  9. Number Counts at 4.5 micron

  10. Number Counts at 5.8 micron

  11. Number Counts at 8.0 micron

  12. Mid-IR Properties of Normal Galaxies at z<1.5 • DEEP redshift sample (>10k galaxies with z) • B, R, I photometry • High resolution 2d-spectrum (Keck DEMOS) • z<1.4

  13. Galaxies: Blue vs Red

  14. Galaxies: Blue vs Red

  15. Galaxies: Blue vs Red

  16. MIR Spectroscopy with IRAC • Really?

  17. UV-IR SED for Blue Galaxies 0.8<z<1.2 0<z<0.5

  18. IR Color Evolution??

  19. 8um Selected Sample

  20. 8um selected sample

  21. DEEP2+BM/BX+LBG

  22. 8 micron Number Counts for each redshift bin

  23. 24um selected sample

  24. 24um selected sample

  25. SEDs of the MIPS 24 micron Galaxies

  26. Morphologies of the 24um Source by J. Lotz et al • Using GINI-M50 Merger Classification to classify all 24um sources at z<1.2 • 50% Late type Spiral, 25% Early Type Spiral, 5% E/S0, 15% Mergers • 13 ULIRGS, half of them are mergers.

  27. IR properties of Galaxy Pairs in EGS

  28. 70um selected sample

  29. 70um selected sample

  30. SCUBA Sources in EGS

  31. SMG SED

  32. SCUBA sources detected in the 24um band

  33. SCUBA sources detected in the 70um band

  34. Radio Sources in EGS • VLA 6 cm covering the whole strip • 48 sources detected at f>0.5 mJy. 34 are single souces, the rest are either double or confused. • Out of 34, 28 are detected in the IRAC Bands, the remaining 6 have no IRAC counterparts.

  35. X-ray Sources in EGS

  36. Conclusion • IRAC colors can characterize galaxy spectra type (blue/red) at z<1.5 • IRAC colors is a good redshift indicator. • The 8 micron and 24 micron selected samples in EGS have significant number of galaxies at z>2 • The MIR band SEDs show that radio and SCUBA galaxies are either starburst or AGN at z>1 • The Chandra sources have a much wider IRAC color distribution than those just with power-law SEDs.

  37. LBG SED

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