Spitzer Observations of Submm/Mm/Radio-Selected Galaxies Eiichi Egami (Univ. of Arizona) MIPS team: E. Le Floc'h, C. Papovich, P. Perez-Gonzalez, G. Rieke, M. Rieke, H. Dole, A. Alonso-Herrero, M. Blaylock, J. Cadien, J. Jones IRAC team: J.-S. Huang, P. Barmby, G. Fazio Lockman Hole SHADES team: J. Dunlop, R. Ivison, + others Bolocam team: J. Glenn + others (Lijia ng)
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Spitzer Observations of Submm/Mm/Radio-Selected Galaxies Eiichi Egami (Univ. of Arizona) MIPS team: E. Le Floc'h, C. Papovich, P. Perez- Gonzalez, G. Rieke,
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Spitzer Observations of
Submm/Mm/Radio-Selected Galaxies Eiichi Egami (Univ. of Arizona)
MIPS team: E. Le Floc'h, C. Papovich, P. Perez-
Gonzalez, G. Rieke, M. Rieke, H. Dole, A. Alonso-
Herrero, M. Blaylock, J. Cadien, J. Jones
IRAC team: J.-S. Huang, P. Barmby, G. Fazio
Lockman Hole
SHADES team: J. Dunlop, R. Ivison, + others
Bolocam team: J. Glenn + others
(Lijiang)
Outline
1. Spitzer deep survey of the Lockman Hole East
● Submm/Mm/Radio selection: why should we care?
● 70/160 um observations
2. Spitzer observations of the brightest cluster
galaxies (BCGs) in strongly cooling cluster cores
● IGM accretion onto a seed mass concentration
-> another way to make galaxies IR-luminous (as
opposed to galaxy-galaxy interaction). May
play an important role at high-z (e.g., z > 3-4).
1. Deep Survey of the Lockman Hole (E)
● Lowest HI column density● Abundance of ancillary data● Especially deep X-ray/radio● Wide submm coverage (SHADES)● Deep optical (R,I,z) coverage
We doubled the MIPS integrationsduring the spring of 2005.
850 um: 8 mJy
24 um: 80 uJy20 cm: 20 uJy
Radio (20cm) data must be very deep to be useful.
Submm/Radio Selection vs. 24 um Selection
Why do we care about submm/mm/radio?
● Submm/Mm
– Potential to detect extremely high-z galaxies (z>3).
– Power to constrain IR SED together with Spitzer.
● Radio
– Accuracy for estimating IR luminosity with the tight