Transcript The IRS/MIPS/NOAO Collaboration IRS/MIPS/NOAO Collaboration To Study NWDFS Bootes Field B.T.Soifer for the collaboration BTS-1

The IRS/MIPS/NOAO Collaboration
IRS/MIPS/NOAO Collaboration
To Study NWDFS Bootes Field
B.T.Soifer for the collaboration
BTS-1
The Collaboration
Cornell
Caltech
Vassilis Charamandaris
Lei Hao
Terry Herter
Jim Higdon
Sarah Higdon
Jim Houck
Dan Weedman
Chao Bian
Tom Soifer (also SSC)
SSC /Caltech
U. Arizona
Lee Armus
Harry Teplitz
Emeric Le Foch'h
Casey Papovich
Marcia Rieke
JD Smith
Leiden University
NOAO
Mike Brown
Arjun Dey
Buell Jannuzi
Bernhard Brandl
BTS-2
Goals of the Project

Identify new classes of Extragalactic Objects at High Redshifts
 Determine the dust enshrouded star formation rate with z
 Identify AGN content in IR selected sample
 Identify unusual galactic sources at high latitude (debris disks,
dust enshrouded late type stars, cold Brown Dwarfs)
BTS-3
Observational Program

MIPS survey of Bootes Field component of NWDS
 High ecliptic latitude required for low IR background, minimum
contamination from asteroids
 Sensitivity set to insure high s/n detection at 24microns of targets whose
spectra can be obtained with IRS/low resolution in 1-2 hrs observing time
(0.75 mJy limit)
 Survey executed – late January 2004

IRS followup spectroscopy of targets found with faint or no optical
counterparts
 MIPS 24um Catalog produced March 2004
 Target selection done 1 April 2004
 Observations planned for next available observing window (June/July 04)

Ground-based follow-up spectroscopy programs
 Hectospec / MMT for sources brighter than ~ 21 mag
 DEIMOS/LRIS/Keck for sources as faint as 25 mag
BTS-4
The Catalog
BTS-5
dN/dS∙S 2.5
BTS-6
MIPS/Optical Position Comparison
Data from Bootes Field Survey
(collaboration between IRS,
MIPS instrument teams and
NOAO team)
Position difference between
24um source and nearest optical
counterpart
Positions good enough to make
Meaningful IDs with deepest
possible optical imaging material
BTS: 7
Some Features of the Sample - 1
BTS: 8
Features - 2
IRS Target Criterion
BTS: 9
Early Spectroscopic Results
Keck Observations – May 15-19
¾ clear night w/LRIS
1 cloudy night w/DEIMOS
8
160 objects observed in 6 masks
112(+0/-2) redshifts obtained
Vast majority narrow lines
Some obvious AGNs
2.97
2.76
2.55
2.34
2.13
1.92
1.71
1.5
1.29
Redshift
cumulative z distribution
120.00%
100.00%
percent
1.08
0.87
0.66
0.45
0.24
6
4
2
0
0.03
Frequency
Redshift distribution
80.00%
60.00%
Percent
40.00%
20.00%
0.00%
0
1
2
3
4
redshfit
BTS: 10
What’s to come??

Spitzer results
 Analysis of planned spectra
 Observations of more targets
 Bolometric corrections from MIPS 70 & 160 micron observations

Ground-based follow-up
 Use of existing data to test, calibrate photo-z from NWDFS
photometry
 Additional optical redshifts for AGN selection, z distribution, photoz calibration
 Near IR spectra for objects with no Spitzer/Optical z
 Photo-z analysis of entire sample

Analysis
 IR selected lum function as function of z
 Lilley/Madeau diagram from 24 micron selected sample
BTS: 11