ZSpec: A Dispersive MillimeterWave Spectrometer

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Z-Spec A Dispersive Millimeter-Wave Spectrometer
Jason Glenn From Z-Machines to ALMA!
Caltech CEA Colorado JPL
ISAS Bret Naylor Lionel Duband James Aguirre
Jamie Bock Hideo Matsuhara Jonas
Zmuidzinas Lieko Earle Matt
Bradford Jason Glenn Mark Dragovan
Cardiff Phil Maloney Hien
Nguyen Peter Ade Corey Wood
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Bolocam 1.1 mm Galaxy Surveys
The Lockman Hole
COSMOS
(Aguirre et al., 2006)
(Laurent et al., 2005 Maloney et al., 2005
Laurent et al., 2006)
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350 ?m Follow Up Photometric Redshifts
5 Galaxies

• Based on 5 galaxies with published spectroscopic
  redshifts
• Photometric redshifts based on radio/FIR
  correlation appear to be too large by ?z ? 1 (1.4
  GHz too low)
• One spectroscopic misidentification out of five?

All redshifted to z2
(Laurent et al., 2006)
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Ultimate Science Goal High-z CO Lines
Model Spectrum with CO Rotational Ladder
Z-Spec bandpass in the galaxy rest frame as a
function of redshift
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Overall Instrument Description
Feedhorn input
3He/4He Fridge

• Observations from the CSO
• ? 1.0 to 1.5 mm
• Waveguide-coupled diffraction grating
• Resolution element 900 MHz
• ? Velocity resolution 1000 km s-1
• 160 Si3N4 micromesh NTD Ge bolometers (BLIP NEP
  10-17 W Hz-1/2 ? design NEP 410-18)
• Technology demonstration for future orbital
  missions SPICA (BLISS), SAFIR, CCAT

WaFIRS Grating 62 48 3.3 cm
60 mK ADR (Salt pill courtesy Peter Timbies
group)
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Waveguide-Coupled Grating Bolometers
Bolometers are mounted on keys with reflecting
backshorts
The parallel plate grating diffracts and focuses
incoming radiation
Waveguide bend blocks couple radiation from the
parallel plate waveguide to the bolometers
Single broadband corrugated input feed
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Assembled
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Z-Spec at the CSO June 2005
Arrival
Beam maps!
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First Light!
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ULIRG Line Survey

• Aiming to reach BLIP limit soon
• ULIRG survey to begin in spring 2006 with
  submillimeter galaxies to follow
• IRAM 30 m?