Z-Spec: A Dispersive Millimeter-Wave Spectrometer

Jason GlennFrom Z-Machines to ALMA!

Caltech CEA Colorado JPL ISASBret Naylor Lionel Duband James Aguirre Jamie Bock Hideo MatsuharaJonas Zmuidzinas Lieko Earle Matt Bradford

Jason Glenn Mark Dragovan Cardiff Phil Maloney Hien NguyenPeter Ade Corey Wood

Bolocam 1.1 mm Galaxy Surveys

(Laurent et al., 2005; Maloney et al., 2005; Laurent et al., 2006)

The Lockman Hole COSMOS

(Aguirre et al., 2006)

350 m Follow Up & Photometric Redshifts

(Laurent et al., 2006)

All redshifted to z=2

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?

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

Overall Instrument Description

•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 = 4×10-18)•Technology demonstration for future orbital missions: SPICA (BLISS), SAFIR, & CCAT

WaFIRS Grating: 62 × 48 × 3.3 cm60 mK ADR

(Salt pill courtesy Peter Timbie’s group)

Feedhorn input

3He/4He Fridge

Waveguide-Coupled Grating & Bolometers

Single broadband corrugated input feed

Waveguide “bend blocks” couple radiation from the parallel plate waveguide to the bolometers

Bolometers are mounted on keys with reflecting backshorts

The parallel plate grating diffracts and focuses incoming radiation

Assembled

Z-Spec at the CSO June 2005

Arrival Beam maps!

First Light!

ULIRG Line Survey

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