Catherine T. Marx

TL;DR: In this article, the authors present an end-to-end optical simulator for the PISCES IFS and plans for the data reduction pipeline (DRP), which enables the transformation of the IFS data to calibrated spectral data cubes using a combination of the IDL (Interactive Data Language)-based PROPER library and Zemax (a MatLab script).

Abstract: We are building a bolometer camera (the Goddard-Iram Superconducting 2-Millimeter Observer, GISMO) for operation in the 2 mm atmospheric window to be used at the IRAM 30 m telescope. The instrument uses a 8x16 planar array of multiplexed TES bolometers which incorporates our newly designed Backshort Under Grid (BUG) architecture. Due to the size and sensitivity of the detector array (the NEP of the detectors is 4×10-17 W/√Hz), this instrument will be unique in that it will be capable of providing significantly greater imaging sensitivity and mapping speed at this wavelength than has previously been possible. The major scientific driver for this instrument is to provide the IRAM 30 m telescope with the capability to rapidly observe galactic and extragalactic dust emission, in particular from high-z ULIRGs and quasars, even in the summer season. The 2 mm spectral range provides a unique window to observe the earliest active dusty galaxies in the universe and is well suited to better confine the star formation rate in these objects. The instrument will fill in the SEDs of high redshift galaxies at the Rayleigh-Jeans part of the dust emission spectrum, even at the highest redshifts. The observational efficiency of a 2 mm camera with respect to bolometer cameras operating at shorter wavelengths increases for objects at redshifts beyond z ~ 1 and is most efficient at the highest redshifts, at the time when the first stars were re-ionizing the universe. Our models predict that at this wavelength one out of four serendipitously detected galaxies will be at a redshift of z > 6.5.

TL;DR: Modeling identified E2 to be the most sensitive element to the grism wavefront error and was used to efficiently align the system and verified the higher efficiency and accuracy of the proposed alignment technique compared with the conventional sensitivity table method.

TL;DR: In this article, the performance of the Wide Field Infrared Survey Telescope (WFIRST) grating prism was evaluated using Diffractive Optical Elements (DOE) to find bright galaxies.

TL;DR: In this paper, the alignment and testing of the EDU grism at ambient and cold operating temperatures were performed using theodolites to set tip/tilt and a Micro-vu noncontact multisensor measurement system was used to set despace, decenter and clocking of each element using the hexapod.