The POLARBEAR Fourier Transform Spectrometer Calibrator and Spectroscopic Characterization of the POLARBEAR Instrument. (arXiv:1904.02901v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Matsuda_F/0/1/0/all/0/1">Frederick Matsuda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lowry_L/0/1/0/all/0/1">Lindsay Lowry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suzuki_A/0/1/0/all/0/1">Aritoki Suzuki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faundez_M/0/1/0/all/0/1">Mario Aguilar Fa'undez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnold_K/0/1/0/all/0/1">Kam Arnold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barron_D/0/1/0/all/0/1">Darcy Barron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bianchini_F/0/1/0/all/0/1">Federico Bianchini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheung_K/0/1/0/all/0/1">Kolen Cheung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chinone_Y/0/1/0/all/0/1">Yuji Chinone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elleflot_T/0/1/0/all/0/1">Tucker Elleflot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fabbian_G/0/1/0/all/0/1">Giulio Fabbian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goeckner_Wald_N/0/1/0/all/0/1">Neil Goeckner-Wald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasegawa_M/0/1/0/all/0/1">Masaya Hasegawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaneko_D/0/1/0/all/0/1">Daisuke Kaneko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katayama_N/0/1/0/all/0/1">Nobuhiko Katayama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keating_B/0/1/0/all/0/1">Brian Keating</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_A/0/1/0/all/0/1">Adrian Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Navaroli_M/0/1/0/all/0/1">Martin Navaroli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nishino_H/0/1/0/all/0/1">Haruki Nishino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paar_H/0/1/0/all/0/1">Hans Paar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puglisi_G/0/1/0/all/0/1">Giuseppe Puglisi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richards_P/0/1/0/all/0/1">Paul Richards</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seibert_J/0/1/0/all/0/1">Joseph Seibert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siritanasak_P/0/1/0/all/0/1">Praween Siritanasak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tajima_O/0/1/0/all/0/1">Osamu Tajima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takatori_S/0/1/0/all/0/1">Sayuri Takatori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tsai_C/0/1/0/all/0/1">Calvin Tsai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Westbrook_B/0/1/0/all/0/1">Ben Westbrook</a>
We describe the Fourier Transform Spectrometer (FTS) used for in-field
testing of the POLARBEAR receiver, an experiment located in the Atacama Desert
measuring the polarization of the cosmic microwave background (CMB). The
POLARBEAR-FTS (PB-FTS) is a Martin-Puplett interferometer specifically designed
to couple to the Huan Tran Telescope (HTT) on which the POLARBEAR receiver is
installed. The PB-FTS employs two fixed parabolic mirrors, one fixed and one
movable roof mirror, and multiple polarizing grids. The PB-FTS parabolic mirror
shape is designed to mimic the shape of the HTT primary reflector which allows
for optimum optical coupling to the POLARBEAR instrument by reducing
aberrations and systematics. One polarizing grid is placed at the output of the
PB-FTS and continuously rotated to provide modulation, allowing for
decomposition of the signal into different harmonics that can be used for
multiple unique spectral characterization analyses. In-field measurements were
taken in April 2014. We discuss the design, construction, and operation of the
PB-FTS and present the spectral characterization of the detectors in the
POLARBEAR receiver based on data from this measurement period, as well as
introduce future applications for the PB-FTS in the next-generation CMB
experiment, the Simons Array.
We describe the Fourier Transform Spectrometer (FTS) used for in-field
testing of the POLARBEAR receiver, an experiment located in the Atacama Desert
measuring the polarization of the cosmic microwave background (CMB). The
POLARBEAR-FTS (PB-FTS) is a Martin-Puplett interferometer specifically designed
to couple to the Huan Tran Telescope (HTT) on which the POLARBEAR receiver is
installed. The PB-FTS employs two fixed parabolic mirrors, one fixed and one
movable roof mirror, and multiple polarizing grids. The PB-FTS parabolic mirror
shape is designed to mimic the shape of the HTT primary reflector which allows
for optimum optical coupling to the POLARBEAR instrument by reducing
aberrations and systematics. One polarizing grid is placed at the output of the
PB-FTS and continuously rotated to provide modulation, allowing for
decomposition of the signal into different harmonics that can be used for
multiple unique spectral characterization analyses. In-field measurements were
taken in April 2014. We discuss the design, construction, and operation of the
PB-FTS and present the spectral characterization of the detectors in the
POLARBEAR receiver based on data from this measurement period, as well as
introduce future applications for the PB-FTS in the next-generation CMB
experiment, the Simons Array.
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