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216 results on '"Galitzki, N"'

1. The Simons Observatory: Cryogenic half wave plate rotation mechanism for the small aperture telescopes

Author: Yamada, K, Bixler, B, Sakurai, Y, Ashton, PC, Sugiyama, J, Arnold, K, Begin, J, Corbett, L, Day-Weiss, S, Galitzki, N, Hill, CA, Johnson, BR, Jost, B, Kusaka, A, Koopman, BJ, Lashner, J, Lee, AT, Mangu, A, Nishino, H, Page, LA, Randall, MJ, Sasaki, D, Song, X, Spisak, J, Tsan, T, Wang, Y, and Williams, PA
Subjects: Engineering, Astronomical Sciences, Physical Sciences, Chemical Sciences, Applied Physics, Chemical sciences, Physical sciences
Abstract: We present the requirements, design, and evaluation of the cryogenic continuously rotating half-wave plate (CHWP) for the Simons Observatory (SO). SO is a cosmic microwave background polarization experiment at Parque Astronómico de Atacama in northern Chile that covers a wide range of angular scales using both small (⌀0.42 m) and large (⌀6 m) aperture telescopes. In particular, the small aperture telescopes (SATs) focus on large angular scales for primordial B-mode polarization. To this end, the SATs employ a CHWP to modulate the polarization of the incident light at 8 Hz, suppressing atmospheric 1/f noise and mitigating systematic uncertainties that would otherwise arise due to the differential response of detectors sensitive to orthogonal polarizations. The CHWP consists of a 505 mm diameter achromatic sapphire HWP and a cryogenic rotation mechanism, both of which are cooled down to ∼50 K to reduce detector thermal loading. Under normal operation, the HWP is suspended by a superconducting magnetic bearing and rotates with a constant 2 Hz frequency, controlled by an electromagnetic synchronous motor. We find that the number of superconductors and the number of magnets that make up the superconducting magnetic bearing are important design parameters, especially for the rotation mechanism's vibration performance. The rotation angle is detected through an angular encoder with a noise level of 0.07 μrad s. During a cooldown process, the rotor is held in place by a grip-and-release mechanism that serves as both an alignment device and a thermal path. In this paper, we provide an overview of the SO SAT CHWP: its requirements, hardware design, and laboratory performance.
Published: 2024

2. The Simons Observatory: Cryogenic Half Wave Plate Rotation Mechanism for the Small Aperture Telescopes

Author: Yamada, K., Bixler, B., Sakurai, Y., Ashton, P. C., Sugiyama, J., Arnold, K., Begin, J., Corbett, L., Day-Weiss, S., Galitzki, N., Hill, C. A., Johnson, B. R., Jost, B., Kusaka, A., Koopman, B. J., Lashner, J., Lee, A. T., Mangu, A., Nishino, H., Page, L. A., Randall, M. J., Sasaki, D., Song, X., Spisak, J., Tsan, T., Wang, Y., and Williams, P. A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present the requirements, design and evaluation of the cryogenic continuously rotating half-wave plate (CHWP) for the Simons Observatory (SO). SO is a cosmic microwave background (CMB) polarization experiment at Parque Astron\'{o}mico Atacama in northern Chile that covers a wide range of angular scales using both small (0.42 m) and large (6 m) aperture telescopes. In particular, the small aperture telescopes (SATs) focus on large angular scales for primordial B-mode polarization. To this end, the SATs employ a CHWP to modulate the polarization of the incident light at 8~Hz, suppressing atmospheric $1/f$ noise and mitigating systematic uncertainties that would otherwise arise due to the differential response of detectors sensitive to orthogonal polarizations. The CHWP consists of a 505 mm diameter achromatic sapphire HWP and a cryogenic rotation mechanism, both of which are cooled down to $\sim$50 K to reduce detector thermal loading. Under normal operation the HWP is suspended by a superconducting magnetic bearing and rotates with a constant 2 Hz frequency, controlled by an electromagnetic synchronous motor. The rotation angle is detected through an angular encoder with a noise level of 0.07$\mu\mathrm{rad}\sqrt{\mathrm{s}}$. During a cooldown, the rotor is held in place by a grip-and-release mechanism that serves as both an alignment device and a thermal path. In this paper we provide an overview of the SO SAT CHWP: its requirements, hardware design, and laboratory performance., Comment: 19 pages, 21 figures, submitted to RSI
Published: 2023
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3. The Simons Observatory: pipeline comparison and validation for large-scale B-modes

Author: Wolz, K., Azzoni, S., Hervias-Caimapo, C., Errard, J., Krachmalnicoff, N., Alonso, D., Baccigalupi, C., Lizancos, A. Baleato, Brown, M. L., Calabrese, E., Chluba, J., Dunkley, J., Fabbian, G., Galitzki, N., Jost, B., Morshed, M., and Nati, F.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The upcoming Simons Observatory Small Aperture Telescopes aim at achieving a constraint on the primordial tensor-to-scalar ratio $r$ at the level of $\sigma(r=0)\lesssim0.003$, observing the polarized CMB in the presence of partial sky coverage, cosmic variance, inhomogeneous non-white noise, and Galactic foregrounds. We present three different analysis pipelines able to constrain $r$ given the latest available instrument performance, and compare their predictions on a set of sky simulations that allow us to explore a number of Galactic foreground models and elements of instrumental noise, relevant for the Simons Observatory. The three pipelines employ different combinations of parametric and non-parametric component separation at the map and power spectrum levels, and use B-mode purification to estimate the CMB B-mode power spectrum. We applied them to a common set of simulated realistic frequency maps, and compared and validated them with focus on their ability to extract robust constraints on the tensor-to-scalar ratio $r$. We evaluated their performance in terms of bias and statistical uncertainty on this parameter. In most of the scenarios the three methodologies achieve similar performance. Nevertheless, several simulations with complex foreground signals lead to a $>2\sigma$ bias on $r$ if analyzed with the default versions of these pipelines, highlighting the need for more sophisticated pipeline components that marginalize over foreground residuals. We show two such extensions, using power-spectrum-based and map-based methods, that are able to fully reduce the bias on $r$ below the statistical uncertainties in all foreground models explored, at a moderate cost in terms of $\sigma(r)$., Comment: 20 pages, 15 figures
Published: 2023
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4. The POLARBEAR-2 and Simons Array Focal Plane Fabrication Status

Author: Westbrook, B., Ade, P. A. R., Aguilar, M., Akiba, Y., Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bender, A. N., Bianchini, F., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Coppi, G., Crowley, K., Cukierman, A., de, T., Dünner, R., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fuller, G., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Halverson, N. W., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Holzapfel, W., Howe, L., Inoue, Y., Jaehnig, G., Jaffe, A., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kisner, T., Krachmalnicoff, N., Kusaka, A., Le, M., Lee, A. T., Leon, D., Linder, E., Lowry, L., Madurowicz, A., Mak, D., Matsuda, F., May, A., Miller, N. J., Minami, Y., Montgomery, J., Navaroli, M., Nishino, H., Peloton, J., Pham, A., Piccirillo, L., Plambeck, D., Poletti, D., Puglisi, G., Raum, C., Rebeiz, G., Reichardt, C. L., Richards, P. L., Roberts, H., Ross, C., Rotermund, K. M., Segawa, Y., Sherwin, B., Silva-Feaver, M., Siritanasak, P., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Tat, R., Teply, G. P., Tikhomirov, A., Tomaru, T., Tsai, C., Whitehorn, N., and Zahn, A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present on the status of POLARBEAR-2 A (PB2-A) focal plane fabrication. The PB2-A is the first of three telescopes in the Simon Array (SA), which is an array of three cosmic microwave background (CMB) polarization sensitive telescopes located at the POLARBEAR (PB) site in Northern Chile. As the successor to the PB experiment, each telescope and receiver combination is named as PB2-A, PB2-B, and PB2-C. PB2-A and -B will have nearly identical receivers operating at 90 and 150 GHz while PB2-C will house a receiver operating at 220 and 270 GHz. Each receiver contains a focal plane consisting of seven close-hex packed lenslet coupled sinuous antenna transition edge sensor bolometer arrays. Each array contains 271 di-chroic optical pixels each of which have four TES bolometers for a total of 7588 detectors per receiver. We have produced a set of two types of candidate arrays for PB2-A. The first we call Version 11 (V11) and uses a silicon oxide (SiOx) for the transmission lines and cross-over process for orthogonal polarizations. The second we call Version 13 (V13) and uses silicon nitride (SiNx) for the transmission lines and cross-under process for orthogonal polarizations. We have produced enough of each type of array to fully populate the focal plane of the PB2-A receiver. The average wirebond yield for V11 and V13 arrays is 93.2% and 95.6% respectively. The V11 arrays had a superconducting transition temperature (Tc) of 452 +/- 15 mK, a normal resistance (Rn) of 1.25 +/- 0.20 Ohms, and saturations powers of 5.2 +/- 1.0 pW and 13 +/- 1.2 pW for the 90 and 150 GHz bands respectively. The V13 arrays had a superconducting transition temperature (Tc) of 456 +/-6 mK, a normal resistance (Rn) of 1.1 +/- 0.2 Ohms, and saturations powers of 10.8 +/- 1.8 pW and 22.9 +/- 2.6 pW for the 90 and 150 GHz bands respectively.
Published: 2022
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5. Improved upper limit on degree-scale CMB B-mode polarization power from the 670 square-degree POLARBEAR survey

Author: The POLARBEAR Collaboration, Adachi, S., Adkins, T., Faúndez, M. A. O. Aguilar, Arnold, K. S., Baccigalupi, C., Barron, D., Chapman, S., Cheung, K., Chinone, Y., Crowley, K. T., Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Halverson, N. W., Hasegawa, M., Hazumi, M., Hirose, H., Howe, L., Ito, J., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Kisner, T., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Linder, E., Lonappan, A. I., Lowry, L. N., Matsuda, F., Matsumura, T., Minami, Y., Murata, M., Nishino, H., Nishinomiya, Y., Poletti, D., Reichardt, C. L., Ross, C., Segawa, Y., Siritanasak, P., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G., Yamada, K., and Zhou, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We report an improved measurement of the degree-scale cosmic microwave background $B$-mode angular-power spectrum over 670 square-degree sky area at 150 GHz with POLARBEAR. In the original analysis of the data, errors in the angle measurement of the continuously rotating half-wave plate, a polarization modulator, caused significant data loss. By introducing an angle-correction algorithm, the data volume is increased by a factor of 1.8. We report a new analysis using the larger data set. We find the measured $B$-mode spectrum is consistent with the $\Lambda$CDM model with Galactic dust foregrounds. We estimate the contamination of the foreground by cross-correlating our data and Planck 143, 217, and 353 GHz measurements, where its spectrum is modeled as a power law in angular scale and a modified blackbody in frequency. We place an upper limit on the tensor-to-scalar ratio $r$ < 0.33 at 95% confidence level after marginalizing over the foreground parameters., Comment: 16 pages, 9 figures, 8 tables, Published in ApJ
Published: 2022
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6. Improved Upper Limit on Degree-scale CMB B-mode Polarization Power from the 670 Square-degree POLARBEAR Survey

Author: Adachi, S, Adkins, T, Faúndez, MAO Aguilar, Arnold, KS, Baccigalupi, C, Barron, D, Chapman, S, Cheung, K, Chinone, Y, Crowley, KT, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Galitzki, N, Halverson, NW, Hasegawa, M, Hazumi, M, Hirose, H, Howe, L, Ito, J, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Linder, E, Lonappan, AI, Lowry, LN, Matsuda, F, Matsumura, T, Minami, Y, Murata, M, Nishino, H, Nishinomiya, Y, Poletti, D, Reichardt, CL, Ross, C, Segawa, Y, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Yamada, K, and Zhou, Y
Subjects: Particle and High Energy Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We report an improved measurement of the degree-scale cosmic microwave background B-mode angular-power spectrum over 670 deg2 sky area at 150 GHz with Polarbear. In the original analysis of the data, errors in the angle measurement of the continuously rotating half-wave plate, a polarization modulator, caused significant data loss. By introducing an angle-correction algorithm, the data volume is increased by a factor of 1.8. We report a new analysis using the larger data set. We find the measured B-mode spectrum is consistent with the ΛCDM model with Galactic dust foregrounds. We estimate the contamination of the foreground by cross-correlating our data and Planck 143, 217, and 353 GHz measurements, where its spectrum is modeled as a power law in angular scale and a modified blackbody in frequency. We place an upper limit on the tensor-to-scalar ratio r < 0.33 at 95% confidence level after marginalizing over the foreground parameters.
Published: 2022

7. A measurement of the CMB E-mode angular power spectrum at subdegree scales from 670 square degrees of POLARBEAR data

Author: Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Dobbs, M., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Goeckner-Wald, N., Groh, J., Hall, G., Hasegawa, M., Hazumi, M., Hirose, H., Jaffe, A. H., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Kikuchi, S., Kisner, T., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Matsumura, T., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Reichardt, C. L., Segawa, Y., Siritanasak, P., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tsai, C., Vergès, C., Westbrook, B., and Zhou, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report a measurement of the E-mode polarization power spectrum of the cosmic microwave background (CMB) using 150 GHz data taken from July 2014 to December 2016 with the POLARBEAR experiment. We reach an effective polarization map noise level of $32\,\mu\mathrm{K}$-$\mathrm{arcmin}$ across an observation area of 670 square degrees. We measure the EE power spectrum over the angular multipole range $500 \leq \ell <3000$, tracing the third to seventh acoustic peaks with high sensitivity. The statistical uncertainty on E-mode bandpowers is $\sim 2.3 \mu {\rm K}^2$ at $\ell \sim 1000$ with a systematic uncertainty of 0.5$\mu {\rm K}^2$. The data are consistent with the standard $\Lambda$CDM cosmological model with a probability-to-exceed of 0.38. We combine recent CMB E-mode measurements and make inferences about cosmological parameters in $\Lambda$CDM as well as in extensions to $\Lambda$CDM. Adding the ground-based CMB polarization measurements to the Planck dataset reduces the uncertainty on the Hubble constant by a factor of 1.2 to $H_0 = 67.20 \pm 0.57 {\rm km\,s^{-1} \,Mpc^{-1}}$. When allowing the number of relativistic species ($N_{eff}$) to vary, we find $N_{eff} = 2.94 \pm 0.16$, which is in good agreement with the standard value of 3.046. Instead allowing the primordial helium abundance ($Y_{He}$) to vary, the data favor $Y_{He} = 0.248 \pm 0.012$. This is very close to the expectation of 0.2467 from Big Bang Nucleosynthesis. When varying both $Y_{He}$ and $N_{eff}$, we find $N_{eff} = 2.70 \pm 0.26$ and $Y_{He} = 0.262 \pm 0.015$., Comment: 15 pages, 5 figures, submitted to ApJ
Published: 2020
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8. The Simons Observatory: Gain, bandpass and polarization-angle calibration requirements for B-mode searches

Author: Abitbol, MH, Alonso, D, Simon, SM, Lashner, J, Crowley, KT, Ali, AM, Azzoni, S, Baccigalupi, C, Barron, D, Brown, ML, Calabrese, E, Carron, J, Chinone, Y, Chluba, J, Coppi, G, Crowley, KD, Devlin, M, Dunkley, J, Errard, J, Fanfani, V, Galitzki, N, Gerbino, M, Hill, JC, Johnson, BR, Jost, B, Keating, B, Krachmalnicoff, N, Kusaka, A, Lee, AT, Louis, T, Madhavacheril, MS, McCarrick, H, McMahon, J, Meerburg, PD, Nati, F, Nishino, H, Page, LA, Poletti, D, Puglisi, G, Randall, MJ, Rotti, A, Spisak, J, Suzuki, A, Teply, GP, Verges, C, Wollack, EJ, Xu, Z, and Zannoni, M
Subjects: CMBR experiments, CMBR polarisation, gravitational waves and CMBR polarization, cosmological parameters from CMBR, astro-ph.CO, astro-ph.IM, Nuclear & Particles Physics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract: We quantify the calibration requirements for systematic uncertainties for next-generation ground-based observatories targeting the large-angle B-mode polarization of the Cosmic Microwave Background, with a focus on the Simons Observatory (SO). We explore uncertainties on gain calibration, bandpass center frequencies, and polarization angles, including the frequency variation of the latter across the bandpass. We find that gain calibration and bandpass center frequencies must be known to percent levels or less to avoid biases on the tensor-to-scalar ratio r on the order of Δ r∼10-3, in line with previous findings. Polarization angles must be calibrated to the level of a few tenths of a degree, while their frequency variation between the edges of the band must be known to O(10) degrees. Given the tightness of these calibration requirements, we explore the level to which residual uncertainties on these systematics would affect the final constraints on r if included in the data model and marginalized over. We find that the additional parameter freedom does not degrade the final constraints on r significantly, broadening the error bar by O(10%) at most. We validate these results by reanalyzing the latest publicly available data from the collaboration within an extended parameter space covering both cosmological, foreground and systematic parameters. Finally, our results are discussed in light of the instrument design and calibration studies carried out within SO.
Published: 2021

9. A measurement of the CMB e-mode angular power spectrum at subdegree scales from 670 square degrees of polarbear data

Author: Adachi, S, Aguilar Faúndez, MAO, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Bianchini, F, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Dobbs, M, El Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Hasegawa, M, Hazumi, M, Hirose, H, Jaffe, AH, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Kikuchi, S, Kisner, T, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, LN, Matsuda, F, Matsumura, T, Minami, Y, Navaroli, M, Nishino, H, Pham, ATP, Poletti, D, Reichardt, CL, Segawa, Y, Siritanasak, P, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, GP, Tsai, C, Vergès, C, Westbrook, B, and Zhou, Y
Subjects: Cosmic microwave background radiation, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: We report a measurement of the E-mode polarization power spectrum of the cosmic microwave background (CMB) using 150 GHz data taken from 2014 July to 2016 December with the POLARBEAR experiment. We reach an effective polarization map noise level of 32 mK-arcmin across an observation area of 670 square degrees. We measure the EE power spectrum over the angular multipole range 500 ≤ ℓ < 3000, tracing the third to seventh acoustic peaks with high sensitivity. The statistical uncertainty on E-mode bandpowers is ∼2.3 μK2 at ℓ ∼ 1000, with a systematic uncertainty of 0.5 mK2. The data are consistent with the standard ΛCDM cosmological model with a probability-to-exceed of 0.38. We combine recent CMB E-mode measurements and make inferences about cosmological parameters in ΛCDM as well as in extensions to ΛCDM. Adding the ground-based CMB polarization measurements to the Planck data set reduces the uncertainty on the Hubble constant by a factor of 1.2 to H0 = 67.20 ±0.57 km s- Mpc- 1 1. When allowing the number of relativistic species (Neff ) to vary, we find Neff = 2.94 ±0.16, which is in good agreement with the standard value of 3.046. Instead allowing the primordial helium abundance (YHe) to vary, the data favor YHe = 0.248 ±0.012. This is very close to the expectation of 0.2467 from big bang nucleosynthesis. When varying both YHe and Neff , we find Neff = 2.70 ±0.26 and YHe = 0.262 ±0.015.
Published: 2020

10. A Measurement of the Degree Scale CMB B-mode Angular Power Spectrum with POLARBEAR

Author: Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Goeckner-Wald, N., Groh, J., Hall, G., Halverson, N., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Howe, L., Inoue, Y., Jaehnig, G., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kikuchi, S., Kisner, T., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Mangu, A., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Segawa, Y., Silva-Feaver, M., Siritanasak, P., Stebor, N., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tsai, C., Verges, C., Westbrook, B., and Zhou, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a measurement of the $B$-mode polarization power spectrum of the cosmic microwave background (CMB) using taken from July 2014 to December 2016 with the POLARBEAR experiment. The CMB power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of $\mathrm{NET}_\mathrm{array}=23\, \mu \mathrm{K} \sqrt{\mathrm{s}}$ on a 670 square degree patch of sky centered at (RA, Dec)=($+0^\mathrm{h}12^\mathrm{m}0^\mathrm{s},-59^\circ18^\prime$). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve $32\,\mu\mathrm{K}$-$\mathrm{arcmin}$ effective polarization map noise with a knee in sensitivity of $\ell = 90$, where the inflationary gravitational wave signal is expected to peak. The measured $B$-mode power spectrum is consistent with a $\Lambda$CDM lensing and single dust component foreground model over a range of multipoles $50 \leq \ell \leq 600$. The data disfavor zero $C_\ell^{BB}$ at $2.2\sigma$ using this $\ell$ range of POLARBEAR data alone. We cross-correlate our data with Planck high frequency maps and find the low-$\ell$ $B$-mode power in the combined dataset to be consistent with thermal dust emission. We place an upper limit on the tensor-to-scalar ratio $r < 0.90$ at 95% confidence level after marginalizing over foregrounds.
Published: 2019
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11. Cross-correlation of POLARBEAR CMB Polarization Lensing with High-$z$ Sub-mm Herschel-ATLAS galaxies

Author: Faundez, M. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Cheung, K., Chinone, Y., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Galitzki, N., Goeckner-Wald, N., Hasegawa, M., Hazumi, M., Howe, L., Kaneko, D., Katayama, N., Keating, B., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Sherwin, B. D., Silva-Feaver, M., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Teply, G. P., Tsai, C., and Verges, C.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We report a 4.8$\sigma$ measurement of the cross-correlation signal between the cosmic microwave background (CMB) lensing convergence reconstructed from measurements of the CMB polarization made by the POLARBEAR experiment and the infrared-selected galaxies of the Herschel-ATLAS survey. This is the first measurement of its kind. We infer a best-fit galaxy bias of $b = 5.76 \pm 1.25$, corresponding to a host halo mass of $\log_{10}(M_h/M_\odot) =13.5^{+0.2}_{-0.3}$ at an effective redshift of $z \sim 2$ from the cross-correlation power spectrum. Residual uncertainties in the redshift distribution of the sub-mm galaxies are subdominant with respect to the statistical precision. We perform a suite of systematic tests, finding that instrumental and astrophysical contaminations are small compared to the statistical error. This cross-correlation measurement only relies on CMB polarization information that, differently from CMB temperature maps, is less contaminated by galactic and extra-galactic foregrounds, providing a clearer view of the projected matter distribution. This result demonstrates the feasibility and robustness of this approach for future high-sensitivity CMB polarization experiments., Comment: 14 pages, 6 figures, updated to match published version on ApJ
Published: 2019
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12. A Measurement of the Degree-scale CMB B-mode Angular Power Spectrum with Polarbear

Author: Adachi, S, Aguilar Faúndez, MAO, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Bouhargani, HE, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, GP, Tsai, C, Verges, C, Westbrook, B, and Zhou, Y
Subjects: Cosmic microwave background radiation, Cosmic inflation, Cosmology, Observational cosmology, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Astronomy & Astrophysics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: We present a measurement of the B-mode polarization power spectrum of the cosmic microwave background (CMB) using data taken from 2014 July to 2016 December with the Polarbear experiment. The CMB power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of NETarray=23μ K√s on a 670 square degree patch of sky centered at (R.A., decl.) = (+0h12m0s, -59°18′). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve 32 μK arcmin effective polarization map noise with a knee in sensitivity of ℓ = 90, where the inflationary gravitational-wave signal is expected to peak. The measured B-mode power spectrum is consistent with a ΛCDM lensing and single dust component foreground model over a range of multipoles 50 ≤ ℓ ≤ 600. The data disfavor zero CℓBB at 2.2σ using this ℓ range of Polarbear data alone. We cross-correlate our data with Planck full mission 143, 217, and 353 GHz frequency maps and find the low-ℓ B-mode power in the combined data set to be consistent with thermal dust emission. We place an upper limit on the tensor-to-scalar ratio r < 0.90 at the 95% confidence level after marginalizing over foregrounds.
Published: 2020

13. Cross-correlation of CMB Polarization Lensing with High-z Submillimeter Herschel-ATLAS Galaxies

Author: Faúndez, M Aguilar, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Cheung, K, Chinone, Y, Bouhargani, H El, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Galitzki, N, Goeckner-Wald, N, Hasegawa, M, Hazumi, M, Howe, L, Kaneko, D, Katayama, N, Keating, B, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, LN, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Sherwin, BD, Silva-Feaver, M, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Teply, GP, Tsai, C, and Vergès, C
Subjects: Particle and High Energy Physics, Physical Sciences, astro-ph.CO, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We report a 4.8σ measurement of the cross-correlation signal between the cosmic microwave background (CMB) lensing convergence reconstructed from measurements of the CMB polarization made by the Polarbear experiment and the infrared-selected galaxies of the Herschel-ATLAS survey. This is the first measurement of its kind. We infer a best-fit galaxy bias of b=5.76\pm 1.25, corresponding to a host halo mass log10(Mh M⊙. =13.5+0.2-0.3 of at an effective redshift of z ∼ 2 from the cross-correlation power spectrum. Residual uncertainties in the redshift distribution of the submillimeter galaxies are subdominant with respect to the statistical precision. We perform a suite of systematic tests, finding that instrumental and astrophysical contaminations are small compared to the statistical error. This cross-correlation measurement only relies on CMB polarization information that, differently from CMB temperature maps, is less contaminated by galactic and extragalactic foregrounds, providing a clearer view of the projected matter distribution. This result demonstrates the feasibility and robustness of this approach for future high-sensitivity CMB polarization experiments.
Published: 2019

14. Design and characterization of a ground-based absolute polarization calibrator for use with polarization sensitive CMB experiments

Author: Navaroli, M. F., Teply, G. P., Crowley, K. D., Kaufman, J. P., Galitzki, N. B., Arnold, K. S., and Keating, B. G.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present the design and characterization of a ground-based absolute polarization angle calibrator accurate to better than 0.1 degrees for use with polarization sensitive cosmic microwave background (CMB) experiments. The calibrator's accuracy requirement is driven by the need to reduce upper limits on cosmic polarization rotation, which is expected to be zero in a large class of cosmological models. Cosmic polarization effects such as cosmic birefringence and primordial magnetic fields can generate spurious B-modes that result in non-zero CMB TB and EB correlations that are degenerate with a misalignment of detector orientation. Common polarized astrophysical sources used for absolute polarization angle calibration have not been characterized to better than 0.5 degrees. Higher accuracy can be achieved through self-calibration methods, however these are subject to astrophysical foreground contamination and inherently assume the absence of effects like cosmic polarization rotation. The deficiencies in these two calibration methods highlight the need for a well characterized polarized source. The calibrator we present utilizes a 76 GHz Gunn oscillator coupled to a frequency doubler, pyramidal horn antenna, and co-rotating wire-grid polarizer. We use an accurate bubble level in combination with four precision-grade aluminum planes located within the enclosure to calibrate the source's linear polarization plane with respect to the local gravity vector to better than the 0.1 degree goal. In 2017 the calibrator was deployed for an engineering test run on the POLARBEAR CMB experiment located in Chile's Atacama Desert and is being upgraded for calibration of the POLARBEAR-2b receiver in 2018. In the following work we present a detailed overview of the calibrator design, systematic control, characterization, deployment, and plans for future CMB experiment absolute polarization calibration., Comment: 15 pages, 7 figures, 2 tables, SPIE conference Austin 2018
Published: 2018
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15. Cold optical design for the Large Aperture Simons Observatory telescope

Author: Dicker, S. R., Gallardo, P. A., Gudmundsson, J. E, Mauskopf, P. D., Ali, A., Ashton, P. C., Coppi, G., Devlin, M. J., Galitzki, N., Ho, S. P., Hill, C. A., Hubmayr, J., Keating, B., Lee, A. T., Limon, M., Matsuda, F., McMahon, J., Niemack, M. D., Orlowski-Scherer, J. L., Piccirillo, L., Salatino, M., Simon, S. M., Staggs, S. T., Thornton, R., Ullom, J. N., Vavagiakis, E. M., Wollack, E. J., Xu, Z., and Zhu, N.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Simons Observatory will consist of a single large (6 m diameter) telescope and a number of smaller (0.5 m diameter) refracting telescopes designed to measure the polarization of the Cosmic Microwave Background to unprecedented accuracy. The large aperture telescope is the same design as the CCAT-prime telescope, a modified Crossed Dragone design with a field-of-view of over 7.8 degrees diameter at 90 GHz. This paper presents an overview of the cold reimaging optics for this telescope and what drove our choice of 350-400 mm diameter silicon lenses in a 2.4 m cryostat over other possibilities. We will also consider the future expandability of this design to CMB Stage-4 and beyond.
Published: 2018

16. Evidence for the Cross-correlation between Cosmic Microwave Background Polarization Lensing from Polarbear and Cosmic Shear from Subaru Hyper Suprime-Cam

Author: Namikawa, T, Chinone, Y, Miyatake, H, Oguri, M, Takahashi, R, Kusaka, A, Katayama, N, Adachi, S, Aguilar, M, Aihara, H, Ali, A, Armstrong, R, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Cheung, K, Corbett, L, Crowley, KT, Bouhargani, H El, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Galitzki, N, Goeckner-Wald, N, Groh, J, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Jeong, O, Kaneko, D, Keating, B, Lee, AT, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Minami, Y, Miyazaki, S, Murayama, H, Navaroli, M, Nishino, H, Nishizawa, AJ, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Speagle, JS, Stompor, R, Suzuki, A, Tait, PJ, Tajima, O, Takada, M, Takakura, S, Takatori, S, Tanabe, D, Tanaka, M, Teply, GP, Tsai, C, Vergés, C, Westbrook, B, and Zhou, Y
Subjects: Particle and High Energy Physics, Physical Sciences, cosmic background radiation, cosmology: observations, gravitational lensing: weak, polarization, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We present the first measurement of cross-correlation between the lensing potential, reconstructed from cosmic microwave background (CMB) polarization data, and the cosmic shear field from galaxy shapes. This measurement is made using data from the Polarbear CMB experiment and the Subaru Hyper Suprime-Cam (HSC) survey. By analyzing an 11 deg2 overlapping region, we reject the null hypothesis at 3.5σ and constrain the amplitude of the cross-spectrum to , where is the amplitude normalized with respect to the Planck 2018 prediction, based on the flat Λ cold dark matter cosmology. The first measurement of this cross-spectrum without relying on CMB temperature measurements is possible owing to the deep Polarbear map with a noise level of ∼6 μK arcmin, as well as the deep HSC data with a high galaxy number density of . We present a detailed study of the systematics budget to show that residual systematics in our results are negligibly small, which demonstrates the future potential of this cross-correlation technique.
Published: 2019

17. The Simons Observatory: Science goals and forecasts

Author: Ade, P, Aguirre, J, Ahmed, Z, Aiola, S, Ali, A, Alonso, D, Alvarez, MA, Arnold, K, Ashton, P, Austermann, J, Awan, H, Baccigalupi, C, Baildon, T, Barron, D, Battaglia, N, Battye, R, Baxter, E, Bazarko, A, Beall, JA, Bean, R, Beck, D, Beckman, S, Beringue, B, Bianchini, F, Boada, S, Boettger, D, Bond, JR, Borrill, J, Brown, ML, Bruno, SM, Bryan, S, Calabrese, E, Calafut, V, Calisse, P, Carron, J, Challinor, A, Chesmore, G, Chinone, Y, Chluba, J, Cho, HMS, Choi, S, Coppi, G, Cothard, NF, Coughlin, K, Crichton, D, Crowley, KD, Crowley, KT, Cukierman, A, D'Ewart, JM, Dünner, R, De Haan, T, Devlin, M, Dicker, S, Didier, J, Dobbs, M, Dober, B, Duell, CJ, Duff, S, Duivenvoorden, A, Dunkley, J, Dusatko, J, Errard, J, Fabbian, G, Feeney, S, Ferraro, S, Fluxà, P, Freese, K, Frisch, JC, Frolov, A, Fuller, G, Fuzia, B, Galitzki, N, Gallardo, PA, Ghersi, JTG, Gao, J, Gawiser, E, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Golec, J, Gordon, S, Gralla, M, Green, D, Grigorian, A, Groh, J, Groppi, C, Guan, Y, Gudmundsson, JE, Han, D, Hargrave, P, Hasegawa, M, Hasselfield, M, Hattori, M, Haynes, V, Hazumi, M, He, Y, Healy, E, Henderson, SW, Hervias-Caimapo, C, and Hill, CA
Subjects: CMBR experiments, CMBR polarisation, cosmological parameters from CMBR, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract: The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping 10% of the sky to a white noise level of 2 μK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r)=0.003. The large aperture telescope will map 40% of the sky at arcminute angular resolution to an expected white noise level of 6 μK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources.
Published: 2019

18. The POLARBEAR-2 and Simons Array Focal Plane Fabrication Status

Author: Westbrook, B, Ade, PAR, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bender, AN, Bianchini, F, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Coppi, G, Crowley, K, Cukierman, A, de Haan, T, Dünner, R, Dobbs, M, Elleflot, T, Errard, J, Fabbian, G, Feeney, SM, Feng, C, Fuller, G, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Halverson, NW, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Holzapfel, W, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Kusaka, A, Le Jeune, M, Lee, AT, Leon, D, Linder, E, Lowry, L, Madurowicz, A, Mak, D, Matsuda, F, May, A, Miller, NJ, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Piccirillo, L, Plambeck, D, Poletti, D, Puglisi, G, Raum, C, Rebeiz, G, Reichardt, CL, Richards, PL, Roberts, H, Ross, C, Rotermund, KM, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Tat, R, Teply, GP, Tikhomirov, A, Tomaru, T, Tsai, C, Whitehorn, N, and Zahn, A
Subjects: Physical Sciences, Classical Physics, Condensed Matter Physics, CMB, Fabrication, Instrumentation, Detectors, Transition edge sensor, Sinuous antenna, Polarization, Inflation, Mathematical Physics, General Physics, Classical physics, Condensed matter physics
Abstract: We present on the status of POLARBEAR-2 A (PB2-A) focal plane fabrication. The PB2-A is the first of three telescopes in the Simons Array, which is an array of three cosmic microwave background polarization-sensitive telescopes located at the POLARBEAR site in Northern Chile. As the successor to the PB experiment, each telescope and receiver combination is named as PB2-A, PB2-B, and PB2-C. PB2-A and -B will have nearly identical receivers operating at 90 and 150 GHz while PB2-C will house a receiver operating at 220 and 270 GHz. Each receiver contains a focal plane consisting of seven close-hex packed lenslet-coupled sinuous antenna transition edge sensor bolometer arrays. Each array contains 271 dichroic optical pixels, each of which has four TES bolometers for a total of 7588 detectors per receiver. We have produced a set of two types of candidate arrays for PB2-A. The first we call Version 11 (V11) uses a silicon oxide (SiOx) for the transmission lines and crossover process for orthogonal polarizations. The second we call Version 13 (V13) uses silicon nitride (SiNx) for the transmission lines and cross-under process for orthogonal polarizations. We have produced enough of each type of array to fully populate the focal plane of the PB2-A receiver. The average wirebond yield for V11 and V13 arrays is 93.2% and 95.6%, respectively. The V11 arrays had a superconducting transition temperature (Tc) of 452±15 mK, a normal resistance (Rn) of 1.25±0.20Ω, and saturation powers of 5.2 ± 1.0 pW and 13 ± 1.2 pW for the 90 and 150 GHz bands, respectively. The V13 arrays had a superconducting transition temperature (Tc) of 456 ± 6 mK, a normal resistance (Rn) of 1.1±0.2Ω, and saturation powers of 10.8 ± 1.8 pW and 22.9 ± 2.6 pW for the 90 and 150 GHz bands, respectively. Production and characterization of arrays for PB2-B are ongoing and are expected to be completed by the summer of 2018. We have fabricated the first three candidate arrays for PB2-C but do not have any characterization results to present at this time.
Published: 2018

19. A Measurement of the Cosmic Microwave Background $B$-Mode Polarization Power Spectrum at Sub-Degree Scales from 2 years of POLARBEAR Data

Author: The POLARBEAR Collaboration, Ade, P. A. R., Aguilar, M., Akiba, Y., Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., Ducout, A., Dünner, R., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fujino, T., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Hamada, T., Hall, G., Halverson, N. W., Hasegawa, M., Hazumi, M., Hill, C., Howe, L., Inoue, Y., Jaehnig, G. C., Jaffe, A. H., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kisner, T., Krachmalnicoff, N., Kusaka, A., Jeune, M. Le, Lee, A. T., Leitch, E. M., Leon, D., Linder, E., Lowry, L., Matsuda, F., Matsumura, T., Minami, Y., Montgomery, J., Navaroli, M., Nishino, H., Paar, H., Peloton, J., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Richards, P. L., Ross, C., Segawa, Y., Sherwin, B. D., Silva-Feaver, M., Siritanasak, P., Stebor, N., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tomaru, T., Tucker, C., Whitehorn, N., and Zahn, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report an improved measurement of the cosmic microwave background (CMB) $B$-mode polarization power spectrum with the POLARBEAR experiment at 150 GHz. By adding new data collected during the second season of observations (2013-2014) to re-analyzed data from the first season (2012-2013), we have reduced twofold the band-power uncertainties. The band powers are reported over angular multipoles $500 \leq \ell \leq 2100$, where the dominant $B$-mode signal is expected to be due to the gravitational lensing of $E$-modes. We reject the null hypothesis of no $B$-mode polarization at a confidence of 3.1$\sigma$ including both statistical and systematic uncertainties. We test the consistency of the measured $B$-modes with the $\Lambda$ Cold Dark Matter ($\Lambda$CDM) framework by fitting for a single lensing amplitude parameter $A_L$ relative to the Planck best-fit model prediction. We obtain $A_L = 0.60 ^{+0.26} _{-0.24} ({\rm stat}) ^{+0.00} _{-0.04}({\rm inst}) \pm 0.14 ({\rm foreground}) \pm 0.04 ({\rm multi})$, where $A_{L}=1$ is the fiducial $\Lambda$CDM value, and the details of the reported uncertainties are explained later in the manuscript., Comment: 16 pages, 10 figures. Minor changes to match the published version. For data and figures, see http://bolo.berkeley.edu/polarbear/data/polarbear_BB_2017/
Published: 2017
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20. On the relation between the column density structures and the magnetic field orientation in the Vela C molecular complex

Author: Soler, J. D., Ade, P. A. R., Angilè, F. E., Ashton, P., Benton, S. J., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Galitzki, N., Gandilo, N. N., Hennebelle, P., Klein, J., Li, Z. -Y., Korotkov, A. L., Martin, P. G., Matthews, T. G., Moncelsi, L., Netterfield, C. B., Novak, G., Pascale, E., Poidevin, F., Santos, F. P., Savini, G., Scott, D., Shariff, J. A., Thomas, N. E., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We statistically evaluate the relative orientation between gas column density structures, inferred from Herschel submillimetre observations, and the magnetic field projected on the plane of sky, inferred from polarized thermal emission of Galactic dust observed by BLASTPol at 250, 350, and 500 micron, towards the Vela C molecular complex. First, we find very good agreement between the polarization orientations in the three wavelength-bands, suggesting that, at the considered common angular resolution of 3.0 arcminutes that corresponds to a physical scale of approximately 0.61 pc, the inferred magnetic field orientation is not significantly affected by temperature or dust grain alignment effects. Second, we find that the relative orientation between gas column density structures and the magnetic field changes progressively with increasing gas column density, from mostly parallel or having no preferred orientation at low column densities to mostly perpendicular at the highest column densities. This observation is in agreement with previous studies by the Planck collaboration towards more nearby molecular clouds. Finally, we find a correspondence between the trends in relative orientation and the shape of the column density probability distribution functions. In the sub-regions of Vela C dominated by one clear filamentary structure, or "ridges", we find a sharp transition from preferentially parallel or having no preferred relative orientation at low column densities to preferentially perpendicular at highest column densities. In the sub-regions of Vela C dominated by several filamentary structures with multiple orientations, or "nests", such a transition is also present, but it is clearly less sharp than in the ridge-like sub-regions. Both of these results suggest that the magnetic field is dynamically important for the formation of density structures in this region., Comment: 16 pages, 17 figures. Submitted to A&A
Published: 2017
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21. Optical Demonstration of THz, Dual-Polarization Sensitive Microwave Kinetic Inductance Detectors

Author: Dober, B., Austermann, J. A., Beall, J. A., Becker, D., Che, G., Cho, H. M., Devlin, M., Duff, S. M., Galitzki, N., Gao, J., Groppi, C., Hilton, G. C., Hubmayr, J., Irwin, K. D., McKenney, C. M., Li, D., Lourie, N., Mauskopf, P., Vissers, M. R., and Wang, Y.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The next generation BLAST experiment (BLAST-TNG) is a suborbital balloon payload that seeks to map polarized dust emission in the 250 $\mu$m, 350 $\mu$m and 500 $\mu$m wavebands. The instrument utilizes a stepped half-wave plate to reduce systematics. The general requirement of the detectors is that they are photon-noise-limited and dual-polarization sensitive. To achieve this goal, we are developing three monolithic arrays of cryogenic sensors, one for each waveband. Each array is feedhorn-coupled and each spatial pixel consists of two orthogonally spaced polarization-sensitive microwave kinetic inductance detectors (MKIDs) fabricated from a Ti/TiN multilayer film. In previous work, we demonstrated photon-noise-limited sensitivity in 250 $\mu$m waveband single polarization devices. In this work, we present the first results of dual-polarization sensitive MKIDs at 250 $\mu$m., Comment: 7 pages, 4 figures, published by JLTP
Published: 2016
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22. A Measurement of the Cosmic Microwave Background B-mode Polarization Power Spectrum at Subdegree Scales from Two Years of POLARBEAR Data

Author: Ade, PAR, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Bianchini, F, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, SM, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, JC, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, AH, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Kusaka, A, Le Jeune, M, Lee, AT, Leitch, EM, Leon, D, Linder, E, Lowry, L, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Richards, PL, Ross, C, Segawa, Y, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, GP, Tomaru, T, Tucker, C, Whitehorn, N, and Zahn, A
Subjects: cosmic background radiation, cosmology: observations, large-scale structure of universe
Published: 2017

23. Performance of a continuously rotating half-wave plate on the POLARBEAR telescope

Author: Takakura, S, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beckman, S, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Cukierman, A, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Fujino, T, Galitzki, N, Goeckner-Wald, N, Halverson, NW, Hasegawa, M, Hattori, K, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaffe, AH, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leon, D, Lowry, L, Matsuda, F, Matsumura, T, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Poletti, D, Puglisi, G, Reichardt, CL, Ross, C, Siritanasak, P, Suzuki, A, Tajima, O, Takatori, S, and Teply, G
Subjects: CMBR experiments, gravitational waves and CMBR polarization, astro-ph.IM, astro-ph.CO, physics.ins-det, Nuclear & Particles Physics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract: A continuously rotating half-wave plate (CRHWP) is a promising tool to improve the sensitivity to large angular scales in cosmic microwave background (CMB) polarization measurements. With a CRHWP, single detectors can measure three of the Stokes parameters, I, Q and U, thereby avoiding the set of systematic errors that can be introduced by mismatches in the properties of orthogonal detector pairs. We focus on the implementation of CRHWPs in large aperture telescopes (i.e. the primary mirror is larger than the current maximum half-wave plate diameter of ∼0.5 m), where the CRHWP can be placed between the primary mirror and focal plane. In this configuration, one needs to address the intensity to polarization (I→P) leakage of the optics, which becomes a source of 1/f noise and also causes differential gain systematics that arise from CMB temperature fluctuations. In this paper, we present the performance of a CRHWP installed in the {\scshape Polarbear} experiment, which employs a Gregorian telescope with a 2.5 m primary illumination pattern. The CRHWP is placed near the prime focus between the primary and secondary mirrors. We find that the I→P leakage is larger than the expectation from the physical properties of our primary mirror, resulting in a 1/f knee of 100 mHz. The excess leakage could be due to imperfections in the detector system, i.e. detector non-linearity in the responsivity and time-constant. We demonstrate, however, that by subtracting the leakage correlated with the intensity signal, the 1/f noise knee frequency is reduced to 32 mHz (ℓ ∼ 39 for our scan strategy), which is very promising to probe the primordial B-mode signal. We also discuss methods for further noise subtraction in future projects where the precise temperature control of instrumental components and the leakage reduction will play a key role.
Published: 2017

24. The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry-BLASTPol: Performance and results from the 2012 Antarctic flight

Author: Galitzki, N., Ade, P. A. R., Angilé, F. E., Benton, S. J., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Gandilo, N. N., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, L., Netterfield, C. B., Novak, G., Nutter, D., Pascale, E., Poidevin, F., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) is a suborbital mapping experiment, designed to study the role played by magnetic fields in the star formation process. BLASTPol observes polarized light using a total power instrument, photolithographic polarizing grids, and an achromatic half-wave plate to modulate the polarization signal. During its second flight from Antarctica in December 2012, BLASTPol made degree scale maps of linearly polarized dust emission from molecular clouds in three wavebands, centered at 250, 350, and 500 microns. The instrumental performance was an improvement over the 2010 BLASTPol flight, with decreased systematics resulting in a higher number of confirmed polarization vectors. The resultant dataset allows BLASTPol to trace magnetic fields in star-forming regions at scales ranging from cores to entire molecular cloud complexes., Comment: Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014
Published: 2014
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25. Thermal design and performance of the balloon-borne large aperture submillimeter telescope for polarimetry BLASTPol

Author: Soler, J. D., Ade, P. A. R., Angilè, F. E., Benton, S. J., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Galitzki, N., Gandilo, N. N., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, L., Mroczkowski, A., Netterfield, C. B., Novak, G., Nutter, D., Pascale, E., Poidevin, F., Savini, G., Scott, D., Shariff, J. A., Thomas, N. E., Truch, M. D., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present the thermal model of the Balloon-borne Large-Aperture Submillimeter Telescope for Polarimetry (BLASTPol). This instrument was successfully flown in two circumpolar flights from McMurdo, Antarctica in 2010 and 2012. During these two flights, BLASTPol obtained unprecedented information about the magnetic field in molecular clouds through the measurement of the polarized thermal emission of interstellar dust grains. The thermal design of the experiment addresses the stability and control of the payload necessary for this kind of measurement. We describe the thermal modeling of the payload including the sun-shielding strategy. We present the in-flight thermal performance of the instrument and compare the predictions of the model with the temperatures registered during the flight. We describe the difficulties of modeling the thermal behavior of the balloon-borne platform and establish landmarks that can be used in the design of future balloon-borne instruments., Comment: 18 pages, 11 figures. Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145
Published: 2014
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26. BLASTbus electronics: general-purpose readout and control for balloon-borne experiments

Author: Benton, S. J., Ade, P. A., Amiri, M., Angilè, F. E., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, H. C., Contaldi, C. R., Crill, B. P., Devlin, M. J., Dober, B., Doré, O. P., Dowell, C. D., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Fukui, Y., Galitzki, N., Gambrel, A. E., Gandilo, N. N., Golwala, S. R., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. D., Klein, J., Korotkov, A. L., Kuo, C. L., MacTavish, C. J., Mason, P. V., Matthews, T. G., Megerian, K. G., Moncelsi, L., Morford, T. A., Mroczkowski, T. K., Nagy, J. M., Netterfield, C. B., Novak, G., Nutter, D., O'Brient, R., Ogburn IV, R. W., Pascale, E., Poidevin, F., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Thomas, N. E., Trangsrud, A., Truch, M. D., Tucker, C. E., Tucker, G. S., Tucker, R. S., Turner, A. D., Ward-Thompson, D., Weber, A. C., Wiebe, D. V., and Young, E. Y.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present the second generation BLASTbus electronics. The primary purposes of this system are detector readout, attitude control, and cryogenic housekeeping, for balloon-borne telescopes. Readout of neutron transmutation doped germanium (NTD-Ge) bolometers requires low noise and parallel acquisition of hundreds of analog signals. Controlling a telescope's attitude requires the capability to interface to a wide variety of sensors and motors, and to use them together in a fast, closed loop. To achieve these different goals, the BLASTbus system employs a flexible motherboard-daughterboard architecture. The programmable motherboard features a digital signal processor (DSP) and field-programmable gate array (FPGA), as well as slots for three daughterboards. The daughterboards provide the interface to the outside world, with versions for analog to digital conversion, and optoisolated digital input/output. With the versatility afforded by this design, the BLASTbus also finds uses in cryogenic, thermometry, and power systems. For accurate timing control to tie everything together, the system operates in a fully synchronous manner. BLASTbus electronics have been successfully deployed to the South Pole, and flown on stratospheric balloons., Comment: Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145
Published: 2014
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27. Attitude determination for balloon-borne experiments

Author: Gandilo, N. N., Ade, P. A. R., Amiri, M., Angile, F. E., Benton, S. J., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, H. C., Contaldi, C. R., Crill, B. P., Devlin, M. J., Dober, B., Dore, O. P., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Fukui, Y., Galitzki, N., Gambrel, A. E., Golwala, S., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. D., Klein, J., Korotkov, A. L., Kuo, C. L., MacTavish, C. J., Mason, P. V., Matthews, T. G., Megerian, K. G., Moncelsi, L., Morford, T. A., Mroczkowski, T. K., Nagy, J. M., Netterfield, C. B., Novak, G., Nutter, D., O'Brient, R., Pascale, E., Poidevin, F., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Thomas, N. E., Trangsrud, A., Truch, M. D., Tucker, C. E., Tucker, G. S., Tucker, R. S., Turner, A. D., Ward-Thompson, D., Weber, A. C., Wiebe, D. V., and Young, E. Y.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: An attitude determination system for balloon-borne experiments is presented. The system provides pointing information in azimuth and elevation for instruments flying on stratospheric balloons over Antarctica. In-flight attitude is given by the real-time combination of readings from star cameras, a magnetometer, sun sensors, GPS, gyroscopes, tilt sensors and an elevation encoder. Post-flight attitude reconstruction is determined from star camera solutions, interpolated by the gyroscopes using an extended Kalman Filter. The multi-sensor system was employed by the Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol), an experiment that measures polarized thermal emission from interstellar dust clouds. A similar system was designed for the upcoming flight of SPIDER, a Cosmic Microwave Background polarization experiment. The pointing requirements for these experiments are discussed, as well as the challenges in designing attitude reconstruction systems for high altitude balloon flights. In the 2010 and 2012 BLASTPol flights from McMurdo Station, Antarctica, the system demonstrated an accuracy of <5' rms in-flight, and <5" rms post-flight., Comment: 16 pages, 10 figures, Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145
Published: 2014
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28. Deployment of Polarbear-2A

Author: Kaneko, Daisuke, Adachi, S., Ade, P. A. R., Aguilar Faúndez, M., Akiba, Y., Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., Dűnner, R., El-Bouhargani, H., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fujino, T., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Hall, G., Halverson, N. W., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Howe, L., Inoue, Y., Jaehnig, G., Jeong, O., Katayama, N., Keating, B., Keskitalo, R., Kikuchi, S., Kisner, T., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Mangu, A., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Peloton, J., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Ross, C., Segawa, Y., Silva-Feaver, M., Siritanasak, P., Stebor, N., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tomaru, T., Tsai, C., Verges, C., Westbrook, B., and Zhou, Y.
Published: 2020
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29. The Simons Observatory: A large-diameter truss for a refracting telescope cooled to 1 K

Author: Crowley, K, Dow, P, Shroyer, J, Groh, J, Dober, B, Spisak, J, Galitzki, N, Bhandarkar, T, Devlin, M, Dicker, S, Gallardo, P, Harrington, K, Iuliano, J, Johnson, B, Johnson, D, Kofman, A, Kusaka, A, Lee, A, Limon, M, Nati, F, Orlowski-Scherer, J, Page, L, Randall, M, Teply, G, Tsan, T, Wollack, E, Xu, Z, Zhu, N, Crowley K. D., Dow P., Shroyer J. E., Groh J. C., Dober B., Spisak J., Galitzki N., Bhandarkar T., Devlin M. J., Dicker S., Gallardo P. A., Harrington K., Iuliano J., Johnson B. R., Johnson D., Kofman A. M., Kusaka A., Lee A., Limon M., Nati F., Orlowski-Scherer J., Page L., Randall M., Teply G., Tsan T., Wollack E. J., Xu Z., Zhu N., Crowley, K, Dow, P, Shroyer, J, Groh, J, Dober, B, Spisak, J, Galitzki, N, Bhandarkar, T, Devlin, M, Dicker, S, Gallardo, P, Harrington, K, Iuliano, J, Johnson, B, Johnson, D, Kofman, A, Kusaka, A, Lee, A, Limon, M, Nati, F, Orlowski-Scherer, J, Page, L, Randall, M, Teply, G, Tsan, T, Wollack, E, Xu, Z, Zhu, N, Crowley K. D., Dow P., Shroyer J. E., Groh J. C., Dober B., Spisak J., Galitzki N., Bhandarkar T., Devlin M. J., Dicker S., Gallardo P. A., Harrington K., Iuliano J., Johnson B. R., Johnson D., Kofman A. M., Kusaka A., Lee A., Limon M., Nati F., Orlowski-Scherer J., Page L., Randall M., Teply G., Tsan T., Wollack E. J., Xu Z., and Zhu N.
Abstract: We present the design and measured performance of a new carbon fiber strut design that is used in a cryogenically cooled truss for the Simons Observatory small aperture telescope. The truss consists of two aluminum 6061 rings separated by 24 struts. Each strut consists of a central carbon fiber tube fitted with two aluminum end caps. We tested the performance of the strut and truss by (i) cryogenically cycling and destructively pull-Testing strut samples, (ii) non-destructively pull-Testing the final truss, and (iii) measuring the thermal conductivity of the carbon fiber tubes. We found that the strut strength is limited by the mounting fasteners and the strut end caps, not the epoxy adhesive or the carbon fiber tube. This result is consistent with our numerical predictions. Our thermal measurements suggest that the conductive heat load through the struts (from 4 to 1 K) will be less than 1 mW. This strut design may be a promising candidate for use in other cryogenic support structures.
Published: 2022

30. Protocalc: an artificial calibrator source for cmb telescopes

Author: Zmuidzinas, J, Gao, JR, Coppi, G, Conenna, G, Savorgnano, S, Carrero, F, Dunner Planella, R, Galitzki, N, Nati, F, Zannoni, M, Coppi G., Conenna G., Savorgnano S., Carrero F., Dunner Planella R., Galitzki N., Nati F., Zannoni M., Zmuidzinas, J, Gao, JR, Coppi, G, Conenna, G, Savorgnano, S, Carrero, F, Dunner Planella, R, Galitzki, N, Nati, F, Zannoni, M, Coppi G., Conenna G., Savorgnano S., Carrero F., Dunner Planella R., Galitzki N., Nati F., and Zannoni M.
Abstract: Cosmic Microwave Background experiments need to measure polarization properties of the incoming radiation very accurately to achieve their scientific goals. As a result of that, it is necessary to properly characterize these instruments. However, there are not natural sources that can be used for this purpose. For this reason, we developed the PROTOtype CALibrator for Cosmology, PROTOCALC, which is a calibrator source designed for the 90 GHz band of these telescopes. This source is purely polarized and the direction of the polarization vector is known with an accuracy better than 0.1°. This source flew for the first time in May 2022 showing promising result.
Published: 2022

31. PROTOCALC: an artificial calibrator source for CMB telescopes

Author: Coppi G., Conenna G., Savorgnano S., Carrero F., Dunner Planella R., Galitzki N., Nati F., Zannoni M., Zmuidzinas, J, Gao, JR, Coppi, G, Conenna, G, Savorgnano, S, Carrero, F, Dunner Planella, R, Galitzki, N, Nati, F, and Zannoni, M
Subjects: FIS/05 - ASTRONOMIA E ASTROFISICA, Polarization, Calibration, Cosmic Microwave Background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: Cosmic Microwave Background experiments need to measure polarization properties of the incoming radiation very accurately to achieve their scientific goals. As a result of that, it is necessary to properly characterize these instruments. However, there are not natural sources that can be used for this purpose. For this reason, we developed the PROTOtype CALibrator for Cosmology, PROTOCALC, which is a calibrator source designed for the 90GHz band of these telescopes. This source is purely polarized and the direction of the polarization vector is known with an accuracy better than 0.1deg. This source flew for the first time in May 2022 showing promising result, Presented at SPIE Astronomical Telescopes + Instrumentation 2022
Published: 2022

32. Erratum: The Simons Observatory Large Aperture Telescope Receiver (ApJS (2021) 256: 23 DOI: 10.3847/1538-4365/ac0db7)

Author: Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., Zannoni M., Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., and Zannoni M.
Abstract: After the publication of the article, it was brought to our attention that the description of Equation (1) may cause potential confusion. Thus, we have decided to provide a newer reference and added a unit for qtot in the description. The updated paragraph should read as the following:.
Published: 2021

33. The effects of inclination on a two stage pulse tube cryocooler for use with a ground based observatory

Author: Tsan, T, Galitzki, N, Ali, A, Arnold, K, Coppi, G, Ervin, T, Foote, L, Keating, B, Lashner, J, Orlowski-Scherer, J, Randall, M, Seibert, J, Spisak, J, Teply, G, Xu, Z, Zhu, N, Tsan T., Galitzki N., Ali A. M., Arnold K., Coppi G., Ervin T., Foote L., Keating B., Lashner J., Orlowski-Scherer J., Randall M. J., Seibert J., Spisak J., Teply G. P., Xu Z., Zhu N., Tsan, T, Galitzki, N, Ali, A, Arnold, K, Coppi, G, Ervin, T, Foote, L, Keating, B, Lashner, J, Orlowski-Scherer, J, Randall, M, Seibert, J, Spisak, J, Teply, G, Xu, Z, Zhu, N, Tsan T., Galitzki N., Ali A. M., Arnold K., Coppi G., Ervin T., Foote L., Keating B., Lashner J., Orlowski-Scherer J., Randall M. J., Seibert J., Spisak J., Teply G. P., Xu Z., and Zhu N.
Abstract: Ground-based observatories across a wide range of wavelengths implement cryogenic cooling techniques to increase the sensitivity of instruments and enable low temperature detector technologies. Commercial pulse tube cryocoolers (PTCs) are frequently used to provide 40 K and 4 K stages as thermal shells in scientific instruments. However, PTC operation is dependent on gravity, giving rise to changes in cooling capacity over the operational tilt range of pointed telescopes. We present a study of the performance of a two stage PTC with a cooling capacity of 1.8 W at 4.2 K and 50 W at 45 K (Cryomech PT420-RM) from 0-55° away from vertical to probe capacity as a function of angle over a set of realistic thermal loading conditions. Our study provides a method to extract temperature estimates given predicted thermal loading conditions across the angular range sampled. We then discuss the design implications for current and future tilted cryogenic systems.
Published: 2021

34. Method for rapid performance validation of large TES bolometer array for POLARBEAR-2A using a coherent millimeter-wave source

Author: Segawa, Y, Hirose, H, Kaneko, D, Hasegawa, M, Adachi, S, Ade, P, Faundez, M, Akiba, Y, Arnold, K, Avva, J, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, De Haan, T, Dobbs, M, Dunner, R, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Ito, J, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Raum, C, Reichardt, C, Ross, C, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Segawa Y., Hirose H., Kaneko D., Hasegawa M., Adachi S., Ade P., Faundez M. A. O. A., Akiba Y., Arnold K., Avva J., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Carron J., Chapman S., Cheung K., Chinone Y., Crowley K., Cukierman A., De Haan T., Dobbs M., Dunner R., Bouhargani H. E., Elleflot T., Errard J., Fabbian G., Feeney S., Feng C., Fujino T., Galitzki N., Goeckner-Wald N., Groh J., Hall G., Halverson N., Hamada T., Hazumi M., Hill C., Howe L., Inoue Y., Ito J., Jaehnig G., Jeong O., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Minami Y., Montgomery J., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Raum C., Reichardt C. L., Ross C., Silva-Feaver M., Siritanasak P., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tsai C., Verges C., Westbrook B., Zhou Y., Segawa, Y, Hirose, H, Kaneko, D, Hasegawa, M, Adachi, S, Ade, P, Faundez, M, Akiba, Y, Arnold, K, Avva, J, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, De Haan, T, Dobbs, M, Dunner, R, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Ito, J, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Raum, C, Reichardt, C, Ross, C, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Segawa Y., Hirose H., Kaneko D., Hasegawa M., Adachi S., Ade P., Faundez M. A. O. A., Akiba Y., Arnold K., Avva J., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Carron J., Chapman S., Cheung K., Chinone Y., Crowley K., Cukierman A., De Haan T., Dobbs M., Dunner R., Bouhargani H. E., Elleflot T., Errard J., Fabbian G., Feeney S., Feng C., Fujino T., Galitzki N., Goeckner-Wald N., Groh J., Hall G., Halverson N., Hamada T., Hazumi M., Hill C., Howe L., Inoue Y., Ito J., Jaehnig G., Jeong O., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Minami Y., Montgomery J., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Raum C., Reichardt C. L., Ross C., Silva-Feaver M., Siritanasak P., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tsai C., Verges C., Westbrook B., and Zhou Y.
Abstract: POLARBEAR-2A is the first receiver for the Simons Array cosmic microwave background polarization experiment. POLARBEAR-2A has transition-edge sensor bolometers on the focal plane. Signals from bolometers are multiplexed and read out by a single SQUID. The receiver was deployed in late 2018 in Atacama, Chile, and operation started in 2019, where rapid confirmation of correspondence between bolometers and multiplexed readout channels was important as an initial step of performance validation. For this purpose, we devised a method using a coherent source that allows us to identify the frequency band and polarization sensitivity angle for each readout channel without detailed bolometer tuning.
Published: 2021

35. Deployment of Polarbear-2A

Author: Kaneko, D, Adachi, S, Ade, P, Aguilar Faundez, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Ross, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Kaneko D., Adachi S., Ade P. A. R., Aguilar Faundez M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Carron J., Chapman S., Cheung K., Chinone Y., Crowley K., Cukierman A., Dobbs M., Dunner R., El-Bouhargani H., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Hall G., Halverson N. W., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jeong O., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Minami Y., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Ross C., Segawa Y., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Verges C., Westbrook B., Zhou Y., Kaneko, D, Adachi, S, Ade, P, Aguilar Faundez, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Ross, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Kaneko D., Adachi S., Ade P. A. R., Aguilar Faundez M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Carron J., Chapman S., Cheung K., Chinone Y., Crowley K., Cukierman A., Dobbs M., Dunner R., El-Bouhargani H., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Hall G., Halverson N. W., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jeong O., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Minami Y., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Ross C., Segawa Y., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Verges C., Westbrook B., and Zhou Y.
Abstract: Polarbear-2A is the first of three receivers in the Simons array, a cosmic microwave background experiment located on the Atacama Plateau in Chile. Polarbear-2A was deployed and achieved the first light in January 2019 by mapping the microwave emission from planet observations. Commissioning work is underway to prepare the receiver for science observations.
Published: 2020

36. Results of gravitational lensing and primordial gravitational waves from the POLARBEAR experiment

Author: Chinone, Y, Adachi, S, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Elbouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Lejeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leitch, E, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Richards, P, Ross, C, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, Chinone Y., Adachi S., Ade P. A. R., Aguilar M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Elbouhargani H., Carron J., Chapman S., Cheung K., Crowley K., Cukierman A., Dunner R., Dobbs M., Ducout A., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Groh J. C., Hall G., Halverson N., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jaffe A. H., Jeong O., Lejeune M., Kaneko D., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leitch E. M., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Matsumura T., Minami Y., Montgomery J., Navaroli M., Nishino H., Paar H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Richards P. L., Ross C., Segawa Y., Sherwin B. D., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Tucker C., Verges C., Westbrook B., Whitehorn N., Zahn A., Zhou Y., Chinone, Y, Adachi, S, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Elbouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Lejeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leitch, E, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Richards, P, Ross, C, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, Chinone Y., Adachi S., Ade P. A. R., Aguilar M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Elbouhargani H., Carron J., Chapman S., Cheung K., Crowley K., Cukierman A., Dunner R., Dobbs M., Ducout A., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Groh J. C., Hall G., Halverson N., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jaffe A. H., Jeong O., Lejeune M., Kaneko D., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leitch E. M., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Matsumura T., Minami Y., Montgomery J., Navaroli M., Nishino H., Paar H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Richards P. L., Ross C., Segawa Y., Sherwin B. D., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Tucker C., Verges C., Westbrook B., Whitehorn N., Zahn A., and Zhou Y.
Abstract: POLARBEAR is a Cosmic Microwave Background radiation (CMB) polarization experiment that is located in the Atacama Desert in Chile. The scientific goals of the experiment are to characterize the B-mode signal from gravitational lensing, as well as to search for B-mode signals created by primordial gravitational waves (PGWs). Polarbear started observations in 2012 and has published a series of results. These include the first measurement of a nonzero B-mode angular auto-power spectrum at sub-degree scales where the dominant signal is gravitational lensing of the CMB. In addition, we have achieved the first measurement of crosscorrelation between the lensing potential, which was reconstructed from the CMB polarization data alone by Polarbear, and the cosmic shear field from galaxy shapes by the Subaru Hyper Suprime-Cam (HSC) survey. In 2014, we installed a continuously rotating half-wave plate (CRHWP) at the focus of the primary mirror to search for PGWs and demonstrated the control of low-frequency noise. We have found that the low-frequency B-mode power in the combined dataset with the Planck high-frequency maps is consistent with Galactic dust foreground, thus placing an upper limit on the tensor-to-scalar ratio of r < 0.90 at the 95% confidence level after marginalizing over the foregrounds.
Published: 2020

37. Characterization, deployment, and in-flight performance of the BLAST-TNG cryogenic receiver

Author: Zmuidzinas J.,Gao J.-R., Lowe, I, Ade, P, Ashton, P, Austermann, J, Coppi, G, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lourie, N, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pisano, G, Romualdez, J, Soler, J, Sinclair, A, Tucker, C, Ullom, J, Vissers, M, Wheeler, C, Williams, P, Lowe I., Ade P. A. R., Ashton P. C., Austermann J. E., Coppi G., Cox E. G., Devlin M. J., Dober B. J., Fanfani V., Fissel L. M., Galitzki N., Gao J., Gordon S., Groppi C. E., Hilton G. C., Hubmayr J., Klein J., Li D., Lourie N. P., Mani H., Mauskopf P., McKenney C., Nati F., Novak G., Pisano G., Romualdez J., Soler J. D., Sinclair A., Tucker C., Ullom J., Vissers M., Wheeler C., Williams P. A., Zmuidzinas J.,Gao J.-R., Lowe, I, Ade, P, Ashton, P, Austermann, J, Coppi, G, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lourie, N, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pisano, G, Romualdez, J, Soler, J, Sinclair, A, Tucker, C, Ullom, J, Vissers, M, Wheeler, C, Williams, P, Lowe I., Ade P. A. R., Ashton P. C., Austermann J. E., Coppi G., Cox E. G., Devlin M. J., Dober B. J., Fanfani V., Fissel L. M., Galitzki N., Gao J., Gordon S., Groppi C. E., Hilton G. C., Hubmayr J., Klein J., Li D., Lourie N. P., Mani H., Mauskopf P., McKenney C., Nati F., Novak G., Pisano G., Romualdez J., Soler J. D., Sinclair A., Tucker C., Ullom J., Vissers M., Wheeler C., and Williams P. A.
Abstract: The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter polarimeter designed to map interstellar dust and galactic foregrounds at 250, 350, and 500 microns during a 24-day Antarctic flight. The BLAST-TNG detector arrays are comprised of 918, 469, and 272 MKID pixels, respectively. The pixels are formed from two orthogonally oriented, crossed, linear-polarization sensitive MKID antennae. The arrays are cooled to sub 300 mK temperatures and stabilized via a closed cycle 3He sorption fridge in combination with a 4He vacuum pot. The detectors are read out through a combination of the second-generation Reconfigurable Open Architecture Computing Hardware (ROACH2) and custom RF electronics designed for BLAST-TNG. The firmware and software designed to readout and characterize these detectors was built from scratch by the BLAST team around these detectors, and has been adapted for use by other MKID instruments such as TolTEC and OLIMPO.1 We present an overview of these systems as well as in-depth methodology of the ground-based characterization and the measured in-flight performance.
Published: 2020

38. The Simons Observatory: Galactic Science Goals and Forecasts

Author: Hensley, B, Clark, S, Fanfani, V, Krachmalnicoff, N, Fabbian, G, Poletti, D, Puglisi, G, Coppi, G, Nibauer, J, Gerasimov, R, Galitzki, N, Choi, S, Ashton, P, Baccigalupi, C, Baxter, E, Burkhart, B, Calabrese, E, Chluba, J, Errard, J, Frolov, A, Herv??as-Caimapo, C, Huffenberger, K, Johnson, B, Jost, B, Keating, B, Mccarrick, H, Nati, F, Sathyanarayana Rao, M, van Engelen, A, Walker, S, Wolz, K, Xu, Z, Zhu, N, Zonca, A, Brandon S. Hensley, Susan E. Clark, Valentina Fanfani, Nicoletta Krachmalnicoff, Giulio Fabbian, Davide Poletti, Giuseppe Puglisi, Gabriele Coppi, Jacob Nibauer, Roman Gerasimov, Nicholas Galitzki, Steve K. Choi, Peter C. Ashton, Carlo Baccigalupi, Eric Baxter, Blakesley Burkhart, Erminia Calabrese, Jens Chluba, Josquin Errard, Andrei V. Frolov, Carlos Herv??as-Caimapo, Kevin M. Huffenberger, Bradley R. Johnson, Baptiste Jost, Brian Keating, Heather McCarrick, Federico Nati, Mayuri Sathyanarayana Rao, Alexander van Engelen, Samantha Walker, Kevin Wolz, Zhilei Xu, Ningfeng Zhu, Andrea Zonca, Hensley, B, Clark, S, Fanfani, V, Krachmalnicoff, N, Fabbian, G, Poletti, D, Puglisi, G, Coppi, G, Nibauer, J, Gerasimov, R, Galitzki, N, Choi, S, Ashton, P, Baccigalupi, C, Baxter, E, Burkhart, B, Calabrese, E, Chluba, J, Errard, J, Frolov, A, Herv??as-Caimapo, C, Huffenberger, K, Johnson, B, Jost, B, Keating, B, Mccarrick, H, Nati, F, Sathyanarayana Rao, M, van Engelen, A, Walker, S, Wolz, K, Xu, Z, Zhu, N, Zonca, A, Brandon S. Hensley, Susan E. Clark, Valentina Fanfani, Nicoletta Krachmalnicoff, Giulio Fabbian, Davide Poletti, Giuseppe Puglisi, Gabriele Coppi, Jacob Nibauer, Roman Gerasimov, Nicholas Galitzki, Steve K. Choi, Peter C. Ashton, Carlo Baccigalupi, Eric Baxter, Blakesley Burkhart, Erminia Calabrese, Jens Chluba, Josquin Errard, Andrei V. Frolov, Carlos Herv??as-Caimapo, Kevin M. Huffenberger, Bradley R. Johnson, Baptiste Jost, Brian Keating, Heather McCarrick, Federico Nati, Mayuri Sathyanarayana Rao, Alexander van Engelen, Samantha Walker, Kevin Wolz, Zhilei Xu, Ningfeng Zhu, and Andrea Zonca
Abstract: Observing in six frequency bands from 27 to 280 GHz over a large sky area, the Simons Observatory (SO) is poised to address many questions in Galactic astrophysics in addition to its principal cosmological goals. In this work, we provide quantitative forecasts on astrophysical parameters of interest for a range of Galactic science cases. We find that SO can: constrain the frequency spectrum of polarized dust emission at a level of Delta beta(d) less than or similar to 0.01 and thus test models of dust composition that predict that beta(d) in polarization differs from that measured in total intensity; measure the correlation coefficient between polarized dust and synchrotron emission with a factor of two greater precision than current constraints; exclude the nonexistence of exo-Oort clouds at roughly 2.9 sigma if the true fraction is similar to the detection rate of giant planets; map more than 850 molecular clouds with at least 50 independent polarization measurements at 1 pc resolution; detect or place upper limits on the polarization fractions of CO(2-1) emission and anomalous microwave emission at the 0.1% level in select regions; and measure the correlation coefficient between optical starlight polarization and microwave polarized dust emission in 1 degrees patches for all lines of sight with N-H greater than or similar to 2 x 10(20) cm(-2). The goals and forecasts outlined here provide a roadmap for other microwave polarization experiments to expand their scientific scope via Milky Way astrophysics.
Published: 2022

39. Dual-Polarization-Sensitive Kinetic Inductance Detectors for Balloon-borne Sub-millimeter Polarimetry

Author: Hubmayr, J., Beall, J. A., Becker, D., Brevik, J. A., Cho, H. M., Che, G., Devlin, M., Dober, B., Gao, J., Galitzki, N., Hilton, G. C., Irwin, K. D., Li, D., Mauskopf, P., Pappas, D. P., Van Lanen, J., and Vissers, M. R.
Published: 2014
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40. The Simons Observatory: modeling optical systematics in the Large Aperture Telescope

Author: Gudmundsson, JE, Gallardo, PA, Puddu, R, Dicker, SR, Adler, AE, Ali, AM, Bazarko, A, Chesmore, GE, Coppi, G, Cothard, NF, Dachlythra, N, Devlin, M, Dunner, R, Fabbian, G, Galitzki, N, Golec, JE, Ho, S-PP, Hargrave, PC, Kofman, AM, Lee, AT, Limon, M, Matsuda, FT, Mauskopf, PD, Moodley, K, Nati, F, Niemack, MD, Orlowski-Scherer, J, Page, LA, Partridge, B, Puglisi, G, Reichardt, CL, Sierra, CE, Simon, SM, Teply, GP, Tucker, C, Wollack, EJ, Xu, Z, Zhu, N, Gudmundsson, JE, Gallardo, PA, Puddu, R, Dicker, SR, Adler, AE, Ali, AM, Bazarko, A, Chesmore, GE, Coppi, G, Cothard, NF, Dachlythra, N, Devlin, M, Dunner, R, Fabbian, G, Galitzki, N, Golec, JE, Ho, S-PP, Hargrave, PC, Kofman, AM, Lee, AT, Limon, M, Matsuda, FT, Mauskopf, PD, Moodley, K, Nati, F, Niemack, MD, Orlowski-Scherer, J, Page, LA, Partridge, B, Puglisi, G, Reichardt, CL, Sierra, CE, Simon, SM, Teply, GP, Tucker, C, Wollack, EJ, Xu, Z, and Zhu, N
Abstract: We present geometrical and physical optics simulation results for the Simons Observatory Large Aperture Telescope. This work was developed as part of the general design process for the telescope, allowing us to evaluate the impact of various design choices on performance metrics and potential systematic effects. The primary goal of the simulations was to evaluate the final design of the reflectors and the cold optics that are now being built. We describe nonsequential ray tracing used to inform the design of the cold optics, including absorbers internal to each optics tube. We discuss ray tracing simulations of the telescope structure that allow us to determine geometries that minimize detector loading and mitigate spurious near-field effects that have not been resolved by the internal baffling. We also describe physical optics simulations, performed over a range of frequencies and field locations, that produce estimates of monochromatic far-field beam patterns, which in turn are used to gauge general optical performance. Finally, we describe simulations that shed light on beam sidelobes from panel gap diffraction.
Published: 2021

41. The Simons Observatory Large Aperture Telescope Receiver

Author: Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Richard Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dünner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keatin, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, J Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Perez Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Ningfeng Zhu, Tanay Bhandarkar, Gabriele Coppi, Anna M. Kofman, John L. Orlowski-Scherer, Zhilei Xu, Shunsuke Adachi, Peter Ade, Simone Aiola, Jason Austermann, Andrew O. Bazarko, James A. Beall, Sanah Bhimani, J. Richard Bond, Grace E. Chesmore, Steve K. Choi, Jake Connors, Nicholas F. Cothard, Mark Devlin, Simon Dicker, Bradley Dober, Cody J. Duell, Shannon M. Duff, Rolando Dünner, Giulio Fabbian, Nicholas Galitzki, Patricio A. Gallardo, Joseph E. Golec, Saianeesh K. Haridas, Kathleen Harrington, Erin Healy, Shuay-Pwu Patty Ho, Zachary B. Huber, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keatin, Kenji Kiuchi, Brian J. Koopman, Jack Lashner, Adrian T. Lee, Yaqiong Li, Michele Limon, Michael Link, Tammy J Lucas, Heather McCarrick, Jenna Moore, Federico Nati, Laura B. Newburgh, Michael D. Niemack, Elena Pierpaoli, Michael J. Randall, Karen Perez Sarmiento, Lauren J. Saunders, Joseph Seibert, Carlos Sierra, Rita Sonka, Jacob Spisak, Shreya Sutariya, Osamu Tajima, Grant P. Teply, Robert J. Thornton, Tran Tsan, Carole Tucker, Joel Ullom, Eve M. Vavagiakis, Michael R. Vissers, Samantha Walker, Benjamin Westbrook, Edward J. Wollack, Mario Zannoni, Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Richard Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dünner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keatin, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, J Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Perez Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Ningfeng Zhu, Tanay Bhandarkar, Gabriele Coppi, Anna M. Kofman, John L. Orlowski-Scherer, Zhilei Xu, Shunsuke Adachi, Peter Ade, Simone Aiola, Jason Austermann, Andrew O. Bazarko, James A. Beall, Sanah Bhimani, J. Richard Bond, Grace E. Chesmore, Steve K. Choi, Jake Connors, Nicholas F. Cothard, Mark Devlin, Simon Dicker, Bradley Dober, Cody J. Duell, Shannon M. Duff, Rolando Dünner, Giulio Fabbian, Nicholas Galitzki, Patricio A. Gallardo, Joseph E. Golec, Saianeesh K. Haridas, Kathleen Harrington, Erin Healy, Shuay-Pwu Patty Ho, Zachary B. Huber, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keatin, Kenji Kiuchi, Brian J. Koopman, Jack Lashner, Adrian T. Lee, Yaqiong Li, Michele Limon, Michael Link, Tammy J Lucas, Heather McCarrick, Jenna Moore, Federico Nati, Laura B. Newburgh, Michael D. Niemack, Elena Pierpaoli, Michael J. Randall, Karen Perez Sarmiento, Lauren J. Saunders, Joseph Seibert, Carlos Sierra, Rita Sonka, Jacob Spisak, Shreya Sutariya, Osamu Tajima, Grant P. Teply, Robert J. Thornton, Tran Tsan, Carole Tucker, Joel Ullom, Eve M. Vavagiakis, Michael R. Vissers, Samantha Walker, Benjamin Westbrook, Edward J. Wollack, and Mario Zannoni
Abstract: The Simons Observatory is a ground-based cosmic microwave background experiment that consists of three 0.4 m small-aperture telescopes and one 6 m Large Aperture Telescope, located at an elevation of 5300 m on Cerro Toco in Chile. The Simons Observatory Large Aperture Telescope Receiver (LATR) is the cryogenic camera that will be coupled to the Large Aperture Telescope. The resulting instrument will produce arcminute-resolution millimeter-wave maps of half the sky with unprecedented precision. The LATR is the largest cryogenic millimeter-wave camera built to date, with a diameter of 2.4 m and a length of 2.6 m. The coldest stage of the camera is cooled to 100 mK, the operating temperature of the bolometric detectors with bands centered around 27, 39, 93, 145, 225, and 280 GHz. Ultimately, the LATR will accommodate 13 40 cm diameter optics tubes, each with three detector wafers and a total of 62,000 detectors. The LATR design must simultaneously maintain the optical alignment of the system, control stray light, provide cryogenic isolation, limit thermal gradients, and minimize the time to cool the system from room temperature to 100 mK. The interplay between these competing factors poses unique challenges. We discuss the trade studies involved with the design, the final optimization, the construction, and ultimate performance of the system.
Published: 2021

42. The Simons Observatory: modeling optical systematics in the Large Aperture Telescope

Author: Gudmundsson, J, Gallardo, P, Puddu, R, Dicker, S, Adler, A, Ali, A, Bazarko, A, Chesmore, G, Coppi, G, Cothard, N, Dachlythra, N, Devlin, M, Dünner, R, Fabbian, G, Galitzki, N, Golec, J, Patty Ho, S, Hargrave, P, Kofman, A, Lee, A, Limon, M, Matsuda, F, Mauskopf, P, Moodley, K, Nati, F, Niemack, M, Orlowski-Scherer, J, Page, L, Partridge, B, Puglisi, G, Reichardt, C, Sierra, C, Simon, S, Teply, G, Tucker, C, Wollack, E, Xu, Z, Zhu, N, Gudmundsson, Jon E., Gallardo, Patricio A., Puddu, Roberto, Dicker, Simon R., Adler, Alexandre E., Ali, Aamir M., Bazarko, Andrew, Chesmore, Grace E., Coppi, Gabriele, Cothard, Nicholas F., Dachlythra, Nadia, Devlin, Mark, Dünner, Rolando, Fabbian, Giulio, Galitzki, Nicholas, Golec, Joseph E., Patty Ho, Shuay-Pwu, Hargrave, Peter C., Kofman, Anna M., Lee, Adrian T., Limon, Michele, Matsuda, Frederick T., Mauskopf, Philip D., Moodley, Kavilan, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John, Page, Lyman A., Partridge, Bruce, Puglisi, Giuseppe, Reichardt, Christian L., Sierra, Carlos E., Simon, Sara M., Teply, Grant P., Tucker, Carole, Wollack, Edward J., Xu, Zhilei, Zhu, Ningfeng, Gudmundsson, J, Gallardo, P, Puddu, R, Dicker, S, Adler, A, Ali, A, Bazarko, A, Chesmore, G, Coppi, G, Cothard, N, Dachlythra, N, Devlin, M, Dünner, R, Fabbian, G, Galitzki, N, Golec, J, Patty Ho, S, Hargrave, P, Kofman, A, Lee, A, Limon, M, Matsuda, F, Mauskopf, P, Moodley, K, Nati, F, Niemack, M, Orlowski-Scherer, J, Page, L, Partridge, B, Puglisi, G, Reichardt, C, Sierra, C, Simon, S, Teply, G, Tucker, C, Wollack, E, Xu, Z, Zhu, N, Gudmundsson, Jon E., Gallardo, Patricio A., Puddu, Roberto, Dicker, Simon R., Adler, Alexandre E., Ali, Aamir M., Bazarko, Andrew, Chesmore, Grace E., Coppi, Gabriele, Cothard, Nicholas F., Dachlythra, Nadia, Devlin, Mark, Dünner, Rolando, Fabbian, Giulio, Galitzki, Nicholas, Golec, Joseph E., Patty Ho, Shuay-Pwu, Hargrave, Peter C., Kofman, Anna M., Lee, Adrian T., Limon, Michele, Matsuda, Frederick T., Mauskopf, Philip D., Moodley, Kavilan, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John, Page, Lyman A., Partridge, Bruce, Puglisi, Giuseppe, Reichardt, Christian L., Sierra, Carlos E., Simon, Sara M., Teply, Grant P., Tucker, Carole, Wollack, Edward J., Xu, Zhilei, and Zhu, Ningfeng
Abstract: We present geometrical and physical optics simulation results for the Simons Observatory Large Aperture Telescope. This work was developed as part of the general design process for the telescope, allowing us to evaluate the impact of various design choices on performance metrics and potential systematic effects. The primary goal of the simulations was to evaluate the final design of the reflectors and the cold optics that are now being built. We describe nonsequential ray tracing used to inform the design of the cold optics, including absorbers internal to each optics tube. We discuss ray tracing simulations of the telescope structure that allow us to determine geometries that minimize detector loading and mitigate spurious near-field effects that have not been resolved by the internal baffling. We also describe physical optics simulations, performed over a range of frequencies and field locations, that produce estimates of monochromatic far-field beam patterns, which in turn are used to gauge general optical performance. Finally, we describe simulations that shed light on beam sidelobes from panel gap diffraction.
Published: 2021

43. Evidence for the Cross-correlation between Cosmic Microwave Background Polarization Lensing from Polarbear and Cosmic Shear from Subaru Hyper Suprime-Cam

Author: Namikawa, T., Miyatake, H., Oguri, M., Takahashi, R., Kusaka, A., Katayama, N., Adachi, S., Aguilar, M., Aihara, H., Ali, A., Armstrong, R., Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beck, D., Beckman, S., Bianchini, F., Boettger, David, Borrill, Julian, Cheung, K., Corbett, L., Crowley, K. T., El, Bouhargani H., Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Feng, C., Galitzki, N., Goeckner-Wald, N., Groh, J., Hamada, T., Hill, C. A., Howe, Logan, Jeong, O., Kaneko, Daisuke, Keating, Brian, Lee, A. T., Leon, D., Linder, E., Lowry, Lindsay N., Mangu, A., Matsuda, F., Minami, Y., Miyazaki, S., Murayama, H., Navaroli, Martin, Nishino, Haruki, Nishizawa, A. J., Pham, A. T. P., Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L., Sherwin, B. D., Silva-Feaver, M., Siritanasak, Praween, Speagle, J. S., Stompor, R., Tait, P. J., Takada, M., Takakura, S., Takatori, Sayuri, Tanabe, D., Tanaka, M., Teply, G. P., Tsai, C., Verges, C., Westbrook, B., Zhou, Y., Chinone, Yuji, Hasegawa, Masaya, Hazumi, Masashi, Suzuki, Aritoki, Tajima, Osamu, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), POLARBEAR, HSC, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Namikawa, T, Chinone, Y, Miyatake, H, Oguri, M, Takahashi, R, Kusaka, A, Katayama, N, Adachi, S, Aguilar, M, Aihara, H, Ali, A, Armstrong, R, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Cheung, K, Corbett, L, Crowley, K, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Galitzki, N, Goeckner-Wald, N, Groh, J, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Jeong, O, Kaneko, D, Keating, B, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Miyazaki, S, Murayama, H, Navaroli, M, Nishino, H, Nishizawa, A, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Speagle, J, Stompor, R, Suzuki, A, Tait, P, Tajima, O, Takada, M, Takakura, S, Takatori, S, Tanabe, D, Tanaka, M, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: Cold dark matter, 010504 meteorology & atmospheric sciences, Cosmic microwave background, cosmic background radiation: polarization, Astrophysics, cosmic background radiation, 01 natural sciences, Physical Chemistry, Atomic, Cosmology, Particle and Plasma Physics, gravitational lensing: weak, QB0980, cosmological model: parameter space, 010303 astronomy & astrophysics, QB, Physics, COSMIC cancer database, Settore FIS/05, Polarization (waves), observations [cosmology], Amplitude, astro-ph.CO, Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Astrophysics - Cosmology and Nongalactic Astrophysics, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, lens, cosmology: observations, polarization, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, Astronomy & Astrophysics, Settore FIS/05 - Astronomia e Astrofisica, weak [gravitational lensing], 0103 physical sciences, Nuclear, cosmic background radiation: power spectrum, 0105 earth and related environmental sciences, cosmology: observation, Cross-correlation, Organic Chemistry, Molecular, Astronomy and Astrophysics, Galaxy, cosmic background radiation: temperature, Space and Planetary Science, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: 著者人数: 73名, Accepted: 2019-07-21, 資料番号: SA1190103000
Published: 2019

44. Simons Observatory large aperture receiver simulation overview

Author: Orlowski-Scherer, J, Zhu, N, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Keating, B, Lee, A, Limon, M, Lungu, M, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Silva-Feaver, M, Simon, S, Thornton, R, Vavagiakis, E, Orlowski-Scherer J. L., Zhu N., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M., Dicker S., Galitzki N., Gallardo P. A., Keating B., Lee A. T., Limon M., Lungu M., May A., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Silva-Feaver M., Simon S. M., Thornton R., Vavagiakis E. M., Orlowski-Scherer, J, Zhu, N, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Keating, B, Lee, A, Limon, M, Lungu, M, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Silva-Feaver, M, Simon, S, Thornton, R, Vavagiakis, E, Orlowski-Scherer J. L., Zhu N., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M., Dicker S., Galitzki N., Gallardo P. A., Keating B., Lee A. T., Limon M., Lungu M., May A., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Silva-Feaver M., Simon S. M., Thornton R., and Vavagiakis E. M.
Abstract: The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales between one arcminute and tens of degrees, contain over 60,000 detectors, and sample frequencies between 27 and 270 GHz. SO will consist of a six-meter-aperture telescope coupled to over 30,000 detectors along with an array of half-meter aperture refractive cameras, which together couple to an additional 30,000+ detectors. SO will measure fundamental cosmological parameters of our universe, find high redshift clusters via the Sunyaev-Zeldovich effect, constrain properties of neutrinos, and seek signatures of dark matter through gravitational lensing. In this paper we will present results of the simulations of the SO large aperture telescope receiver (LATR). We will show details of simulations performed to ensure the structural integrity and thermal performance of our receiver, as well as will present the results of finite element analyses (FEA) of designs for the structural support system. Additionally, a full thermal model for the LATR will be described. The model will be used to ensure we meet our design requirements. Finally, we will present the results of FEA used to identify the primary vibrational modes, and planned methods for suppressing these modes. Design solutions to each of these problems that have been informed by simulation will be presented.
Published: 2018

45. Simons Observatory large aperture telescope receiver design overview

Author: Zmuidzinas J.,Gao J.-R., Zhu, N, Orlowski-Scherer, J, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Henderson, S, Ho, S, Hubmayr, J, Keating, B, Lee, A, Limon, M, Lungu, M, Mauskopf, P, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Rao, M, Salatino, M, Silva-Feaver, M, Simon, S, Staggs, S, Thornton, R, Ullom, J, Vavagiakis, E, Westbrook, B, Wollack, E, Zhu N., Orlowski-Scherer J. L., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M. J., Dicker S., Galitzki N., Gallardo P. A., Henderson S. W., Ho S. -P. P., Hubmayr J., Keating B., Lee A. T., Limon M., Lungu M., Mauskopf P. D., May A. J., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Rao M. S., Salatino M., Silva-Feaver M., Simon S. M., Staggs S., Thornton R., Ullom J. N., Vavagiakis E. M., Westbrook B., Wollack E. J., Zmuidzinas J.,Gao J.-R., Zhu, N, Orlowski-Scherer, J, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Henderson, S, Ho, S, Hubmayr, J, Keating, B, Lee, A, Limon, M, Lungu, M, Mauskopf, P, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Rao, M, Salatino, M, Silva-Feaver, M, Simon, S, Staggs, S, Thornton, R, Ullom, J, Vavagiakis, E, Westbrook, B, Wollack, E, Zhu N., Orlowski-Scherer J. L., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M. J., Dicker S., Galitzki N., Gallardo P. A., Henderson S. W., Ho S. -P. P., Hubmayr J., Keating B., Lee A. T., Limon M., Lungu M., Mauskopf P. D., May A. J., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Rao M. S., Salatino M., Silva-Feaver M., Simon S. M., Staggs S., Thornton R., Ullom J. N., Vavagiakis E. M., Westbrook B., and Wollack E. J.
Abstract: The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales between one arcminute and tens of degrees and sample frequencies between 27 and 270 GHz. Here we present the current design of the large aperture telescope receiver (LATR), a 2.4m diameter cryostat that will be mounted on the SO 6m telescope and will be the largest CMB receiver to date. The cryostat size was chosen to take advantage of the large focal plane area having high Strehl ratios, which is inherent to the Cross-Dragone telescope design. The LATR will be able to accommodate thirteen optics tubes, each having a 36 cm diameter aperture and illuminating several thousand transition-edge sensor (TES) bolometers. This set of equipment will provide an opportunity to make measurements with unparalleled sensitivity. However, the size and complexity of the LATR also pose numerous technical challenges. In the following paper, we present the design of the LATR and include how we address these challenges. The solutions we develop in the process of designing the LATR will be informative for the general CMB community, and for future CMB experiments like CMB-S4.
Published: 2018

46. BoloCalc: A sensitivity calculator for the design of Simons Observatory

Author: Hill, C, Bruno, S, Simon, S, Ali, A, Arnold, K, Ashton, P, Barron, D, Bryan, S, Chinone, Y, Coppi, G, Crowley, K, Cukierman, A, Dicker, S, Dunkley, J, Fabbian, G, Galitzki, N, Gallardo, P, Gudmundsson, J, Hubmayr, J, Keating, B, Kusaka, A, Lee, A, Matsuda, F, Mauskopf, P, Mcmahon, J, Niemack, M, Puglisi, G, Rao, M, Salatino, M, Sierra, C, Staggs, S, Suzuki, A, Teply, G, Ullom, J, Westbrook, B, Xu, Z, Zhu, N, Hill C. A., Bruno S. M. M., Simon S. M., Ali A., Arnold K. S., Ashton P. C., Barron D., Bryan S., Chinone Y., Coppi G., Crowley K. T., Cukierman A., Dicker S., Dunkley J., Fabbian G., Galitzki N., Gallardo P. A., Gudmundsson J. E., Hubmayr J., Keating B., Kusaka A., Lee A. T., Matsuda F., Mauskopf P. D., McMahon J., Niemack M. D., Puglisi G., Rao M. S., Salatino M., Sierra C., Staggs S., Suzuki A., Teply G., Ullom J. N., Westbrook B., Xu Z., Zhu N., Hill, C, Bruno, S, Simon, S, Ali, A, Arnold, K, Ashton, P, Barron, D, Bryan, S, Chinone, Y, Coppi, G, Crowley, K, Cukierman, A, Dicker, S, Dunkley, J, Fabbian, G, Galitzki, N, Gallardo, P, Gudmundsson, J, Hubmayr, J, Keating, B, Kusaka, A, Lee, A, Matsuda, F, Mauskopf, P, Mcmahon, J, Niemack, M, Puglisi, G, Rao, M, Salatino, M, Sierra, C, Staggs, S, Suzuki, A, Teply, G, Ullom, J, Westbrook, B, Xu, Z, Zhu, N, Hill C. A., Bruno S. M. M., Simon S. M., Ali A., Arnold K. S., Ashton P. C., Barron D., Bryan S., Chinone Y., Coppi G., Crowley K. T., Cukierman A., Dicker S., Dunkley J., Fabbian G., Galitzki N., Gallardo P. A., Gudmundsson J. E., Hubmayr J., Keating B., Kusaka A., Lee A. T., Matsuda F., Mauskopf P. D., McMahon J., Niemack M. D., Puglisi G., Rao M. S., Salatino M., Sierra C., Staggs S., Suzuki A., Teply G., Ullom J. N., Westbrook B., Xu Z., and Zhu N.
Abstract: The Simons Observatory (SO) is an upcoming experiment that will study temperature and polarization fluctuations in the cosmic microwave background (CMB) from the Atacama Desert in Chile. SO will field both a large aperture telescope (LAT) and an array of small aperture telescopes (SATs) that will observe in six bands with center frequencies spanning from 27 to 270 GHz. Key considerations during the SO design phase are vast, including the number of cameras per telescope, focal plane magnification and pixel density, in-band optical power and camera throughput, detector parameter tolerances, and scan strategy optimization. To inform the SO design in a rapid, organized, and traceable manner, we have created a Python-based sensitivity calculator with several state-of-the-art features, including detector-to-detector optical white-noise correlations, a handling of simulated and measured bandpasses, and propagation of low-level parameter uncertainties to uncertainty in on-sky noise performance. We discuss the mathematics of the sensitivity calculation, the calculator's object-oriented structure and key features, how it has informed the design of SO, and how it can enhance instrument design in the broader CMB community, particularly for CMB-S4.
Published: 2018

47. Cooldown strategies and transient thermal simulations for the Simons Observatory

Author: Coppi, G, Xu, Z, Ali, A, Galitzki, N, Gallardo, P, May, A, Orlowski-Scherer, J, Zhu, N, Devlin, M, Dicker, S, Keating, B, Limon, M, Lungu, M, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Simon, S, Teply, G, Thornton, R, Vavagiakis, E, Coppi G., Xu Z., Ali A., Galitzki N., Gallardo P. A., May A. J., Orlowski-Scherer J. L., Zhu N., Devlin M. J., Dicker S., Keating B., Limon M., Lungu M., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Simon S. M., Teply G., Thornton R., Vavagiakis E. M., Coppi, G, Xu, Z, Ali, A, Galitzki, N, Gallardo, P, May, A, Orlowski-Scherer, J, Zhu, N, Devlin, M, Dicker, S, Keating, B, Limon, M, Lungu, M, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Simon, S, Teply, G, Thornton, R, Vavagiakis, E, Coppi G., Xu Z., Ali A., Galitzki N., Gallardo P. A., May A. J., Orlowski-Scherer J. L., Zhu N., Devlin M. J., Dicker S., Keating B., Limon M., Lungu M., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Simon S. M., Teply G., Thornton R., and Vavagiakis E. M.
Abstract: The Simons Observatory (SO) will provide precision polarimetry of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales from arc-minutes to tens of degrees, contain over 60,000 detectors, and observe in frequency bands between 27 GHz and 270 GHz. SO will consist of a six-meter-aperture telescope initially coupled to roughly 35,000 detectors along with an array of half-meter aperture refractive cameras, coupled to an additional 30,000+ detectors. The large aperture telescope receiver (LATR) is coupled to the SO six-meter crossed Dragone telescope and will be 2.4 m in diameter, weigh over 3 metric tons, and have five cryogenic stages (80 K, 40 K, 4 K, 1 K and 100 mK). The LATR is coupled to the telescope via 13 independent optics tubes containing cryogenic optical elements and detectors. The cryostat will be cooled by two Cryomech PT90 (80 K) and three Cryomech PT420 (40 K and 4 K) pulse tube cryocoolers, with cooling of the 1 K and 100 mK stages by a commercial dilution refrigerator system. The secondo component, the small aperture telescope (SAT), is a single optics tube refractive cameras of 42 cm diameter. Cooling of the SAT stages will be provided by two Cryomech PT420, one of which is dedicated to the dilution refrigeration system which will cool the focal plane to 100 mK. SO will deploy a total of three SATs. In order to estimate the cool down time of the camera systems given their size and complexity, a finite difference code based on an implicit solver has been written to simulate the transient thermal behavior of both cryostats. The result from the simulations presented here predict a 35 day cool down for the LATR. The simulations suggest additional heat switches between stages would be effective in distribution cool down power and reducing the time it takes for the LATR to reach its base temperatures. The SAT is predicted to cool down in one week, which meets the SO design goals.
Published: 2018

48. Cold optical design for the large aperture Simons' Observatory telescope

Author: Dicker, S, Gallardo, P, Gudmudsson, J, Mauskopf, P, Ali, A, Ashton, P, Coppi, G, Devlin, M, Galitzki, N, Ho, S, Hill, C, Hubmayr, J, Keating, B, Lee, A, Limon, M, Matsuda, F, Mcmahon, J, Niemack, M, Orlowski-Scherer, J, Piccirillo, L, Salatino, M, Simon, S, Staggs, S, Thornton, R, Ullom, J, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Dicker S. R., Gallardo P. A., Gudmudsson J. E., Mauskopf P. D., Ali A., Ashton P. C., Coppi G., Devlin M. J., Galitzki N., Ho S. P., Hill C. A., Hubmayr J., Keating B., Lee A. T., Limon M., Matsuda F., McMahon J., Niemack M. D., Orlowski-Scherer J. L., Piccirillo L., Salatino M., Simon S. M., Staggs S. T., Thornton R., Ullom J. N., Vavagiakis E. M., Wollack E. J., Xu Z., Zhu N., Dicker, S, Gallardo, P, Gudmudsson, J, Mauskopf, P, Ali, A, Ashton, P, Coppi, G, Devlin, M, Galitzki, N, Ho, S, Hill, C, Hubmayr, J, Keating, B, Lee, A, Limon, M, Matsuda, F, Mcmahon, J, Niemack, M, Orlowski-Scherer, J, Piccirillo, L, Salatino, M, Simon, S, Staggs, S, Thornton, R, Ullom, J, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Dicker S. R., Gallardo P. A., Gudmudsson J. E., Mauskopf P. D., Ali A., Ashton P. C., Coppi G., Devlin M. J., Galitzki N., Ho S. P., Hill C. A., Hubmayr J., Keating B., Lee A. T., Limon M., Matsuda F., McMahon J., Niemack M. D., Orlowski-Scherer J. L., Piccirillo L., Salatino M., Simon S. M., Staggs S. T., Thornton R., Ullom J. N., Vavagiakis E. M., Wollack E. J., Xu Z., and Zhu N.
Abstract: The Simons Observatory will consist of a single large (6 m diameter) telescope and a number of smaller (∼0.5 m diameter) refracting telescopes designed to measure the polarization of the Cosmic Microwave Background to unprecedented accuracy. The large aperture telescope is the same design as the CCAT-prime telescope, a modified Crossed Dragone design with a field-of-view of over 7.8 degrees diameter at 90 GHz. This paper presents an overview of the cold reimaging optics for this telescope and what drove our choice of 350-400 mm diameter silicon lenses in a 2.4 m cryostat over other possibilities. We will also consider the future expandability of this design to CMB Stage-4 and beyond.
Published: 2018

49. Studies of Systematic uncertainties in the Simons Observatory: Optical effects and sensitivity considerations

Author: Gallardo, P, Gudmundsson, J, Koopman, B, Matsuda, F, Simon, S, Ali, A, Bryan, S, Chinone, Y, Coppi, G, Cothard, N, Devlin, M, Dicker, S, Fabbian, G, Galitzki, N, Hill, C, Keating, B, Kusaka, A, Lashner, J, Lee, A, Limon, M, Mauskopf, P, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Puglisi, G, Reichardt, C, Salatino, M, Staggs, S, Suzuki, A, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Gallardo P. A., Gudmundsson J., Koopman B. J., Matsuda F. T., Simon S. M., Ali A., Bryan S., Chinone Y., Coppi G., Cothard N., Devlin M. J., Dicker S., Fabbian G., Galitzki N., Hill C. A., Keating B., Kusaka A., Lashner J., Lee A. T., Limon M., Mauskopf P. D., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Puglisi G., Reichardt C. L., Salatino M., Staggs S., Suzuki A., Vavagiakis E. M., Wollack E. J., Xu Z., Zhu N., Gallardo, P, Gudmundsson, J, Koopman, B, Matsuda, F, Simon, S, Ali, A, Bryan, S, Chinone, Y, Coppi, G, Cothard, N, Devlin, M, Dicker, S, Fabbian, G, Galitzki, N, Hill, C, Keating, B, Kusaka, A, Lashner, J, Lee, A, Limon, M, Mauskopf, P, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Puglisi, G, Reichardt, C, Salatino, M, Staggs, S, Suzuki, A, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Gallardo P. A., Gudmundsson J., Koopman B. J., Matsuda F. T., Simon S. M., Ali A., Bryan S., Chinone Y., Coppi G., Cothard N., Devlin M. J., Dicker S., Fabbian G., Galitzki N., Hill C. A., Keating B., Kusaka A., Lashner J., Lee A. T., Limon M., Mauskopf P. D., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Puglisi G., Reichardt C. L., Salatino M., Staggs S., Suzuki A., Vavagiakis E. M., Wollack E. J., Xu Z., and Zhu N.
Abstract: The Simons Observatory (SO) is a new experiment that aims to measure the cosmic microwave background (CMB) in temperature and polarization. SO will measure the polarized sky over a large range of microwave frequencies and angular scales using a combination of small (∼0.5 m) and large (∼6 m) aperture telescopes and will be located in the Atacama Desert in Chile. This work is part of a series of papers studying calibration, sensitivity, and systematic errors for SO. In this paper, we discuss current efforts to model optical systematic effects, how these have been used to guide the design of the SO instrument, and how these studies can be used to inform instrument design of future experiments like CMB-S4. While optical systematics studies are underway for both the small aperture and large aperture telescopes, we limit the focus of this paper to the more mature large aperture telescope design for which our studies include: pointing errors, optical distortions, beam ellipticity, cross-polar response, instrumental polarization rotation and various forms of sidelobe pickup.
Published: 2018

50. The Simons Observatory: Instrument overview

Author: Jonas Zmuidzinas, Jian-Rong Gao, Galitzki, N, Ali, A, Arnold, K, Ashton, P, Austermann, J, Baccigalupi, C, Baildon, T, Barron, D, Beall, J, Beckman, S, Bruno, S, Bryan, S, Calisse, P, Chesmore, G, Chinone, Y, Choi, S, Coppi, G, Crowley, K, Cukierman, A, Devlin, M, Dicker, S, Dober, B, Duff, S, Dunkley, J, Fabbian, G, Gallardo, P, Gerbino, M, Goeckner-Wald, N, Golec, J, Gudmundsson, J, Healy, E, Henderson, S, Hill, C, Hilton, G, Ho, S, Howe, L, Hubmayr, J, Jeong, O, Keating, B, Koopman, B, Kiuchi, K, Kusaka, A, Lashner, J, Lee, A, Li, Y, Limon, M, Lungu, M, Matsuda, F, Mauskopf, P, May, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Piccirillo, L, Sathyanarayana Rao, M, Raum, C, Salatino, M, Seibert, J, Sierra, C, Silva-Feaver, M, Simon, S, Staggs, S, Stevens, J, Suzuki, A, Teply, G, Thornton, R, Tsai, C, Ullom, J, Vavagiakis, E, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Galitzki N., Ali A., Arnold K. S., Ashton P. C., Austermann J. E., Baccigalupi C., Baildon T., Barron D., Beall J. A., Beckman S., Bruno S. M. M., Bryan S., Calisse P. G., Chesmore G. E., Chinone Y., Choi S. K., Coppi G., Crowley K. D., Crowley K. T., Cukierman A., Devlin M. J., Dicker S., Dober B., Duff S. M., Dunkley J., Fabbian G., Gallardo P. A., Gerbino M., Goeckner-Wald N., Golec J. E., Gudmundsson J. E., Healy E. E., Henderson S., Hill C. A., Hilton G. C., Ho S. -P. P., Howe L. A., Hubmayr J., Jeong O., Keating B., Koopman B. J., Kiuchi K., Kusaka A., Lashner J., Lee A. T., Li Y., Limon M., Lungu M., Matsuda F., Mauskopf P. D., May A. J., McCallum N., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Piccirillo L., Sathyanarayana Rao M., Raum C., Salatino M., Seibert J. S., Sierra C., Silva-Feaver M., Simon S. M., Staggs S. T., Stevens J. R., Suzuki A., Teply G., Thornton R., Tsai C., Ullom J. N., Vavagiakis E. M., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., Zhu N., Jonas Zmuidzinas, Jian-Rong Gao, Galitzki, N, Ali, A, Arnold, K, Ashton, P, Austermann, J, Baccigalupi, C, Baildon, T, Barron, D, Beall, J, Beckman, S, Bruno, S, Bryan, S, Calisse, P, Chesmore, G, Chinone, Y, Choi, S, Coppi, G, Crowley, K, Cukierman, A, Devlin, M, Dicker, S, Dober, B, Duff, S, Dunkley, J, Fabbian, G, Gallardo, P, Gerbino, M, Goeckner-Wald, N, Golec, J, Gudmundsson, J, Healy, E, Henderson, S, Hill, C, Hilton, G, Ho, S, Howe, L, Hubmayr, J, Jeong, O, Keating, B, Koopman, B, Kiuchi, K, Kusaka, A, Lashner, J, Lee, A, Li, Y, Limon, M, Lungu, M, Matsuda, F, Mauskopf, P, May, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Piccirillo, L, Sathyanarayana Rao, M, Raum, C, Salatino, M, Seibert, J, Sierra, C, Silva-Feaver, M, Simon, S, Staggs, S, Stevens, J, Suzuki, A, Teply, G, Thornton, R, Tsai, C, Ullom, J, Vavagiakis, E, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Galitzki N., Ali A., Arnold K. S., Ashton P. C., Austermann J. E., Baccigalupi C., Baildon T., Barron D., Beall J. A., Beckman S., Bruno S. M. M., Bryan S., Calisse P. G., Chesmore G. E., Chinone Y., Choi S. K., Coppi G., Crowley K. D., Crowley K. T., Cukierman A., Devlin M. J., Dicker S., Dober B., Duff S. M., Dunkley J., Fabbian G., Gallardo P. A., Gerbino M., Goeckner-Wald N., Golec J. E., Gudmundsson J. E., Healy E. E., Henderson S., Hill C. A., Hilton G. C., Ho S. -P. P., Howe L. A., Hubmayr J., Jeong O., Keating B., Koopman B. J., Kiuchi K., Kusaka A., Lashner J., Lee A. T., Li Y., Limon M., Lungu M., Matsuda F., Mauskopf P. D., May A. J., McCallum N., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Piccirillo L., Sathyanarayana Rao M., Raum C., Salatino M., Seibert J. S., Sierra C., Silva-Feaver M., Simon S. M., Staggs S. T., Stevens J. R., Suzuki A., Teply G., Thornton R., Tsai C., Ullom J. N., Vavagiakis E. M., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., and Zhu N.
Abstract: The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales between 1 arcminute and tens of degrees, contain over 40,000 detectors, and sample frequencies between 27 and 270 GHz. SO will consist of a six-meter-aperture telescope coupled to over 20,000 detectors along with an array of half-meter aperture refractive cameras, coupled to an additional 20,000+ detectors. The unique combination of large and small apertures in a single CMB observatory, which will be located in the Atacama Desert at an altitude of 5190 m, will allow us to sample a wide range of angular scales over a common survey area. SO will measure fundamental cosmological parameters of our universe, find high redshift clusters via the Sunyaev-Zeldovich effect, constrain properties of neutrinos, and seek signatures of dark matter through gravitational lensing. The complex set of technical and science requirements for this experiment has led to innovative instrumentation solutions which we will discuss. The large aperture telescope will couple to a cryogenic receiver that is 2.4 m in diameter and over 2 m long, creating a number of interesting technical challenges. Concurrently, we are designing an array of half-meter-aperture cryogenic cameras which also have compelling design challenges. We will give an overview of the drivers for and designs of the SO telescopes and the cryogenic cameras that will house the cold optical components and detector arrays.
Published: 2018

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