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837 results on '"Coppi, G"'

1. Measuring the CMB spectral distortions with COSMO: the multi-mode antenna system

Author

Manzan, E., Albano, L., Franceschet, C., Battistelli, E. S., de Bernardis, P., Bersanelli, M., Cacciotti, F., Capponi, A., Columbro, F., Conenna, G., Coppi, G., Coppolecchia, A., D'Alessandro, G., De Gasperis, G., De Petris, M., Gervasi, M., Isopi, G., Lamagna, L., Limonta, A., Marchitelli, E., Masi, S., Mennella, A., Montonati, F., Nati, F., Occhiuzzi, A., Paiella, A., Pettinari, G., Piacentini, F., Piccirillo, L., Pisano, G., Tucker, C., and Zannoni, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In this work, we present the design and manufacturing of the two multi-mode antenna arrays of the COSMO experiment and the preliminary beam pattern measurements of their fundamental mode compared with simulations. COSMO is a cryogenic Martin-Puplett Fourier Transform Spectrometer that aims at measuring the isotropic y-type spectral distortion of the Cosmic Microwave Background from Antarctica, by performing differential measurements between the sky and an internal, cryogenic reference blackbody. To reduce the atmospheric contribution, a spinning wedge mirror performs fast sky-dips at varying elevations while fast, low-noise Kinetic Inductance detectors scan the interferogram. Two arrays of antennas couple the radiation to the detectors. Each array consists of nine smooth-walled multi-mode feed-horns, operating in the $120-180$ GHz and $210-300$ GHz range, respectively. The multi-mode propagation helps increase the instrumental sensitivity without employing large focal planes with hundreds of detectors. The two arrays have a step-linear and a linear profile, respectively, and are obtained by superimposing aluminum plates made with CNC milling. The simulated multi-mode beam pattern has a $\sim 20^{\circ} - 26^{\circ}$ FWHM for the low-frequency array and $\sim 16^{\circ}$ FWHM for the high-frequency one. The side lobes are below $-15$ dB. To characterize the antenna response, we measured the beam pattern of the fundamental mode using a Vector Network Analyzer, in far-field conditions inside an anechoic chamber at room temperature. We completed the measurements of the low-frequency array and found a good agreement with the simulations. We also identified a few non-idealities that we attribute to the measuring setup and will further investigate. A comprehensive multi-mode measurement will be feasible at cryogenic temperature once the full receiver is integrated., Comment: To appear in Proceedings of the SPIE Astronomical Telescopes + Instrumentation, 2024

Published
2024

2. The Simons Observatory: impact of bandpass, polarization angle and calibration uncertainties on small-scale power spectrum analysis

Author

Giardiello, S., Gerbino, M., Pagano, L., Alonso, D., Beringue, B., Bolliet, B., Calabrese, E., Coppi, G., Errard, J., Fabbian, G., Harrison, I., Hill, J. C., Jense, H. T., Keating, B., La Posta, A., Lattanzi, M., Lonappan, A. I., Puglisi, G., Reichardt, C. L., and Simon, S. M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We study the effects due to mismatches in passbands, polarization angles, and temperature and polarization calibrations in the context of the upcoming cosmic microwave background experiment Simons Observatory (SO). Using the SO multi-frequency likelihood, we estimate the bias and the degradation of constraining power in cosmological and astrophysical foreground parameters assuming different levels of knowledge of the instrumental effects. We find that incorrect but reasonable assumptions about the values of all the systematics examined here can have significant effects on cosmological analyses, hence requiring marginalization approaches at the likelihood level. When doing so, we find that the most relevant effect is due to bandpass shifts. When marginalizing over them, the posteriors of parameters describing astrophysical microwave foregrounds (such as radio point sources or dust) get degraded, while cosmological parameters constraints are not significantly affected. Marginalization over polarization angles with up to 0.25$^\circ$ uncertainty causes an irrelevant bias $\lesssim 0.05 \sigma$ in all parameters. Marginalization over calibration factors in polarization broadens the constraints on the effective number of relativistic degrees of freedom $N_\mathrm{eff}$ by a factor 1.2, interpreted here as a proxy parameter for non standard model physics targeted by high-resolution CMB measurements., Comment: 61 pages (27 of which are appendices), 26 figures, 12 tables. (Replacement to update the acknowledgments)

Published
2024
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3. Polarization fraction of Planck Galactic cold clumps and forecasts for the Simons Observatory

Author

Clancy, J., Puglisi, G., Clark, S. E., Coppi, G., Fabbian, G., Hervias-Caimapo, C., Hill, J. C., Nati, F., and Reichardt, C. L.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We measure the polarization fraction of a sample of $6282$ Galactic cold clumps at $353 \, \mathrm{GHz} $, consisting of $Planck$ Galactic cold clump (PGCC) catalogue category 1 objects (flux densities measured with signal-to-noise ratio $(\mathrm{S/N}) > 4$). We find the mean-squared polarization fraction at $353 \, \mathrm{GHz} $ to be $ \langle \Pi ^ 2 \rangle = [ 4.79 \pm 0.44 ] \times 10 ^ {-4} $ equating to an $ 11 \, \sigma $ detection of polarization. We test if the polarization fraction depends on the clumps' physical properties, including flux density, luminosity, Galactic latitude and physical distance. We see a trend towards increasing polarization fraction with increasing Galactic latitude, but find no evidence that polarization depends on the other tested properties. The Simons Observatory, with an angular resolution of order $1 \, \mathrm{arcmin } $ and noise levels between $22$ and $54$ $ \mu \mathrm{ K-arcmin } $ at high frequencies, will substantially enhance our ability to determine the magnetic field structure in Galactic cold clumps. At $\ge5\,\sigma$ significance, we predict the Simons Observatory will detect at least $\sim12,000$ cold clumps in intensity and $\sim430$ cold clumps in polarization. This number of polarization detections would represent a two orders of magnitude increase over the current $Planck$ results. We also release software that can be used to mask these Galactic cold clumps in other analyses., Comment: 12 pages, 12 figures, accepted by MNRAS; section 5 number counts revised and improved

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. The COSmic Monopole Observer (COSMO)

Author

Masi, S., Battistelli, E., de Bernardis, P., Coppolecchia, A., Columbro, F., D'Alessandro, G., De Petris, M., Lamagna, L., Marchitelli, E., Mele, L., Paiella, A., Piacentini, F., Pisano, G., Bersanelli, M., Franceschet, C., Manzan, E., Mennella, D., Realini, S., Cibella, S., Martini, F., Pettinari, G., Coppi, G., Gervasi, M., Limonta, A., Zannoni, M., Piccirillo, L., and Tucker, C.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The COSmic Monopole Observer (COSMO) is an experiment to measure low-level spectral distortions in the isotropic component of the Cosmic Microwave Background (CMB). Deviations from a pure blackbody spectrum are expected at low level ($<$ 1 ppm) due to several astrophysical and cosmological phenomena, and promise to provide important independent information on the early and late phases of the universe. They have not been detected yet, due to the extreme accuracy required, the best upper limits being still those from the COBE-FIRAS mission. COSMO is based on a cryogenic differential Fourier Transform Spectrometer, measuring the spectral brightness difference between the sky and an accurate cryogenic blackbody. The first implementation of COSMO, funded by the Italian PRIN and PNRA programs, will operate from the Concordia station at Dome-C, in Antarctica, and will take advantage of a fast sky-dip technique to get rid of atmospheric emission and its fluctuations, separating them from the monopole component of the sky brightness. Here we describe the instrument design, its capabilities, the current status. We also discuss its subsequent implementation in a balloon-flight, which has been studied within the COSMOS program of the Italian Space Agency., Comment: To be published on the proceedings of the 16th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Astrophysics and Relativistic Field Theories (MG16) - 5-9 July 2021. Online Conference, Italy - http://www.icra.it/mg/mg16/

Published
2021

6. Science and Innovation with Stratospheric Balloons: The Olimpo & Lspe/Swipe Projects

Author

Volpe, A., Albano, M., Ade, P. A. R., Baldini, A. M., Baù, A., Battistelli, E., de Bernardis, P., Biasotti, M., Boscaleri, A., Cei, F., Colantoni, I., Columbro, F., Coppi, G., Coppolecchia, A., D’Alessandro, G., De Petris, M., Fafone, V., Fontanelli, F., Gervasi, M., Galli, L., Gatti, F., Grosso, D., Lamagna, L., Magneville, C., Masi, S., Mauskopf, P., May, A., Mele, L., Paiella, A., Pettinari, G., Passerini, A., Piacentini, F., Piccirillo, L., Pisano, G., Polenta, G., Presta, G., Schillaci, A., Signorelli, G., Siri, B., Spinella, F., Tartari, A., Tommasi, E., Tucker, C., Vaccaro, D., Vdovin, V. F., Zannoni, M., and Yvon, D.

Published
2023
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7. The large scale polarization explorer (LSPE) for CMB measurements: performance forecast

Author

The LSPE collaboration, Addamo, G., Ade, P. A. R., Baccigalupi, C., Baldini, A. M., Battaglia, P. M., Battistelli, E. S., Baù, A., de Bernardis, P., Bersanelli, M., Biasotti, M., Boscaleri, A., Caccianiga, B., Caprioli, S., Cavaliere, F., Cei, F., Cleary, K. A., Columbro, F., Coppi, G., Coppolecchia, A., Cuttaia, F., D'Alessandro, G., De Gasperis, G., De Petris, M., Fafone, V., Farsian, F., Barusso, L. Ferrari, Fontanelli, F., Franceschet, C., Gaier, T. C., Galli, L., Gatti, F., Genova-Santos, R., Gerbino, M., Gervasi, M., Ghigna, T., Grosso, D., Gruppuso, A., Gualtieri, R., Incardona, F., Jones, M. E., Kangaslahti, P., Krachmalnicoff, N., Lamagna, L., Lattanzi, M., López-Caraballo, C. H., Lumia, M., Mainini, R., Maino, D., Mandelli, S., Maris, M., Masi, S., Matarrese, S., May, A., Mele, L., Mena, P., Mennella, A., Molina, R., Molinari, D., Morgante, G., Natale, U., Nati, F., Natoli, P., Pagano, L., Paiella, A., Panico, F., Paonessa, F., Paradiso, S., Passerini, A., Perez-de-Taoro, M., Peverini, O. A., Piacentini, F., Piccirillo, L., Pisano, G., Poletti, D., Presta, G., Realini, S., Reyes, N., Rubino-Martin, J. A., Sandri, M., Sartor, S., Pezzotta, F., Polenta, G., Rocchi, A., Schillaci, A., Signorelli, G., Siri, B., Soria, M., Spinella, F., Tapia, V., Tartari, A., Taylor, A. C., Terenzi, L., Tomasi, M., Tommasi, E., Tucker, C., Vaccaro, D., Vigano, D. M., Villa, F., Virone, G., Vittorio, N., Volpe, A., Watkins, R. E. J., Zacchei, A., and Zannoni, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

[Abridged] The measurement of the polarization of the Cosmic Microwave Background radiation is one of the current frontiers in cosmology. In particular, the detection of the primordial B-modes, could reveal the presence of gravitational waves in the early Universe. The detection of such component is at the moment the most promising technique to probe the inflationary theory describing the very early evolution of the Universe. We present the updated performance forecast of the Large Scale Polarization Explorer (LSPE), a program dedicated to the measurement of the CMB polarization. LSPE is composed of two instruments: Strip, a radiometer-based telescope on the ground in Tenerife, and SWIPE (Short-Wavelength Instrument for the Polarization Explorer) a bolometer-based instrument designed to fly on a winter arctic stratospheric long-duration balloon. The program is among the few dedicated to observation of the Northern Hemisphere, while most of the international effort is focused into ground-based observation in the Southern Hemisphere. Measurements are currently scheduled in Winter 2021/22 for SWIPE, with a flight duration up to 15 days, and in Summer 2021 with two years observations for Strip. We describe the main features of the two instruments, identifying the most critical aspects of the design, in terms of impact into performance forecast. We estimate the expected sensitivity of each instrument and propagate their combined observing power to the sensitivity to cosmological parameters, including the effect of scanning strategy, component separation, residual foregrounds and partial sky coverage. We also set requirements on the control of the most critical systematic effects and describe techniques to mitigate their impact. LSPE can reach a sensitivity in tensor-to-scalar ratio of $\sigma_r<0.01$, and improve constrains on other cosmological parameters., Comment: Submitted to JCAP. Abstract abridged for arXiv submission

Published
2020
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8. Progress report on the Large Scale Polarization Explorer

Author

Lamagna, L., Addamo, G., Ade, P. A. R., Baccigalupi, C., Baldini, A. M., Battaglia, P. M., Battistelli, E., Baù, A., Bersanelli, M., Biasotti, M., Boragno, C., Boscaleri, A., Caccianiga, B., Caprioli, S., Cavaliere, F., Cei, F., Cleary, K. A., Columbro, F., Coppi, G., Coppolecchia, A., Corsini, D., Cuttaia, F., D'Alessandro, G., de Bernardis, P., De Gasperis, G., De Petris, M., Del Torto, F., Fafone, V., Farooqui, Z., Farsian, F., Fontanelli, F., Franceschet, C., Gaier, T. C., Gatti, F., Genova-Santos, R., Gervasi, M., Ghigna, T., Grassi, M., Grosso, D., Gualtieri, R., Incardona, F., Jones, M., Kangaslahti, P., Krachmalnicoff, N., Mainini, R., Maino, D., Mandelli, S., Maris, M., Masi, S., Matarrese, S., May, A., Mena, P., Mennella, A., Molina, R., Molinari, D., Morgante, G., Nati, F., Natoli, P., Pagano, L., Paiella, A., Paonessa, F., Passerini, A., Perez-de-Taoro, M., Peverini, O. A., Pezzotta, F., Piacentini, F., Piccirillo, L., Pisano, G., Polastri, L., Polenta, G., Poletti, D., Presta, G., Realini, S., Reyes, N., Rocchi, A., Rubiño-Martin, J. A., Sandri, M., Sartor, S., Schillaci, A., Signorelli, G., Siri, B., Soria, M., Spinella, F., Tapia, V., Tartari, A., Taylor, A., Terenzi, L., Tomasi, M., Tommasi, E., Tucker, C., Vaccaro, D., Vigano, D. M., Villa, F., Virone, G., Vittorio, N., Volpe, A., Watkins, B., Zacchei, A., and Zannoni, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Large Scale Polarization Explorer (LSPE) is a cosmology program for the measurement of large scale curl-like features (B-modes) in the polarization of the Cosmic Microwave Background. Its goal is to constrain the background of inflationary gravity waves traveling through the universe at the time of matter-radiation decoupling. The two instruments of LSPE are meant to synergically operate by covering a large portion of the northern microwave sky. LSPE/STRIP is a coherent array of receivers planned to be operated from the Teide Observatory in Tenerife, for the control and characterization of the low-frequency polarized signals of galactic origin; LSPE/SWIPE is a balloon-borne bolometric polarimeter based on 330 large throughput multi-moded detectors, designed to measure the CMB polarization at 150 GHz and to monitor the polarized emission by galactic dust above 200 GHz. The combined performance and the expected level of systematics mitigation will allow LSPE to constrain primordial B-modes down to a tensor/scalar ratio of $10^{-2}$. We here report the status of the STRIP pre-commissioning phase and the progress in the characterization of the key subsystems of the SWIPE payload (namely the cryogenic polarization modulation unit and the multi-moded TES pixels) prior to receiver integration., Comment: 8 pages, 5 figures, Accepted for publication in Journal of Low Temperature Physics

Published
2020
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9. QUBIC: the Q & U Bolometric Interferometer for Cosmology

Author

Battistelli, E. S., Ade, P., Alberro, J. G., Almela, A., Amico, G., Arnaldi, L. H., Auguste, D., Aumont, J., Azzoni, S., Banfi, S., Battaglia, P., Baù, A., Bèlier, B., Bennett, D., Bergè, L., Bernard, J. -Ph., Bersanelli, M., Bigot-Sazy, M. -A., Bleurvacq, N., Bonaparte, J., Bonis, J., Bottani, A., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Chapron, C., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., D'Alessandro, G., de Bernardis, P., De Gasperis, G., De Leo, M., De Petris, M., Dheilly, S., Di Donato, A., Dumoulin, L., Etchegoyen, A., Fasciszewski, A., Ferreyro, L. P., Fracchia, D., Franceschet, C., Lerena, M. M. Gamboa, Ganga, K., Garcìa, B., Redondo, M. E. Garcìa, Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Gilles, V., Giraud-Heraud, Y., Berisso, M. Gòmez, Gonzàlez, M., Gradziel, M., Grandsire, L., Hamilton, J. -Ch., Harari, D., Haynes, V., Henrot-Versillè, S., Hoang, D. T., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Luterstein, R., Maffei, B., Marnieros, S., Marty, W., Masi, S., Mattei, A., May, A., McCulloch, M., Medina, M. C., Mele, L., Melhuish, S., Mennella, A., Montier, L., Mousset, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., Nati, F., Olivieri, E., Oriol, C., O'Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perciballi, M., Pezzotta, F., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Platino, M., Polenta, G., Prèle, D., Puddu, R., Rambaud, D., Ringegni, P., Romero, G. E., Salatino, M., Salum, J. M., Schillaci, A., Scòccola, C., Scully, S., Spinelli, S., Stankowiak, G., Stolpovskiy, M., Suarez, F., Tartari, A., Thermeau, J. -P., Timbie, P., Tomasi, M., Torchinsky, S., Tristram, M., Tucker, C., Tucker, G., Vanneste, S., Viganò, D., Vittorio, N., Voisin, F., Watson, B., Wicek, F., Zannoni, M., and Zullo, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Q & U Bolometric Interferometer for Cosmology, QUBIC, is an innovative experiment designed to measure the polarization of the Cosmic Microwave Background and in particular the signature left therein by the inflationary expansion of the Universe. The expected signal is extremely faint, thus extreme sensitivity and systematic control are necessary in order to attempt this measurement. QUBIC addresses these requirements using an innovative approach combining the sensitivity of Transition Edge Sensor cryogenic bolometers, with the deep control of systematics characteristic of interferometers. This makes QUBIC unique with respect to others classical imagers experiments devoted to the CMB polarization. In this contribution we report a description of the QUBIC instrument including recent achievements and the demonstration of the bolometric interferometry performed in lab. QUBIC will be deployed at the observation site in Alto Chorrillos, in Argentina at the end of 2019., Comment: Accepted for publication in the Journal of Low Temperature Physics

Published
2020
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10. 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

11. Measuring CMB Spectral Distortions from Antarctica with COSMO: Blackbody Calibrator Design and Performance Forecast

Author

Mele, L., Battistelli, E. S., de Bernardis, P., Bersanelli, M., Columbro, F., Coppi, G., Coppolecchia, A., D’Alessandro, G., De Petris, M., Franceschet, C., Gervasi, M., Lamagna, L., Limonta, A., Manzan, E., Marchitelli, E., Masi, S., Mennella, A., Nati, F., Paiella, A., Pettinari, G., Piacentini, F., Piccirillo, L., Pisano, G., Realini, S., Tucker, C., and Zannoni, M.

Published
2022
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12. QUBIC: using NbSi TESs with a bolometric interferometer to characterize the polarisation of the CMB

Author

Piat, M., Bélier, B., Bergé, L., Bleurvacq, N., Chapron, C., Dheilly, S., Dumoulin, L., González, M., Grandsire, L., Hamilton, J. -Ch., Henrot-Versillé, S., Hoang, D. T., Marnieros, S., Marty, W., Montier, L., Olivieri, E., Oriol, C., Perbost, C., Prêle, D., Rambaud, D., Salatino, M., Stankowiak, G., Thermeau, J. -P., Torchinsky, S., Voisin, F., Ade, P., Alberro, J. G., Almela, A., Amico, G., Arnaldi, L. H., Auguste, D., Aumont, J., Azzoni, S., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bennett, D., Bernard, J. -Ph., Bersanelli, M., Bigot-Sazy, M. -A., Bonaparte, J., Bonis, J., Bottani, A., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., D'Alessandro, G., de Bernardis, P., De Gasperis, G., De Leo, M., De Petris, M., Di Donato, A., Etchegoyen, A., Fasciszewski, A., Ferreyro, L. P., Fracchia, D., Franceschet, C., Lerena, M. M. Gamboa, Ganga, K., García, B., Redondo, M. E. García, Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Gilles, V., Giraud-Heraud, Y., Berisso, M. Gómez, Gradziel, M., Harari, D., Haynes, V., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Luterstein, R., Maffei, B., Masi, S., Mattei, A., May, A., McCulloch, M., Medina, M. C., Mele, L., Melhuish, S., Mennella, A., Mousset, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., Nati, F., O'Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perciballi, M., Pezzotta, F., Piacentini, F., Piccirillo, L., Pisano, G., Platino, M., Polenta, G., Puddu, R., Ringegni, P., Romero, G. E., Salum, J. M., Schillaci, A., Scóccola, C., Scully, S., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Tomasi, M., Tucker, C., Tucker, G., Vanneste, S., Viganò, D., Vittorio, N., Watson, B., Wicek, F., Zannoni, M., and Zullo, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

QUBIC (Q \& U Bolometric Interferometer for Cosmology) is an international ground-based experiment dedicated in the measurement of the polarized fluctuations of the Cosmic Microwave Background (CMB). It is based on bolometric interferometry, an original detection technique which combine the immunity to systematic effects of an interferometer with the sensitivity of low temperature incoherent detectors. QUBIC will be deployed in Argentina, at the Alto Chorrillos mountain site near San Antonio de los Cobres, in the Salta province. The QUBIC detection chain consists in 2048 NbSi Transition Edge Sensors (TESs) cooled to 350mK.The voltage-biased TESs are read out with Time Domain Multiplexing based on Superconducting QUantum Interference Devices (SQUIDs) at 1 K and a novel SiGe Application-Specific Integrated Circuit (ASIC) at 60 K allowing to reach an unprecedented multiplexing (MUX) factor equal to 128. The QUBIC experiment is currently being characterized in the lab with a reduced number of detectors before upgrading to the full instrument. I will present the last results of this characterization phase with a focus on the detectors and readout system., Comment: Conference proceedings submitted to the Journal of Low Temperature Physics for LTD18

Published
2019

14. A SQUID controller unit for space-based TES sensor readout

Author

Zannoni, M., Passerini, A., Signorelli, G., Cliche, J.-F., Coppi, G., Bo, P. Dal, Torre, S. Della, Giorgi, E. Di, Dobbs, M., Galli, L., Gervasi, M., Limonta, A., Massa, M., Moggi, A., Montgomery, J., Nati, F., Nicolò, D., Pinchera, M., Poletti, D., Smecher, G., Spinella, F., and Tartari, A.

Published
2023
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15. Thermal architecture for the QUBIC cryogenic receiver

Author

May, A. J., Chapron, C., Coppi, G., D'Alessandro, G., de Bernardis, P., Masi, S., Melhuish, S., Piat, M., Piccirillo, L., Schillaci, A., Thermeau, J. -P., Ade, P., Amico, G., Auguste, D., Aumont, J., Banfi, S., Barbara, G., Battaglia, P., Battistelli, E., Bau, A., Belier, B., Bennett, D., Berge, L., Bernard, J. -Ph., Bersanelli, M., Bigot-Sazy, M. -A., Bleurvacq, N., Bonaparte, J., Bonis, J., Bordier, G., Breelle, E., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Charlassier, R., Columbro, F., Coppolecchia, A., Couchot, F., D'Agostino, R., De Gasperis, G., De Leo, M., De Petris, M., Di Donato, A., Dumoulin, L., Etchegoyen, A., Fasciszewski, A., Franceschet, C., Lerena, M. M. Gamboa, Garcia, B., Garrido, X., Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Giraud-Heraud, Y., Berisso, M. Gomez, Gonzalez, M., Gradziel, M., Grandsire, L., Guerrard, E., Hamilton, J. -Ch., Harari, D., Haynes, V., Henrot-Versille, S., Hoang, D. T., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Lowitz, A., Lukovic, V., Luterstein, R., Maffei, B., Marnieros, S., Mattei, A., McCulloch, M. A., Medina, M. C., Mele, L., Mennella, A., Montier, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., O'Sullivan, C., Olivieri, E., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perdereau, O., Pezzotta, F., Piacentini, F., Pisano, G., Polenta, G., Prele, D., Puddu, R., Rambaud, D., Ringegni, P., Romero, G. E., Salatino, M., Scoccola, C. G., Scully, S., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Torchinsky, S. A., Tristram, M., Truongcanh, V., Tucker, C., Tucker, G., Vanneste, S., Vigano, D., Vittorio, N., Voisin, F., Watson, B., Wicek, F., Zannoni, M., and Zullo, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

QUBIC, the QU Bolometric Interferometer for Cosmology, is a novel forthcoming instrument to measure the B-mode polarization anisotropy of the Cosmic Microwave Background. The detection of the B-mode signal will be extremely challenging; QUBIC has been designed to address this with a novel approach, namely bolometric interferometry. The receiver cryostat is exceptionally large and cools complex optical and detector stages to 40 K, 4 K, 1 K and 350 mK using two pulse tube coolers, a novel 4He sorption cooler and a double-stage 3He/4He sorption cooler. We discuss the thermal and mechanical design of the cryostat, modelling and thermal analysis, and laboratory cryogenic testing.

Published
2018

16. 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

17. QUBIC - The Q&U Bolometric Interferometer for Cosmology - A novel way to look at the polarized Cosmic Microwave Background

Author

Mennella, A., Ade, P. A. R., Aumont, J., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bélier, B., Bennett, D., Bergé, L., Bernard, J. Ph., Bersanelli, M., Bigot-Sazy, M. A., Bleurvacq, N., Bordier, G., Brossard, J., Bunn, E. F., Burke, D. P., Buzi, D., Buzzelli, A., Cammilleri, D., Cavaliere, F., Chanial, P., Chapron, C., Columbro, F., Coppi, G., Coppolecchia, A., Couchot, F., D'Agostino, R., D'Alessandro, G., de Bernardis, P., De Gasperis, G., De Leo, M., De Petris, M., Decourcelle, T., Del Torto, F., Dumoulin, L., Etchegoyen, A., Franceschet, C., Garcia, B., Gault, A., Gayer, D., Gervasi, M., Ghribi, A., Giard, M., Giraud-Héraud, Y., Gradziel, M., Grandsire, L., Hamilton, J. Ch., Harari, D., Haynes, V., Henrot-Versillé, S., Holtzer, N., Incardona, F., Kaplan, J., Korotkov, A., Krachmalnicoff, N., Lamagna, L., Lande, J., Loucatos, S., Lowitz, A., Lukovic, V., Maffei, B., Marnieros, S., Martino, J., Masi, S., May, A., McCulloch, M., Medina, M. C., Mele, L., Melhuish, S., Montier, L., Murphy, A., Néel, D., Ng, M. W., O'Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pelosi, A., Perbost, C., Perdereau, O., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Préle, D., Puddu, R., Rambaud, D., Rigaut, O., Romero, G. E., Salatino, M., Schillaci, A., Scully, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Torchinsky, S., Tristram, M., Tucker, C., Tucker, G., Viganò, D., Vittorio, N., Voisin, F., Watson, B., Zannoni, M., and Zullo, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

In this paper we describe QUBIC, an experiment that takes up the challenge posed by the detection of primordial gravitational waves with a novel approach, that combines the sensitivity of state-of-the art bolometric detectors with the systematic effects control typical of interferometers. The so-called "self-calibration" is a technique deeply rooted in the interferometric nature of the instrument and allows us to clean the measured data from instrumental effects. The first module of QUBIC is a dual band instrument (150 GHz and 220 GHz) that will be deployed in Argentina during the Fall 2018., Comment: Presented at the EPS Conference on High Energy Physics, Venice (Italy), 5-12 July 2017 Accepted for publication in conference proceedings

Published
2018

18. 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

19. 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

20. QUBIC Technical Design Report

Author

Aumont, J., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bélier, B., Bennett, D., Bergé, L., Bernard, J. Ph., Bersanelli, M., Bigot-Sazy, M. A., Bleurvacq, N., Bordier, G., Brossard, J., Bunn, E. F., Buzi, D., Buzzelli, A., Cammilleri, D., Cavaliere, F., Chanial, P., Chapron, C., Coppi, G., Coppolecchia, A., Couchot, F., D'Agostino, R., D'Alessandro, G., de Bernardis, P., De Gasperis, G., De Petris, M., Decourcelle, T., Del Torto, F., Dumoulin, L., Etchegoyen, A., Franceschet, C., Garcia, B., Gault, A., Gayer, D., Gervasi, M., Ghribi, A., Giard, M., Giraud-Héraud, Y., Gradziel, M., Grandsire, L., Hamilton, J. Ch., Harari, D., Haynes, V., Henrot-Versillé, S., Holtzer, N., Kaplan, J., Korotkov, A., Lamagna, L., Lande, J., Loucatos, S., Lowitz, A., Lukovic, V., Maffei, B., Marnieros, S., Martino, J., Masi, S., May, A., McCulloch, M., Medina, M. C., Melhuish, S., Mennella, A., Montier, L., Murphy, A., Néel, D., Ng, M. W., O'Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pelosi, A., Perbost, C., Perdereau, O., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Prêle, D., Puddu, R., Rambaud, D., Rigaut, O., Romero, G. E., Salatino, M., Schillaci, A., Scully, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Tristram, M., Tucker, G., Viganò, D., Vittori, N., Voisin, F., Watson, B., Zannoni, M., and Zullo, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

QUBIC is an instrument aiming at measuring the B mode polarisation anisotropies at medium scales angular scales (30-200 multipoles). The search for the primordial CMB B-mode polarization signal is challenging, because of many difficulties: smallness of the expected signal, instrumental systematics that could possibly induce polarization leakage from the large E signal into B, brighter than anticipated polarized foregrounds (dust) reducing to zero the initial hope of finding sky regions clean enough to have a direct primordial B-modes observation. The QUBIC instrument is designed to address all aspects of this challenge with a novel kind of instrument, a Bolometric Interferometer, combining the background-limited sensitivity of Transition-Edge-Sensors and the control of systematics allowed by the observation of interference fringe patterns, while operating at two frequencies to disentangle polarized foregrounds from primordial B mode polarization. Its characteristics are described in details in this Technological Design Report., Comment: 139 pages ; high resolution version can be found on the qubic website (http://qubic.in2p3.fr/QUBIC/Home.html) minor changes : update author list & affiliations ; correct title

Published
2016

21. Design and performance test of a modular readout electronic for the kinetic inductance detectors for the COSMO experiment based on commercial components

Author

Zmuidzinas, J, Gao, JR, Conenna, G, Limonta, A, Meinardi, S, Passerini, A, Coppi, G, Gervasi, M, Nati, F, Zannoni, M, Albano, L, Battistelli, E, Bersanelli, M, Boussaha, F, Cacciotti, F, Capponi, A, Columbro, F, Coppolecchia, A, D'Alessandro, G, de Bernardis, P, De Gasperis, G, de Petris, M, Franceschet, C, Isopi, G, Lamagna, L, Manzan, E, Marchitelli, E, Masi, S, Mennella, A, Montonati, F, Occhiuzzi, A, Paiella, A, Pettinari, G, Piacentini, F, Piccirillo, L, Pisano, G, Tartari, A, Tucker, C, Conenna, Giulia, Limonta, Andrea, Meinardi, Stefano, Passerini, Andrea, Coppi, Gabriele, Gervasi, Massimo, Nati, Federico, Zannoni, Mario, Albano, Lorenzo, Battistelli, Elia S., Bersanelli, Marco, Boussaha, Faouzi M., Cacciotti, Federico, Capponi, Alessandro, Columbro, Fabio, Coppolecchia, Alessandro, D'Alessandro, Giuseppe, de Bernardis, Paolo, De Gasperis, Giancarlo, de Petris, Marco, Franceschet, Cristian, Isopi, Giovanni, Lamagna, Luca, Manzan, Elenia, Marchitelli, Elisabetta, Masi, Silvia, Mennella, Aniello, Montonati, Filippo, Occhiuzzi, Andrea, Paiella, Alessandro, Pettinari, Giorgio, Piacentini, Francesco, Piccirillo, Lucio, Pisano, Gampaolo, Tartari, Andrea, Tucker, Carole, Zmuidzinas, J, Gao, JR, Conenna, G, Limonta, A, Meinardi, S, Passerini, A, Coppi, G, Gervasi, M, Nati, F, Zannoni, M, Albano, L, Battistelli, E, Bersanelli, M, Boussaha, F, Cacciotti, F, Capponi, A, Columbro, F, Coppolecchia, A, D'Alessandro, G, de Bernardis, P, De Gasperis, G, de Petris, M, Franceschet, C, Isopi, G, Lamagna, L, Manzan, E, Marchitelli, E, Masi, S, Mennella, A, Montonati, F, Occhiuzzi, A, Paiella, A, Pettinari, G, Piacentini, F, Piccirillo, L, Pisano, G, Tartari, A, Tucker, C, Conenna, Giulia, Limonta, Andrea, Meinardi, Stefano, Passerini, Andrea, Coppi, Gabriele, Gervasi, Massimo, Nati, Federico, Zannoni, Mario, Albano, Lorenzo, Battistelli, Elia S., Bersanelli, Marco, Boussaha, Faouzi M., Cacciotti, Federico, Capponi, Alessandro, Columbro, Fabio, Coppolecchia, Alessandro, D'Alessandro, Giuseppe, de Bernardis, Paolo, De Gasperis, Giancarlo, de Petris, Marco, Franceschet, Cristian, Isopi, Giovanni, Lamagna, Luca, Manzan, Elenia, Marchitelli, Elisabetta, Masi, Silvia, Mennella, Aniello, Montonati, Filippo, Occhiuzzi, Andrea, Paiella, Alessandro, Pettinari, Giorgio, Piacentini, Francesco, Piccirillo, Lucio, Pisano, Gampaolo, Tartari, Andrea, and Tucker, Carole

Published
2024

22. Measuring the CMB spectral distortions with COSMO: the multi-mode antenna system

Author

Zmuidzinas, Jonas, Manzan, E, Albano, L, Franceschet, C, Battistelli, E, De Bernardis, P, Bersanelli, M, Cacciotti, F, Capponi, A, Columbro, F, Conenna, G, Coppi, G, Coppolecchia, A, D'Alessandro, G, De Gasperis, G, De Petris, M, Gervasi, M, Isopi, G, Lamagna, L, Limonta, A, Marchitelli, E, Masi, S, Mennella, A, Montonati, F, Nati, F, Occhiuzzi, A, Paiella, A, Pettinari, G, Piacentini, F, Piccirillo, L, Pisano, G, Tucker, C, Zannoni, M, Manzan, Elenia, Albano, Lorenzo, Franceschet, Cristian, Battistelli, Elia S., De Bernardis, Paolo, Bersanelli, Marco, Cacciotti, Federico, Capponi, Alessandro, Columbro, Fabio, Conenna, Giulia, Coppi, Gabriele, Coppolecchia, Alessandro, D'Alessandro, Giuseppe, De Gasperis, Giancarlo, De Petris, Marco, Gervasi, Massimo, Isopi, Giovanni, Lamagna, Luca, Limonta, Andrea, Marchitelli, Elisabetta, Masi, Silvia, Mennella, Aniello, Montonati, Filippo, Nati, Federico, Occhiuzzi, Andrea, Paiella, Alessandro, Pettinari, Giorgio, Piacentini, Francesco, Piccirillo, Lucio, Pisano, Giampaolo, Tucker, Carole, Zannoni, Mario, Zmuidzinas, Jonas, Manzan, E, Albano, L, Franceschet, C, Battistelli, E, De Bernardis, P, Bersanelli, M, Cacciotti, F, Capponi, A, Columbro, F, Conenna, G, Coppi, G, Coppolecchia, A, D'Alessandro, G, De Gasperis, G, De Petris, M, Gervasi, M, Isopi, G, Lamagna, L, Limonta, A, Marchitelli, E, Masi, S, Mennella, A, Montonati, F, Nati, F, Occhiuzzi, A, Paiella, A, Pettinari, G, Piacentini, F, Piccirillo, L, Pisano, G, Tucker, C, Zannoni, M, Manzan, Elenia, Albano, Lorenzo, Franceschet, Cristian, Battistelli, Elia S., De Bernardis, Paolo, Bersanelli, Marco, Cacciotti, Federico, Capponi, Alessandro, Columbro, Fabio, Conenna, Giulia, Coppi, Gabriele, Coppolecchia, Alessandro, D'Alessandro, Giuseppe, De Gasperis, Giancarlo, De Petris, Marco, Gervasi, Massimo, Isopi, Giovanni, Lamagna, Luca, Limonta, Andrea, Marchitelli, Elisabetta, Masi, Silvia, Mennella, Aniello, Montonati, Filippo, Nati, Federico, Occhiuzzi, Andrea, Paiella, Alessandro, Pettinari, Giorgio, Piacentini, Francesco, Piccirillo, Lucio, Pisano, Giampaolo, Tucker, Carole, and Zannoni, Mario

Published
2024

23. The Simons Observatory: Beam Characterization for the Small Aperture Telescopes

Author

Dachlythra, N, Duivenvoorden, A, Gudmundsson, J, Hasselfield, M, Coppi, G, Adler, A, Alonso, D, Azzoni, S, Chesmore, G, Fabbian, G, Ganga, K, Gerras, R, Jaffe, A, Johnson, B, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Lungu, M, Matsuda, F, Naess, S, Page, L, Puddu, R, Puglisi, G, Simon, S, Teply, G, Tsan, T, Wollack, E, Wolz, K, Xu, Z, Dachlythra, Nadia, Duivenvoorden, Adriaan J., Gudmundsson, Jon E., Hasselfield, Matthew, Coppi, Gabriele, Adler, Alexandre E., Alonso, David, Azzoni, Susanna, Chesmore, Grace E., Fabbian, Giulio, Ganga, Ken, Gerras, Remington G., Jaffe, Andrew H., Johnson, Bradley R., Keating, Brian, Keskitalo, Reijo, Kisner, Theodore S., Krachmalnicoff, Nicoletta, Lungu, Marius, Matsuda, Frederick, Naess, Sigurd, Page, Lyman, Puddu, Roberto, Puglisi, Giuseppe, Simon, Sara M., Teply, Grant, Tsan, Tran, Wollack, Edward J., Wolz, Kevin, Xu, Zhilei, Dachlythra, N, Duivenvoorden, A, Gudmundsson, J, Hasselfield, M, Coppi, G, Adler, A, Alonso, D, Azzoni, S, Chesmore, G, Fabbian, G, Ganga, K, Gerras, R, Jaffe, A, Johnson, B, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Lungu, M, Matsuda, F, Naess, S, Page, L, Puddu, R, Puglisi, G, Simon, S, Teply, G, Tsan, T, Wollack, E, Wolz, K, Xu, Z, Dachlythra, Nadia, Duivenvoorden, Adriaan J., Gudmundsson, Jon E., Hasselfield, Matthew, Coppi, Gabriele, Adler, Alexandre E., Alonso, David, Azzoni, Susanna, Chesmore, Grace E., Fabbian, Giulio, Ganga, Ken, Gerras, Remington G., Jaffe, Andrew H., Johnson, Bradley R., Keating, Brian, Keskitalo, Reijo, Kisner, Theodore S., Krachmalnicoff, Nicoletta, Lungu, Marius, Matsuda, Frederick, Naess, Sigurd, Page, Lyman, Puddu, Roberto, Puglisi, Giuseppe, Simon, Sara M., Teply, Grant, Tsan, Tran, Wollack, Edward J., Wolz, Kevin, and Xu, Zhilei

Abstract

We use time-domain simulations of Jupiter observations to test and develop a beam reconstruction pipeline for the Simons Observatory Small Aperture Telescopes. The method relies on a mapmaker that estimates and subtracts correlated atmospheric noise and a beam fitting code designed to compensate for the bias caused by the mapmaker. We test our reconstruction performance for four different frequency bands against various algorithmic parameters, atmospheric conditions, and input beams. We additionally show the reconstruction quality as a function of the number of available observations and investigate how different calibration strategies affect the beam uncertainty. For all of the cases considered, we find good agreement between the fitted results and the input beam model within an ∼1.5% error for a multipole range l = 30-700 and an ∼0.5% error for a multipole range l = 50-200. We conclude by using a harmonic-domain component separation algorithm to verify that the beam reconstruction errors and biases observed in our analysis do not significantly bias the Simons Observatory r-measurement

Published
2024

24. QUBIC: Using NbSi TESs with a Bolometric Interferometer to Characterize the Polarization of the CMB

Author

Piat, M., Bélier, B., Bergé, L., Bleurvacq, N., Chapron, C., Dheilly, S., Dumoulin, L., González, M., Grandsire, L., Hamilton, J.-Ch., Henrot-Versillé, S., Hoang, D. T., Marnieros, S., Marty, W., Montier, L., Olivieri, E., Oriol, C., Perbost, C., Prêle, D., Rambaud, D., Salatino, M., Stankowiak, G., Thermeau, J.-P., Torchinsky, S., Voisin, F., Ade, P., Alberro, J. G., Almela, A., Amico, G., Arnaldi, L. H., Auguste, D., Aumont, J., Azzoni, S., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bennett, D., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bonaparte, J., Bonis, J., Bottani, A., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., D’Alessandro, G., de Bernardis, P., De Gasperis, G., De Leo, M., De Petris, M., Di Donato, A., Etchegoyen, A., Fasciszewski, A., Ferreyro, L. P., Fracchia, D., Franceschet, C., Gamboa Lerena, M. M., Ganga, K., García, B., García Redondo, M. E., Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Gilles, V., Giraud-Heraud, Y., Gómez Berisso, M., Gradziel, M., Harari, D., Haynes, V., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Luterstein, R., Maffei, B., Masi, S., Mattei, A., May, A., McCulloch, M., Medina, M. C., Mele, L., Melhuish, S., Mennella, A., Mousset, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., Nati, F., O’Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perciballi, M., Pezzotta, F., Piacentini, F., Piccirillo, L., Pisano, G., Platino, M., Polenta, G., Puddu, R., Ringegni, P., Romero, G. E., Salum, J. M., Schillaci, A., Scóccola, C., Scully, S., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Tomasi, M., Tucker, C., Tucker, G., Vanneste, S., Viganò, D., Vittorio, N., Watson, B., Wicek, F., Zannoni, M., and Zullo, A.

Published
2020
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26. Polarization fraction of Planck Galactic cold clumps and forecasts for the Simons Observatory

Author

Clancy, J, Puglisi, G, Clark, S, Coppi, G, Fabbian, G, Hervías-Caimapo, C, Hill, J, Nati, F, Reichardt, C, Clancy J., Puglisi G., Clark S. E., Coppi G., Fabbian G., Hervías-Caimapo C., Hill J. C., Nati F., Reichardt C. L., Clancy, J, Puglisi, G, Clark, S, Coppi, G, Fabbian, G, Hervías-Caimapo, C, Hill, J, Nati, F, Reichardt, C, Clancy J., Puglisi G., Clark S. E., Coppi G., Fabbian G., Hervías-Caimapo C., Hill J. C., Nati F., and Reichardt C. L.

Abstract

We measure the mean-squared polarization fraction of a sample of 6282 Galactic cold clumps at 353 GHz, consisting of Planck Galactic cold clump (PGCC) catalogue category 1 objects [flux densities measured with signal-to-noise ratio (S/N) > 4]. At 353 GHz, we find the mean-squared polarization fraction, which we define as the mean-squared polarization divided by the mean-squared intensity, to be (4.79 ± 0.44) × 10-4 equation to an detection of polarization. We test if the polarization fraction depends on the clumps' physical properties, including flux density, luminosity, Galactic latitude, and physical distance. We see a trend towards increasing polarization fraction with increasing Galactic latitude, but find no evidence that polarization depends on the other tested properties. The Simons Observatory, with angular resolution of order 1 arcmin and noise levels between 22 and K-arcmin at high frequencies, will substantially enhance our ability to determine the magnetic field structure in Galactic cold clumps. At significance, we predict the Simons Observatory will detect at least ∼12 000 cold clumps in intensity and ∼430 cold clumps in polarization. This number of polarization detections would represent a two orders of magnitude increase over the current Planck results. We also release software that can be used to mask these Galactic cold clumps in other analyses.

Published
2023

27. Measuring the CMB spectral distortions with COSMO: the multimode antenna system

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Manzan, E., Albano, L., Franceschet, C., Battistelli, E., De Bernardis, P., Bersanelli, M., Cacciotti, F., Capponi, A., Columbro, F., Conenna, G., Coppi, G., Coppolecchia, A., D'Alessandro, G., De Gasperis, G., De Petris, M., Gervasi, M., Isopi, G., Lamagna, L., Limonta, A., Marchitelli, E., Masi, S., Mennella, A., Montonati, F., Nati, F., Occhiuzzi, A., Paiella, A., Pettinari, G., Piacentini, F., Piccirillo, L., Pisano, G., Tucker, C., and Zannoni, M.

Published
2024
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29. Choices of Stent and Cerebral Protection in the Ongoing ACST-2 Trial: A Descriptive Study

Author

Fraedrich, G., Rantner, B., Gizewski, E., Gruber, I., Hendriks, J., Cras, P., Lauwers, P., van Scheil, P., Vermassen, F., Van Herzeele, I., Geenens, M., Hemelsoet, D., Lerut, P., Lambrecht, B., Saad, G., Peeters, A., Bosiers, M., da Silva, E., de Luccia, N., Sitrangulo, J.C., Jr., Estenssoro, A.E.V., Presti, C., Casella, I., Monteiro, J.A.T., Campos, W., Jr., Puech-Leao, P., Petrov, V., Bachvarov, C., Hill, M., Mitha, A., Wong, J., Liu, C.-W., Bao, L., Yu, C., Cvjetko, I., Vidjak, V., Fiedler, J., Ostry, S., Sterba, L., Kostal, P., Staffa, R., Vlachovsky, R., Privara, M., Kriz, Z., Vojtisek, B., Krupa, P., Reif, M., Benes, V., Buchvald, P., Endrych, L., Prochazka, V., Kuliha, M., Otahal, D., Hrbac, T., Netuka, D., Mohapl, M., Kramier, F., Eldessoki, M., Heshmat, H., Abd-Allah, F., Palmiste, V., Margus, S., Toomsoo, T., Becquemin, J.-P., Bergeron, P., Abdulamit, T., Cardon, J.-M., Debus, S., Thomalla, G., Fiehler, J., Gerloss, C., Grzyska, U., Storck, M., LaMacchia, E., Eckstein, H.H., Söllner, H., Berger, H., Kallmayer, M., Popert, H., Zimmermann, A., Guenther, A., Klingner, C., Mayer, T., Schubert, J., Zanow, J., Scheinert, D., Banning-Eichenseer, U., Bausback, Y., Branzan, D., Braünilch, S., Lenzer, J., Schidt, A., Staab, H., Ulirch, M., Barlinn, J., Haase, K., Abramyuk, A., Bodechtel, U., Gerber, J., Reeps, C., Pfeiffer, T., Torello, G., Cöster, A., Giannoukas, A., Spanos, K., Matsagkas, M., Koutias, S., Vasdekis, S., Kakisis, J., Moulakakis, K., Lazaris, A., Liapas, C., Brountzos, E., Lazarides, M., Ioannou, N., Polydorou, A., Fulop, B., Fako, E., Voros, E., Bodosi, M., Nemeth, T., Barzo, P., Pazdernyik, S., Entz, L., Szeberin, Z., Dosa, E., Nemes, B., Jaranyi, Z., Pazdernyia, S., Madhaban, P., Hoffman, A., Nikolsky, E., Beyar, R., Casana, R., Tolva, V., Silingardi, R., Lauricella, A., Coppi, G., Nicoloci, E., Tusini, N., Strozzi, F., Vecchiati, E., Ferri, M., Ferrero, E., Psacharopulo, D., Gaggiano, A., Viazzo, A., Farchioni, L., Parlani, G., Caso, V., De Rangoy, P., Verzini, F., Castelli, P., DeLodovici, M.L., Carrafiello, G., Ierardi, A.M., Piffaretti, G., Nano, G., Occhiuto, M.T., Malacrida, G., Tealdi, D., Steghter, S., Stella, A., Pini, R., Faggioli, G., Sacca, S., Negri, M.D., Palombo, M., Perfumo, M.C., Fadda, G.F., Kasemi, H., Cernetti, C., Tonello, D., Visonà, A., Mangialardi, N., Ronchey, S., Altavista, M.C., Michelagnoli, S., Chisci, E., Speziale, F., Capoccia, L., Veroux, P., Giaquinta, A., Patti, F., Pulli, R., Boggia, P., Angiletta, D., Amatucci, G., Spinetti, F., Mascoli, F., Tsolaki, E., Civilini, E., Reimers, B., Setacci, C., Pogany, G., Odero, A., Accrocca, F., Bajardi, G., Takashi, I., Masayuki, E., Hidenori, E., Aidashova, B., Kospanov, N., Bakke, S., Skjelland, M., Czlonkowska, A., Kobayashi, A., Proczka, R., Dowzenko, A., Czepel, W., Polanski, J., Bialek, P., Ozkinis, G., Snoch-Ziólkiewicz, M., Gabriel, M., Stanisic, M., Iwanowski, W., Andziak, P., Gonçalves, F.B., Starodubtsev, V., Ignatenko, P., Karpenko, A., Radak, D., Aleksic, N., Sagic, D., Davidovic, L., Koncar, I., Tomic, I., Colic, M., Bartkoy, D., Rusnak, F., Gaspirini, M., Praczek, P., Milosevic, Z., Flis, V., Bergauer, A., Kobilica, N., Miksic, K., Matela, J., Blanco, E., Guerra, M., Riambau, V., Gillgren, P., Skioldebrand, C., Nymen, N., Berg, B., Delle, M., Formgren, J., Kally, T.B., Qvarfordt, P., Plate, G., Pärson, H., Lindgren, H., Bjorses, K., Gottsäter, A., Warvsten, M., Kristmundsson, T., Forssell, C., Malina, M., Holst, J., Kuhme, T., Sonesson, B., Lindblad, B., Kolbel, T., Acosta, S., Bonati, L., Traenka, C., Mueller, M., Lattman, T., Wasner, M., Mujagic, E., Von Hessling, A., Isaak, A., Stierli, P., Eugster, T., Mariani, L., Stippich, C., Wolff, T., Kahles, T., de Borst, G.J., Toorop, R., Moll, F., Lo, R., Meershoek, A., Jahrome, A.K., Vos, A.W.F., Schuiling, W., Keunen, R., Reijnen, M., Macsweeney, S., McConachie, N., Southam, A., Stansby, G., Lees, T., Lambert, D., Clarke, M., Wyatt, M., Kappadath, S., Wales, L., Jackson, R., Raudonaitis, A., MacDonald, S., Dunlop, P., Brown, A., Vetrivel, S., Bajoriene, M., Gopi, R., McCollum, C., Wolowczyk, L., Ghosh, J., Seriki, D., Ashleigh, R., Butterfield, J., Welch, M., Smyth, J.V., Briley, D., Schulz, U., Perkins, J., Hands, L., Kuker, W., Darby, C., Handa, A., Sekaran, L., Poskitt, K., Bulbulia, R., Morrison, J., Guyler, P., Grunwald, I., Brown, J., Jakeways, M., Tysoe, S., Hargroves, D., Gunathilagan, G., Insall, R., Senaratne, J., Beard, J., Cleveland, T., Nawaz, S., Lonsdale, R., Turner, D., Gaines, P., Nair, R., Chetter, I., Robinson, G., Akomolafe, B., Hatfield, J., Saastamoinen, K., Crinnion, J., Egun, A.A., Thomas, J., Drinkwater, S., D'Souza, S., Thomson, G., Gregory, B., Babu, S., Ashley, S., Joseph, T., Gibbs, R., Tebit, G., Mehrzad, A., Enevoldson, P., Mendalow, D., Parry, A., Tervitt, G., Clifton, A., Nazzel, M., Halliday, A., Peto, R., Pan, H., Potter, J., Bullbulia, R., Mihaylova, B., Flather, M., Mansfield, A., Simpson, D., Thomas, D., Gray, W., Farrell, B., Davies, C., Rahimi, K., Gough, M., Cao, P., Rothwell, P., Belli, A., Mafham, M., Herrington, W., Sandercock, P., Gray, R., Shearman, C., Molyneux, A., Gray, A., Clarke, A., Sneade, M., Tully, L., Brudlo, W., Lay, M., Munday, A., Berry, C., Tochlin, S., Cox, J., Kurien, R., Chester, J., de Waard, D.D., Huibers, A., and Bonati, L.H.

Published
2017
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30. Editor's Choice – Management of Descending Thoracic Aorta Diseases: Clinical Practice Guidelines of the European Society for Vascular Surgery (ESVS)

Author

Riambau, V., Böckler, D., Brunkwall, J., Cao, P., Chiesa, R., Coppi, G., Czerny, M., Fraedrich, G., Haulon, S., Jacobs, M.J., Lachat, M.L., Moll, F.L., Setacci, C., Taylor, P.R., Thompson, M., Trimarchi, S., Verhagen, H.J., Verhoeven, E.L., ESVS Guidelines Committee, Kolh, P., de Borst, G.J., Chakfé, N., Debus, E.S., Hinchliffe, R.J., Kakkos, S., Koncar, I., Lindholt, J.S., Vega de Ceniga, M., Vermassen, F., Verzini, F., Document Reviewers, Black, J.H., III, Busund, R., Björck, M., Dake, M., Dick, F., Eggebrecht, H., Evangelista, A., Grabenwöger, M., Milner, R., Naylor, A.R., Ricco, J.-B., Rousseau, H., and Schmidli, J.

Published
2017
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31. A New Readout Electronic for Kinetic Inductance Detectors

Author

Limonta, A, Zannoni, M, Coppi, G, Conenna, G, Boussaha, F, Tartari, A, Gervasi, M, Nati, F, Passerini, A, de Bernardis, P, Coppolecchia, A, D’Alessandro, G, Masi, S, Paiella, A, Bersanelli, M, Franceschet, C, Manzan, E, Mennella, A, Limonta, A., Zannoni, M., Coppi, G., Conenna, G., Boussaha, F., Tartari, A., Gervasi, M., Nati, F., Passerini, A., de Bernardis, P., Coppolecchia, A., D’Alessandro, G., Masi, S., Paiella, A., Bersanelli, M., Franceschet, C., Manzan, E., Mennella, A., Limonta, A, Zannoni, M, Coppi, G, Conenna, G, Boussaha, F, Tartari, A, Gervasi, M, Nati, F, Passerini, A, de Bernardis, P, Coppolecchia, A, D’Alessandro, G, Masi, S, Paiella, A, Bersanelli, M, Franceschet, C, Manzan, E, Mennella, A, Limonta, A., Zannoni, M., Coppi, G., Conenna, G., Boussaha, F., Tartari, A., Gervasi, M., Nati, F., Passerini, A., de Bernardis, P., Coppolecchia, A., D’Alessandro, G., Masi, S., Paiella, A., Bersanelli, M., Franceschet, C., Manzan, E., and Mennella, A.

Abstract

With this contribution we show the readout electronics for kinetic inductance detectors (KIDs) that we are developing based on commercial IQ transceivers from National Instruments and using a Virtex 5 class FPGA. It will be the readout electronics of the COSmic Monopole Observer (COSMO) experiment, a ground based cryogenic Martin–Puplett Interferometer searching for the cosmic microwave background spectral distortions. The readout electronics require a sampling rate in the range of tens of kHz, which is both due to a fast rotating mirror modulating the signal and the time constant of the COSMO KIDs. In this contribution we show the capabilities of our readout electronics using Niobium KIDs developed by Paris Observatory for our 5 K cryogenic system. In particular, we demonstrate the capability to detect 23 resonators from frequency sweeps and to readout the state of each resonator with a sampling rate of about 8 kHz. The readout is based on a finite-state machine where the first two states look for the resonances and generate the comb of tones, while the third one performs the acquisition of phase and amplitude of each detector in free running. Our electronics are based on commercial modules, which brings two key advantages: they can be acquired easily and it is relative simple to write and modify the firmware within the LabView environment in order to meet the needs of the experiment.

Published
2022

32. 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

33. A SQUID controller unit for space-based TES sensor readout

Author

Zannoni, M, Passerini, A, Signorelli, G, Cliche, J, Coppi, G, Bo, P, Torre, S, Giorgi, E, Dobbs, M, Galli, L, Gervasi, M, Limonta, A, Massa, M, Moggi, A, Montgomery, J, Nati, F, Nicolo, D, Pinchera, M, Poletti, D, Smecher, G, Spinella, F, Tartari, A, Zannoni, M, Passerini, A, Signorelli, G, Cliche, J, Coppi, G, Bo, P, Torre, S, Giorgi, E, Dobbs, M, Galli, L, Gervasi, M, Limonta, A, Massa, M, Moggi, A, Montgomery, J, Nati, F, Nicolo, D, Pinchera, M, Poletti, D, Smecher, G, Spinella, F, and Tartari, A

Abstract

We have developed a Superconducting Quantum Interference Device (SQUID) controller unit for Transition Edge Sensors (TES) readout, designed to be used in a space mission. The unit is made of 8 boards and each board can condition four SQUID array amplifiers. The board design is inspired by a similar one developed for ground based experiments, but specific changes have been made to adopt Components Off The Shelf (COTS) with space grade equivalents, to implement redundancy and cross-strapping capabilities. The design also includes the thermal path to lift the heat off the boards towards an in-house designed monolithic aluminum rack.

Published
2023

40. Background

Author

Piccirillo, L., primary, Coppi, G., additional, and May, A., additional

Published
2018
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41. Readout electronics for kinetic inductance detectors for COSMO

Author

Conenna G., Limonta A., Zannoni M., Coppi G., Boussaha F., Tartari A., Gervasi M., Nati F., Passerini A., De Bernardis P., Coppolecchia A., D'Alessandro G., Masi S., Paiella A., Bersanelli M., Franceschet C., Manzan E., Mennella A., Zmuidzinas, J, Gao, JR, Conenna, G, Limonta, A, Zannoni, M, Coppi, G, Boussaha, F, Tartari, A, Gervasi, M, Nati, F, Passerini, A, De Bernardis, P, Coppolecchia, A, D'Alessandro, G, Masi, S, Paiella, A, Bersanelli, M, Franceschet, C, Manzan, E, and Mennella, A

Subjects
FIS/05 - ASTRONOMIA E ASTROFISICA, electronic readout, KID, CMB, γ-distortion
Abstract

We describe the readout electronics for Kinetic Inductance Detectors (KIDs) that we are developing based on a commercial IQ transceivers from National Instruments and using a Virtex 5 class FPGA. It will be the readout electronics of the COSmic Monopole Observer (COSMO) experiment, a ground based cryogenic Martin-Puplett Interferometer searching for the Cosmic Microwave Background spectral y-distortions. The COSMO readout electronics requires a sampling rate in the range of tens of kHz, due to both a fast modulation of the signal with a spinning optical element and the short time constant of the Kinetic Inductance Detectors (KIDs) used in COSMO. In this contribution we show the capabilities of our readout electronics using Niobium KIDs developed by Paris Observatory for our 5 K cryogenic system. In particular, we demonstrate the capability to detect 23 resonators from frequency sweeps and to readout the state of each resonator with a sampling rate at about 12 kHz.

Published
2022

42. 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

43. The COSmic Monopole Observer (COSMO)

Author

Masi, S., primary, Battistelli, E., additional, de Bernardis, P., additional, Columbro, F., additional, Coppolecchia, A., additional, D’Alessandro, G., additional, De Petris, M., additional, Lamagna, L., additional, Marchitelli, E., additional, Mele, L., additional, Paiella, A., additional, Piacentini, F., additional, Pisano, G., additional, Bersanelli, M., additional, Franceschet, C., additional, Manzan, E., additional, Mennella, D., additional, Realini, S., additional, Cibella, S., additional, Martini, F., additional, Pettinari, G., additional, Coppi, G., additional, Gervasi, M., additional, Limonta, A., additional, Zannoni, M., additional, Piccirillo, L., additional, and Tucker, C., additional

Published
2023
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45. 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

46. 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

48. In-flight performance of the BLAST-TNG Kinetic Inductance Detector arrays and Readout Electronics

Author

Sinclair, A, Gordon, S, Ade, P, Ashton, P, Cho, H, Coppi, G, Corso, A, Devlin, M, Dicker, S, Dober, B, Fissel, L, Galitzky, N, Gao, J, Groppi, C, Hilton, G, Hubmayr, J, Irwin, K, Klein, J, Li, D, Lourie, N, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Soler, J, Tucker, C, Underhil, M, Vissers, M, Wheeler, C, Williams, P, Sinclair A., Gordon S. B., Ade P., Ashton P., Cho H. -M., Coppi G., Corso A., Devlin M., Dicker S., Dober B., Fissel L., Galitzky N., Gao J., Groppi C., Hilton G. C., Hubmayr J., Irwin K., Klein J., Li D., Lourie N., Lowe I., Mani H., Mauskopf P. D., McKenney C., Nati F., Novak G., Pascale E., Pisano G., Soler J., Tucker C., Underhil M., Vissers M., Wheeler C., Williams P., Sinclair, A, Gordon, S, Ade, P, Ashton, P, Cho, H, Coppi, G, Corso, A, Devlin, M, Dicker, S, Dober, B, Fissel, L, Galitzky, N, Gao, J, Groppi, C, Hilton, G, Hubmayr, J, Irwin, K, Klein, J, Li, D, Lourie, N, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Soler, J, Tucker, C, Underhil, M, Vissers, M, Wheeler, C, Williams, P, Sinclair A., Gordon S. B., Ade P., Ashton P., Cho H. -M., Coppi G., Corso A., Devlin M., Dicker S., Dober B., Fissel L., Galitzky N., Gao J., Groppi C., Hilton G. C., Hubmayr J., Irwin K., Klein J., Li D., Lourie N., Lowe I., Mani H., Mauskopf P. D., McKenney C., Nati F., Novak G., Pascale E., Pisano G., Soler J., Tucker C., Underhil M., Vissers M., Wheeler C., and Williams P.

Published
2020

49. QUBIC: Using NbSi TESs with a Bolometric Interferometer to Characterize the Polarization of the CMB

Author

Piat, M, Bélier, B, Bergé, L, Bleurvacq, N, Chapron, C, Dheilly, S, Dumoulin, L, González, M, Grandsire, L, Hamilton, J, Henrot-Versillé, S, Hoang, D, Marnieros, S, Marty, W, Montier, L, Olivieri, E, Oriol, C, Perbost, C, Prêle, D, Rambaud, D, Salatino, M, Stankowiak, G, Thermeau, J, Torchinsky, S, Voisin, F, Ade, P, Alberro, J, Almela, A, Amico, G, Arnaldi, L, Auguste, D, Aumont, J, Azzoni, S, Banfi, S, Battaglia, P, Battistelli, E, Baù, A, Bennett, D, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bonaparte, J, Bonis, J, Bottani, A, Bunn, E, Burke, D, Buzi, D, Buzzelli, A, Cavaliere, F, Chanial, P, Charlassier, R, Columbro, F, Coppi, G, Coppolecchia, A, D’Alessandro, G, de Bernardis, P, De Gasperis, G, De Leo, M, De Petris, M, Di Donato, A, Etchegoyen, A, Fasciszewski, A, Ferreyro, L, Fracchia, D, Franceschet, C, Gamboa Lerena, M, Ganga, K, García, B, García Redondo, M, Gaspard, M, Gault, A, Gayer, D, Gervasi, M, Giard, M, Gilles, V, Giraud-Heraud, Y, Gómez Berisso, M, Gradziel, M, Harari, D, Haynes, V, Incardona, F, Jules, E, Kaplan, J, Korotkov, A, Kristukat, C, Lamagna, L, Loucatos, S, Louis, T, Luterstein, R, Maffei, B, Masi, S, Mattei, A, May, A, Mcculloch, M, Medina, M, Mele, L, Melhuish, S, Mennella, A, Mousset, L, Mundo, L, Murphy, J, Nati, F, O’Sullivan, C, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perciballi, M, Pezzotta, F, Piacentini, F, Piccirillo, L, Pisano, G, Platino, M, Polenta, G, Puddu, R, Ringegni, P, Romero, G, Salum, J, Schillaci, A, Scóccola, C, Scully, S, Spinelli, S, Stolpovskiy, M, Suarez, F, Tartari, A, Timbie, P, Tomasi, M, Tucker, C, Tucker, G, Vanneste, S, Viganò, D, Vittorio, N, Watson, B, Wicek, F, Zannoni, M, Zullo, A, Piat, M., Bélier, B., Bergé, L., Bleurvacq, N., Chapron, C., Dheilly, S., Dumoulin, L., González, M., Grandsire, L., Hamilton, J. -Ch., Henrot-Versillé, S., Hoang, D. T., Marnieros, S., Marty, W., Montier, L., Olivieri, E., Oriol, C., Perbost, C., Prêle, D., Rambaud, D., Salatino, M., Stankowiak, G., Thermeau, J. -P., Torchinsky, S., Voisin, F., Ade, P., Alberro, J. G., Almela, A., Amico, G., Arnaldi, L. H., Auguste, D., Aumont, J., Azzoni, S., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bennett, D., Bernard, J. -Ph., Bersanelli, M., Bigot-Sazy, M. -A., Bonaparte, J., Bonis, J., Bottani, A., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., D’Alessandro, G., de Bernardis, P., De Gasperis, G., De Leo, M., De Petris, M., Di Donato, A., Etchegoyen, A., Fasciszewski, A., Ferreyro, L. P., Fracchia, D., Franceschet, C., Gamboa Lerena, M. M., Ganga, K., García, B., García Redondo, M. E., Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Gilles, V., Giraud-Heraud, Y., Gómez Berisso, M., Gradziel, M., Harari, D., Haynes, V., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Luterstein, R., Maffei, B., Masi, S., Mattei, A., May, A., McCulloch, M., Medina, M. C., Mele, L., Melhuish, S., Mennella, A., Mousset, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., Nati, F., O’Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perciballi, M., Pezzotta, F., Piacentini, F., Piccirillo, L., Pisano, G., Platino, M., Polenta, G., Puddu, R., Ringegni, P., Romero, G. E., Salum, J. M., Schillaci, A., Scóccola, C., Scully, S., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Tomasi, M., Tucker, C., Tucker, G., Vanneste, S., Viganò, D., Vittorio, N., Watson, B., Wicek, F., Zannoni, M., Zullo, A., Piat, M, Bélier, B, Bergé, L, Bleurvacq, N, Chapron, C, Dheilly, S, Dumoulin, L, González, M, Grandsire, L, Hamilton, J, Henrot-Versillé, S, Hoang, D, Marnieros, S, Marty, W, Montier, L, Olivieri, E, Oriol, C, Perbost, C, Prêle, D, Rambaud, D, Salatino, M, Stankowiak, G, Thermeau, J, Torchinsky, S, Voisin, F, Ade, P, Alberro, J, Almela, A, Amico, G, Arnaldi, L, Auguste, D, Aumont, J, Azzoni, S, Banfi, S, Battaglia, P, Battistelli, E, Baù, A, Bennett, D, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bonaparte, J, Bonis, J, Bottani, A, Bunn, E, Burke, D, Buzi, D, Buzzelli, A, Cavaliere, F, Chanial, P, Charlassier, R, Columbro, F, Coppi, G, Coppolecchia, A, D’Alessandro, G, de Bernardis, P, De Gasperis, G, De Leo, M, De Petris, M, Di Donato, A, Etchegoyen, A, Fasciszewski, A, Ferreyro, L, Fracchia, D, Franceschet, C, Gamboa Lerena, M, Ganga, K, García, B, García Redondo, M, Gaspard, M, Gault, A, Gayer, D, Gervasi, M, Giard, M, Gilles, V, Giraud-Heraud, Y, Gómez Berisso, M, Gradziel, M, Harari, D, Haynes, V, Incardona, F, Jules, E, Kaplan, J, Korotkov, A, Kristukat, C, Lamagna, L, Loucatos, S, Louis, T, Luterstein, R, Maffei, B, Masi, S, Mattei, A, May, A, Mcculloch, M, Medina, M, Mele, L, Melhuish, S, Mennella, A, Mousset, L, Mundo, L, Murphy, J, Nati, F, O’Sullivan, C, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perciballi, M, Pezzotta, F, Piacentini, F, Piccirillo, L, Pisano, G, Platino, M, Polenta, G, Puddu, R, Ringegni, P, Romero, G, Salum, J, Schillaci, A, Scóccola, C, Scully, S, Spinelli, S, Stolpovskiy, M, Suarez, F, Tartari, A, Timbie, P, Tomasi, M, Tucker, C, Tucker, G, Vanneste, S, Viganò, D, Vittorio, N, Watson, B, Wicek, F, Zannoni, M, Zullo, A, Piat, M., Bélier, B., Bergé, L., Bleurvacq, N., Chapron, C., Dheilly, S., Dumoulin, L., González, M., Grandsire, L., Hamilton, J. -Ch., Henrot-Versillé, S., Hoang, D. T., Marnieros, S., Marty, W., Montier, L., Olivieri, E., Oriol, C., Perbost, C., Prêle, D., Rambaud, D., Salatino, M., Stankowiak, G., Thermeau, J. -P., Torchinsky, S., Voisin, F., Ade, P., Alberro, J. G., Almela, A., Amico, G., Arnaldi, L. H., Auguste, D., Aumont, J., Azzoni, S., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bennett, D., Bernard, J. -Ph., Bersanelli, M., Bigot-Sazy, M. -A., Bonaparte, J., Bonis, J., Bottani, A., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., D’Alessandro, G., de Bernardis, P., De Gasperis, G., De Leo, M., De Petris, M., Di Donato, A., Etchegoyen, A., Fasciszewski, A., Ferreyro, L. P., Fracchia, D., Franceschet, C., Gamboa Lerena, M. M., Ganga, K., García, B., García Redondo, M. E., Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Gilles, V., Giraud-Heraud, Y., Gómez Berisso, M., Gradziel, M., Harari, D., Haynes, V., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Luterstein, R., Maffei, B., Masi, S., Mattei, A., May, A., McCulloch, M., Medina, M. C., Mele, L., Melhuish, S., Mennella, A., Mousset, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., Nati, F., O’Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perciballi, M., Pezzotta, F., Piacentini, F., Piccirillo, L., Pisano, G., Platino, M., Polenta, G., Puddu, R., Ringegni, P., Romero, G. E., Salum, J. M., Schillaci, A., Scóccola, C., Scully, S., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Tomasi, M., Tucker, C., Tucker, G., Vanneste, S., Viganò, D., Vittorio, N., Watson, B., Wicek, F., Zannoni, M., and Zullo, A.

Abstract

Q & U Bolometric Interferometer for Cosmology (QUBIC) is an international ground-based experiment dedicated in the measurement of the polarized fluctuations of the Cosmic Microwave Background. It is based on bolometric interferometry, an original detection technique which combines the immunity to systematic effects of an interferometer with the sensitivity of low-temperature incoherent detectors. QUBIC will be deployed in Argentina, at the Alto Chorrillos mountain site near San Antonio de los Cobres, in the Salta Province. The QUBIC detection chain consists in 2048 NbSi transition edge sensors (TESs) cooled to 350 mK.The voltage-biased TESs are read out with time domain multiplexing based on Superconducting QUantum Interference Devices at 1 K and a novel SiGe application-specific integrated circuit at 60 K allowing to reach an unprecedented multiplexing factor equal to 128. The QUBIC experiment is currently being characterized in the laboratory with a reduced number of detectors before upgrading to the full instrument. I will present the last results of this characterization phase with a focus on the detectors and readout system.

Published
2020

50. Progress Report on the Large-Scale Polarization Explorer

Author

Lamagna, L, Addamo, G, Ade, P, Baccigalupi, C, Baldini, A, Battaglia, P, Battistelli, E, Baù, A, Bersanelli, M, Biasotti, M, Boragno, C, Boscaleri, A, Caccianiga, B, Caprioli, S, Cavaliere, F, Cei, F, Cleary, K, Columbro, F, Coppi, G, Coppolecchia, A, Corsini, D, Cuttaia, F, D’Alessandro, G, de Bernardis, P, De Gasperis, G, De Petris, M, Torto, F, Fafone, V, Farooqui, Z, Farsian, F, Fontanelli, F, Franceschet, C, Gaier, T, Gatti, F, Genova-Santos, R, Gervasi, M, Ghigna, T, Grassi, M, Grosso, D, Incardona, F, Jones, M, Kangaslahti, P, Krachmalnicoff, N, Mainini, R, Maino, D, Mandelli, S, Maris, M, Masi, S, Matarrese, S, May, A, Mena, P, Mennella, A, Molina, R, Molinari, D, Morgante, G, Nati, F, Natoli, P, Pagano, L, Paiella, A, Paonessa, F, Passerini, A, Perez-de-Taoro, M, Peverini, O, Pezzotta, F, Piacentini, F, Piccirillo, L, Pisano, G, Polastri, L, Polenta, G, Poletti, D, Presta, G, Realini, S, Reyes, N, Rocchi, A, Rubino-Martin, J, Sandri, M, Sartor, S, Schillaci, A, Signorelli, G, Soria, M, Spinella, F, Tapia, V, Tartari, A, Taylor, A, Terenzi, L, Tomasi, M, Tommasi, E, Tucker, C, Vaccaro, D, Vigano, D, Villa, F, Virone, G, Vittorio, N, Volpe, A, Watkins, B, Zacchei, A, Zannoni, M, Lamagna, L., Addamo, G., Ade, P. A. R., Baccigalupi, C., Baldini, A. M., Battaglia, P. M., Battistelli, E., Baù, A., Bersanelli, M., Biasotti, M., Boragno, C., Boscaleri, A., Caccianiga, B., Caprioli, S., Cavaliere, F., Cei, F., Cleary, K. A., Columbro, F., Coppi, G., Coppolecchia, A., Corsini, D., Cuttaia, F., D’Alessandro, G., de Bernardis, P., De Gasperis, G., De Petris, M., Torto, F. Del, Fafone, V., Farooqui, Z., Farsian, F., Fontanelli, F., Franceschet, C., Gaier, T. C., Gatti, F., Genova-Santos, R., Gervasi, M., Ghigna, T., Grassi, M., Grosso, D., Incardona, F., Jones, M., Kangaslahti, P., Krachmalnicoff, N., Mainini, R., Maino, D., Mandelli, S., Maris, M., Masi, S., Matarrese, S., May, A., Mena, P., Mennella, A., Molina, R., Molinari, D., Morgante, G., Nati, F., Natoli, P., Pagano, L., Paiella, A., Paonessa, F., Passerini, A., Perez-de-Taoro, M., Peverini, O. 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Abstract

The large-scale polarization explorer (LSPE) is a cosmology program for the measurement of large-scale curl-like features (B-modes) in the polarization of the cosmic microwave background. Its goal is to constrain the background of inflationary gravity waves traveling through the universe at the time of matter-radiation decoupling. The two instruments of LSPE are meant to synergically operate by covering a large portion of the northern microwave sky. LSPE/STRIP is a coherent array of receivers planned to be operated from the Teide Observatory in Tenerife, for the control and characterization of the low-frequency polarized signals of galactic origin; LSPE/SWIPE is a balloon-borne bolometric polarimeter based on 330 large throughput multi-moded detectors, designed to measure the CMB polarization at 150 GHz and to monitor the polarized emission by galactic dust above 200 GHz. The combined performance and the expected level of systematics mitigation will allow LSPE to constrain primordial B-modes down to a tensor/scalar ratio of 10^−2. We here report the status of the STRIP pre-commissioning phase and the progress in the characterization of the key subsystems of the SWIPE payload (namely the cryogenic polarization modulation unit and the multi-moded TES pixels) prior to receiver integration.

Published
2020

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