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13 results on '"Lamagna, L"'

1. Sensitivity Modeling for LiteBIRD

Author

Hasebe, T, Ade, P, Adler, A, Allys, E, Alonso, D, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Azzoni, S, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Bartolo, N, Basak, S, Battistelli, E, Bautista, L, Beall, J, Beck, D, Beckman, S, Benabed, K, Bermejo-Ballesteros, J, Bersanelli, M, Bonis, J, Borrill, J, Bouchet, F, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Calvo, M, Campeti, P, Carones, A, Casas, F, Catalano, A, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Columbro, F, Coulton, W, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, K, de Bernardis, P, de Haan, T, dela Hoz, E, De Petris, M, Torre, S, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Douillet, D, Duband, L, Ducout, A, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galli, S, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Giardiello, S, Gjerlow, E, Gradziel, M, Grain, J, Grandsire, L, Grupp, F, Gruppuso, A, Gudmundsson, J, Halverson, N, Hamilton, J, Hargrave, P, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versille, S, Hergt, L, Herman, D, Herranz, D, Hill, C, Hilton, G, Hivon, E, Hlozek, R, Hoang, T, Hornsby, A, Hoshino, Y, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Jones, M, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Laquaniello, G, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Macias-Perez, J, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Maris, M, Martinez-Gonzalez, E, Masi, S, Massa, M, Matarrese, S, Matsuda, F, Matsumura, T, Mele, L, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Moggi, A, Monfardini, A, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Nakano, R, Namikawa, T, Nati, F, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, Noviello, F, O'Sullivan, C, Odagiri, K, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Passerini, A, Patanchon, G, Pelgrim, V, Peloton, J, Piacentini, F, Piat, M, Pisano, G, Polenta, G, Poletti, D, Prouve, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Spinella, F, Stever, S, Stompor, R, Sugiyama, S, Sullivan, R, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Tavagnacco, D, Taylor, A, Taylor, E, Terao, Y, Thermeau, J, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vacher, L, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wandelt, B, Wang, W, Watanuki, K, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zacchei, A, Zannoni, M, Zonca, A, Hasebe T., Ade P. A. R., Adler A., Allys E., Alonso D., Arnold K., Auguste D., Aumont J., Aurlien R., Austermann J., Azzoni S., Baccigalupi C., Banday A. J., Banerji R., Barreiro R. B., Bartolo N., Basak S., Battistelli E., Bautista L., Beall J., Beck D., Beckman S., Benabed K., Bermejo-Ballesteros J., Bersanelli M., Bonis J., Borrill J., Bouchet F., Boulanger F., Bounissou S., Brilenkov M., Brown M. L., Bucher M., Calabrese E., Calvo M., Campeti P., Carones A., Casas F. J., Catalano A., Challinor A., Chan V., Cheung K., Chinone Y., Cliche J., Columbro F., Coulton W., Cubas J., Cukierman A., Curtis D., D'Alessandro G., Dachlythra K., de Bernardis P., de Haan T., dela Hoz E., De Petris M., Torre S. D., Dickinson C., Diego-Palazuelos P., Dobbs M., Dotani T., Douillet D., Duband L., Ducout A., Duff S., Duval J. M., Ebisawa K., Elleflot T., Eriksen H. K., Errard J., Essinger-Hileman T., Finelli F., Flauger R., Franceschet C., Fuskeland U., Galli S., Galloway M., Ganga K., Gao J. R., Genova-Santos R. T., Gerbino M., Gervasi M., Ghigna T., Giardiello S., Gjerlow E., Gradziel M. L., Grain J., Grandsire L., Grupp F., Gruppuso A., Gudmundsson J. E., Halverson N. W., Hamilton J., Hargrave P., Hasegawa M., Hattori M., Hazumi M., Henrot-Versille S., Hergt L. T., Herman D., Herranz D., Hill C. A., Hilton G., Hivon E., Hlozek R. A., Hoang T. D., Hornsby A. L., Hoshino Y., Hubmayr J., Ichiki K., Iida T., Imada H., Ishimura K., Ishino H., Jaehnig G., Jones M., Kaga T., Kashima S., Katayama N., Kato A., Kawasaki T., Keskitalo R., Kisner T., Kobayashi Y., Kogiso N., Kogut A., Kohri K., Komatsu E., Komatsu K., Konishi K., Krachmalnicoff N., Kreykenbohm I., Kuo C. L., Kushino A., Lamagna L., Lanen J. V., Laquaniello G., Lattanzi M., Lee A. T., Leloup C., Levrier F., Linder E., Louis T., Luzzi G., Macias-Perez J., Maciaszek T., Maffei B., Maino D., Maki M., Mandelli S., Maris M., Martinez-Gonzalez E., Masi S., Massa M., Matarrese S., Matsuda F. T., Matsumura T., Mele L., Mennella A., Migliaccio M., Minami Y., Mitsuda K., Moggi A., Monfardini A., Montgomery J., Montier L., Morgante G., Mot B., Murata Y., Murphy J. A., Nagai M., Nagano Y., Nagasaki T., Nagata R., Nakamura S., Nakano R., Namikawa T., Nati F., Natoli P., Nerval S., Nishibori T., Nishino H., Noviello F., O'Sullivan C., Odagiri K., Ogawa H., Oguri S., Ohsaki H., Ohta I. S., Okada N., Pagano L., Paiella A., Paoletti D., Passerini A., Patanchon G., Pelgrim V., Peloton J., Piacentini F., Piat M., Pisano G., Polenta G., Poletti D., Prouve T., Puglisi G., Rambaud D., Raum C., Realini S., Reinecke M., Remazeilles M., Ritacco A., Roudil G., Rubino-Martin J., Russell M., Sakurai H., Sakurai Y., Sandri M., Sasaki M., Savini G., Scott D., Seibert J., Sekimoto Y., Sherwin B., Shinozaki K., Shiraishi M., Shirron P., Signorelli G., Smecher G., Spinella F., Stever S., Stompor R., Sugiyama S., Sullivan R., Suzuki A., Suzuki J., Svalheim T. L., Switzer E., Takaku R., Takakura H., Takakura S., Takase Y., Takeda Y., Tartari A., Tavagnacco D., Taylor A., Taylor E., Terao Y., Thermeau J., Thommesen H., Thompson K. L., Thorne B., Toda T., Tomasi M., Tominaga M., Trappe N., Tristram M., Tsuji M., Tsujimoto M., Tucker C., Ullom J., Vacher L., Vermeulen G., Vielva P., Villa F., Vissers M., Vittorio N., Wandelt B., Wang W., Watanuki K., Wehus I. K., Weller J., Westbrook B., Wilms J., Winter B., Wollack E. J., Yamasaki N. Y., Yoshida T., Yumoto J., Zacchei A., Zannoni M., Zonca A., Hasebe, T, Ade, P, Adler, A, Allys, E, Alonso, D, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Azzoni, S, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Bartolo, N, Basak, S, Battistelli, E, Bautista, L, Beall, J, Beck, D, Beckman, S, Benabed, K, Bermejo-Ballesteros, J, Bersanelli, M, Bonis, J, Borrill, J, Bouchet, F, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Calvo, M, Campeti, P, Carones, A, Casas, F, Catalano, A, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Columbro, F, Coulton, W, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, K, de Bernardis, P, de Haan, T, dela Hoz, E, De Petris, M, Torre, S, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Douillet, D, Duband, L, Ducout, A, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galli, S, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Giardiello, S, Gjerlow, E, Gradziel, M, Grain, J, Grandsire, L, Grupp, F, Gruppuso, A, Gudmundsson, J, Halverson, N, Hamilton, J, Hargrave, P, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versille, S, Hergt, L, Herman, D, Herranz, D, Hill, C, Hilton, G, Hivon, E, Hlozek, R, Hoang, T, Hornsby, A, Hoshino, Y, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Jones, M, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Laquaniello, G, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Macias-Perez, J, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Maris, M, Martinez-Gonzalez, E, Masi, S, Massa, M, Matarrese, S, Matsuda, F, Matsumura, T, Mele, L, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Moggi, A, Monfardini, A, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Nakano, R, Namikawa, T, Nati, F, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, Noviello, F, O'Sullivan, C, Odagiri, K, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Passerini, A, Patanchon, G, Pelgrim, V, Peloton, J, Piacentini, F, Piat, M, Pisano, G, Polenta, G, Poletti, D, Prouve, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Spinella, F, Stever, S, Stompor, R, Sugiyama, S, Sullivan, R, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Tavagnacco, D, Taylor, A, Taylor, E, Terao, Y, Thermeau, J, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vacher, L, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wandelt, B, Wang, W, Watanuki, K, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zacchei, A, Zannoni, M, Zonca, A, Hasebe T., Ade P. A. R., Adler A., Allys E., Alonso D., Arnold K., Auguste D., Aumont J., Aurlien R., Austermann J., Azzoni S., Baccigalupi C., Banday A. J., Banerji R., Barreiro R. B., Bartolo N., Basak S., Battistelli E., Bautista L., Beall J., Beck D., Beckman S., Benabed K., Bermejo-Ballesteros J., Bersanelli M., Bonis J., Borrill J., Bouchet F., Boulanger F., Bounissou S., Brilenkov M., Brown M. L., Bucher M., Calabrese E., Calvo M., Campeti P., Carones A., Casas F. J., Catalano A., Challinor A., Chan V., Cheung K., Chinone Y., Cliche J., Columbro F., Coulton W., Cubas J., Cukierman A., Curtis D., D'Alessandro G., Dachlythra K., de Bernardis P., de Haan T., dela Hoz E., De Petris M., Torre S. D., Dickinson C., Diego-Palazuelos P., Dobbs M., Dotani T., Douillet D., Duband L., Ducout A., Duff S., Duval J. M., Ebisawa K., Elleflot T., Eriksen H. K., Errard J., Essinger-Hileman T., Finelli F., Flauger R., Franceschet C., Fuskeland U., Galli S., Galloway M., Ganga K., Gao J. R., Genova-Santos R. T., Gerbino M., Gervasi M., Ghigna T., Giardiello S., Gjerlow E., Gradziel M. L., Grain J., Grandsire L., Grupp F., Gruppuso A., Gudmundsson J. E., Halverson N. W., Hamilton J., Hargrave P., Hasegawa M., Hattori M., Hazumi M., Henrot-Versille S., Hergt L. T., Herman D., Herranz D., Hill C. A., Hilton G., Hivon E., Hlozek R. A., Hoang T. D., Hornsby A. L., Hoshino Y., Hubmayr J., Ichiki K., Iida T., Imada H., Ishimura K., Ishino H., Jaehnig G., Jones M., Kaga T., Kashima S., Katayama N., Kato A., Kawasaki T., Keskitalo R., Kisner T., Kobayashi Y., Kogiso N., Kogut A., Kohri K., Komatsu E., Komatsu K., Konishi K., Krachmalnicoff N., Kreykenbohm I., Kuo C. L., Kushino A., Lamagna L., Lanen J. V., Laquaniello G., Lattanzi M., Lee A. T., Leloup C., Levrier F., Linder E., Louis T., Luzzi G., Macias-Perez J., Maciaszek T., Maffei B., Maino D., Maki M., Mandelli S., Maris M., Martinez-Gonzalez E., Masi S., Massa M., Matarrese S., Matsuda F. T., Matsumura T., Mele L., Mennella A., Migliaccio M., Minami Y., Mitsuda K., Moggi A., Monfardini A., Montgomery J., Montier L., Morgante G., Mot B., Murata Y., Murphy J. A., Nagai M., Nagano Y., Nagasaki T., Nagata R., Nakamura S., Nakano R., Namikawa T., Nati F., Natoli P., Nerval S., Nishibori T., Nishino H., Noviello F., O'Sullivan C., Odagiri K., Ogawa H., Oguri S., Ohsaki H., Ohta I. S., Okada N., Pagano L., Paiella A., Paoletti D., Passerini A., Patanchon G., Pelgrim V., Peloton J., Piacentini F., Piat M., Pisano G., Polenta G., Poletti D., Prouve T., Puglisi G., Rambaud D., Raum C., Realini S., Reinecke M., Remazeilles M., Ritacco A., Roudil G., Rubino-Martin J., Russell M., Sakurai H., Sakurai Y., Sandri M., Sasaki M., Savini G., Scott D., Seibert J., Sekimoto Y., Sherwin B., Shinozaki K., Shiraishi M., Shirron P., Signorelli G., Smecher G., Spinella F., Stever S., Stompor R., Sugiyama S., Sullivan R., Suzuki A., Suzuki J., Svalheim T. L., Switzer E., Takaku R., Takakura H., Takakura S., Takase Y., Takeda Y., Tartari A., Tavagnacco D., Taylor A., Taylor E., Terao Y., Thermeau J., Thommesen H., Thompson K. L., Thorne B., Toda T., Tomasi M., Tominaga M., Trappe N., Tristram M., Tsuji M., Tsujimoto M., Tucker C., Ullom J., Vacher L., Vermeulen G., Vielva P., Villa F., Vissers M., Vittorio N., Wandelt B., Wang W., Watanuki K., Wehus I. K., Weller J., Westbrook B., Wilms J., Winter B., Wollack E. J., Yamasaki N. Y., Yoshida T., Yumoto J., Zacchei A., Zannoni M., and Zonca A.

Abstract

LiteBIRD is a future satellite mission designed to observe the polarization of the cosmic microwave background radiation in order to probe the inflationary universe. LiteBIRD is set to observe the sky using three telescopes with transition-edge sensor bolometers. In this work we estimated the LiteBIRD instrumental sensitivity using its current design. We estimated the detector noise due to the optical loadings using physical optics and ray-tracing simulations. The noise terms associated with thermal carrier and readout noise were modeled in the detector noise calculation. We calculated the observational sensitivities over fifteen bands designed for the LiteBIRD telescopes using assumed observation time efficiency.

Published
2023

2. Pulse Tube Cooler with > 100 m Flexible Lines for Operation of Cryogenic Detector Arrays at Large Radiotelescopes.

Author

Coppolecchia, A., Battistelli, E. S., Masi, S., Marongiu, P., Barbavara, E., de Bernardis, P., Cacciotti, F., Carretti, E., Columbro, F., Cruciani, A., D'Alessandro, G., De Petris, M., Govoni, F., Isopi, G., Lamagna, L., Mele, L., Molinari, E., Murgia, M., Navarrini, A., and Orlati, A.

Subjects
DETECTORS, LUMPED elements, ELECTRIC noise, RADIO telescopes, TUBES, TELESCOPES
Abstract

Large radio and mm–wave telescopes use very sensitive detectors requiring cryogenic cooling to reduce detector noise. Pulse Tubes (PT) cryocoolers are widely used to reach temperatures of a few K, defining the base temperature of further sub–K stages. This technology represents an effective solution for continuous operation, featuring high stability and reduced vibration levels on the detectors. However, the compressor used to operate the PT is a significant source of microphonics and electrical noise, making its use at the focus of large steerable telescopes not advisable. This calls for long flexible helium lines between the compressor, operated at the base of the radio telescope, and the cold–head, mounted in the receivers cabin with the receiver detectors. The distance between the receiver cabin and the base can be >100 m long for large radio telescopes. In the framework of our development of the MIllimetric Sardinia radio Telescope Receiver based on Array of Lumped elements kids (MISTRAL), a W–band camera working at the Gregorian focus of the 64 m aperture Sardinia Radio Telescope (SRT) with an array of Lumped Elements Kinetic Inductance Detectors (LEKID), we have developed a cryogenic system based on a PT refrigerator as the first cooling stage. Here we describe the MISTRAL cryogenic system and focus on the validation of the use of a commercial PT Cryocooler with 100 m helium lines running from the cold head to the compressor unit. The configuration allows us to operate the 0.9 W PT reaching below 4.2 K with 0.5 W dissipation. [ABSTRACT FROM AUTHOR]

Published
2023
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3. A Testbed for Modeling Validation and Characterization of Quasi-optical Elements in Microwave Receivers.

Author

Lamagna, L., Basilicata, M., Occhiuzzi, A., Columbro, F., Coppolecchia, A., D'Alessandro, G., Bernardis, P. de, Masi, S., Mele, L., Paiella, A., and Pisano, G.

Subjects
*COSMIC background radiation, *FOURIER transform spectrometers, *MODEL validation, *DIELECTRIC materials, *SUPERCONDUCTING transitions, *OPTICAL communications
Abstract

We describe the setup for the broadband millimeter/submillimeter characterization of the quasi-optical elements and the dielectric materials commonly used in microwave receivers operated in microwave astronomy. The setup is made of a large aperture (100 mm) Fourier transform spectrometer coupled to a transition edge superconducting detector. The system has been assembled and characterized in different configurations and operation modes for the acquisition of interferograms from various kinds of samples. After the initial test runs, the configuration is now being updated to ensure a broader range of measurements, including reflectance and scattering. We plan to first use this testbed for the characterization of the dielectric materials used in the LSPE/SWIPE experiment, devoted to the study the polarization of the Cosmic Microwave Background. [ABSTRACT FROM AUTHOR]

Published
2022
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4. 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., and Pettinari, G.

Subjects
COSMIC background radiation, REFLECTANCE, MEASURING instruments
Abstract

COSMO is a ground-based instrument to measure the spectral distortions (SD) of the Cosmic Microwave Background (CMB). In this paper, we present preliminary results of electromagnetic simulations of its reference blackbody calibrator. HFSS simulations provide a calibrator reflection coefficient of R ∼ 10 - 6 , corresponding to an emissivity ϵ = 1 - R = 0.999999 . We also provide a forecast for the instrument performance by using an ILC-based simulation. We show that COSMO can extract the isotropic Comptonization parameter (modeled as | y | = 1.77 · 10 - 6 ) as | y | = (1.79 ± 0.19) · 10 - 6 , in the presence of the main Galactic foreground (thermal dust) and of CMB anisotropies, and assuming perfect atmospheric emission removal. [ABSTRACT FROM AUTHOR]

Published
2022
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5. MISTRAL and its KIDs.

Author

Paiella, A., de Bernardis, P., Cacciotti, F., Coppolecchia, A., Masi, S., Barbavara, E., Battistelli, E. S., Carretti, E., Columbro, F., Cruciani, A., D'Alessandro, G., De Petris, M., Govoni, F., Isopi, G., Lamagna, L., Marongiu, P., Mele, L., Molinari, E., Murgia, M., and Navarrini, A.

Subjects
FOCAL planes, RADIO telescopes, LUMPED elements, ASTROPHYSICS, ASTRONOMICAL surveys, SYSTEMS theory
Abstract

The MIllimetric Sardinia radio Telescope Receiver based on Array of Lumped elements KIDs, MISTRAL, is a cryogenic W-band (77–103 GH) LEKID camera which will be integrated at the Gregorian focus of the 64 m aperture Sardinia Radio Telescope, in Italy, in Autumn 2022. This instrument, thanks to its high angular resolution ( ∼ 13 arcsec ) and the wide instantaneous field of view ( ∼ 4 arcmin ), will allow continuum surveys of the mm-wave sky with a variety of scientific targets, spanning from extragalactic astrophysics to solar system science. In this contribution, we will describe the design of the MISTRAL camera, with a particular focus on the optimisation and test of a prototype of the focal plane. [ABSTRACT FROM AUTHOR]

Published
2022
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6. A chemically etched corrugated feedhorn array for D-band CMB observations.

Author

Mandelli, S., Manzan, E., Mennella, A., Cavaliere, F., Viganò, D., Franceschet, C., de Bernardis, P., Bersanelli, M., Castellano, M. G., Coppolecchia, A., Cruciani, A., Gervasi, M., Lamagna, L., Limonta, A., Masi, S., Paiella, A., Passerini, A., Pettinari, G., Piacentini, F., and Tommasi, E.

Subjects
COSMIC background radiation, ELECTROMAGNETIC measurements, ALUMINUM plates, ETCHING, TEMPERATURE measurements
Abstract

We present the design, manufacturing, and testing of a 37-element array of corrugated feedhorns for Cosmic Microwave Background CMB) measurements between 140 and 170 GHz. The array was designed to be coupled to Kinetic Inductance Detector arrays, either directly (for total power measurements) or through an orthomode transducer (for polarization measurements). We manufactured the array in platelets by chemically etching aluminum plates of 0.3 mm and 0.4 mm thickness. The process is fast, low-cost, scalable, and yields high-performance antennas compared to other techniques in the same frequency range. Room temperature electromagnetic measurements show excellent repeatability with an average cross polarization level about − 20 dB, return loss about − 25 dB, first sidelobes below − 25 dB and far sidelobes below − 35 dB. Our results qualify this process as a valid candidate for state-of-the-art CMB experiments, where large detector arrays with high sensitivity and polarization purity are of paramount importance in the quest for the discovery of CMB polarization B-modes. [ABSTRACT FROM AUTHOR]

Published
2021
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7. Selective Laser Melting Process of Al–Based Pyramidal Horns for the W-Band: Fabrication and Testing.

Author

Lamagna, L., Paiella, A., Masi, S., Bottini, L., Boschetto, A., and Veniali, F.

Subjects
*HORN antennas, *MELTING, *LASERS, *SURFACE roughness
Abstract

In the context of exploring the possibility of using Al-powder Selective Laser Melting to fabricate horn antennas for astronomical applications at millimeter wavelengths, we describe the design, the fabrication, the mechanical characterization, and the electromagnetic performance of additive manufactured horn antennas for the W-band. Our aim, in particular, is to evaluate the performance impact of two basic kinds of surface post-processing (manual grinding and sand-blasting) to deal with the well-known issue of high surface roughness in 3D printed devices. We performed comparative tests of co-polar and cross-polar angular response across the whole W-band, assuming a commercially available rectangular horn antenna as a reference. Based on gain and directivity measurements of the manufactured samples, we find decibel-level detectable deviations from the behavior of the reference horn antenna, and marginal evidence of performance degradation at the top edge of the W-band. We conclude that both kinds of post-processing allow achieving good performance for the W-band, but the higher reliability and uniformity of the sand-blasting post-process encourage exploring similar techniques for further development of aluminum devices at these frequencies. [ABSTRACT FROM AUTHOR]

Published
2021
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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., and Coppolecchia, A.

Subjects
*COSMIC background radiation, *GRAVITY waves, *EXPLORERS, *PROGRESS, *POLARISCOPE
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. [ABSTRACT FROM AUTHOR]

Published
2020
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9. SWIPE Multi-mode Pixel Assembly Design and Beam Pattern Measurements at Cryogenic Temperature.

Author

Columbro, F., Madonia, P. G., Lamagna, L., Battistelli, E. S., Coppolecchia, A., de Bernardis, P., Gualtieri, R., Masi, S., Paiella, A., Piacentini, F., Presta, G., Biasotti, M., D'Alessandro, G., Gatti, F., Mele, L., and Siri, B.

Subjects
BOLOMETERS, PIXELS, TEMPERATURE measurements, METAL mesh, DESIGN, ARTIFICIAL rubber, DETECTORS
Abstract

In this paper, we present beam pattern tests performed on the SWIPE multi-mode bolometric detector pixel assembly. A 20-mm-aperture horn is coupled to a large detector absorber (10 mm diameter) with a TES sensor located on the side. The pixel assembly has been tested at the bolometer base temperature of 340 mK, inside a custom cryogenic test bed, looking at a Gunn oscillator (128 GHz) located in the far field. We developed a custom cryogenic neoprene absorber, in addition to the stack of standard metal meshes low-pass filters, to reduce the background on the detector at a level similar to the one expected in flight, allowing to measure the main beam of the pixel assembly. The measured FWHM is 21 ∘ , slightly narrower than the expected one (24 ∘ ), due to vignetting produced by the filters stack. [ABSTRACT FROM AUTHOR]

Published
2020
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10. In-Flight Performance of the LEKIDs of the OLIMPO Experiment.

Author

Paiella, A., Ade, P. A. R., Battistelli, E. S., Castellano, M. G., Colantoni, I., Columbro, F., Coppolecchia, A., D'Alessandro, G., de Bernardis, P., De Petris, M., Gordon, S., Lamagna, L., Magneville, C., Masi, S., Mauskopf, P., Pettinari, G., Piacentini, F., Pisano, G., Polenta, G., and Presta, G.

Subjects
COSMIC rays, FOURIER transform spectrometers, DIFFRACTION patterns, LUMPED elements, SPACE environment, TELESCOPES
Abstract

We describe the in-flight performance of the horn-coupled lumped element kinetic inductance detector arrays of the balloon-borne OLIMPO experiment. These arrays have been designed to match the spectral bands of OLIMPO: 150, 250, 350, and 460 GHz , and they have been operated at 0.3 K and at an altitude of 37.8 km during the stratospheric flight of the OLIMPO payload, in Summer 2018. During the first hours of flight, we tuned the detectors and verified their large dynamics under the radiative background variations due to elevation increase of the telescope and to the insertion of the plug-in room-temperature differential Fourier transform spectrometer into the optical chain. We have found that the detector noise equivalent powers are close to be photon noise limited and lower than those measured on the ground. Moreover, the data contamination due to primary cosmic rays hitting the arrays is less than 3% for all the pixels of all the arrays and less than 1% for most of the pixels. These results can be considered the first step of KID technology validation in a representative space environment. [ABSTRACT FROM AUTHOR]

Published
2020
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11. W-band Lumped Element Kinetic Inductance Detector Array for Large Ground-Based Telescopes.

Author

Coppolecchia, A., Paiella, A., Lamagna, L., Presta, G., Battistelli, E. S., de Bernardis, P., Castellano, M. G., Columbro, F., Masi, S., Mele, L., Pettinari, G., and Piacentini, F.

Subjects
LUMPED elements, ELECTRIC inductance, RADIO telescopes, DETECTORS, QUALITY factor, TELESCOPES, RESONATORS
Abstract

We describe the development of a W-band lumped element kinetic inductance detector array for application in large ground-based telescopes, like the Sardinia radio telescope. Based on the previous studies, we use a Ti/Al bi-layer film (10 nm thick Ti + 25 nm thick Al) for the resonators, to cover frequencies greater than 65 GHz. Optical simulations have been performed using ANSYS HFSS software suite, to optimize the absorber geometry, the illumination configuration, and the thickness of the dielectric substrate. Simulations suggest that the best geometry of the absorber is a front-illuminated third-order Hilbert curve, with a Si substrate 235 μ m thick, coupled to a single-mode circular waveguide. Electrical simulations have been performed using SONNET, to complete the design of the detectors by choosing the size of the capacitor, the bias coupling, and the feedline. In addition, the electrical simulations allow us to verify the lumped condition, to tune the feedline impedance and resonant frequencies, to constrain the coupling quality factor, and to minimize the electrical cross-talk between different pixels of the same array. [ABSTRACT FROM AUTHOR]

Published
2020
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12. Multi-mode TES Bolometer Optimization for the LSPE-SWIPE Instrument.

Author

Gualtieri, R., Battistelli, E., Cruciani, A., Bernardis, P., Biasotti, M., Corsini, D., Gatti, F., Lamagna, L., and Masi, S.

Subjects
PARTICLE detectors, BOLOMETERS, PROCESS optimization, WAVELENGTHS, POLARISCOPE, CRYOSTATS
Abstract

In this paper, we explore the possibility of using transition edge sensor (TES) detectors in multi-mode configuration in the focal plane of the Short Wavelength Instrument for the Polarization Explorer (SWIPE) of the balloon-borne polarimeter Large-Scale Polarization Explorer (LSPE) for the Cosmic Microwave Background (CMB) polarization. This study is motivated by the fact that maximizing the sensitivity of TES bolometers, under the augmented background due to the multi-mode design, requires a non-trivial choice of detector parameters. We evaluate the best parameter combination taking into account scanning strategy, noise constraints, saturation power, and operating temperature of the cryostat during the flight. [ABSTRACT FROM AUTHOR]

Published
2016
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13. The MISTRAL Instrument and the Characterization of Its Detector Array.

Author

Paiella, A., Cacciotti, F., Isopi, G., Barbavara, E., Battistelli, E. S., de Bernardis, P., Capalbo, V., Carbone, A., Carretti, E., Ciccalotti, E., Columbro, F., Coppolecchia, A., Cruciani, A., D’Alessandro, G., De Petris, M., Govoni, F., Lamagna, L., Levati, E., Marongiu, P., and Mascia, A.

Subjects
*FOCAL planes, *RADIO telescopes, *OPTICAL detectors, *OPTICAL measurements, *LUMPED elements
Abstract

The MIllimeter Sardinia radio Telescope Receiver based on Array of Lumped elements KIDs, MISTRAL, is a cryogenic LEKID camera, operating in the W band (77-103GHz\documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$${77}{-}{103\,\textrm{GHz}}$$\end{document}) from the Gregorian focus of the 64-m aperture Sardinia Radio Telescope (SRT), in Italy. This instrument features a high angular resolution (∼12arcsec\documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$\sim {12\,\textrm{arcsec}}$$\end{document}) and a wide instantaneous field of view (∼4arcmin\documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$\sim {4\,\textrm{arcmin}}$$\end{document}), allowing continuum surveys of the mm-wave sky with many scientific targets, including observations of galaxy clusters via the Sunyaev–Zel’dovich effect. In May 2023, MISTRAL has been installed at SRT for the technical commissioning. In this contribution, we will describe the MISTRAL instrument focusing on the laboratory characterization of its focal plane: a ∼400\documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$\sim {400}$$\end{document}-pixel LEKID array. We will show the optical performance of the detectors highlighting the procedure for the identification of the pixels on the focal plane, the measurements of the optical responsivity and NEP, and the estimation of the optical efficiency. [ABSTRACT FROM AUTHOR]

Published
2024
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