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1. QUIJOTE scientific results -- XVIII. New constraints on the polarization of the Anomalous Microwave Emission in bright Galactic regions: $\rho$\,Ophiuchi, Perseus and W43

Author: González-González, R., Génova-Santos, R. T., Rubiño-Martín, J. A., Peel, M. W., Guidi, F., López-Caraballo, C. H., Fernández-Torreiro, M., Rebolo, R., Hernández-Monteagudo, C., Adak, D., Artal, E., Ashdown, M., Barreiro, R. B., Casas, F. J., de la Hoz, E., Fasano, A., Herranz, D., Hoyland, R. J., Martínez-González, E., Pascual-Cisneros, G., Piccirillo, L., Poidevin, F., Ruiz-Granados, B., Tramonte, D., Vansyngel, F., Vielva, P., and Watson, R. A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This work focuses on the study of the AME, an important emission mechanism between 10 and 60 GHz whose polarization properties are not yet fully understood, and is therefore a potential contaminant for future CMB polarization observations. We use new QUIJOTE-MFI maps 11, 13, 17 and 19 GHz, together with other public ancillary data including WMAP and Planck, to study the polarization properties of the AME in three Galactic regions: rho-Ophiuchi, Perseus and W43. We have obtained the SEDs for those three regions over the frequency range 0.4-3000 GHz, both in intensity and polarization. The intensity SEDs are well described by a combination of free-free emission, thermal dust, AME and CMB anisotropies. In polarization, we extracted the flux densities using all available data between 11 and 353 GHz. We implemented an improved intensity-to-polarization leakage correction that has allowed for the first time to derive reliable polarization constraints well below the 1% level from Planck-LFI data. A frequency stacking of maps in the range 10-60 GHz has allowed us to reduce the statistical noise and to push the upper limits on the AME polarization level. We have obtained upper limits on the AME polarization fraction of order <1% (95% confidence level) for the three regions. In particular we get Pi_AME < 1.1% (at 28.4 GHz), Pi_AME < 1.1% (at 22.8 GHz) and Pi_AME < 0.28% (at 33 GHz) in rho-Ophiuchi, Perseus and W43 respectively. At the QUIJOTE 17 GHz frequency band, we get Pi_AME< 5.1% for rho-Ophiuchi, Pi_AME< 3.5% for Perseus and Pi_AME< 0.85% for W43. Our final upper limits derived using the stacking procedure are Pi_AME < 0.58% for rho-Ophiuchi, Pi_AME < 1.64% for Perseus and Pi_AME < 0.31% for W43. Altogether, these are the most stringent constraints to date on the AME polarization fraction of these three star-forming regions., Comment: 26 pages. 15 figures. Submitted to A&A. Comments welcome
Published: 2024

2. Multi-dimensional optimisation of the scanning strategy for the LiteBIRD space mission

Author: Takase, Y., Vacher, L., Ishino, H., Patanchon, G., Montier, L., Stever, S. L., Ishizaka, K., Nagano, Y., Wang, W., Aumont, J., Aizawa, K., Anand, A., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Bersanelli, M., Bortolami, M., Brinckmann, T., Calabrese, E., Campeti, P., Carinos, E., Carones, A., Casas, F. J., Cheung, K., Clermont, L., Columbro, F., Coppolecchia, A., Cuttaia, F., de Bernardis, P., de Haan, T., de la Hoz, E., Della Torre, S., Diego-Palazuelos, P., D'Alessandro, G., Eriksen, H. K., Errard, J., Finelli, F., Fuskeland, U., Galloni, G., Galloway, M., Gervasi, M., Ghigna, T., Giardiello, S., Gimeno-Amo, C., Gjerløw, E., González, R. González, Gruppuso, A., Hazumi, M., Henrot-Versillé, S., Hergt, L. T., Ikuma, K., Kohri, K., Lamagna, L., Lattanzi, M., Leloup, C., Lembo, M., Levrier, F., Lonappan, A. I., López-Caniego, M., Luzzi, G., Maffei, B., Martínez-González, E., Masi, S., Matarrese, S., Matsuda, F. T., Matsumura, T., Micheli, S., Migliaccio, M., Monelli, M., Morgante, G., Mot, B., Nagata, R., Namikawa, T., Novelli, A., Odagiri, K., Oguri, S., Omae, R., Pagano, L., Paoletti, D., Piacentini, F., Pinchera, M., Polenta, G., Porcelli, L., Raffuzzi, N., Remazeilles, M., Ritacco, A., Ruiz-Granda, M., Sakurai, Y., Scott, D., Sekimoto, Y., Shiraishi, M., Signorelli, G., Sullivan, R. M., Takakura, H., Terenzi, L., Tomasi, M., Tristram, M., van Tent, B., Vielva, P., Wehus, I. K., Westbrook, B., Weymann-Despres, G., Wollack, E. J., Zannoni, M., and Zhou, Y.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Large angular scale surveys in the absence of atmosphere are essential for measuring the primordial $B$-mode power spectrum of the Cosmic Microwave Background (CMB). Since this proposed measurement is about three to four orders of magnitude fainter than the temperature anisotropies of the CMB, in-flight calibration of the instruments and active suppression of systematic effects are crucial. We investigate the effect of changing the parameters of the scanning strategy on the in-flight calibration effectiveness, the suppression of the systematic effects themselves, and the ability to distinguish systematic effects by null-tests. Next-generation missions such as LiteBIRD, modulated by a Half-Wave Plate (HWP), will be able to observe polarisation using a single detector, eliminating the need to combine several detectors to measure polarisation, as done in many previous experiments and hence avoiding the consequent systematic effects. While the HWP is expected to suppress many systematic effects, some of them will remain. We use an analytical approach to comprehensively address the mitigation of these systematic effects and identify the characteristics of scanning strategies that are the most effective for implementing a variety of calibration strategies in the multi-dimensional space of common spacecraft scan parameters. We also present Falcons, a fast spacecraft scanning simulator that we developed to investigate this scanning parameter space.
Published: 2024

3. LiteBIRD Science Goals and Forecasts. Mapping the Hot Gas in the Universe

Author: Remazeilles, M., Douspis, M., Rubiño-Martín, J. A., Banday, A. J., Chluba, J., de Bernardis, P., De Petris, M., Hernández-Monteagudo, C., Luzzi, G., Macias-Perez, J., Masi, S., Namikawa, T., Salvati, L., Tanimura, H., Aizawa, K., Anand, A., Aumont, J., Baccigalupi, C., Ballardini, M., Barreiro, R. B., Bartolo, N., Basak, S., Bersanelli, M., Blinov, D., Bortolami, M., Brinckmann, T., Calabrese, E., Campeti, P., Carinos, E., Carones, A., Casas, F. J., Cheung, K., Clermont, L., Columbro, F., Coppolecchia, A., Cuttaia, F., de Haan, T., de la Hoz, E., Della Torre, S., Diego-Palazuelos, P., D'Alessandro, G., Eriksen, H. K., Finelli, F., Fuskeland, U., Galloni, G., Galloway, M., Gervasi, M., Génova-Santos, R. T., Ghigna, T., Giardiello, S., Gimeno-Amo, C., Gjerløw, E., González, R. González, Gruppuso, A., Hazumi, M., Henrot-Versillé, S., Hergt, L. T., Herranz, D., Kohri, K., Komatsu, E., Lamagna, L., Lattanzi, M., Leloup, C., Levrier, F., Lonappan, A. I., López-Caniego, M., Maffei, B., Martínez-González, E., Matarrese, S., Matsumura, T., Micheli, S., Migliaccio, M., Monelli, M., Montier, L., Morgante, G., Nagano, Y., Nagata, R., Novelli, A., Omae, R., Pagano, L., Paoletti, D., Pavlidou, V., Piacentini, F., Pinchera, M., Polenta, G., Porcelli, L., Ritacco, A., Ruiz-Granda, M., Sakurai, Y., Scott, D., Shiraishi, M., Stever, S. L., Sullivan, R. M., Takase, Y., Tassis, K., Terenzi, L., Tomasi, M., Tristram, M., Vacher, L., van Tent, B., Vielva, P., Wehus, I. K., Westbrook, B., Weymann-Despres, G., Wollack, E. J., Zannoni, M., and Zhou, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We assess the capabilities of the LiteBIRD mission to map the hot gas distribution in the Universe through the thermal Sunyaev-Zeldovich (SZ) effect. Our analysis relies on comprehensive simulations incorporating various sources of Galactic and extragalactic foreground emission, while accounting for specific instrumental characteristics of LiteBIRD, such as detector sensitivities, frequency-dependent beam convolution, inhomogeneous sky scanning, and $1/f$ noise. We implement a tailored component-separation pipeline to map the thermal SZ Compton $y$-parameter over 98% of the sky. Despite lower angular resolution for galaxy cluster science, LiteBIRD provides full-sky coverage and, compared to the Planck satellite, enhanced sensitivity, as well as more frequency bands to enable the construction of an all-sky $y$-map, with reduced foreground contamination at large and intermediate angular scales. By combining LiteBIRD and Planck channels in the component-separation pipeline, we obtain an optimal $y$-map that leverages the advantages of both experiments, with the higher angular resolution of the Planck channels enabling the recovery of compact clusters beyond the LiteBIRD beam limitations, and the numerous sensitive LiteBIRD channels further mitigating foregrounds. The added value of LiteBIRD is highlighted through the examination of maps, power spectra, and one-point statistics of the various sky components. After component separation, the $1/f$ noise from LiteBIRD is effectively mitigated below the thermal SZ signal at all multipoles. Cosmological constraints on $S_8=\sigma_8\left(\Omega_{\rm m}/0.3\right)^{0.5}$ obtained from the LiteBIRD-Planck combined $y$-map power spectrum exhibits a 15% reduction in uncertainty compared to constraints from Planck alone. This improvement can be attributed to the increased portion of uncontaminated sky available in the LiteBIRD-Planck combined $y$-map., Comment: 38 pages, 13 figures, abstract shortened. Updated to match version accepted by JCAP
Published: 2024

4. The LiteBIRD mission to explore cosmic inflation

Author: Ghigna, T., Adler, A., Aizawa, K., Akamatsu, H., Akizawa, R., Allys, E., Anand, A., Aumont, J., Austermann, J., Azzoni, S., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Basyrov, A., Beckman, S., Bersanelli, M., Bortolami, M., Bouchet, F., Brinckmann, T., Campeti, P., Carinos, E., Carones, A., Casas, F. J., Cheung, K., Chinone, Y., Clermont, L., Columbro, F., Coppolecchia, A., Curtis, D., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Monache, G. Delle, Di Giorgi, E., Dickinson, C., Diego-Palazuelos, P., García, J. J. Díaz, Dobbs, M., Dotani, T., D'Alessandro, G., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Farias, N., Ferreira, E., Franceschet, C., Fuskeland, U., Galloni, G., Galloway, M., Ganga, K., Gerbino, M., Gervasi, M., Génova-Santos, R. T., Giardiello, S., Gimeno-Amo, C., Gjerløw, E., González, R. González, Grandsire, L., Gruppuso, A., Halverson, N. W., Hargrave, P., Harper, S. E., Hazumi, M., Henrot-Versillé, S., Hergt, L. T., Herranz, D., Hivon, E., Hlozek, R. A., Hoang, T. D., Hubmayr, J., Ichiki, K., Ikuma, K., Ishino, H., Jaehnig, G., Jost, B., Kohri, K., Konishi, K., Lamagna, L., Lattanzi, M., Leloup, C., Levrier, F., Lonappan, A. I., Luzzi, G., Macias-Perez, J., Maffei, B., Marchitelli, E., Martínez-González, E., Masi, S., Matarrese, S., Matsumura, T., Micheli, S., Migliaccio, M., Monelli, M., Montier, L., Morgante, G., Mousset, L., Nagano, Y., Nagata, R., Natoli, P., Novelli, A., Noviello, F., Obata, I., Occhiuzzi, A., Odagiri, K., Omae, R., Pagano, L., Paiella, A., Paoletti, D., Pascual-Cisneros, G., Patanchon, G., Pavlidou, V., Piacentini, F., Piat, M., Piccirilli, G., Pinchera, M., Pisano, G., Porcelli, L., Raffuzzi, N., Raum, C., Remazeilles, M., Ritacco, A., Rubino-Martin, J., Ruiz-Granda, M., Sakurai, Y., Savini, G., Scott, D., Sekimoto, Y., Shiraishi, M., Signorelli, G., Stever, S. L., Sullivan, R. M., Suzuki, A., Takaku, R., Takakura, H., Takakura, S., Tartari, Y. Takase. A., Tassis, K., Thompson, K. L., Tomasi, M., Tristram, M., Tucker, C., Vacher, L., van Tent, B., Vielva, P., Watanuki, K., Wehus, I. K., Westbrook, B., Weymann-Despres, G., Winter, B., Wollack, E. J., Zacchei, A., Zannoni, M., Zhou, Y., and Collaboration, the LiteBIRD
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Physics - Instrumentation and Detectors
Abstract: LiteBIRD, the next-generation cosmic microwave background (CMB) experiment, aims for a launch in Japan's fiscal year 2032, marking a major advancement in the exploration of primordial cosmology and fundamental physics. Orbiting the Sun-Earth Lagrangian point L2, this JAXA-led strategic L-class mission will conduct a comprehensive mapping of the CMB polarization across the entire sky. During its 3-year mission, LiteBIRD will employ three telescopes within 15 unique frequency bands (ranging from 34 through 448 GHz), targeting a sensitivity of 2.2\,$\mu$K-arcmin and a resolution of 0.5$^\circ$ at 100\,GHz. Its primary goal is to measure the tensor-to-scalar ratio $r$ with an uncertainty $\delta r = 0.001$, including systematic errors and margin. If $r \geq 0.01$, LiteBIRD expects to achieve a $>5\sigma$ detection in the $\ell=$2-10 and $\ell=$11-200 ranges separately, providing crucial insight into the early Universe. We describe LiteBIRD's scientific objectives, the application of systems engineering to mission requirements, the anticipated scientific impact, and the operations and scanning strategies vital to minimizing systematic effects. We will also highlight LiteBIRD's synergies with concurrent CMB projects., Comment: 23 pages, 9 figures, 1 table, SPIE Astronomical Telescopes + Instrumentation 2024
Published: 2024

5. QUIJOTE Scientific Results -- XVII. Studying the Anomalous Microwave Emission in the Andromeda Galaxy with QUIJOTE-MFI

Author: Fernández-Torreiro, M., Génova-Santos, R. T., Rubiño-Martín, J. A., López-Caraballo, C. H., Peel, M. W., Arce-Tord, C., Rebolo, R., Artal, E., Ashdown, M., Barreiro, R. B., Casas, F. J., de la Hoz, E., Guidi, F., Herranz, D., Hoyland, R., Lasenby, A., Martínez-Gonzalez, E., Piccirillo, L., Poidevin, F., Ruiz-Granados, B., Tramonte, D., Vansyngel, F., Vielva, P., and Watson, R. A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The Andromeda Galaxy (M31) is the Local Group galaxy that is most similar to the Milky Way (MW). The similarities between the two galaxies make M31 useful for studying integrated properties common to spiral galaxies. We use the data from the recent QUIJOTE-MFI Wide Survey, together with new raster observations focused on M31, to study its integrated emission. The addition of raster data improves the sensitivity of QUIJOTE-MFI maps by almost a factor 3. Our main interest is to confirm if anomalous microwave emission (AME) is present in M31, as previous studies have suggested. To do so, we built the integrated spectral energy distribution of M31 between 0.408 and 3000 GHz. We then performed a component separation analysis taking into account synchrotron, free-free, AME and thermal dust components. AME in M31 is modelled as a log-normal distribution with maximum amplitude, $A_{\rm AME}$, equal to $1.03\pm0.32$ Jy. It peaks at $\nu_{\rm AME}=17.2\pm3.2$ GHz with a width of $W_{\rm AME}=0.58\pm0.16$. Both the Akaike and Bayesian Information Criteria find the model without AME to be less than 1 % as probable as the one taking AME into consideration. We find that the AME emissivity per 100 $\mu$m intensity in M31 is $\epsilon_{\rm AME}^{\rm 28.4\,GHz}=9.6\pm3.1$ $\mu$K/(MJy/sr), similar to that computed for the MW. We also provide the first upper limits for the AME polarization fraction in an extragalactic object. M31 remains the only galaxy where an AME measurement has been made of its integrated spectrum., Comment: 17 pages, 9 figures. Accepted for publication in MNRAS. QUIJOTE data maps available at https://research.iac.es/proyecto/quijote
Published: 2023
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6. QUIJOTE scientific results -- X. Spatial variations of Anomalous Microwave Emission along the Galactic plane

Author: Fernández-Torreiro, M., Rubiño-Martín, J. A., López-Caraballo, C. H., Génova-Santos, R. T., Peel, M. W., Guidi, F., Harper, S. E., Artal, E., Ashdown, M., Barreiro, R. B., Casas, F. J., de la Hoz, E., Herranz, D., Hoyland, R., Lasenby, A., Martínez-Gonzalez, E., Piccirillo, L., Poidevin, F., Rebolo, R., Ruiz-Granados, B., Tramonte, D., Vansyngel, F., Vielva, P., and Watson, R. A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Anomalous Microwave Emission (AME) is an important emission component between 10 and 60 GHz that is not yet fully understood. It seems to be ubiquituous in our Galaxy and is observed at a broad range of angular scales. Here we use the new QUIJOTE-MFI wide survey data at 11, 13, 17 and 19 GHz to constrain the AME in the Galactic plane ($|b|<10^\circ$) on degree scales. We built the spectral energy distribution between 0.408 and 3000 GHz for each of the 5309 0.9$^\circ$ pixels in the Galactic plane, and fitted a parametric model by considering five emission components: synchrotron, free-free, AME, thermal dust and CMB anisotropies. We show that not including QUIJOTE-MFI data points leads to the underestimation (up to 50 %) of the AME signal in favour of free-free emission. The parameters describing these components are then intercompared, looking for relations that help to understand AME physical processes. We find median values for the AME width, $W_{\rm AME}$, and for its peak frequency, $\nu_{\rm AME}$, respectively of $0.560^{+0.059}_{-0.050}$ and $20.7^{+2.0}_{-1.9}$ GHz, slightly in tension with current theoretical models. We find spatial variations throughout the Galactic plane for $\nu_{\rm AME}$, but only with reduced statistical significance. We report correlations of AME parameters with certain ISM properties, such as that between the AME emissivity (which shows variations with the Galactic longitude) and the interstellar radiation field, and that between the AME peak frequency and dust temperature. Finally, we discuss the implications of our results on the possible molecules responsible for AME., Comment: 32 pages, 31 figures. Accepted for publication in MNRAS. Derived data products available at https://research.iac.es/proyecto/quijote
Published: 2023
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7. Tensor-to-scalar ratio forecasts for extended LiteBIRD frequency configurations

Author: Fuskeland, U., Aumont, J., Aurlien, R., Baccigalupi, C., Banday, A. J., Eriksen, H. K., Errard, J., Génova-Santos, R. T., Hasebe, T., Hubmayr, J., Imada, H., Krachmalnicoff, N., Lamagna, L., Pisano, G., Poletti, D., Remazeilles, M., Thompson, K. L., Vacher, L., Wehus, I. K., Azzoni, S., Ballardini, M., Barreiro, R. B., Bartolo, N., Basyrov, A., Beck, D., Bersanelli, M., Bortolami, M., Brilenkov, M., Calabrese, E., Carones, A., Casas, F. J., Cheung, K., Chluba, J., Clark, S. E., Clermont, L., Columbro, F., Coppolecchia, A., D'Alessandro, G., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Diego-Palazuelos, P., Finelli, F., Franceschet, C., Galloni, G., Galloway, M., Gerbino, M., Gervasi, M., Ghigna, T., Giardiello, S., Gjerløw, E., Gruppuso, A., Hargrave, P., Hattori, M., Hazumi, M., Hergt, L. T., Herman, D., Herranz, D., Hivon, E., Hoang, T. D., Kohri, K., Lattanzi, M., Lee, A. T., Leloup, C., Levrier, F., Lonappan, A. I., Luzzi, G., Maffei, B., Martínez-González, E., Masi, S., Matarrese, S., Matsumura, T., Migliaccio, M., Montier, L., Morgante, G., Mot, B., Mousset, L., Nagata, R., Namikawa, T., Nati, F., Natoli, P., Nerval, S., Novelli, A., Pagano, L., Paiella, A., Paoletti, D., Pascual-Cisneros, G., Patanchon, G., Pelgrims, V., Piacentini, F., Piccirilli, G., Polenta, G., Puglisi, G., Raffuzzi, N., Ritacco, A., Rubino-Martin, J. A., Savini, G., Scott, D., Sekimoto, Y., Shiraishi, M., Signorelli, G., Stever, S. L., Stutzer, N., Sullivan, R. M., Takakura, H., Terenzi, L., Thommesen, H., Tristram, M., Tsuji, M., Vielva, P., Weller, J., Westbrook, B., Weymann-Despres, G., Wollack, E. J., and Zannoni, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: LiteBIRD is a planned JAXA-led CMB B-mode satellite experiment aiming for launch in the late 2020s, with a primary goal of detecting the imprint of primordial inflationary gravitational waves. Its current baseline focal-plane configuration includes 15 frequency bands between 40 and 402 GHz, fulfilling the mission requirements to detect the amplitude of gravitational waves with the total uncertainty on the tensor-to-scalar ratio, $\delta r$, down to $\delta r<0.001$. A key aspect of this performance is accurate astrophysical component separation, and the ability to remove polarized thermal dust emission is particularly important. In this paper we note that the CMB frequency spectrum falls off nearly exponentially above 300 GHz relative to the thermal dust SED, and a relatively minor high frequency extension can therefore result in even lower uncertainties and better model reconstructions. Specifically, we compare the baseline design with five extended configurations, while varying the underlying dust modeling, in each of which the HFT (High-Frequency Telescope) frequency range is shifted logarithmically towards higher frequencies, with an upper cutoff ranging between 400 and 600 GHz. In each case, we measure the tensor-to-scalar ratio $r$ uncertainty and bias using both parametric and minimum-variance component-separation algorithms. When the thermal dust sky model includes a spatially varying spectral index and temperature, we find that the statistical uncertainty on $r$ after foreground cleaning may be reduced by as much as 30--50 % by extending the upper limit of the frequency range from 400 to 600 GHz, with most of the improvement already gained at 500 GHz. We also note that a broader frequency range leads to better ability to discriminate between models through higher $\chi^2$ sensitivity. (abridged), Comment: 18 pages, 13 figures. Published in A&A
Published: 2023
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8. QUIJOTE scientific results -- IX. Radio sources in the QUIJOTE-MFI wide survey maps

Author: Herranz, D., López-Caniego, M., López-Caraballo, C. H., Génova-Santos, R. T., Perrott, Y. C., Rubiño-Martín, J. A., Rebolo, R., Artal, E., Ashdown, M., Barreiro, R. B., Casas, F. J., de la Hoz, E., Fernández-Torreiro, M., Guidi, F., Hoyland, R. J., Lasenby, A. N., Martínez-González, E., Peel, M. W., Piccirillo, L., Poidevin, F., Ruiz-Granados, B., Tramonte, D., Vansyngel, F., Vielva, P., and Watson, R. A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the catalogue of Q-U-I JOint TEnerife (QUIJOTE) Wide Survey radio sources extracted from the maps of the Multi-Frequency Instrument compiled between 2012 and 2018. The catalogue contains 786 sources observed in intensity and polarization, and is divided into two separate sub-catalogues: one containing 47 bright sources previously studied by the \emph{Planck} collaboration and an extended catalogue of 739 sources either selected from the \emph{Planck} Second Catalogue of Compact Sources or found through a blind search carried out with a Mexican Hat 2 wavelet. A significant fraction of the sources in our catalogue (38.7 per cent) are within the $|b| \leq 20^\circ$ region of the Galactic plane. We determine statistical properties for those sources that are likely to be extragalactic. We find that these statistical properties are compatible with currently available models, with a $\sim$1.8 Jy completeness limit at 11 GHz. We provide the polarimetric properties of (38, 33, 31, 23) sources with P detected above the $99.99\%$ significance level at (11, 13, 17, 19) GHz, respectively. Median polarization fractions are in the $2.8$-$4.7$\% range in the 11-19 GHz frequency interval. We do not distinguish between Galactic and extragalactic sources here. The results presented here are consistent with those reported in the literature for flat- and steep-spectrum radio sources., Comment: 21 pages, 13 figures, 7 tables
Published: 2023
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9. QUIJOTE scientific results -- VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI

Author: de la Hoz, E., Barreiro, R. B., Vielva, P., Martínez-González, E., Rubiño-Martín, J. A., Casaponsa, B., Guidi, F., Ashdown, M., Génova-Santos, R. T., Artal, E., Casas, F. J., Fernández-Cobos, R., Fernández-Torreiro, M., Herranz, D., Hoyland, R. J., Lasenby, A. N., López-Caniego, M., López-Caraballo, C. H., Peel, M. W., Piccirillo, L., Poidevin, F., Rebolo, R., Ruiz-Granados, B., Tramonte, D., Vansyngel, F., and Watson, R. A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We derive linearly polarized astrophysical component maps in the Northern Sky from the QUIJOTE-MFI data at 11 and 13 GHz in combination with the WMAP K and Ka bands (23 and 33 GHz) and all Planck polarized channels (30-353 GHz), using the parametric component separation method B-SeCRET. The addition of QUIJOTE-MFI data significantly improves the parameter estimation of the low-frequency foregrounds, especially the estimation of the synchrotron spectral index, $\beta_s$. We present the first detailed $\beta_s$ map of the Northern Celestial Hemisphere at a smoothing scale of $2^{\circ}$. We find statistically significant spatial variability across the sky. We obtain an average value of $-3.08$ and a dispersion of $0.13$, considering only pixels with reliable goodness-of-fit. The power law model of the synchrotron emission provides a good fit to the data outside the Galactic plane but fails to track the complexity within this region. Moreover, when we assume a synchrotron model with uniform curvature, $c_s$, we find a value of $c_s = -0.0797 \pm 0.0012$. However, there is insufficient statistical significance to determine which model is favoured, either the power law or the power law with uniform curvature. Furthermore, we estimate the thermal dust spectral parameters in polarization. Our CMB, synchrotron, and thermal dust maps are highly correlated with the corresponding products of the PR4 Planck release, although some large-scale differences are observed in the synchrotron emission. Finally, we find that the $\beta_s$ estimation in the high signal-to-noise synchrotron emission areas is prior-independent while, outside these regions, the prior governs the $\beta_s$ estimation., Comment: 25 pages, 29 figures, Accepted for publication in MNRAS
Published: 2023
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10. QUIJOTE Scientific Results -- VII. Galactic AME sources in the QUIJOTE-MFI Northern Hemisphere Wide-Survey

Author: Poidevin, F., Génova-Santos, R. T., Rubiño-Martín, J. A., López-Caraballo, C. H., Watson, R. A., Artal, E., Ashdown, M., Barreiro, R. B., Casas, F. J., de la Hoz, E., Fernández-Torreiro, M., Guidi, F., Herranz, D., Hoyland, R. J., Lasenby, A. N., Martinez-Gonzalez, E., Peel, M. W., Piccirillo, L., Rebolo, R., Ruiz-Granados, B., Tramonte, D., Vansyngel, F., and Vielva, P.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The QUIJOTE-MFI Northern Hemisphere Wide-Survey has provided maps of the sky above declinations $-30^\circ$ at 11, 13, 17 and 19$\,$GHz. These data are combined with ancillary data to produce Spectral Energy Distributions in intensity in the frequency range 0.4--3\,000$\,$GHz on a sample of 52 candidate compact sources harbouring anomalous microwave emission (AME). We apply a component separation analysis at 1$^\circ$ scale on the full sample from which we identify 44 sources with high AME significance. We explore correlations between different fitted parameters on this last sample. QUIJOTE-MFI data contribute to notably improve the characterisation of the AME spectrum, and its separation from the other components. In particular, ignoring the 10--20\,GHz data produces on average an underestimation of the AME amplitude, and an overestimation of the free-free component. We find an average AME peak frequency of 23.6 $\pm$ 3.6$\,$GHz, about 4$\,$GHz lower than the value reported in previous studies. The strongest correlation is found between the peak flux density of the thermal dust and of the AME component. A mild correlation is found between the AME emissivity ($A_{\rm AME}/\tau_{250}$) and the interstellar radiation field. On the other hand no correlation is found between the AME emissivity and the free-free radiation Emission Measure. Our statistical results suggest that the interstellar radiation field could still be the main driver of the intensity of the AME as regards spinning dust excitation mechanisms. On the other hand, it is not clear whether spinning dust would be most likely associated with cold phases of the interstellar medium rather than with hot phases dominated by free-free radiation., Comment: 36 pages. Accepted for publication in MNRAS. Maps and derived data products available at https://research.iac.es/proyecto/quijote/
Published: 2023
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11. QUIJOTE scientific results -- VI. The Haze as seen by QUIJOTE

Author: Guidi, F., Génova-Santos, R. T., Rubiño-Martín, J. A., Peel, M. W., Fernández-Torreiro, M., López-Caraballo, C. H., Vignaga, R., de la Hoz, E., Vielva, P., Watson, R. A., Ashdown, M., Dickinson, C., Artal, E., Barreiro, R. B., Casas, F. J., Herranz, D., Hoyland, R. J., Lasenby, A. N., Martinez-Gonzalez, E., Piccirillo, L., Poidevin, F., Rebolo, R., Ruiz-Granados, B., Tramonte, D., and Vansyngel, F.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: The Haze is an excess of microwave intensity emission surrounding the Galactic centre. It is spatially correlated with the $\gamma$-ray Fermi bubbles, and with the S-PASS radio polarization plumes, suggesting a possible common provenance. The models proposed to explain the origin of the Haze, including energetic events at the Galactic centre and dark matter decay in the Galactic halo, do not yet provide a clear physical interpretation. In this paper we present a re-analysis of the Haze including new observations from the Multi-Frequency Instrument (MFI) of the Q-U-I JOint TEnerife (QUIJOTE) experiment, at 11 and 13 GHz. We analyze the Haze in intensity and polarization, characterizing its spectrum. We detect an excess of diffuse intensity signal ascribed to the Haze. The spectrum at frequencies 11$\,\leq\nu\leq\,$70 GHz is a power-law with spectral index $\beta^{\rm H}=-2.79\pm0.08$, which is flatter than the Galactic synchrotron in the same region ($\beta^{\rm S}=-2.98\pm0.04$), but steeper than that obtained from previous works ($\beta^{\rm H}\sim-2.5$ at 23$\,\leq\,\nu\leq\,$70 GHz). We also observe an excess of polarized signal in the QUIJOTE-MFI maps in the Haze area. This is a first hint detection of polarized Haze, or a consequence of curvature of the synchrotron spectrum in that area. Finally, we show that the spectrum of polarized structures associated with Galactic centre activity is steep at low frequencies ($\beta \sim -3.2$ at 2.3 $\leq\nu\leq$ 23 GHz), and becomes flatter above 11 GHz., Comment: 31 pages. Accepted for publication in MNRAS
Published: 2023
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12. QUIJOTE scientific results -- V. The microwave intensity and polarisation spectra of the Galactic regions W49, W51 and IC443

Author: Tramonte, D., Génova-Santos, R. T., Rubiño-Martín, J. A., Vielva, P., Poidevin, F., López-Caraballo, C. H., Peel, M. W., Ashdown, M., Artal, E., Barreiro, R. B., Casas, F. J., de la Hoz, E., Fernández-Torreiro, M., Guidi, F., Herranz, D., Hoyland, R. J., Lasenby, A. N., Martinez-Gonzalez, E., Piccirillo, L., Rebolo, R., Ruiz-Granados, B., Vansyngel, F., and Watson, R. A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present new intensity and polarisation maps obtained with the QUIJOTE experiment towards the Galactic regions W49, W51 and IC443, covering the frequency range from 10 to 20 GHz at $\sim$ 1 deg angular resolution, with a sensitivity in the range 35-79 ${\mu}$K/beam for total intensity and 13-23 ${\mu}$K/beam for polarisation. For each region, we combine QUIJOTE maps with ancillary data at frequencies ranging from 0.4 to 3000 GHz, reconstruct the spectral energy distribution and model it with a combination of known foregrounds. We detect anomalous microwave emission (AME) in total intensity towards W49 at 4.7${\sigma}$ and W51 at 4.0${\sigma}$ with peak frequencies ${\nu}_{AME}$ = (20.0 $\pm$ 1.4) GHz and ${\nu}_{AME}$ = (17.7 $\pm$ 3.6) GHz respectively; this is the first detection of AME towards W51. The contamination from ultra-compact HII regions to the residual AME flux density is estimated at 10% in W49 and 5% in W51, and does not rule out the AME detection. The polarised SEDs reveal a synchrotron contribution with spectral indices ${\alpha}_s$ = -0.67 $\pm$ 0.10 in W49 and ${\alpha}_s$ = -0.51 $\pm$ 0.07 in W51, ascribed to the diffuse Galactic emission and to the local supernova remnant respectively. Towards IC443 in total intensity we measure a broken power-law synchrotron spectrum with cut-off frequency ${\nu}_{0,s}$ = (114 $\pm$ 73) GHz, in agreement with previous studies; our analysis, however, rules out any AME contribution which had been previously claimed towards IC443. No evidence of polarised AME emission is detected in this study., Comment: 29 pages, 11 figures. Accepted for publication in MNRAS
Published: 2023
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13. QUIJOTE scientific results -- IV. A northern sky survey in intensity and polarization at 10-20GHz with the Multi-Frequency Instrument

Author: Rubino-Martin, J. A., Guidi, F., Genova-Santos, R. T., Harper, S. E., Herranz, D., Hoyland, R. J., Lasenby, A. N., Poidevin, F., Rebolo, R., Ruiz-Granados, B., Vansyngel, F., Vielva, P., Watson, R. A., Artal, E., Ashdown, M., Barreiro, R. B., Bilbao-Ahedo, J. D., Casas, F. J., Casaponsa, B., Cepeda-Arroita, R., de la Hoz, E., Dickinson, C., Fernandez-Cobos, R., Fernandez-Torreiro, M., Gonzalez-Gonzalez, R., Hernandez-Monteagudo, C., Lopez-Caniego, M., Lopez-Caraballo, C., Martinez-Gonzalez, E., Peel, M. W., Pelaez-Santos, A. E., Perrott, Y., Piccirillo, L., Razavi-Ghods, N., Scott, P., Titterington, D., Tramonte, D., and Vignaga, R.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present QUIJOTE intensity and polarization maps in four frequency bands centred around 11, 13, 17 and 19GHz, and covering approximately 29000 deg$^2$, including most of the Northern sky region. These maps result from 9000 h of observations taken between May 2013 and June 2018 with the first QUIJOTE instrument (MFI), and have angular resolutions of around $1^\circ$, and sensitivities in polarization within the range 35-40 $\mu$K per 1-degree beam, being a factor $\sim 2$-$4$ worse in intensity. We discuss the data processing pipeline employed, and the basic characteristics of the maps in terms of real space statistics and angular power spectra. A number of validation tests have been applied to characterise the accuracy of the calibration and the residual level of systematic effects, finding a conservative overall calibration uncertainty of 5%. We also discuss flux densities for four bright celestial sources (Tau A, Cas A, Cyg A and 3C274) which are often used as calibrators at microwave frequencies. The polarization signal in our maps is dominated by synchrotron emission. The distribution of spectral index values between the 11GHz and WMAP 23GHz map peaks at $\beta=-3.09$ with a standard deviation of 0.14. The measured BB/EE ratio at scales of $\ell=80$ is $0.26\pm 0.07$ for a Galactic cut $|b|>10^\circ$. We find a positive TE correlation for 11GHz at large angular scales ($\ell \lesssim 50$), while the EB and TB signals are consistent with zero in the multipole range $30 \lesssim \ell \lesssim 150$. The maps discussed in this paper are publicly available., Comment: 60 pages. Accepted for publication in MNRAS. Maps and derived data products available at https://research.iac.es/proyecto/quijote/
Published: 2023
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14. Probing cosmic inflation with the LiteBIRD cosmic microwave background polarization survey

Author: Allys, E, Arnold, K, Aumont, J, Aurlien, R, Azzoni, S, Baccigalupi, C, Banday, AJ, Banerji, R, Barreiro, RB, Bartolo, N, Bautista, L, Beck, D, Beckman, S, Bersanelli, M, Boulanger, F, Brilenkov, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, FJ, Catalano, A, Chan, V, Cheung, K, Chinone, Y, Clark, SE, Columbro, F, D’Alessandro, G, de Bernardis, P, de Haan, T, de la Hoz, E, De Petris, M, Torre, S Della, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duval, JM, Elleflot, T, Eriksen, HK, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gerbino, M, Gervasi, M, Génova-Santos, RT, Ghigna, T, Giardiello, S, Gjerløw, E, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, JE, Halverson, NW, Hargrave, P, Hasebe, T, Hasegawa, M, Hazumi, M, Henrot-Versillé, S, Hensley, B, Hergt, LT, Herman, D, Hivon, E, Hlozek, RA, Hornsby, AL, Hoshino, Y, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishino, H, Jaehnig, G, Katayama, N, Kato, A, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kuo, CL, Lamagna, L, Lattanzi, M, Lee, AT, Leloup, C, Levrier, F, Linder, E, Luzzi, G, Macias-Perez, J, Maciaszek, T, Maffei, B, Maino, D, and Mandelli, S
Subjects: Particle and High Energy Physics, Space Sciences, Physical Sciences, Mathematical Sciences
Abstract: LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. The Japan Aerospace Exploration Agency (JAXA) selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with an expected launch in the late 2020s using JAXA’s H3 rocket. LiteBIRD is planned to orbit the Sun–Earth Lagrangian point L2, where it will map the cosmic microwave background polarization over the entire sky for three years, with three telescopes in 15 frequency bands between 34 and 448 GHz, to achieve an unprecedented total sensitivity of 2.2 μK-arcmin, with a typical angular resolution of 0.5◦ at 100 GHz. The primary scientific objective of LiteBIRD is to search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. We provide an overview of the LiteBIRD project, including scientific objectives, mission and system requirements, operation concept, spacecraft and payload module design, expected scientific outcomes, potential design extensions, and synergies with other projects.
Published: 2023

15. Robustness of cosmic birefringence measurement against Galactic foreground emission and instrumental systematics

Author: Diego-Palazuelos, P., Martínez-González, E., Vielva, P., Barreiro, R. B., Tristram, M., de la Hoz, E., Eskilt, J. R., Minami, Y., Sullivan, R. M., Banday, A. J., Górski, K. M., Keskitalo, R., Komatsu, E., and Scott, D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The polarization of the cosmic microwave background (CMB) can be used to search for parity-violating processes like that predicted by a Chern-Simons coupling to a light pseudoscalar field. Such an interaction rotates $E$ modes into $B$ modes in the observed CMB signal by an effect known as cosmic birefringence. Even though isotropic birefringence can be confused with the rotation produced by a miscalibration of the detectors' polarization angles the degeneracy between both effects is broken when Galactic foreground emission is used as a calibrator. In this work, we use realistic simulations of the High-Frequency Instrument of the Planck mission to test the impact that Galactic foreground emission and instrumental systematics have on the recent birefringence measurements obtained through this technique. Our results demonstrate the robustness of the methodology against the miscalibration of polarization angles and other systematic effects, like intensity-to-polarization leakage, beam leakage, or cross-polarization effects. However, our estimator is sensitive to the $EB$ correlation of polarized foreground emission. Here we propose to correct the bias induced by dust $EB$ by modeling the foreground signal with templates produced in Bayesian component-separation analyses that fit parametric models to CMB data. Acknowledging the limitations of currently available dust templates like that of the Commander sky model, high-precision CMB data and a characterization of dust beyond the modified blackbody paradigm are needed to obtain a definitive measurement of cosmic birefringence in the future., Comment: 36 pages, 19 figures, matches the version accepted for publication at JCAP
Published: 2022
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16. Robustness of cosmic birefringence measurement against Galactic foreground emission and instrumental systematics

Author: Diego-Palazuelos, P, Martínez-González, E, Vielva, P, Barreiro, RB, Tristram, M, de la Hoz, E, Eskilt, JR, Minami, Y, Sullivan, RM, Banday, AJ, Górski, KM, Keskitalo, R, Komatsu, E, and Scott, D
Subjects: Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics
Abstract: The polarization of the cosmic microwave background (CMB) can be used to search for parity-violating processes like that predicted by a Chern-Simons coupling to a light pseudoscalar field. Such an interaction rotates E modes into E modes in the observed CMB signal through an effect known as cosmic birefringence. Even though isotropic birefringence can be confused with the rotation produced by a miscalibration of the detectors' polarization angles, the degeneracy between both effects is broken when Galactic foreground emission is used as a calibrator. In this work, we use realistic simulations of the High-Frequency Instrument of the Planck mission to test the impact that Galactic foreground emission and instrumental systematics have on the recent birefringence measurements obtained through this technique. Our results demonstrate the robustness of the methodology against the miscalibration of polarization angles and other systematic effects, like intensity-to-polarization leakage, beam leakage, or cross-polarization effects. However, our estimator is sensitive to the EB correlation of polarized foreground emission. Here we propose to correct the bias induced by dust EB by modeling the foreground signal with templates produced in Bayesian component-separation analyses that fit parametric models to CMB data. Acknowledging the limitations of currently available dust templates like that of the Commander sky model, high-precision CMB data and a characterization of dust beyond the modified blackbody paradigm are needed to obtain a definitive measurement of cosmic birefringence in the future.
Published: 2023

17. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI

Author: de la Hoz, E.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Polarized component maps in the Northern Sky are derived from the QUIJOTE-MFI wide survey data at 11 and 13 GHz, the WMAP K and Ka bands and all Planck polarized channels using the parametric component separation method B-SeCRET. The addition of QUIJOTE-MFI data significantly improves the uncertainty in the parameter estimation of the low frequency dominant foreground, in particular the estimation of the synchrotron spectral index. We find statistically significant spatial variability across the sky. A power law model of the synchrotron emission provides a good fit of the data outside the galactic plane but fails to track the complexity of this region. Moreover, when we assume a synchrotron model with uniform curvature we find, in the 95% confidence region, a non-zero $c_s$ value. However, there is not sufficient statistical significance to determine which model is favoured., Comment: 4 pages, 2 figures, contribution to the 2022 Cosmology session of the 56th Rencontres de Moriond, acknowledgements added
Published: 2022

18. Probing Cosmic Inflation with the LiteBIRD Cosmic Microwave Background Polarization Survey

Author: LiteBIRD Collaboration, Allys, E., Arnold, K., Aumont, J., Aurlien, R., Azzoni, S., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Bartolo, N., Bautista, L., Beck, D., Beckman, S., Bersanelli, M., Boulanger, F., Brilenkov, M., Bucher, M., Calabrese, E., Campeti, P., Carones, A., Casas, F. J., Catalano, A., Chan, V., Cheung, K., Chinone, Y., Clark, S. E., Columbro, F., D'Alessandro, G., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Duval, J. M., Elleflot, T., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Finelli, F., Flauger, R., Franceschet, C., Fuskeland, U., Galloway, M., Ganga, K., Gerbino, M., Gervasi, M., Génova-Santos, R. T., Ghigna, T., Giardiello, S., Gjerløw, E., Grain, J., Grupp, F., Gruppuso, A., Gudmundsson, J. E., Halverson, N. W., Hargrave, P., Hasebe, T., Hasegawa, M., Hazumi, M., Henrot-Versillé, S., Hensley, B., Hergt, L. T., Herman, D., Hivon, E., Hlozek, R. A., Hornsby, A. L., Hoshino, Y., Hubmayr, J., Ichiki, K., Iida, T., Imada, H., Ishino, H., Jaehnig, G., Katayama, N., Kato, A., Keskitalo, R., Kisner, T., Kobayashi, Y., Kogut, A., Kohri, K., Komatsu, E., Komatsu, K., Konishi, K., Krachmalnicoff, N., Kuo, C. L., Lamagna, L., Lattanzi, M., Lee, A. T., Leloup, C., Levrier, F., Linder, E., Luzzi, G., Macias-Perez, J., Maciaszek, T., Maffei, B., Maino, D., Mandelli, S., Martínez-González, E., Masi, S., Massa, M., Matarrese, S., Matsuda, F. T., Matsumura, T., Mele, L., Migliaccio, M., Minami, Y., Moggi, A., Montgomery, J., Montier, L., Morgante, G., Mot, B., Nagano, Y., Nagasaki, T., Nagata, R., Nakano, R., Namikawa, T., Nati, F., Natoli, P., Nerval, S., Noviello, F., Odagiri, K., Oguri, S., Ohsaki, H., Pagano, L., Paiella, A., Paoletti, D., Passerini, A., Patanchon, G., Piacentini, F., Piat, M., Pisano, G., Polenta, G., Poletti, D., Prouvé, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Remazeilles, M., Ritacco, A., Roudil, G., Rubino-Martin, J. A., Russell, M., Sakurai, H., Sakurai, Y., Sasaki, M., Scott, D., Sekimoto, Y., Shinozaki, K., Shiraishi, M., Shirron, P., Signorelli, G., Spinella, F., Stever, S., Stompor, R., Sugiyama, S., Sullivan, R. M., Suzuki, A., Svalheim, T. L., Switzer, E., Takaku, R., Takakura, H., Takase, Y., Tartari, A., Terao, Y., Thermeau, J., Thommesen, H., Thompson, K. L., Tomasi, M., Tominaga, M., Tristram, M., Tsuji, M., Tsujimoto, M., Vacher, L., Vielva, P., Vittorio, N., Wang, W., Watanuki, K., Wehus, I. K., Weller, J., Westbrook, B., Wilms, J., Winter, B., Wollack, E. J., Yumoto, J., and Zannoni, M.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. The Japan Aerospace Exploration Agency (JAXA) selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with an expected launch in the late 2020s using JAXA's H3 rocket. LiteBIRD is planned to orbit the Sun-Earth Lagrangian point L2, where it will map the cosmic microwave background (CMB) polarization over the entire sky for three years, with three telescopes in 15 frequency bands between 34 and 448 GHz, to achieve an unprecedented total sensitivity of 2.2$\mu$K-arcmin, with a typical angular resolution of 0.5$^\circ$ at 100 GHz. The primary scientific objective of LiteBIRD is to search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. We provide an overview of the LiteBIRD project, including scientific objectives, mission and system requirements, operation concept, spacecraft and payload module design, expected scientific outcomes, potential design extensions and synergies with other projects., Comment: 155 pages, accepted for publication in PTEP
Published: 2022
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19. Polarization angle requirements for CMB B-mode experiments. Application to the LiteBIRD satellite

Author: Vielva, P., Martínez-González, E., Casas, F. J., Matsumura, T., Henrot-Versillé, S., Komatsu, E., Aumont, J., Aurlien, R., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Calabrese, E., Cheung, K., Columbro, F., Coppolecchia, A., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Diego-Palazuelos, P., Eriksen, H. K., Errard, J., Finelli, F., Franceschet, C., Fuskeland, U., Galloway, M., Ganga, K., Gervasi, M., Génova-Santos, R. T., Ghigna, T., Gjerløw, E., Gruppuso, A., Hazumi, M., Herranz, D., Hivon, E., Kohri, K., Lamagna, L., Leloup, C., Macias-Perez, J., Masi, S., Matsuda, F. T., Morgante, G., Nakano, R., Nati, F., Natoli, P., Nerval, S., Odagiri, K., Oguri, S., Pagano, L., Paiella, A., Paoletti, D., Piacentini, F., Polenta, G., Puglisi, G., Remazeilles, M., Ritacco, A., Rubino-Martin, J. A., Scott, D., Sekimoto, Y., Shiraishi, M., Signorelli, G., Takakura, H., Tartari, A., Thompson, K. L., Tristram, M., Vacher, L., Vittorio, N., Wehus, I. K., and Zannoni, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A methodology to provide the polarization angle requirements for different sets of detectors, at a given frequency of a CMB polarization experiment, is presented. The uncertainties in the polarization angle of each detector set are related to a given bias on the tensor-to-scalar ratio $r$ parameter. The approach is grounded in using a linear combination of the detector sets to obtain the CMB polarization signal. In addition, assuming that the uncertainties on the polarization angle are in the small angle limit (lower than a few degrees), it is possible to derive analytic expressions to establish the requirements. The methodology also accounts for possible correlations among detectors, that may originate from the optics, wafers, etc. The approach is applied to the LiteBIRD space mission. We show that, for the most restrictive case (i.e., full correlation of the polarization angle systematics among detector sets), the requirements on the polarization angle uncertainties are of around 1 arcmin at the most sensitive frequency bands (i.e., $\approx 150$ GHz) and of few tens of arcmin at the lowest (i.e., $\approx 40$ GHz) and highest (i.e., $\approx 400$ GHz) observational bands. Conversely, for the least restrictive case (i.e., no correlation of the polarization angle systematics among detector sets), the requirements are $\approx 5$ times less restrictive than for the previous scenario. At the global and the telescope levels, polarization angle knowledge of a few arcmins is sufficient for correlated global systematic errors and can be relaxed by a factor of two for fully uncorrelated errors in detector polarization angle. The reported uncertainty levels are needed in order to have the bias on $r$ due to systematics below the limit established by the LiteBIRD collaboration., Comment: 26 pages, 6 figures. Minor changes to match the final version in JCAP
Published: 2022
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20. Determination of Polarization Angles in CMB Experiments and Application to CMB Component Separation Analyses

Author: de la Hoz, E., Diego-Palazuelos, P., Martínez-González, E., Vielva, P., Barreiro, R. B., and Bilbao-Ahedo, J. D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The new generation of CMB polarization experiments will reach limits of sensitivity never achieved before to detect the primordial B-mode signal. However, all these efforts will be futile if we lack a tight control of systematics. Here, we focus on the systematic that arises from the uncertainty on the calibration of polarization angles. Miscalibrated polarization angles induce a mixing of E- and B-modes that obscures the primordial B-mode signal. We introduce an iterative angular power spectra maximum likelihood-based method to calculate polarization angles from the multi-frequency signal. The basis behind this methodology grounds on nulling the EB power spectra. To simplify the likelihood, we assume that the rotation angles are small (<6 deg) and, the maximum likelihood solution for the rotation angles is obtained by applying an iterative process where the covariance matrix does not depend on the angles per iteration, i.e., the rotation angles are fixed to the estimated angles in the previous iteration. With these assumptions, we obtain an analytical linear system which leads to a very fast computational implementation. We show that with this methodology we are able to determine the rotation angle for each frequency with sufficiently good accuracy. To prove the latter point we perform component separation analyses using the parametric component separation method B-SeCRET with two different approaches. In the first approach we apply the B-SeCRET pipeline to the signal de-rotated with the estimation of the angles, while in the second, the rotation angles are treated as model parameters using the estimation of the angles as a prior information. We obtain that the rotation angles estimations improve after applying the second approach, and show that the systematic residuals due to the non-null calibration polarization angles are mitigated to the order of a 1% at the power spectrum level., Comment: 28 pages, 12 figures, submitted to JCAP
Published: 2021
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21. In-flight polarization angle calibration for LiteBIRD: blind challenge and cosmological implications

Author: collaboration, The LiteBIRD, Krachmalnicoff, N, Matsumura, T, de la Hoz, E, Basak, S, Gruppuso, A, Minami, Y, Baccigalupi, C, Komatsu, E, Martínez-González, E, Vielva, P, Aumont, J, Aurlien, R, Azzoni, S, Banday, AJ, Barreiro, RB, Bartolo, N, Bersanelli, M, Calabrese, E, Carones, A, Casas, FJ, Cheung, K, Chinone, Y, Columbro, F, de Bernardis, P, Diego-Palazuelos, P, Errard, J, Finelli, F, Fuskeland, U, Galloway, M, Genova-Santos, RT, Gerbino, M, Ghigna, T, Giardiello, S, Gjerløw, E, Hazumi, M, Henrot-Versillé, S, Kisner, T, Lamagna, L, Lattanzi, M, Levrier, F, Luzzi, G, Maino, D, Masi, S, Migliaccio, M, Montier, L, Morgante, G, Mot, B, Nagata, R, Nati, F, Natoli, P, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Remazeilles, M, Rubino-Martin, J, Sasaki, M, Shiraishi, M, Signorelli, G, Stever, S, Tartari, A, Tristram, M, Tsuji, M, Vacher, L, Wehus, IK, and Zannoni, M
Subjects: Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics
Abstract: We present a demonstration of the in-flight polarization angle calibration for the JAXA/ISAS second strategic large class mission, LiteBIRD, and estimate its impact on the measurement of the tensor-to-scalar ratio parameter, r, using simulated data. We generate a set of simulated sky maps with CMB and polarized foreground emission, and inject instrumental noise and polarization angle offsets to the 22 (partially overlapping) LiteBIRD frequency channels. Our in-flight angle calibration relies on nulling the EB cross correlation of the polarized signal in each channel. This calibration step has been carried out by two independent groups with a blind analysis, allowing an accuracy of the order of a few arc-minutes to be reached on the estimate of the angle offsets. Both the corrected and uncorrected multi-frequency maps are propagated through the foreground cleaning step, with the goal of computing clean CMB maps. We employ two component separation algorithms, the Bayesian-Separation of Components and Residuals Estimate Tool (B-SeCRET), and the Needlet Internal Linear Combination (NILC). We find that the recovered CMB maps obtained with algorithms that do not make any assumptions about the foreground properties, such as NILC, are only mildly affected by the angle miscalibration. However, polarization angle offsets strongly bias results obtained with the parametric fitting method. Once the miscalibration angles are corrected by EB nulling prior to the component separation, both component separation algorithms result in an unbiased estimation of the r parameter. While this work is motivated by the conceptual design study for LiteBIRD, its framework can be broadly applied to any CMB polarization experiment. In particular, the combination of simulation plus blind analysis provides a robust forecast by taking into account not only detector sensitivity but also systematic effects.
Published: 2022

22. Overview of the Medium and High Frequency Telescopes of the LiteBIRD satellite mission

Author: Montier, L., Mot, B., de Bernardis, P., Maffei, B., Pisano, G., Columbro, F., Gudmundsson, J. E., Henrot-Versillé, S., Lamagna, L., Montgomery, J., Prouvé, T., Russell, M., Savini, G., Stever, S., Thompson, K. L., Tsujimoto, M., Tucker, C., Westbrook, B., Ade, P. A. R., Adler, A., Allys, E., Arnold, K., Auguste, D., Aumont, J., Aurlien, R., Austermann, J., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Basak, S., Beall, J., Beck, D., Beckman, S., Bermejo, J., Bersanelli, M., Bonis, J., Borrill, J., Boulanger, F., Bounissou, S., Brilenkov, M., Brown, M., Bucher, M., Calabrese, E., Campeti, P., Carones, A., Casas, F. J., Challinor, A., Chan, V., Cheung, K., Chinone, Y., Cliche, J. F., Colombo, L., Cubas, J., Cukierman, A., Curtis, D., D'Alessandro, G., Dachlythra, N., De Petris, M., Dickinson, C., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Duband, L., 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., Galloway, M., Ganga, K., Gao, J. R., Genova-Santos, R., Gerbino, M., Gervasi, M., Ghigna, T., Gjerløw, E., Gradziel, M. L., Grain, J., Grupp, F., Gruppuso, A., de Haan, T., Halverson, N. W., Hargrave, P., Hasebe, T., Hasegawa, M., Hattori, M., Hazumi, M., Herman, D., Herranz, D., Hill, C. A., Hilton, G., Hirota, Y., Hivon, E., Hlozek, R. A., Hoshino, Y., de la Hoz, E., Hubmayr, J., Ichiki, K., Iida, T., Imada, H., Ishimura, K., Ishino, H., Jaehnig, G., 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., Lanen, J. V., Lattanzi, M., Lee, A. T., Leloup, C., Levrier, F., Linder, E., Louis, T., Luzzi, G., Maciaszek, T., Maino, D., Maki, M., Mandelli, S., Martinez-Gonzalez, E., Masi, S., Matsumura, T., Mennella, A., Migliaccio, M., Minami, Y., Mitsuda, K., Morgante, G., Murata, Y., Murphy, J. A., Nagai, M., Nagano, Y., Nagasaki, T., Nagata, R., Nakamura, S., Namikawa, T., Natoli, P., Nerval, S., Nishibori, T., Nishino, H., O'Sullivan, C., Ogawa, H., Oguri, S., Ohsaki, H., Ohta, I. S., Okada, N., Pagano, L., Paiella, A., Paoletti, D., Patanchon, G., Peloton, J., Piacentini, F., Polenta, G., Poletti, D., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Remazeilles, M., Ritacco, A., Roudil, G., Rubino-Martin, J. A., Sakurai, H., Sakurai, Y., Sandri, M., Sasaki, M., Scott, D., Seibert, J., Sekimoto, Y., Sherwin, B., Shinozaki, K., Shiraishi, M., Shirron, P., Signorelli, G., Smecher, G., Stompor, R., Sugai, H., Sugiyama, S., Suzuki, A., Suzuki, J., Svalheim, T. L., Switzer, E., Takaku, R., Takakura, H., Takakura, S., Takase, Y., Takeda, Y., Tartari, A., Taylor, E., Terao, Y., Thommesen, H., Thorne, B., Toda, T., Tomasi, M., Tominaga, M., Trappe, N., Tristram, M., Tsuji, M., Ullom, J., Vermeulen, G., Vielva, P., Villa, F., Vissers, M., Vittorio, N., Wehus, I., Weller, J., Wilms, J., Winter, B., Wollack, E. J., Yamasaki, N. Y., Yoshida, T., Yumoto, J., Zannoni, M., and Zonca, A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34GHz to 448GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium- and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89-224GHz) and the High-Frequency Telescope (166-448GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD., Comment: SPIE Conference
Published: 2021
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23. LiteBIRD: JAXA's new strategic L-class mission for all-sky surveys of cosmic microwave background polarization

Author: Hazumi, M., Ade, P. A. R., Adler, A., Allys, E., Arnold, K., Auguste, D., Aumont, J., Aurlien, R., Austermann, J., Baccigalupi, C., Banday, A. J., Banjeri, R., Barreiro, R. B., Basak, S., Beall, J., Beck, D., Beckman, S., Bermejo, J., de Bernardis, P., Bersanelli, M., Bonis, J., Borrill, J., Boulanger, F., Bounissou, S., Brilenkov, M., Brown, M., Bucher, M., Calabrese, E., Campeti, P., Carones, A., Casas, F. J., Challinor, A., Chan, V., Cheung, K., Chinone, Y., Cliche, J. F., Colombo, L., Columbro, F., Cubas, J., Cukierman, A., Curtis, D., D'Alessandro, G., Dachlythra, N., De Petris, M., Dickinson, C., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Duband, L., 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., Galloway, M., Ganga, K., Gao, J. R., Genova-Santos, R., Gerbino, M., Gervasi, M., Ghigna, T., Gjerløw, E., Gradziel, M. L., Grain, J., Grupp, F., Gruppuso, A., Gudmundsson, J. E., de Haan, T., Halverson, N. W., Hargrave, P., Hasebe, T., Hasegawa, M., Hattori, M., Henrot-Versillé, S., Herman, D., Herranz, D., Hill, C. A., Hilton, G., Hirota, Y., Hivon, E., Hlozek, R. A., Hoshino, Y., de la Hoz, E., Hubmayr, J., Ichiki, K., Iida, T., Imada, H., Ishimura, K., Ishino, H., Jaehnig, G., 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., Lattanzi, M., Lee, A. T., Leloup, C., Levrier, F., Linder, E., Louis, T., Luzzi, G., Maciaszek, T., Maffei, B., Maino, D., Maki, M., Mandelli, S., Martinez-Gonzalez, E., Masi, S., Matsumura, T., Mennella, A., Migliaccio, M., Minami, Y., Mitsuda, K., Montgomery, J., Montier, L., Morgante, G., Mot, B., Murata, Y., Murphy, J. A., Nagai, M., Nagano, Y., Nagasaki, T., Nagata, R., Nakamura, S., Namikawa, T., Natoli, P., Nerval, S., Nishibori, T., Nishino, H., Noviello, F., O'Sullivan, C., Ogawa, H., Oguri, S., Ohsaki, H., Ohta, I. S., Okada, N., Pagano, L., Paiella, A., Paoletti, D., Patanchon, G., Peloton, J., Piacentini, F., Pisano, G., Polenta, G., Poletti, D., Prouvé, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Remazeilles, M., Ritacco, A., Roudil, G., Rubino-Martin, J. A., 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., Stever, S., Stompor, R., Sugai, H., Sugiyama, S., Suzuki, A., Suzuki, J., Svalheim, T. L., Switzer, E., Takaku, R., Takakura, H., Takakura, S., Takase, Y., Takeda, Y., Tartari, A., Taylor, E., Terao, Y., 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., Vermeulen, G., Vielva, P., Villa, F., Vissers, M., Vittorio, N., Wehus, I., Weller, J., Westbrook, B., Wilms, J., Winter, B., Wollack, E. J., Yamasaki, N. Y., Yoshida, T., Yumoto, J., Zannoni, M., and Zonca, A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract: LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. JAXA selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with its expected launch in the late 2020s using JAXA's H3 rocket. LiteBIRD plans to map the cosmic microwave background (CMB) polarization over the full sky with unprecedented precision. Its main scientific objective is to carry out a definitive search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with an insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. To this end, LiteBIRD will perform full-sky surveys for three years at the Sun-Earth Lagrangian point L2 for 15 frequency bands between 34 and 448 GHz with three telescopes, to achieve a total sensitivity of 2.16 micro K-arcmin with a typical angular resolution of 0.5 deg. at 100GHz. We provide an overview of the LiteBIRD project, including scientific objectives, mission requirements, top-level system requirements, operation concept, and expected scientific outcomes., Comment: 20 pages, 9 figures
Published: 2021
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24. Concept Design of Low Frequency Telescope for CMB B-mode Polarization satellite LiteBIRD

Author: Sekimoto, Y., Ade, P. A. R., Adler, A., Allys, E., Arnold, K., Auguste, D., Aumont, J., Aurlien, R., Austermann, J., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Basak, S., Beall, J., Beck, D., Beckman, S., Bermejo, J., de Bernardis, P., Bersanelli, M., Bonis, J., Borrill, J., Boulanger, F., Bounissou, S., Brilenkov, M., Brown, M., Bucher, M., Calabrese, E., Campeti, P., Carones, A., Casas, F. J., Challinor, A., Chan, V., Cheung, K., Chinone, Y., Cliche, J. F., Colombo, L., Columbro, F., Cubas, J., Cukierman, A., Curtis, D., D'Alessandro, G., Dachlythra, N., De Petris, M., Dickinson, C., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Duband, L., 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., Galloway, M., Ganga, K., Gao, J. R., Genova-Santos, R., Gerbino, M., Gervasi, M., Ghigna, T., Gjerløw, E., Gradziel, M. L., Grain, J., Grupp, F., Gruppuso, A., Gudmundsson, J. E., de Haan, T., Halverson, N. W., Hargrave, P., Hasebe, T., Hasegawa, M., Hattori, M., Hazumi, M., Henrot-Versillé, S., Herman, D., Herranz, D., Hill, C. A., Hilton, G., Hirota, Y., Hivon, E., Hlozek, R. A., Hoshino, Y., de la Hoz, E., Hubmayr, J., Ichiki, K., iida, T., Imada, H., Ishimura, K., Ishino, H., Jaehnig, G., 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., Lattanzi, M., Lee, A. T., Leloup, C., Levrier, F., Linder, E., Louis, T., Luzzi, G., Maciaszek, T., Maffei, B., Maino, D., Maki, M., Mandelli, S., Martinez-Gonzalez, E., Masi, S., Matsumura, T., Mennella, A., Migliaccio, M., Minanmi, Y., Mitsuda, K., Montgomery, J., Montier, L., Morgante, G., Mot, B., Murata, Y., Murphy, J. A., Nagai, M., Nagano, Y., Nagasaki, T., Nagata, R., Nakamura, S., Namikawa, T., Natoli, P., Nerval, S., Nishibori, T., Nishino, H., O'Sullivan, C., Ogawa, H., Oguri, S., Ohsaki, H., Ohta, I. S., Okada, N., Pagano, L., Paiella, A., Paoletti, D., Patanchon, G., Peloton, J., Piacentini, F., Pisano, G., Polenta, G., Poletti, D., Prouvé, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Remazeilles, M., Ritacco, A., Roudil, G., Rubino-Martin, J. A., Russell, M., Sakurai, H., Sakurai, Y., Sandri, M., Sasaki, M., Savini, G., Scott, D., Seibert, J., Sherwin, B., Shinozaki, K., Shiraishi, M., Shirron, P., Signorelli, G., Smecher, G., Stever, S., Stompor, R., Sugai, H., Sugiyama, S., Suzuki, A., Suzuki, J., Svalheim, T. L., Switzer, E., Takaku, R., Takakura, H., Takakura, S., Takase, Y., Takeda, Y., Tartari, A., Taylor, E., Terao, Y., 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., Vermeulen, G., Vielva, P., Villa, F., Vissers, M., Vittorio, N., Wehus, I., Weller, J., Westbrook, B., Wilms, J., Winter, B., Wollack, E. J., Yamasaki, N. Y., Yoshida, T., Yumoto, J., Zannoni, M., and Zonca, A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: LiteBIRD has been selected as JAXA's strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) $B$-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of $-56$ dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT : 34--161 GHz), one of LiteBIRD's onboard telescopes. It has a wide field-of-view ($18^\circ \times 9^\circ$) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90$^\circ$ are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at $5\,$K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented., Comment: 21 pages, 14 figures
Published: 2021
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25. On the Detection of CMB B-modes from Ground at Low Frequency

Author: de la Hoz, E., Vielva, P., Barreiro, R. B., and Martínez-González, E.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The primordial CMB $B$-mode search is on the spotlight of the scientific community due to the large amount of cosmological information that is encoded in the primeval signal. However, the detection of this signal is challenging from the data analysis point of view, due to the relative low amplitude compared to the foregrounds, the lensing contamination coming from the leakage of $E$-modes, and the instrumental noise. Here, we studied the viability of the detection of the primordial polarization $B$-mode with a ground-based telescope operating in the microwave low-frequency regime (i.e., from 10GHz-120GHz) in a handful of different scenarios: i. the instrument's channels distribution and noise, ii. the tensor-to-scalar ratio ($r$) detectability considering different possible $r$ values and degrees of delensing, iii. the effect of including a possible source of polarized anomalous microwave emission (AME), iv. the strengths and weaknesses of different observational strategies and, v. the atmospheric and systematic noise impact on the recovery. We focused mainly on the removal of galactic foregrounds as well as noise contamination by applying a full-parametric pixel-based maximum likelihood component separation technique. Moreover, we developed a numerical methodology to estimate the residuals power spectrum left after component separation, which allow us to mitigate possible biases introduced in the primordial $B$-mode power spectrum reconstruction. Among many other results, we found that this sort of experiment is capable of detecting Starobinsky's $r$ even when no delensing is performed or, a possible polarized AME contribution is taken into account. Besides, we showed that this experiment is a powerful complement to other on-ground or satellite missions, such as LiteBIRD, since it can help significantly with the low-frequency foregrounds characterization., Comment: 28 pages, 18 figures, submitted to JCAP
Published: 2020
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26. Sensitivity Modeling for LiteBIRD

Author: 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., de la Hoz, E., De Petris, M., Torre, S. Della, 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., Gjerløw, 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-Versillé, 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., Martínez-González, 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., Ogawa, H., Oguri, S., Ohsaki, H., Ohta, I. S., Okada, N., 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., Prouvé, 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.
Published: 2022
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27. Optical Characterization of OMT-Coupled TES Bolometers for LiteBIRD

Author: Hubmayr, J., Ade, P. A. R., Adler, A., Allys, E., Alonso, D., Arnold, K., Auguste, D., Aumont, J., Aurlien, R., Austermann, J. E., Azzoni, S., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Bartolo, N., Basak, S., Battistelli, E., Bautista, L., Beall, J. A., 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., Chiocchetta, C., Clark, S. E., Clermont, L., Clesse, S., Cliche, J., Columbro, F., Connors, J. A., Coppolecchia, A., Coulton, W., Cubas, J., Cukierman, A., Curtis, D., Cuttaia, F., D’Alessandro, G., Dachlythra, K., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Daz Garca, J. J., Dickinson, C., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Douillet, D., Doumayrou, E., Duband, L., Ducout, A., Duff, S. M., Duval, J. M., Ebisawa, K., Elleflot, T., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Farrens, S., Finelli, F., Flauger, R., Fleury-Frenette, K., Franceschet, C., Fuskeland, U., Galli, L., Galli, S., Galloway, M., Ganga, K., Gao, J. R., Genova-Santos, R. T., Georges, M., Gerbino, M., Gervasi, M., Ghigna, T., Giardiello, S., Gjerlw, E., Gonzles, R. Gonzlez, Gradziel, M. L., Grain, J., Grandsire, L., Grupp, F., Gruppuso, A., Gudmundsson, J. E., Halverson, N. W., Hamilton, J., Hargrave, P., Hasebe, T., Hasegawa, M., Hattori, M., Hazumi, M., Henrot-Versill, S., Hensley, B., Herman, D., Herranz, D., Hilton, G. C., Hivon, E., Hlozek, R. A., Hoang, D., Hornsby, A. L., Hoshino, Y., Ichiki, K., Iida, T., Ikemoto, T., Imada, H., Ishimura, K., Ishino, H., Jaehnig, G., Jones, M., Kaga, T., Kashima, S., Katayama, N., Kato, A., Kawasaki, T., Keskitalo, R., Kintziger, C., 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., Link, M. J., Lonappan, A. I., Louis, T., Luzzi, G., Macias-Perez, J., Maciaszek, T., Maffei, B., Maino, D., Maki, M., Mandelli, S., Maris, M., Marquet, B., Martnez-Gonzlez, E., Martire, F. A., Masi, S., Massa, M., Masuzawa, M., Matarrese, S., Matsuda, F. T., Matsumura, T., Mele, L., Mennella, A., Migliaccio, M., Minami, Y., Mitsuda, K., Moggi, A., Monelli, M., 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., Neto Godry Farias, N., Nishibori, T., Nishino, H., Noviello, F., O’Neil, G. C., O’Sullivan, C., Odagiri, K., Ochi, H., Ogawa, H., Ogawa, H., Oguri, S., Ohsaki, H., Ohta, I. S., Okada, N., Pagano, L., Paiella, A., Paoletti, D., Pascual Cisneros, G., Passerini, A., Patanchon, G., Pelgrim, V., Peloton, J., Pettorino, V., Piacentini, F., Piat, M., Piccirilli, G., Pinsard, F., Pisano, G., Plesseria, J., Polenta, G., Poletti, D., Prouv, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Reintsema, C. D., Remazeilles, M., Ritacco, A., Rosier, P., 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., Shitvov, A., Signorelli, G., Smecher, G., Spinella, F., Starck, J., Stever, S., Stompor, R., Sudiwala, R., Sugiyama, S., Sullivan, R., Suzuki, A., Suzuki, J., Suzuki, T., 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., Terenzi, L., 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., Ueki, R., Ullom, J. N., Umemori, K., Vacher, L., Van Lanen, J., Vermeulen, G., Vielva, P., Villa, F., Vissers, M. R., Vittorio, N., Wandelt, B., Wang, W., Wehus, I. K., Weller, J., Westbrook, B., Weymann-Despres, G., Wilms, J., Winter, B., Wollack, E. J., Yamasaki, N. Y., Yoshida, T., Yumoto, J., Watanuki, K., Zacchei, A., Zannoni, M., and Zonca, A.
Published: 2022
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28. The European Low Frequency Survey

Author: Mennella A., Arnold K., Azzoni S., Baccigalupi C., Banday A., Barreiro R.B., Barron D., Bersanelli M., Casey S., Colombo L., de la Hoz E., Franceschet C., Jones M.E., Genova-Santos R.T., Hoyland R.J., Lee A.T., Martinez-Gonzalez E., Montonati F., Rubiño-Martin J.A., Taylor A., and Vielva P.
Subjects: Physics, QC1-999
Abstract: In this paper we present the European Low Frequency Survey (ELFS), a project that will enable the detection of primordial B-mode polarization by measuring the Galactic and extra-Galactic foregrounds in the 5– 120 GHz frequency window. Indeed, the main difficulty in measuring the Bmode polarization comes not just from its sheer faintness, but from the fact that many other objects in the Universe also emit polarized microwaves, which mask the faint CMB signal. The first stage of this project will be carried out in synergy with the Simons Array (SA) collaboration, installing a 5.5–11 GHz coherent receiver at the focus of one of the three 3.5m SA telescopes in Atacama, Chile (“ELFS on SA”). The receiver will be equipped with a fully digital backend based on the latest Xilinx RF System-on-Chip devices that will provide frequency resolution of 1MHz across the whole observing band, allowing us to clean the scientific signal from unwanted radio frequency interference, particularly from low-Earth orbit satellite mega-constellations. This paper reviews the scientific motivation for ELFS and its instrumental characteristics, and provides an update on the development of ELFS on SA.
Published: 2024
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29. QUIJOTE Scientific Results – XVII. Studying the anomalous microwave emission in the Andromeda Galaxy with QUIJOTE-MFI

Author: Fernández-Torreiro, M, primary, Génova-Santos, R T, additional, Rubiño-Martín, J A, additional, López-Caraballo, C H, additional, Peel, M W, additional, Arce-Tord, C, additional, Rebolo, R, additional, Artal, E, additional, Ashdown, M, additional, Barreiro, R B, additional, Casas, F J, additional, de la Hoz, E, additional, Guidi, F, additional, Herranz, D, additional, Hoyland, R, additional, Lasenby, A, additional, Martínez-Gonzalez, E, additional, Piccirillo, L, additional, Poidevin, F, additional, Ruiz-Granados, B, additional, Tramonte, D, additional, Vansyngel, F, additional, Vielva, P, additional, and Watson, R A, additional
Published: 2023
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30. QUIJOTE scientific results – XIII. Intensity and polarization study of the microwave spectra of supernova remnants in the QUIJOTE-MFI wide survey: CTB 80, Cygnus Loop, HB 21, CTA 1, Tycho and HB 9

Author: López-Caraballo, C H, primary, Ruiz-Granados, B, additional, Génova-Santos, R T, additional, Fernández-Torreiro, M, additional, Rubiño-Martín, J A, additional, Peel, M W, additional, Poidevin, F, additional, Artal, E, additional, Ashdown, M, additional, Barreiro, R B, additional, Casas, F J, additional, de la Hoz, E, additional, González-González, R, additional, Guidi, F, additional, Herranz, D, additional, Hoyland, R, additional, Lasenby, A, additional, Martínez-González, E, additional, Piccirillo, L, additional, Rebolo, R, additional, Tramonte, D, additional, Vansyngel, F, additional, Vielva, P, additional, and Watson, R A, additional
Published: 2023
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31. QUIJOTE scientific results – X. Spatial variations of Anomalous Microwave Emission along the Galactic plane

Author: Fernández-Torreiro, M, primary, Rubiño-Martín, J A, additional, López-Caraballo, C H, additional, Génova-Santos, R T, additional, Peel, M W, additional, Guidi, F, additional, Harper, S E, additional, Artal, E, additional, Ashdown, M, additional, Barreiro, R B, additional, Casas, F J, additional, de la Hoz, E, additional, Herranz, D, additional, Hoyland, R, additional, Lasenby, A, additional, Martínez-Gonzalez, E, additional, Piccirillo, L, additional, Poidevin, F, additional, Rebolo, R, additional, Ruiz-Granados, B, additional, Tramonte, D, additional, Vansyngel, F, additional, Vielva, P, additional, and Watson, R A, additional
Published: 2023
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32. Tensor-to-scalar ratio forecasts for extended LiteBIRD frequency configurations

Author: Fuskeland, U., primary, Aumont, J., additional, Aurlien, R., additional, Baccigalupi, C., additional, Banday, A. J., additional, Eriksen, H. K., additional, Errard, J., additional, Génova-Santos, R. T., additional, Hasebe, T., additional, Hubmayr, J., additional, Imada, H., additional, Krachmalnicoff, N., additional, Lamagna, L., additional, Pisano, G., additional, Poletti, D., additional, Remazeilles, M., additional, Thompson, K. L., additional, Vacher, L., additional, Wehus, I. K., additional, Azzoni, S., additional, Ballardini, M., additional, Barreiro, R. B., additional, Bartolo, N., additional, Basyrov, A., additional, Beck, D., additional, Bersanelli, M., additional, Bortolami, M., additional, Brilenkov, M., additional, Calabrese, E., additional, Carones, A., additional, Casas, F. J., additional, Cheung, K., additional, Chluba, J., additional, Clark, S. E., additional, Clermont, L., additional, Columbro, F., additional, Coppolecchia, A., additional, D’Alessandro, G., additional, de Bernardis, P., additional, de Haan, T., additional, de la Hoz, E., additional, De Petris, M., additional, Della Torre, S., additional, Diego-Palazuelos, P., additional, Finelli, F., additional, Franceschet, C., additional, Galloni, G., additional, Galloway, M., additional, Gerbino, M., additional, Gervasi, M., additional, Ghigna, T., additional, Giardiello, S., additional, Gjerløw, E., additional, Gruppuso, A., additional, Hargrave, P., additional, Hattori, M., additional, Hazumi, M., additional, Hergt, L. T., additional, Herman, D., additional, Herranz, D., additional, Hivon, E., additional, Hoang, T. D., additional, Kohri, K., additional, Lattanzi, M., additional, Lee, A. T., additional, Leloup, C., additional, Levrier, F., additional, Lonappan, A. I., additional, Luzzi, G., additional, Maffei, B., additional, Martínez-González, E., additional, Masi, S., additional, Matarrese, S., additional, Matsumura, T., additional, Migliaccio, M., additional, Montier, L., additional, Morgante, G., additional, Mot, B., additional, Mousset, L., additional, Nagata, R., additional, Namikawa, T., additional, Nati, F., additional, Natoli, P., additional, Nerval, S., additional, Novelli, A., additional, Pagano, L., additional, Paiella, A., additional, Paoletti, D., additional, Pascual-Cisneros, G., additional, Patanchon, G., additional, Pelgrims, V., additional, Piacentini, F., additional, Piccirilli, G., additional, Polenta, G., additional, Puglisi, G., additional, Raffuzzi, N., additional, Ritacco, A., additional, Rubino-Martin, J. A., additional, Savini, G., additional, Scott, D., additional, Sekimoto, Y., additional, Shiraishi, M., additional, Signorelli, G., additional, Stever, S. L., additional, Stutzer, N., additional, Sullivan, R. M., additional, Takakura, H., additional, Terenzi, L., additional, Thommesen, H., additional, Tristram, M., additional, Tsuji, M., additional, Vielva, P., additional, Weller, J., additional, Westbrook, B., additional, Weymann-Despres, G., additional, Wollack, E. J., additional, and Zannoni, M., additional
Published: 2023
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33. QUIJOTE Scientific Results – XVII. Studying the anomalous microwave emission in the Andromeda Galaxy with QUIJOTE-MFI.

Author: Fernández-Torreiro, M, Génova-Santos, R T, Rubiño-Martín, J A, López-Caraballo, C H, Peel, M W, Arce-Tord, C, Rebolo, R, Artal, E, Ashdown, M, Barreiro, R B, Casas, F J, de la Hoz, E, Guidi, F, Herranz, D, Hoyland, R, Lasenby, A, Martínez-Gonzalez, E, Piccirillo, L, Poidevin, F, and Ruiz-Granados, B
Subjects: ANDROMEDA Galaxy, SPECTRAL energy distribution, MILKY Way, GALAXY clusters, LOGNORMAL distribution
Abstract: The Andromeda Galaxy (M31) is the Local Group galaxy that is most similar to the Milky Way (MW). The similarities between the two galaxies make M31 useful for studying integrated properties common to spiral galaxies. We use the data from the recent QUIJOTE-MFI Wide Survey, together with new raster observations focused on M31, to study its integrated emission. The addition of raster data improves the sensitivity of QUIJOTE-MFI maps by almost a factor 3. Our main interest is to confirm if anomalous microwave emission (AME) is present in M31, as previous studies have suggested. To do so, we built the integrated spectral energy distribution of M31 between 0.408 and 3000 GHz. We then performed a component separation analysis taking into account synchrotron, free–free, AME, and thermal dust components. AME in M31 is modelled as a log-normal distribution with maximum amplitude, A AME, equal to 1.03 ± 0.32 Jy. It peaks at |${\nu _{\rm AME}}=17.2\pm 3.2{\rm \, GHz}{}$| with a width of W AME = 0.58 ± 0.16. Both the Akaike and Bayesian information criteria find the model without AME to be less than 1 per cent as probable as the one taking AME into consideration. We find that the AME emissivity per 100 |$\mu$| m intensity in M31 is |${\epsilon _{\rm AME}^{\rm 28.4\, GHz}}=9.6\pm 3.1\,\mu$| K MJy−1 sr, similar to that of the MW. We also provide the first upper limits for the AME polarization fraction in an extragalactic object. M31 remains the only galaxy where an AME measurement has been made of its integrated spectrum. [ABSTRACT FROM AUTHOR]
Published: 2024
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34. QUIJOTE scientific results – XIII. Intensity and polarization study of the microwave spectra of supernova remnants in the QUIJOTE-MFI wide survey: CTB 80, Cygnus Loop, HB 21, CTA 1, Tycho, and HB 9.

Author: López-Caraballo, C H, Ruiz-Granados, B, Génova-Santos, R T, Fernández-Torreiro, M, Rubiño-Martín, J A, Peel, M W, Poidevin, F, Artal, E, Ashdown, M, Barreiro, R B, Casas, F J, de la Hoz, E, González-González, R, Guidi, F, Herranz, D, Hoyland, R, Lasenby, A, Martínez-González, E, Piccirillo, L, and Rebolo, R
Subjects: SUPERNOVA remnants, SUPERNOVAE spectra, LARGE magellanic cloud, SPECTRAL energy distribution, MICROWAVES, COSMIC background radiation, SYNCHROTRON radiation
Abstract: We use the new QUIJOTE-MFI wide survey (11, 13, 17, and 19 GHz) to produce spectral energy distributions (SEDs), on an angular scale of 1°, of the supernova remnants (SNRs) CTB 80, Cygnus Loop, HB 21, CTA 1, Tycho, and HB 9. We provide new measurements of the polarized synchrotron radiation in the microwave range. The intensity and polarization SEDs are obtained and modelled by combining QUIJOTE-MFI maps with ancillary data. In intensity, we confirm the curved spectra of CTB 80 and HB 21 with a break frequency νb at 2.0 |$^{+1.2}_{-0.5}$| and 5.0 |$^{+1.2}_{-1.0}$| GHz, respectively; and spectral indices above the break of |$-0.6^{+0.04}_{-0.05}$| and |$-0.86^{+0.04}_{-0.05}$|⁠. We provide constraints on the Anomalous Microwave Emission, suggesting that it is negligible towards these SNRs. From a simultaneous intensity and polarization fit, we recover synchrotron spectral indices as flat as −0.24, and the whole sample has a mean and scatter of −0.44 ± 0.12. The polarization fractions have a mean and scatter of 6.1 ± 1.9 per cent. When combining our results with the measurements from other QUIJOTE (Q-U-I JOint TEnerife CMB experiment) studies of SNRs, we find that radio spectral indices are flatter for mature SNRs, and particularly flatter for CTB 80 (⁠|$-0.24^{+0.07}_{-0.06}$|⁠) and HB 21 (⁠|$-0.34^{+0.04}_{-0.03}$|⁠). In addition, the evolution of the spectral indices against the SNRs age is modelled with a power-law function, providing an exponent −0.07 ± 0.03 and amplitude −0.49 ± 0.02 (at 10 kyr), which are conservative with respect to previous studies of our Galaxy and the Large Magellanic Cloud. [ABSTRACT FROM AUTHOR]
Published: 2024
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35. Optical Characterization of OMT-Coupled TES Bolometers for LiteBIRD

Author: Hubmayr, J, 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, Chiocchetta, C, Clark, S, Clermont, L, Clesse, S, Cliche, J, Columbro, F, Connors, J, Coppolecchia, A, Coulton, W, Cubas, J, Cukierman, A, Curtis, D, Cuttaia, F, D’Alessandro, G, Dachlythra, K, de Bernardis, P, de Haan, T, de la Hoz, E, De Petris, M, Della Torre, S, Daz Garca, J, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Douillet, D, Doumayrou, E, Duband, L, Ducout, A, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Farrens, S, Finelli, F, Flauger, R, Fleury-Frenette, K, Franceschet, C, Fuskeland, U, Galli, L, Galli, S, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Georges, M, Gerbino, M, Gervasi, M, Ghigna, T, Giardiello, S, Gjerlw, E, Gonzles, R, Gradziel, M, Grain, J, Grandsire, L, Grupp, F, Gruppuso, A, Gudmundsson, J, Halverson, N, Hamilton, J, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versill, S, Hensley, B, Herman, D, Herranz, D, Hilton, G, Hivon, E, Hlozek, R, Hoang, D, Hornsby, A, Hoshino, Y, Ichiki, K, Iida, T, Ikemoto, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Jones, M, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kintziger, C, 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, Link, M, Lonappan, A, Louis, T, Luzzi, G, Macias-Perez, J, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Maris, M, Marquet, B, Martnez-Gonzlez, E, Martire, F, Masi, S, Massa, M, Masuzawa, M, Matarrese, S, Matsuda, F, Matsumura, T, Mele, L, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Moggi, A, Monelli, M, 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, Neto Godry Farias, N, Nishibori, T, Nishino, H, Noviello, F, O’Neil, G, O’Sullivan, C, Odagiri, K, Ochi, H, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Pascual Cisneros, G, Passerini, A, Patanchon, G, Pelgrim, V, Peloton, J, Pettorino, V, Piacentini, F, Piat, M, Piccirilli, G, Pinsard, F, Pisano, G, Plesseria, J, Polenta, G, Poletti, D, Prouv, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Reintsema, C, Remazeilles, M, Ritacco, A, Rosier, P, 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, Shitvov, A, Signorelli, G, Smecher, G, Spinella, F, Starck, J, Stever, S, Stompor, R, Sudiwala, R, Sugiyama, S, Sullivan, R, Suzuki, A, Suzuki, J, Suzuki, T, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Tavagnacco, D, Taylor, A, Taylor, E, Terao, Y, Terenzi, L, Thermeau, J, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ueki, R, Ullom, J, Umemori, K, Vacher, L, Van Lanen, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wandelt, B, Wang, W, Wehus, I, Weller, J, Westbrook, B, Weymann-Despres, G, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Watanuki, K, Zacchei, A, Zannoni, M, Zonca, A, Hubmayr, J., Ade, P. A. R., Adler, A., Allys, E., Alonso, D., Arnold, K., Auguste, D., Aumont, J., Aurlien, R., Austermann, J. E., Azzoni, S., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Bartolo, N., Basak, S., Battistelli, E., Bautista, L., Beall, J. A., 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., Chiocchetta, C., Clark, S. E., Clermont, L., Clesse, S., Cliche, J., Columbro, F., Connors, J. A., Coppolecchia, A., Coulton, W., Cubas, J., Cukierman, A., Curtis, D., Cuttaia, F., D’Alessandro, G., Dachlythra, K., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Daz Garca, J. J., Dickinson, C., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Douillet, D., Doumayrou, E., Duband, L., Ducout, A., Duff, S. M., Duval, J. M., Ebisawa, K., Elleflot, T., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Farrens, S., Finelli, F., Flauger, R., Fleury-Frenette, K., Franceschet, C., Fuskeland, U., Galli, L., Galli, S., Galloway, M., Ganga, K., Gao, J. R., Genova-Santos, R. T., Georges, M., Gerbino, M., Gervasi, M., Ghigna, T., Giardiello, S., Gjerlw, E., Gonzles, R. Gonzlez, Gradziel, M. L., Grain, J., Grandsire, L., Grupp, F., Gruppuso, A., Gudmundsson, J. E., Halverson, N. W., Hamilton, J., Hargrave, P., Hasebe, T., Hasegawa, M., Hattori, M., Hazumi, M., Henrot-Versill, S., Hensley, B., Herman, D., Herranz, D., Hilton, G. C., Hivon, E., Hlozek, R. A., Hoang, D., Hornsby, A. L., Hoshino, Y., Ichiki, K., Iida, T., Ikemoto, T., Imada, H., Ishimura, K., Ishino, H., Jaehnig, G., Jones, M., Kaga, T., Kashima, S., Katayama, N., Kato, A., Kawasaki, T., Keskitalo, R., Kintziger, C., 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., Link, M. J., Lonappan, A. I., Louis, T., Luzzi, G., Macias-Perez, J., Maciaszek, T., Maffei, B., Maino, D., Maki, M., Mandelli, S., Maris, M., Marquet, B., Martnez-Gonzlez, E., Martire, F. A., Masi, S., Massa, M., Masuzawa, M., Matarrese, S., Matsuda, F. T., Matsumura, T., Mele, L., Mennella, A., Migliaccio, M., Minami, Y., Mitsuda, K., Moggi, A., Monelli, M., 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., Neto Godry Farias, N., Nishibori, T., Nishino, H., Noviello, F., O’Neil, G. C., O’Sullivan, C., Odagiri, K., Ochi, H., Ogawa, H., Oguri, S., Ohsaki, H., Ohta, I. S., Okada, N., Pagano, L., Paiella, A., Paoletti, D., Pascual Cisneros, G., Passerini, A., Patanchon, G., Pelgrim, V., Peloton, J., Pettorino, V., Piacentini, F., Piat, M., Piccirilli, G., Pinsard, F., Pisano, G., Plesseria, J., Polenta, G., Poletti, D., Prouv, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Reintsema, C. D., Remazeilles, M., Ritacco, A., Rosier, P., 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., Shitvov, A., Signorelli, G., Smecher, G., Spinella, F., Starck, J., Stever, S., Stompor, R., Sudiwala, R., Sugiyama, S., Sullivan, R., Suzuki, A., Suzuki, J., Suzuki, T., 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., Terenzi, L., 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., Ueki, R., Ullom, J. N., Umemori, K., Vacher, L., Van Lanen, J., Vermeulen, G., Vielva, P., Villa, F., Vissers, M. R., Vittorio, N., Wandelt, B., Wang, W., Wehus, I. K., Weller, J., Westbrook, B., Weymann-Despres, G., Wilms, J., Winter, B., Wollack, E. J., Yamasaki, N. Y., Yoshida, T., Yumoto, J., Watanuki, K., Zacchei, A., Zannoni, M., Zonca, A., Hubmayr, J, 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, Chiocchetta, C, Clark, S, Clermont, L, Clesse, S, Cliche, J, Columbro, F, Connors, J, Coppolecchia, A, Coulton, W, Cubas, J, Cukierman, A, Curtis, D, Cuttaia, F, D’Alessandro, G, Dachlythra, K, de Bernardis, P, de Haan, T, de la Hoz, E, De Petris, M, Della Torre, S, Daz Garca, J, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Douillet, D, Doumayrou, E, Duband, L, Ducout, A, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Farrens, S, Finelli, F, Flauger, R, Fleury-Frenette, K, Franceschet, C, Fuskeland, U, Galli, L, Galli, S, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Georges, M, Gerbino, M, Gervasi, M, Ghigna, T, Giardiello, S, Gjerlw, E, Gonzles, R, Gradziel, M, Grain, J, Grandsire, L, Grupp, F, Gruppuso, A, Gudmundsson, J, Halverson, N, Hamilton, J, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versill, S, Hensley, B, Herman, D, Herranz, D, Hilton, G, Hivon, E, Hlozek, R, Hoang, D, Hornsby, A, Hoshino, Y, Ichiki, K, Iida, T, Ikemoto, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Jones, M, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kintziger, C, 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, Link, M, Lonappan, A, Louis, T, Luzzi, G, Macias-Perez, J, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Maris, M, Marquet, B, Martnez-Gonzlez, E, Martire, F, Masi, S, Massa, M, Masuzawa, M, Matarrese, S, Matsuda, F, Matsumura, T, Mele, L, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Moggi, A, Monelli, M, 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, Neto Godry Farias, N, Nishibori, T, Nishino, H, Noviello, F, O’Neil, G, O’Sullivan, C, Odagiri, K, Ochi, H, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Pascual Cisneros, G, Passerini, A, Patanchon, G, Pelgrim, V, Peloton, J, Pettorino, V, Piacentini, F, Piat, M, Piccirilli, G, Pinsard, F, Pisano, G, Plesseria, J, Polenta, G, Poletti, D, Prouv, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Reintsema, C, Remazeilles, M, Ritacco, A, Rosier, P, 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, Shitvov, A, Signorelli, G, Smecher, G, Spinella, F, Starck, J, Stever, S, Stompor, R, Sudiwala, R, Sugiyama, S, Sullivan, R, Suzuki, A, Suzuki, J, Suzuki, T, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Tavagnacco, D, Taylor, A, Taylor, E, Terao, Y, Terenzi, L, Thermeau, J, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ueki, R, Ullom, J, Umemori, K, Vacher, L, Van Lanen, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wandelt, B, Wang, W, Wehus, I, Weller, J, Westbrook, B, Weymann-Despres, G, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Watanuki, K, Zacchei, A, Zannoni, M, Zonca, A, Hubmayr, J., Ade, P. A. R., Adler, A., Allys, E., Alonso, D., Arnold, K., Auguste, D., Aumont, J., Aurlien, R., Austermann, J. E., Azzoni, S., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Bartolo, N., Basak, S., Battistelli, E., Bautista, L., Beall, J. A., 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., Chiocchetta, C., Clark, S. E., Clermont, L., Clesse, S., Cliche, J., Columbro, F., Connors, J. A., Coppolecchia, A., Coulton, W., Cubas, J., Cukierman, A., Curtis, D., Cuttaia, F., D’Alessandro, G., Dachlythra, K., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Daz Garca, J. J., Dickinson, C., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Douillet, D., Doumayrou, E., Duband, L., Ducout, A., Duff, S. M., Duval, J. M., Ebisawa, K., Elleflot, T., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Farrens, S., Finelli, F., Flauger, R., Fleury-Frenette, K., Franceschet, C., Fuskeland, U., Galli, L., Galli, S., Galloway, M., Ganga, K., Gao, J. R., Genova-Santos, R. T., Georges, M., Gerbino, M., Gervasi, M., Ghigna, T., Giardiello, S., Gjerlw, E., Gonzles, R. Gonzlez, Gradziel, M. L., Grain, J., Grandsire, L., Grupp, F., Gruppuso, A., Gudmundsson, J. E., Halverson, N. W., Hamilton, J., Hargrave, P., Hasebe, T., Hasegawa, M., Hattori, M., Hazumi, M., Henrot-Versill, S., Hensley, B., Herman, D., Herranz, D., Hilton, G. C., Hivon, E., Hlozek, R. A., Hoang, D., Hornsby, A. L., Hoshino, Y., Ichiki, K., Iida, T., Ikemoto, T., Imada, H., Ishimura, K., Ishino, H., Jaehnig, G., Jones, M., Kaga, T., Kashima, S., Katayama, N., Kato, A., Kawasaki, T., Keskitalo, R., Kintziger, C., 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., Link, M. J., Lonappan, A. I., Louis, T., Luzzi, G., Macias-Perez, J., Maciaszek, T., Maffei, B., Maino, D., Maki, M., Mandelli, S., Maris, M., Marquet, B., Martnez-Gonzlez, E., Martire, F. A., Masi, S., Massa, M., Masuzawa, M., Matarrese, S., Matsuda, F. T., Matsumura, T., Mele, L., Mennella, A., Migliaccio, M., Minami, Y., Mitsuda, K., Moggi, A., Monelli, M., 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., Neto Godry Farias, N., Nishibori, T., Nishino, H., Noviello, F., O’Neil, G. C., O’Sullivan, C., Odagiri, K., Ochi, H., Ogawa, H., Oguri, S., Ohsaki, H., Ohta, I. S., Okada, N., Pagano, L., Paiella, A., Paoletti, D., Pascual Cisneros, G., Passerini, A., Patanchon, G., Pelgrim, V., Peloton, J., Pettorino, V., Piacentini, F., Piat, M., Piccirilli, G., Pinsard, F., Pisano, G., Plesseria, J., Polenta, G., Poletti, D., Prouv, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Reintsema, C. D., Remazeilles, M., Ritacco, A., Rosier, P., 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., Shitvov, A., Signorelli, G., Smecher, G., Spinella, F., Starck, J., Stever, S., Stompor, R., Sudiwala, R., Sugiyama, S., Sullivan, R., Suzuki, A., Suzuki, J., Suzuki, T., 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., Terenzi, L., 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., Ueki, R., Ullom, J. N., Umemori, K., Vacher, L., Van Lanen, J., Vermeulen, G., Vielva, P., Villa, F., Vissers, M. R., Vittorio, N., Wandelt, B., Wang, W., Wehus, I. K., Weller, J., Westbrook, B., Weymann-Despres, G., Wilms, J., Winter, B., Wollack, E. J., Yamasaki, N. Y., Yoshida, T., Yumoto, J., Watanuki, K., Zacchei, A., Zannoni, M., and Zonca, A.
Abstract: Feedhorn- and orthomode transducer- (OMT) coupled transition edge sensor (TES) bolometers have been designed and micro-fabricated to meet the optical specifications of the LiteBIRD high frequency telescope (HFT) focal plane. We discuss the design and optical characterization of two LiteBIRD HFT detector types: dual-polarization, dual-frequency-band pixels with 195/280 GHz and 235/337 GHz band centers. Results show well-matched passbands between orthogonal polarization channels and frequency centers within 3% of the design values. The optical efficiency of each frequency channel is conservatively reported to be within the range 0.64−0.72, determined from the response to a cryogenic, temperature-controlled thermal source. These values are in good agreement with expectations and either exceed or are within 10% of the values used in the LiteBIRD sensitivity forecast. Lastly, we report a measurement of loss in Nb/SiNx/Nb microstrip at 100 mK and over the frequency range 200–350 GHz, which is comparable to values previously reported in the literature
Published: 2022

36. In-flight polarization angle calibration for LiteBIRD: Blind challenge and cosmological implications

Author: Krachmalnicoff, N, Matsumura, T, De La Hoz, E, Basak, S, Gruppuso, A, Minami, Y, Baccigalupi, C, Komatsu, E, Martinez-Gonzalez, E, Vielva, P, Aumont, J, Aurlien, R, Azzoni, S, Banday, A, Barreiro, R, Bartolo, N, Bersanelli, M, Calabrese, E, Carones, A, Casas, F, Cheung, K, Chinone, Y, Columbro, F, De Bernardis, P, Diego-Palazuelos, P, Errard, J, Finelli, F, Fuskeland, U, Galloway, M, Genova-Santos, R, Gerbino, M, Ghigna, T, Giardiello, S, Gjerlow, E, Hazumi, M, Henrot-Versille, S, Kisner, T, Lamagna, L, Lattanzi, M, Levrier, F, Luzzi, G, Maino, D, Masi, S, Migliaccio, M, Montier, L, Morgante, G, Mot, B, Nagata, R, Nati, F, Natoli, P, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Remazeilles, M, Rubino-Martin, J, Sasaki, M, Shiraishi, M, Signorelli, G, Stever, S, Tartari, A, Tristram, M, Tsuji, M, Vacher, L, Wehus, I, Zannoni, M, Krachmalnicoff N., Matsumura T., De La Hoz E., Basak S., Gruppuso A., Minami Y., Baccigalupi C., Komatsu E., Martinez-Gonzalez E., Vielva P., Aumont J., Aurlien R., Azzoni S., Banday A. J., Barreiro R. B., Bartolo N., Bersanelli M., Calabrese E., Carones A., Casas F. J., Cheung K., Chinone Y., Columbro F., De Bernardis P., Diego-Palazuelos P., Errard J., Finelli F., Fuskeland U., Galloway M., Genova-Santos R. T., Gerbino M., Ghigna T., Giardiello S., Gjerlow E., Hazumi M., Henrot-Versille S., Kisner T., Lamagna L., Lattanzi M., Levrier F., Luzzi G., Maino D., Masi S., Migliaccio M., Montier L., Morgante G., Mot B., Nagata R., Nati F., Natoli P., Pagano L., Paiella A., Paoletti D., Patanchon G., Piacentini F., Polenta G., Poletti D., Puglisi G., Remazeilles M., Rubino-Martin J., Sasaki M., Shiraishi M., Signorelli G., Stever S., Tartari A., Tristram M., Tsuji M., Vacher L., Wehus I. K., Zannoni M., Krachmalnicoff, N, Matsumura, T, De La Hoz, E, Basak, S, Gruppuso, A, Minami, Y, Baccigalupi, C, Komatsu, E, Martinez-Gonzalez, E, Vielva, P, Aumont, J, Aurlien, R, Azzoni, S, Banday, A, Barreiro, R, Bartolo, N, Bersanelli, M, Calabrese, E, Carones, A, Casas, F, Cheung, K, Chinone, Y, Columbro, F, De Bernardis, P, Diego-Palazuelos, P, Errard, J, Finelli, F, Fuskeland, U, Galloway, M, Genova-Santos, R, Gerbino, M, Ghigna, T, Giardiello, S, Gjerlow, E, Hazumi, M, Henrot-Versille, S, Kisner, T, Lamagna, L, Lattanzi, M, Levrier, F, Luzzi, G, Maino, D, Masi, S, Migliaccio, M, Montier, L, Morgante, G, Mot, B, Nagata, R, Nati, F, Natoli, P, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Remazeilles, M, Rubino-Martin, J, Sasaki, M, Shiraishi, M, Signorelli, G, Stever, S, Tartari, A, Tristram, M, Tsuji, M, Vacher, L, Wehus, I, Zannoni, M, Krachmalnicoff N., Matsumura T., De La Hoz E., Basak S., Gruppuso A., Minami Y., Baccigalupi C., Komatsu E., Martinez-Gonzalez E., Vielva P., Aumont J., Aurlien R., Azzoni S., Banday A. J., Barreiro R. B., Bartolo N., Bersanelli M., Calabrese E., Carones A., Casas F. J., Cheung K., Chinone Y., Columbro F., De Bernardis P., Diego-Palazuelos P., Errard J., Finelli F., Fuskeland U., Galloway M., Genova-Santos R. T., Gerbino M., Ghigna T., Giardiello S., Gjerlow E., Hazumi M., Henrot-Versille S., Kisner T., Lamagna L., Lattanzi M., Levrier F., Luzzi G., Maino D., Masi S., Migliaccio M., Montier L., Morgante G., Mot B., Nagata R., Nati F., Natoli P., Pagano L., Paiella A., Paoletti D., Patanchon G., Piacentini F., Polenta G., Poletti D., Puglisi G., Remazeilles M., Rubino-Martin J., Sasaki M., Shiraishi M., Signorelli G., Stever S., Tartari A., Tristram M., Tsuji M., Vacher L., Wehus I. K., and Zannoni M.
Abstract: We present a demonstration of the in-flight polarization angle calibration for the JAXA/ISAS second strategic large class mission, LiteBIRD, and estimate its impact on the measurement of the tensor-to-scalar ratio parameter, r, using simulated data. We generate a set of simulated sky maps with CMB and polarized foreground emission, and inject instrumental noise and polarization angle offsets to the 22 (partially overlapping) LiteBIRD frequency channels. Our in-flight angle calibration relies on nulling the EB cross correlation of the polarized signal in each channel. This calibration step has been carried out by two independent groups with a blind analysis, allowing an accuracy of the order of a few arc-minutes to be reached on the estimate of the angle offsets. Both the corrected and uncorrected multi-frequency maps are propagated through the foreground cleaning step, with the goal of computing clean CMB maps. We employ two component separation algorithms, the Bayesian-Separation of Components and Residuals Estimate Tool (B-SeCRET), and the Needlet Internal Linear Combination (NILC). We find that the recovered CMB maps obtained with algorithms that do not make any assumptions about the foreground properties, such as NILC, are only mildly affected by the angle miscalibration. However, polarization angle offsets strongly bias results obtained with the parametric fitting method. Once the miscalibration angles are corrected by EB nulling prior to the component separation, both component separation algorithms result in an unbiased estimation of the r parameter. While this work is motivated by the conceptual design study for LiteBIRD, its framework can be broadly applied to any CMB polarization experiment. In particular, the combination of simulation plus blind analysis provides a robust forecast by taking into account not only detector sensitivity but also systematic effects.
Published: 2022

37. Polarization angle requirements for CMB B-mode experiments. Application to the LiteBIRD satellite

Author: Vielva, P, Martinez-Gonzalez, E, Casas, F, Matsumura, T, Henrot-Versille, S, Komatsu, E, Aumont, J, Aurlien, R, Baccigalupi, C, Banday, A, Barreiro, R, Bartolo, N, Calabrese, E, Cheung, K, Columbro, F, Coppolecchia, A, De Bernardis, P, De Haan, T, De La Hoz, E, De Petris, M, Della Torre, S, Diego-Palazuelos, P, Eriksen, H, Errard, J, Finelli, F, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gervasi, M, Genova-Santos, R, Ghigna, T, Gjerlow, E, Gruppuso, A, Hazumi, M, Herranz, D, Hivon, E, Kohri, K, Lamagna, L, Leloup, C, Macias-Perez, J, Masi, S, Matsuda, F, Morgante, G, Nakano, R, Nati, F, Natoli, P, Nerval, S, Odagiri, K, Oguri, S, Pagano, L, Paiella, A, Paoletti, D, Piacentini, F, Polenta, G, Puglisi, G, Remazeilles, M, Ritacco, A, Rubino-Martin, J, Scott, D, Sekimoto, Y, Shiraishi, M, Signorelli, G, Takakura, H, Tartari, A, Thompson, K, Tristram, M, Vacher, L, Vittorio, N, Wehus, I, Zannoni, M, Vielva P., Martinez-Gonzalez E., Casas F. J., Matsumura T., Henrot-Versille S., Komatsu E., Aumont J., Aurlien R., Baccigalupi C., Banday A. J., Barreiro R. B., Bartolo N., Calabrese E., Cheung K., Columbro F., Coppolecchia A., De Bernardis P., De Haan T., De La Hoz E., De Petris M., Della Torre S., Diego-Palazuelos P., Eriksen H. K., Errard J., Finelli F., Franceschet C., Fuskeland U., Galloway M., Ganga K., Gervasi M., Genova-Santos R. T., Ghigna T., Gjerlow E., Gruppuso A., Hazumi M., Herranz D., Hivon E., Kohri K., Lamagna L., Leloup C., Macias-Perez J., Masi S., Matsuda F. T., Morgante G., Nakano R., Nati F., Natoli P., Nerval S., Odagiri K., Oguri S., Pagano L., Paiella A., Paoletti D., Piacentini F., Polenta G., Puglisi G., Remazeilles M., Ritacco A., Rubino-Martin J. A., Scott D., Sekimoto Y., Shiraishi M., Signorelli G., Takakura H., Tartari A., Thompson K. L., Tristram M., Vacher L., Vittorio N., Wehus I. K., Zannoni M., Vielva, P, Martinez-Gonzalez, E, Casas, F, Matsumura, T, Henrot-Versille, S, Komatsu, E, Aumont, J, Aurlien, R, Baccigalupi, C, Banday, A, Barreiro, R, Bartolo, N, Calabrese, E, Cheung, K, Columbro, F, Coppolecchia, A, De Bernardis, P, De Haan, T, De La Hoz, E, De Petris, M, Della Torre, S, Diego-Palazuelos, P, Eriksen, H, Errard, J, Finelli, F, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gervasi, M, Genova-Santos, R, Ghigna, T, Gjerlow, E, Gruppuso, A, Hazumi, M, Herranz, D, Hivon, E, Kohri, K, Lamagna, L, Leloup, C, Macias-Perez, J, Masi, S, Matsuda, F, Morgante, G, Nakano, R, Nati, F, Natoli, P, Nerval, S, Odagiri, K, Oguri, S, Pagano, L, Paiella, A, Paoletti, D, Piacentini, F, Polenta, G, Puglisi, G, Remazeilles, M, Ritacco, A, Rubino-Martin, J, Scott, D, Sekimoto, Y, Shiraishi, M, Signorelli, G, Takakura, H, Tartari, A, Thompson, K, Tristram, M, Vacher, L, Vittorio, N, Wehus, I, Zannoni, M, Vielva P., Martinez-Gonzalez E., Casas F. J., Matsumura T., Henrot-Versille S., Komatsu E., Aumont J., Aurlien R., Baccigalupi C., Banday A. J., Barreiro R. B., Bartolo N., Calabrese E., Cheung K., Columbro F., Coppolecchia A., De Bernardis P., De Haan T., De La Hoz E., De Petris M., Della Torre S., Diego-Palazuelos P., Eriksen H. K., Errard J., Finelli F., Franceschet C., Fuskeland U., Galloway M., Ganga K., Gervasi M., Genova-Santos R. T., Ghigna T., Gjerlow E., Gruppuso A., Hazumi M., Herranz D., Hivon E., Kohri K., Lamagna L., Leloup C., Macias-Perez J., Masi S., Matsuda F. T., Morgante G., Nakano R., Nati F., Natoli P., Nerval S., Odagiri K., Oguri S., Pagano L., Paiella A., Paoletti D., Piacentini F., Polenta G., Puglisi G., Remazeilles M., Ritacco A., Rubino-Martin J. A., Scott D., Sekimoto Y., Shiraishi M., Signorelli G., Takakura H., Tartari A., Thompson K. L., Tristram M., Vacher L., Vittorio N., Wehus I. K., and Zannoni M.
Abstract: A methodology to provide the polarization angle requirements for different sets of detectors, at a given frequency of a CMB polarization experiment, is presented. The uncertainties in the polarization angle of each detector set are related to a given bias on the tensor-to-scalar ratio r parameter. The approach is grounded in using a linear combination of the detector sets to obtain the CMB polarization signal. In addition, assuming that the uncertainties on the polarization angle are in the small angle limit (lower than a few degrees), it is possible to derive analytic expressions to establish the requirements. The methodology also accounts for possible correlations among detectors, that may originate from the optics, wafers, etc. The approach is applied to the LiteBIRD space mission. We show that, for the most restrictive case (i.e., full correlation of the polarization angle systematics among detector sets), the requirements on the polarization angle uncertainties are of around 1 arcmin at the most sensitive frequency bands (i.e., ≈ 150 GHz) and of few tens of arcmin at the lowest (i.e., ≈ 40 GHz) and highest (i.e., ≈ 400 GHz) observational bands. Conversely, for the least restrictive case (i.e., no correlation of the polarization angle systematics among detector sets), the requirements are ≈ 5 times less restrictive than for the previous scenario. At the global and the telescope levels, polarization angle knowledge of a few arcmins is sufficient for correlated global systematic errors and can be relaxed by a factor of two for fully uncorrelated errors in detector polarization angle. The reported uncertainty levels are needed in order to have the bias on r due to systematics below the limit established by the LiteBIRD collaboration.
Published: 2022

38. QUIJOTE scientific results – IV. A northern sky survey in intensity and polarization at 10–20 GHz with the multifrequency instrument

Author: Rubiño-Martín, J A, primary, Guidi, F, additional, Génova-Santos, R T, additional, Harper, S E, additional, Herranz, D, additional, Hoyland, R J, additional, Lasenby, A N, additional, Poidevin, F, additional, Rebolo, R, additional, Ruiz-Granados, B, additional, Vansyngel, F, additional, Vielva, P, additional, Watson, R A, additional, Artal, E, additional, Ashdown, M, additional, Barreiro, R B, additional, Bilbao-Ahedo, J D, additional, Casas, F J, additional, Casaponsa, B, additional, Cepeda-Arroita, R, additional, de la Hoz, E, additional, Dickinson, C, additional, Fernández-Cobos, R, additional, Fernández-Torreiro, M, additional, González-González, R, additional, Hernández-Monteagudo, C, additional, López-Caniego, M, additional, López-Caraballo, C, additional, Martínez-González, E, additional, Peel, M W, additional, Peláez-Santos, A E, additional, Perrott, Y, additional, Piccirillo, L, additional, Razavi-Ghods, N, additional, Scott, P, additional, Titterington, D, additional, Tramonte, D, additional, and Vignaga., R, additional
Published: 2023
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39. QUIJOTE scientific results – VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey

Author: Poidevin, F, primary, Génova-Santos, R T, additional, Rubiño-Martín, J A, additional, López-Caraballo, C H, additional, Watson, R A, additional, Artal, E, additional, Ashdown, M, additional, Barreiro, R B, additional, Casas, F J, additional, de la Hoz, E, additional, Fernández-Torreiro, M, additional, Guidi, F, additional, Herranz, D, additional, Hoyland, R J, additional, Lasenby, A N, additional, Martinez-Gonzalez, E, additional, Peel, M W, additional, Piccirillo, L, additional, Rebolo, R, additional, Ruiz-Granados, B, additional, Tramonte, D, additional, Vansyngel, F, additional, and Vielva, P, additional
Published: 2023
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40. QUIJOTE scientific results – VI. The Haze as seen by QUIJOTE

Author: Guidi, F, primary, Génova-Santos, R T, additional, Rubiño-Martín, J A, additional, Peel, M W, additional, Fernández-Torreiro, M, additional, López-Caraballo, C H, additional, Vignaga, R, additional, de la Hoz, E, additional, Vielva, P, additional, Watson, R A, additional, Ashdown, M, additional, Dickinson, C, additional, Artal, E, additional, Barreiro, R B, additional, Casas, F J, additional, Herranz, D, additional, Hoyland, R J, additional, Lasenby, A N, additional, Martinez-Gonzalez, E, additional, Piccirillo, L, additional, Poidevin, F, additional, Rebolo, R, additional, Ruiz-Granados, B, additional, Tramonte, D, additional, and Vansyngel, F, additional
Published: 2023
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41. QUIJOTE scientific results – V. The microwave intensity and polarization spectra of the Galactic regions W49, W51 and IC443

Author: Tramonte, D, primary, Génova-Santos, R T, additional, Rubiño-Martín, J A, additional, Vielva, P, additional, Poidevin, F, additional, López-Caraballo, C H, additional, Peel, M W, additional, Ashdown, M, additional, Artal, E, additional, Barreiro, R B, additional, Casas, F J, additional, de la Hoz, E, additional, Fernández-Torreiro, M, additional, Guidi, F, additional, Herranz, D, additional, Hoyland, R J, additional, Lasenby, A N, additional, Martinez-Gonzalez, E, additional, Piccirillo, L, additional, Rebolo, R, additional, Ruiz-Granados, B, additional, Vansyngel, F, additional, and Watson, R A, additional
Published: 2023
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42. QUIJOTE scientific results – IX. Radio sources in the QUIJOTE-MFI wide survey maps

Author: Herranz, D, primary, López-Caniego, M, additional, López-Caraballo, C H, additional, Génova-Santos, R T, additional, Perrott, Y C, additional, Rubiño-Martín, J A, additional, Rebolo, R, additional, Artal, E, additional, Ashdown, M, additional, Barreiro, R B, additional, Casas, F J, additional, de la Hoz, E, additional, Fernández-Torreiro, M, additional, Guidi, F, additional, Hoyland, R J, additional, Lasenby, A N, additional, Martínez-González, E, additional, Peel, M W, additional, Piccirillo, L, additional, Poidevin, F, additional, Ruiz-Granados, B, additional, Tramonte, D, additional, Vansyngel, F, additional, Vielva, P, additional, and Watson, R A, additional
Published: 2023
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43. QUIJOTE scientific results – VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI

Author: de la Hoz, E, primary, Barreiro, R B, additional, Vielva, P, additional, Martínez-González, E, additional, Rubiño-Martín, J A, additional, Casaponsa, B, additional, Guidi, F, additional, Ashdown, M, additional, Génova-Santos, R T, additional, Artal, E, additional, Casas, F J, additional, Fernández-Cobos, R, additional, Fernández-Torreiro, M, additional, Herranz, D, additional, Hoyland, R J, additional, Lasenby, A N, additional, López-Caniego, M, additional, López-Caraballo, C H, additional, Peel, M W, additional, Piccirillo, L, additional, Poidevin, F, additional, Rebolo, R, additional, Ruiz-Granados, B, additional, Tramonte, D, additional, Vansyngel, F, additional, and Watson., R A, additional
Published: 2023
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44. Polarization angle requirements for CMB B-mode experiments. Application to the LiteBIRD satellite

Author: Vielva, P., additional, Martínez-González, E., additional, Casas, F.J., additional, Matsumura, T., additional, Henrot-Versillé, S., additional, Komatsu, E., additional, Aumont, J., additional, Aurlien, R., additional, Baccigalupi, C., additional, Banday, A.J., additional, Barreiro, R.B., additional, Bartolo, N., additional, Calabrese, E., additional, Cheung, K., additional, Columbro, F., additional, Coppolecchia, A., additional, de Bernardis, P., additional, de Haan, T., additional, de la Hoz, E., additional, De Petris, M., additional, Della Torre, S., additional, Diego-Palazuelos, P., additional, Eriksen, H.K., additional, Errard, J., additional, Finelli, F., additional, Franceschet, C., additional, Fuskeland, U., additional, Galloway, M., additional, Ganga, K., additional, Gervasi, M., additional, Génova-Santos, R.T., additional, Ghigna, T., additional, Gjerløw, E., additional, Gruppuso, A., additional, Hazumi, M., additional, Herranz, D., additional, Hivon, E., additional, Kohri, K., additional, Lamagna, L., additional, Leloup, C., additional, Macias-Perez, J., additional, Masi, S., additional, Matsuda, F.T., additional, Morgante, G., additional, Nakano, R., additional, Nati, F., additional, Natoli, P., additional, Nerval, S., additional, Odagiri, K., additional, Oguri, S., additional, Pagano, L., additional, Paiella, A., additional, Paoletti, D., additional, Piacentini, F., additional, Polenta, G., additional, Puglisi, G., additional, Remazeilles, M., additional, Ritacco, A., additional, Rubino-Martin, J.A., additional, Scott, D., additional, Sekimoto, Y., additional, Shiraishi, M., additional, Signorelli, G., additional, Takakura, H., additional, Tartari, A., additional, Thompson, K.L., additional, Tristram, M., additional, Vacher, L., additional, Vittorio, N., additional, Wehus, I.K., additional, and Zannoni, M., additional
Published: 2022
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45. Determination of polarization angles in CMB experiments and application to CMB component separation analyses

Author: de la Hoz, E., primary, Diego-Palazuelos, P., additional, Martínez-González, E., additional, Vielva, P., additional, Barreiro, R.B., additional, and Bilbao-Ahedo, J.D., additional
Published: 2022
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46. In-flight polarization angle calibration for LiteBIRD: blind challenge and cosmological implications

Author: Krachmalnicoff, N., additional, Matsumura, T., additional, de la Hoz, E., additional, Basak, S., additional, Gruppuso, A., additional, Minami, Y., additional, Baccigalupi, C., additional, Komatsu, E., additional, Martínez-González, E., additional, Vielva, P., additional, Aumont, J., additional, Aurlien, R., additional, Azzoni, S., additional, Banday, A.J., additional, Barreiro, R.B., additional, Bartolo, N., additional, Bersanelli, M., additional, Calabrese, E., additional, Carones, A., additional, Casas, F.J., additional, Cheung, K., additional, Chinone, Y., additional, Columbro, F., additional, de Bernardis, P., additional, Diego-Palazuelos, P., additional, Errard, J., additional, Finelli, F., additional, Fuskeland, U., additional, Galloway, M., additional, Genova-Santos, R.T., additional, Gerbino, M., additional, Ghigna, T., additional, Giardiello, S., additional, Gjerløw, E., additional, Hazumi, M., additional, Henrot-Versillé, S., additional, Kisner, T., additional, Lamagna, L., additional, Lattanzi, M., additional, Levrier, F., additional, Luzzi, G., additional, Maino, D., additional, Masi, S., additional, Migliaccio, M., additional, Montier, L., additional, Morgante, G., additional, Mot, B., additional, Nagata, R., additional, Nati, F., additional, Natoli, P., additional, Pagano, L., additional, Paiella, A., additional, Paoletti, D., additional, Patanchon, G., additional, Piacentini, F., additional, Polenta, G., additional, Poletti, D., additional, Puglisi, G., additional, Remazeilles, M., additional, Rubino-Martin, J., additional, Sasaki, M., additional, Shiraishi, M., additional, Signorelli, G., additional, Stever, S., additional, Tartari, A., additional, Tristram, M., additional, Tsuji, M., additional, Vacher, L., additional, Wehus, I.K., additional, and Zannoni, M., additional
Published: 2022
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47. Overview of the medium and high frequency telescopes of the LiteBIRD space mission

Author: Lystrup, Makenzie, Montier, L, Mot, B, de Bernardis, P, Maffei, B, Pisano, G, Columbro, F, Gudmundsson, J, Henrot-Versillé, S, Lamagna, L, Montgomery, J, Prouvé, T, Russell, M, Savini, G, Stever, S, Thompson, K, Tsujimoto, M, Tucker, C, Westbrook, B, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, 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, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Morgante, G, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, Montier, Ludovic, Mot, Baptiste, de Bernardis, Paolo, Maffei, Bruno, Pisano, Giampaolo, Columbro, Fabio, Gudmundsson, Jon E., Henrot-Versillé, Sophie, Lamagna, Luca, Montgomery, Joshua, Prouvé, Thomas, Russell, Megan, Savini, Giorgio, Stever, Samantha, Thompson, Keith L., Tsujimoto, Masahiro, Tucker, Carole, Westbrook, Benjamin, Ade, Peter A., Adler, Alexandre, Allys, Erwan, Arnold, Kam, Auguste, Didier, Aumont, Jonathan, Aurlien, Ragnhild, Austermann, Jason, Baccigalupi, Carlo, Banday, Anthony J., Banerji, Ranajoy, Barreiro, Rita B., Basak, Soumen, Beall, Jim, Beck, Dominic, Beckman, Shawn, Bermejo, Juan, Bersanelli, Marco, Bonis, Julien, Borrill, Julian, Boulanger, Francois, Bounissou, Sophie, Brilenkov, Maksym, Brown, Michael, Bucher, Martin, Calabrese, Erminia, Campeti, Paolo, Carones, Alessandro, Casas, Francisco J., Challinor, Anthony, Chan, Victor, Cheung, Kolen, Chinone, Yuji, Cliche, Jean F., Colombo, Loris, Cubas, Javier, Cukierman, Ari, Curtis, David, D'Alessandro, Giuseppe, Dachlythra, Nadia, De Petris, Marco, Dickinson, Clive, Diego-Palazuelos, Patricia, Dobbs, Matt, Dotani, Tadayasu, Duband, Lionel, Duff, Shannon, Duval, Jean M., Ebisawa, Ken, Elleflot, Tucker, Eriksen, Hans K., Errard, Josquin, Essinger-Hileman, Thomas, Finelli, Fabio, Flauger, Raphael, Franceschet, Cristian, Fuskeland, Unni, Galloway, Mathew, Ganga, Ken, Gao, Jian R., Genova-Santos, Ricardo, Gerbino, Martina, Gervasi, Massimo, Ghigna, Tommaso, Gjerløw, Eirik, Gradziel, Marcin L., Grain, Julien, Grupp, Frank, Gruppuso, Alessandro, de Haan, Tijmen, Halverson, Nils W., Hargrave, Peter, Hasebe, Takashi, Hasegawa, Masaya, Hattori, Makoto, Hazumi, Masashi, Herman, Daniel, Herranz, Diego, Hill, Charles A., Hilton, Gene, Hirota, Yukimasa, Hivon, Eric, Hlozek, Renee A., Hoshino, Yurika, de la Hoz, Elena, Hubmayr, Johannes, Ichiki, Kiyotomo, Iida, Teruhito, Imada, Hiroaki, Ishimura, Kosei, Ishino, Hirokazu, Jaehnig, Greg, Kaga, Tooru, Kashima, Shingo, Katayama, Nobuhiko, Kato, Akihiro, Kawasaki, Takeo, Keskitalo, Reijo, Kisner, Theodore, Kobayashi, Yohei, Kogiso, Nozomu, Kogut, Alan, Kohri, Kazunori, Komatsu, Eiichiro, Komatsu, Kunimoto, Konishi, Kuniaki, Krachmalnicoff, Nicoletta, Kreykenbohm, Ingo, Kuo, Chao-Lin L., Kushino, Akihiro, Lanen, Jeff V., Lattanzi, Massimiliano, Lee, Adrian T., Leloup, Clément, Levrier, François, Linder, Eric, Louis, Thibaut, Luzzi, Gemma, Maciaszek, Thierry, Maino, Davide, Maki, Muneyoshi, Mandelli, Stefano, Martinez-Gonzalez, Enrique, Masi, Silvia, Matsumura, Tomotake, Mennella, Aniello, Migliaccio, Marina, Minami, Yuto, Mitsuda, Kazuhisa, Morgante, Gianluca, Murata, Yasuhiro, Murphy, John A., Nagai, Makoto, Nagano, Yuya, Nagasaki, Taketo, Nagata, Ryo, Nakamura, Shogo, Namikawa, Toshiya, Natoli, Paolo, Nerval, Simran, Nishibori, Toshiyuki, Nishino, Haruki, O'Sullivan, Créidhe, Ogawa, Hideo, Ogawa, Hiroyuki, Oguri, Shugo, Ohsaki, Hiroyuki, Ohta, Izumi S., Okada, Norio, Okada, Nozomi, Pagano, Luca, Paiella, Alessandro, Paoletti, Daniela, Patanchon, Guillaume, Peloton, Julien, Piacentini, Francesco, Polenta, Gianluca, Poletti, Davide, Puglisi, Giuseppe, Rambaud, Damien, Raum, Christopher, Realini, Sabrina, Reinecke, Martin, Remazeilles, Mathieu, Ritacco, Alessia, Roudil, Gilles, Rubino-Martin, Jose A., Sakurai, Haruyuki, Sakurai, Yuki, Sandri, Maura, Sasaki, Manami, Scott, Douglas, Seibert, Joseph, Sekimoto, Yutaro, Sherwin, Blake, Shinozaki, Keisuke, Shiraishi, Maresuke, Shirron, Peter, Signorelli, Giovanni, Smecher, Graeme, Stompor, Radek, Sugai, Hajime, Sugiyama, Shinya, Suzuki, Aritoki, Suzuki, Junichi, Svalheim, Trygve L., Switzer, Eric, Takaku, Ryota, Takakura, Hayato, Takakura, Satoru, Takase, Yusuke, Takeda, Youichi, Tartari, Andrea, Taylor, Ellen, Terao, Yutaka, Thommesen, Harald, Thorne, Ben, Toda, Takayuki, Tomasi, Maurizio, Tominaga, Mayu, Trappe, Neil, Tristram, Matthieu, Tsuji, Masatoshi, Ullom, Joe, Vermeulen, Gerard, Vielva, Patricio, Villa, Fabrizio, Vissers, Michael, Vittorio, Nicola, Wehus, Ingunn, Weller, Jochen, Wilms, Joern, Winter, Berend, Wollack, Edward J., Yamasaki, Noriko Y., Yoshida, Tetsuya, Yumoto, Junji, Zannoni, Mario, Zonca, Andrea, Lystrup, Makenzie, Montier, L, Mot, B, de Bernardis, P, Maffei, B, Pisano, G, Columbro, F, Gudmundsson, J, Henrot-Versillé, S, Lamagna, L, Montgomery, J, Prouvé, T, Russell, M, Savini, G, Stever, S, Thompson, K, Tsujimoto, M, Tucker, C, Westbrook, B, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, 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, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Morgante, G, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, Montier, Ludovic, Mot, Baptiste, de Bernardis, Paolo, Maffei, Bruno, Pisano, Giampaolo, Columbro, Fabio, Gudmundsson, Jon E., Henrot-Versillé, Sophie, Lamagna, Luca, Montgomery, Joshua, Prouvé, Thomas, Russell, Megan, Savini, Giorgio, Stever, Samantha, Thompson, Keith L., Tsujimoto, Masahiro, Tucker, Carole, Westbrook, Benjamin, Ade, Peter A., Adler, Alexandre, Allys, Erwan, Arnold, Kam, Auguste, Didier, Aumont, Jonathan, Aurlien, Ragnhild, Austermann, Jason, Baccigalupi, Carlo, Banday, Anthony J., Banerji, Ranajoy, Barreiro, Rita B., Basak, Soumen, Beall, Jim, Beck, Dominic, Beckman, Shawn, Bermejo, Juan, Bersanelli, Marco, Bonis, Julien, Borrill, Julian, Boulanger, Francois, Bounissou, Sophie, Brilenkov, Maksym, Brown, Michael, Bucher, Martin, Calabrese, Erminia, Campeti, Paolo, Carones, Alessandro, Casas, Francisco J., Challinor, Anthony, Chan, Victor, Cheung, Kolen, Chinone, Yuji, Cliche, Jean F., Colombo, Loris, Cubas, Javier, Cukierman, Ari, Curtis, David, D'Alessandro, Giuseppe, Dachlythra, Nadia, De Petris, Marco, Dickinson, Clive, Diego-Palazuelos, Patricia, Dobbs, Matt, Dotani, Tadayasu, Duband, Lionel, Duff, Shannon, Duval, Jean M., Ebisawa, Ken, Elleflot, Tucker, Eriksen, Hans K., Errard, Josquin, Essinger-Hileman, Thomas, Finelli, Fabio, Flauger, Raphael, Franceschet, Cristian, Fuskeland, Unni, Galloway, Mathew, Ganga, Ken, Gao, Jian R., Genova-Santos, Ricardo, Gerbino, Martina, Gervasi, Massimo, Ghigna, Tommaso, Gjerløw, Eirik, Gradziel, Marcin L., Grain, Julien, Grupp, Frank, Gruppuso, Alessandro, de Haan, Tijmen, Halverson, Nils W., Hargrave, Peter, Hasebe, Takashi, Hasegawa, Masaya, Hattori, Makoto, Hazumi, Masashi, Herman, Daniel, Herranz, Diego, Hill, Charles A., Hilton, Gene, Hirota, Yukimasa, Hivon, Eric, Hlozek, Renee A., Hoshino, Yurika, de la Hoz, Elena, Hubmayr, Johannes, Ichiki, Kiyotomo, Iida, Teruhito, Imada, Hiroaki, Ishimura, Kosei, Ishino, Hirokazu, Jaehnig, Greg, Kaga, Tooru, Kashima, Shingo, Katayama, Nobuhiko, Kato, Akihiro, Kawasaki, Takeo, Keskitalo, Reijo, Kisner, Theodore, Kobayashi, Yohei, Kogiso, Nozomu, Kogut, Alan, Kohri, Kazunori, Komatsu, Eiichiro, Komatsu, Kunimoto, Konishi, Kuniaki, Krachmalnicoff, Nicoletta, Kreykenbohm, Ingo, Kuo, Chao-Lin L., Kushino, Akihiro, Lanen, Jeff V., Lattanzi, Massimiliano, Lee, Adrian T., Leloup, Clément, Levrier, François, Linder, Eric, Louis, Thibaut, Luzzi, Gemma, Maciaszek, Thierry, Maino, Davide, Maki, Muneyoshi, Mandelli, Stefano, Martinez-Gonzalez, Enrique, Masi, Silvia, Matsumura, Tomotake, Mennella, Aniello, Migliaccio, Marina, Minami, Yuto, Mitsuda, Kazuhisa, Morgante, Gianluca, Murata, Yasuhiro, Murphy, John A., Nagai, Makoto, Nagano, Yuya, Nagasaki, Taketo, Nagata, Ryo, Nakamura, Shogo, Namikawa, Toshiya, Natoli, Paolo, Nerval, Simran, Nishibori, Toshiyuki, Nishino, Haruki, O'Sullivan, Créidhe, Ogawa, Hideo, Ogawa, Hiroyuki, Oguri, Shugo, Ohsaki, Hiroyuki, Ohta, Izumi S., Okada, Norio, Okada, Nozomi, Pagano, Luca, Paiella, Alessandro, Paoletti, Daniela, Patanchon, Guillaume, Peloton, Julien, Piacentini, Francesco, Polenta, Gianluca, Poletti, Davide, Puglisi, Giuseppe, Rambaud, Damien, Raum, Christopher, Realini, Sabrina, Reinecke, Martin, Remazeilles, Mathieu, Ritacco, Alessia, Roudil, Gilles, Rubino-Martin, Jose A., Sakurai, Haruyuki, Sakurai, Yuki, Sandri, Maura, Sasaki, Manami, Scott, Douglas, Seibert, Joseph, Sekimoto, Yutaro, Sherwin, Blake, Shinozaki, Keisuke, Shiraishi, Maresuke, Shirron, Peter, Signorelli, Giovanni, Smecher, Graeme, Stompor, Radek, Sugai, Hajime, Sugiyama, Shinya, Suzuki, Aritoki, Suzuki, Junichi, Svalheim, Trygve L., Switzer, Eric, Takaku, Ryota, Takakura, Hayato, Takakura, Satoru, Takase, Yusuke, Takeda, Youichi, Tartari, Andrea, Taylor, Ellen, Terao, Yutaka, Thommesen, Harald, Thorne, Ben, Toda, Takayuki, Tomasi, Maurizio, Tominaga, Mayu, Trappe, Neil, Tristram, Matthieu, Tsuji, Masatoshi, Ullom, Joe, Vermeulen, Gerard, Vielva, Patricio, Villa, Fabrizio, Vissers, Michael, Vittorio, Nicola, Wehus, Ingunn, Weller, Jochen, Wilms, Joern, Winter, Berend, Wollack, Edward J., Yamasaki, Noriko Y., Yoshida, Tetsuya, Yumoto, Junji, Zannoni, Mario, and Zonca, Andrea
Abstract: LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD.
Published: 2020

48. O–234 Influence of assisted reproductive technologies in the prevalence of congenital defects. Study on low risk of congenital defects population

Author: Garcia Cabrera, M., Zurit, M.J, Sainz, J.A, De la Hoz, E., Caballero, V., and Garrido, R.
Published: 2011

49. Phagocyte Fcγ receptors expression in HIV infected patients with active tuberculosis: Effect of anti-tuberculous therapy: 138

Author: Escobar, M. A., García-Egido, A. A., Ruiz, P., Gomez-Soto, F., Fernandez, F. J., Aparicio, J. M., De la Hoz, E., Rivera, C., and Gomez, F.
Published: 2006

50. Increased morbidity and mortality in patients with hyperglycemia during hospitalization: 30

Author: Bernal, J. A., Escobar, M. A., García-Egido, A. A., Fernandez-Delgado, F. J., de la Hoz, E., Aparicio, J. M., Romero, S. P., Ruiz, P., García-Gil, D., and Gomez, F.
Published: 2005

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