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101. Comparison of one-year real-world outcomes between red (670 nm) subthreshold micropulse laser treatment and intravitreal aflibercept injection for treatment-naïve diabetic macular edema

Author

Wataru Kikushima, Yukiko Furuhata, Taiyo Shijo, Mizuki Matsumoto, Yoichi Sakurada, Daphne Viel Tsuru, and Kenji Kashiwagi

Subjects
Treatment-naïve DME, Red SMPL, Anti-VEGF agent, aflibercept, OCTA, Medicine (General), R5-920
Abstract

Purpose: To evaluate the treatment outcomes of subthreshold micropulse laser (SMPL) with a wavelength of 670 nm (red) for treatment-naïve diabetic macular edema (DME). Methods: A retrospective observational study which included 42 eyes in 34 patients diagnosed with treatment-naïve DME was conducted. Twenty-one eyes underwent red SMPL and the other 21 eyes underwent intravitreal injection of aflibercept (IVA) as initial treatment and were followed up for 12 months. Best-corrected visual acuity (BCVA), central retinal thickness (CRT) on optical coherence tomography (OCT), vessel density (VD), and foveal avascular zone area on OCT angiography (OCTA) were measured and compared between the two groups. Results: In the red SMPL group, the mean BCVA slightly improved from 0.29 ± 0.28 at baseline to 0.22 ± 0.29 at 12 months (p = 0.18), while the mean CRT significantly decreased from 472 ± 200 µm at baseline to 320 ± 136 µm at 12 months (p = 0.003). At 12 months from baseline, the mean change in BCVA and CRT were similar between the red SMPL and IVA groups (p = 0.79 and p = 0.31, respectively). No significant change was detected in OCTA parameters except for VD at the nasal section in the red SMPL group. Conclusion: Red SMPL for treatment-naïve DME maintained BCVA and significantly reduced CRT at 12 months. These treatment outcomes were equivalent to IVA in real-world settings, which tend to be inferior to clinical trials.

Published
2025
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102. Euclid preparation: XXII. Selection of Quiescent Galaxies from Mock Photometry using Machine Learning

Author

Euclid Collaboration, Humphrey, A., Bisigello, L., Cunha, P. A. C., Bolzonella, M., Fotopoulou, S., Caputi, K., Tortora, C., Zamorani, G., Papaderos, P., Vergani, D., Brinchmann, J., Moresco, M., Amara, A., Auricchio, N., Baldi, M., Bender, R., Bonino, D., Branchini, E., Brescia, M., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Frailis, M., Franceschi, E., Fumana, M., Gomez-Alvarez, P., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Guzzo, L., Haugan, S. V. H., Holmes, W., Hormuth, F., Jahnke, K., Kummel, M., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., McCracken, H. J., Medinaceli, E., Melchior, M., Meneghetti, M., Merlin, E., Meylan, G., Moscardini, L., Munari, E., Nakajima, R., Niemi, S. M., Nightingale, J., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sapone, D., Sartoris, B., Scaramella, R., Schneider, P., Scodeggio, M., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespi, P., Tavagnacco, D., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valenziano, L., Vassallo, T., Wang, Y., Weller, J., Zacchei, A., Zoubian, J., Andreon, S., Bardelli, S., Boucaud, A., Farinelli, R., Gracia-Carpio, J., Maino, D., Mauri, N., Mei, S., Morisset, N., Sureau, F., Tenti, M., Tramacere, A., Zucca, E., Baccigalupi, C., Balaguera-Antolinez, A., Biviano, A., Blanchard, A., Borgani, S., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Cooray, A. R., Coupon, J., Courtois, H. M., Cucciati, O., Davini, S., De Lucia, G., Dole, H., Escartin, J. A., Escoffier, S., Fabricius, M., Farina, M., Finelli, F., Ganga, K., Garcia-Bellido, J., George, K., Giacomini, F., Gozaliasl, G., Hook, I., Huertas-Company, M., Joachimi, B., Kansal, V., Kashlinsky, A., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maoli, R., Marcin, S., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., Morgante, G., Nucita, A. A., Patrizii, L., Peel, A., Pollack, J. E., Popa, V., Porciani, C., Potter, D., Reimberg, P., Sanchez, A. G., Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Stadel, J., Teyssier, R., Valieri, C., Valiviita, J., Viel, M., Calura, F., and Hildebrandt, H.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The Euclid Space Telescope will provide deep imaging at optical and near-infrared wavelengths, along with slitless near-infrared spectroscopy, across ~15,000 sq deg of the sky. Euclid is expected to detect ~12 billion astronomical sources, facilitating new insights into cosmology, galaxy evolution, and various other topics. To optimally exploit the expected very large data set, there is the need to develop appropriate methods and software. Here we present a novel machine-learning based methodology for selection of quiescent galaxies using broad-band Euclid I_E, Y_E, J_E, H_E photometry, in combination with multiwavelength photometry from other surveys. The ARIADNE pipeline uses meta-learning to fuse decision-tree ensembles, nearest-neighbours, and deep-learning methods into a single classifier that yields significantly higher accuracy than any of the individual learning methods separately. The pipeline has `sparsity-awareness', so that missing photometry values are still informative for the classification. Our pipeline derives photometric redshifts for galaxies selected as quiescent, aided by the `pseudo-labelling' semi-supervised method. After application of the outlier filter, our pipeline achieves a normalized mean absolute deviation of ~< 0.03 and a fraction of catastrophic outliers of ~< 0.02 when measured against the COSMOS2015 photometric redshifts. We apply our classification pipeline to mock galaxy photometry catalogues corresponding to three main scenarios: (i) Euclid Deep Survey with ancillary ugriz, WISE, and radio data; (ii) Euclid Wide Survey with ancillary ugriz, WISE, and radio data; (iii) Euclid Wide Survey only. Our classification pipeline outperforms UVJ selection, in addition to the Euclid I_E-Y_E, J_E-H_E and u-I_E,I_E-J_E colour-colour methods, with improvements in completeness and the F1-score of up to a factor of 2. (Abridged), Comment: 37 pages (including appendices), 26 figures; accepted for publication in Astronomy & Astrophysics

Published
2022
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103. Euclid preparation XXVI. The Euclid Morphology Challenge. Towards structural parameters for billions of galaxies

Author

Euclid Collaboration, Bretonnière, H., Kuchner, U., Huertas-Company, M., Merlin, E., Castellano, M., Tuccillo, D., Buitrago, F., Conselice, C. J., Boucaud, A., Häußler, B., Kümmel, M., Hartley, W. G., Ayllon, A. Alvarez, Bertin, E., Ferrari, F., Ferreira, L., Gavazzi, R., Hernández-Lang, D., Lucatelli, G., Robotham, A. S. G., Schefer, M., Wang, L., Cabanac, R., Sánchez, H. Domínguez, Duc, P. -A., Fotopoulou, S., Kruk, S., La Marca, A., Margalef-Bentabol, B., Marleau, F. R., Tortora, C., Aghanim, N., Amara, A., Auricchio, N., Azzollini, R., Baldi, M., Bender, R., Bodendorf, C., Branchini, E., Brescia, M., Brinchmann, J., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Cropper, M., Da Silva, A., Degaudenzi, H., Dinis, J., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Frailis, M., Franceschi, E., Fumana, M., Galeotta, S., Garilli, B., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hornstrup, A., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kohley, R., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., McCracken, H. J., Medinaceli, E., Melchior, M., Meneghetti, M., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Percival, W., Pettorino, V., Polenta, G., Poncet, M., Pozzetti, L., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Rosset, C., Rossetti, E., Saglia, R., Sapone, D., Sartoris, B., Schneider, P., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Skottfelt, J., Starck, J. -L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Tutusaus, I., Valentijn, E. A., Valenziano, L., Vassallo, T., Wang, Y., Weller, J., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Colodro-Conde, C., Di Ferdinando, D., Graciá-Carpio, J., Lindholm, V., Mauri, N., Mei, S., Scottez, V., Zucca, E., Baccigalupi, C., Ballardini, M., Bernardeau, F., Biviano, A., Borgani, S., Borlaff, A. S., Burigana, C., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Cooray, A. R., Coupon, J., Courtois, H. M., Davini, S., De Lucia, G., Desprez, G., Escartin, J. A., Escoffier, S., Fabricius, M., Farina, M., Fontana, A., Ganga, K., Garcia-Bellido, J., George, K., Gozaliasl, G., Hildebrandt, H., Hook, I., Ilbert, O., Ilić, S., Joachimi, B., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Loureiro, A., Macias-Perez, J., Magliocchetti, M., Maoli, R., Marcin, S., Martinelli, M., Martinet, N., Maturi, M., Monaco, P., Morgante, G., Nadathur, S., Nucita, A. A., Patrizii, L., Popa, V., Porciani, C., Potter, D., Pourtsidou, A., Pöntinen, M., Reimberg, P., Sánchez, A. G., Sakr, Z., Schirmer, M., Sefusatti, E., Sereno, M., Stadel, J., Teyssier, R., Valiviita, J., van Mierlo, S. E., Veropalumbo, A., Viel, M., Weaver, J. R., and Scott, D.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The various Euclid imaging surveys will become a reference for studies of galaxy morphology by delivering imaging over an unprecedented area of 15 000 square degrees with high spatial resolution. In order to understand the capabilities of measuring morphologies from Euclid-detected galaxies and to help implement measurements in the pipeline, we have conducted the Euclid Morphology Challenge, which we present in two papers. While the companion paper by Merlin et al. focuses on the analysis of photometry, this paper assesses the accuracy of the parametric galaxy morphology measurements in imaging predicted from within the Euclid Wide Survey. We evaluate the performance of five state-of-the-art surface-brightness-fitting codes DeepLeGATo, Galapagos-2, Morfometryka, Profit and SourceXtractor++ on a sample of about 1.5 million simulated galaxies resembling reduced observations with the Euclid VIS and NIR instruments. The simulations include analytic S\'ersic profiles with one and two components, as well as more realistic galaxies generated with neural networks. We find that, despite some code-specific differences, all methods tend to achieve reliable structural measurements (10% scatter on ideal S\'ersic simulations) down to an apparent magnitude of about 23 in one component and 21 in two components, which correspond to a signal-to-noise ratio of approximately 1 and 5 respectively. We also show that when tested on non-analytic profiles, the results are typically degraded by a factor of 3, driven by systematics. We conclude that the Euclid official Data Releases will deliver robust structural parameters for at least 400 million galaxies in the Euclid Wide Survey by the end of the mission. We find that a key factor for explaining the different behaviour of the codes at the faint end is the set of adopted priors for the various structural parameters., Comment: Accepted by A&A. 30 pages, 23+6 figures, Euclid pre-launch key paper. Companion paper: Euclid Collaboration XXV: Merlin et al. 2022 Minor corrections after journal review

Published
2022
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104. Euclid preparation. XXV. The Euclid Morphology Challenge -- Towards model-fitting photometry for billions of galaxies

Author

Euclid Collaboration, Merlin, E., Castellano, M., Bretonnière, H., Huertas-Company, M., Kuchner, U., Tuccillo, D., Buitrago, F., Peterson, J. R., Conselice, C. J., Caro, F., Dimauro, P., Nemani, L., Fontana, A., Kümmel, M., Häußler, B., Hartley, W. G., Ayllon, A. Alvarez, Bertin, E., Dubath, P., Ferrari, F., Ferreira, L., Gavazzi, R., Hernández-Lang, D., Lucatelli, G., Robotham, A. S. G., Schefer, M., Tortora, C., Aghanim, N., Amara, A., Amendola, L., Auricchio, N., Baldi, M., Bender, R., Bodendorf, C., Branchini, E., Brescia, M., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Cropper, M., Da Silva, A., Degaudenzi, H., Dinis, J., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Frailis, M., Franceschi, E., Franzetti, P., Galeotta, S., Garilli, B., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hornstrup, A., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kitching, T., Kohley, R., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., McCracken, H. J, Medinaceli, E., Melchior, M., Meneghetti, M., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Percival, W. J., Polenta, G., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Rossetti, E., Saglia, R., Sapone, D., Sartoris, B., Schneider, P., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Skottfelt, J., Starck, J. -L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Tutusaus, I., Valenziano, L., Vassallo, T., Wang, Y., Weller, J., Zacchei, A., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Boucaud, A., Colodro-Conde, C., Di Ferdinando, D., Graciá-Carpio, J., Lindholm, V., Mauri, N., Mei, S., Neissner, C., Scottez, V., Tramacere, A., Zucca, E., Baccigalupi, C., Balaguera-Antolínez, A., Ballardini, M., Bernardeau, F., Biviano, A., Borgani, S., Borlaff, A. S., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Cooray, A. R., Coupon, J., Courtois, H. M., Cucciati, O., Davini, S., De Lucia, G., Desprez, G., Escartin, J. A., Escoffier, S., Farina, M., Ganga, K., Garcia-Bellido, J., George, K., Gozaliasl, G., Hildebrandt, H., Hook, I., Ilbert, O., Ilic, S., Joachimi, B., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Loureiro, A., Macias-Perez, J., Magliocchetti, M., Mainetti, G., Maoli, R., Marcin, S., Martinelli, M., Martinet, N., Matthew, S., Maturi, M., Metcalf, R. B., Monaco, P., Morgante, G., Nadathur, S., Nucita, A. A., Patrizii, L., Popa, V., Porciani, C., Potter, D., Pourtsidou, A., Pöntinen, M., Reimberg, P., Sánchez, A. G., Sakr, Z., Schirmer, M., Sereno, M., Stadel, J., Teyssier, R., Valieri, C., Valiviita, J., van Mierlo, S. E., Veropalumbo, A., Viel, M., Weaver, J. R., and Scott, D.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The ESA Euclid mission will provide high-quality imaging for about 1.5 billion galaxies. A software pipeline to automatically process and analyse such a huge amount of data in real time is being developed by the Science Ground Segment of the Euclid Consortium; this pipeline will include a model-fitting algorithm, which will provide photometric and morphological estimates of paramount importance for the core science goals of the mission and for legacy science. The Euclid Morphology Challenge is a comparative investigation of the performance of five model-fitting software packages on simulated Euclid data, aimed at providing the baseline to identify the best suited algorithm to be implemented in the pipeline. In this paper we describe the simulated data set, and we discuss the photometry results. A companion paper (Euclid Collaboration: Bretonni\`ere et al. 2022) is focused on the structural and morphological estimates. We created mock Euclid images simulating five fields of view of 0.48 deg2 each in the $I_E$ band of the VIS instrument, each with three realisations of galaxy profiles (single and double S\'ersic, and 'realistic' profiles obtained with a neural network); for one of the fields in the double S\'ersic realisation, we also simulated images for the three near-infrared $Y_E$, $J_E$ and $H_E$ bands of the NISP-P instrument, and five Rubin/LSST optical complementary bands ($u$, $g$, $r$, $i$, and $z$). To analyse the results we created diagnostic plots and defined ad-hoc metrics. Five model-fitting software packages (DeepLeGATo, Galapagos-2, Morfometryka, ProFit, and SourceXtractor++) were compared, all typically providing good results. (cut), Comment: 29 pages, 33 figures. Euclid pre-launch key paper. Companion paper: Bretonniere et al. 2022

Published
2022
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105. Performance of novel VUV-sensitive Silicon Photo-Multipliers for nEXO

Author

Gallina, G., Guan, Y., Retiere, F., Cao, G., Bolotnikov, A., Kotov, I., Rescia, S., Soma, A. K., Tsang, T., Darroch, L., Brunner, T., Bolster, J., Cohen, J. R., Franco, T. Pinto, Gillis, W. C., Smalley, H. Peltz, Thibado, S., Pocar, A., Bhat, A., Jamil, A., Moore, D. C., Adhikari, G., Kharusi, S. Al, Angelico, E., Arnquist, I. J., Arsenault, P., Badhrees, I., Bane, J., Belov, V., Bernard, E. P., Bhatta, T., Brodsky, J. P., Brown, E., Caden, E., Cao, L., Chambers, C., Chana, B., Charlebois, S. A., Chernyak, D., Chiu, M., Cleveland, B., Collister, R., Cvitan, M., Dalmasson, J., Daniels, T., Deslandes, K., DeVoe, R., di Vacri, M. L., Ding, Y., Dolinski, M. J., Dragone, A., Echevers, J., Eckert, B., Elbeltagi, M., Fabris, L., Fairbank, W., Farine, J., Fu, Y. S., Gallacher, D., Gautam, P., Giacomini, G., Gingras, C., Goeldi, D., Gornea, R., Gratta, G., Hardy, C. A., Hedges, S., Heffner, M., Hein, E., Holt, J., Hoppe, E. W., Hößl, J., House, A., Hunt, W., Iverson, A., Jiang, X. S., Karelin, A., Kaufman, L. J., Krücken, R., Kuchenkov, A., Kumar, K. S., Larson, A., Leach, K. G., Lenardo, B. G., Leonard, D. S., Lessard, G., Li, G., Li, S., Li, Z., Licciardi, C., Lindsay, R., MacLellan, R., Mahtab, M., Majidi, S., Malbrunot, C., Margetak, P., Martel-Dion, P., Martin, L., Masbou, J., Massacret, N., McMichael, K., Mong, B., Murray, K., Nattress, J., Natzke, C. R., Ngwadla, X. E., Ondze, J. C. Nzobadila, Odian, A., Orrell, J. L., Ortega, G. S., Overman, C. T., Parent, S., Perna, A., Piepke, A., Pletskova, N., Pratte, J. F., Radeka, V., Raguzin, E., Ramonnye, G. J., Rao, T., Rasiwala, H., Raymond, K., Rebeiro, B. M., Richardson, G., Ringuette, J., Riot, V., Rossignol, T., Rowson, P. C., Rudolph, L., Saldanha, R., Sangiorgio, S., Shang, X., Spadoni, F., Stekhanov, V., Sun, X. L., Tidball, A., Totev, T., Triambak, S., Tsang, R. H. M., Tyuka, O. A., Vachon, F., Vidal, M., Viel, S., Visser, G., Wagenpfeil, M., Walent, M., Wamba, K., Wang, Q., Wang, W., Wang, Y., Watts, M., Wei, W., Wen, L. J., Wichoski, U., Wilde, S., Worcester, M., Wu, W. H., Wu, X., Xie, L., Yan, W., Yang, H., Yang, L., Zeldovich, O., Zhao, J., and Ziegler, T.

Subjects
Physics - Instrumentation and Detectors
Abstract

Liquid xenon time projection chambers are promising detectors to search for neutrinoless double beta decay (0$\nu \beta \beta$), due to their response uniformity, monolithic sensitive volume, scalability to large target masses, and suitability for extremely low background operations. The nEXO collaboration has designed a tonne-scale time projection chamber that aims to search for 0$\nu \beta \beta$ of \ce{^{136}Xe} with projected half-life sensitivity of $1.35\times 10^{28}$~yr. To reach this sensitivity, the design goal for nEXO is $\leq$1\% energy resolution at the decay $Q$-value ($2458.07\pm 0.31$~keV). Reaching this resolution requires the efficient collection of both the ionization and scintillation produced in the detector. The nEXO design employs Silicon Photo-Multipliers (SiPMs) to detect the vacuum ultra-violet, 175 nm scintillation light of liquid xenon. This paper reports on the characterization of the newest vacuum ultra-violet sensitive Fondazione Bruno Kessler VUVHD3 SiPMs specifically designed for nEXO, as well as new measurements on new test samples of previously characterised Hamamatsu VUV4 Multi Pixel Photon Counters (MPPCs). Various SiPM and MPPC parameters, such as dark noise, gain, direct crosstalk, correlated avalanches and photon detection efficiency were measured as a function of the applied over voltage and wavelength at liquid xenon temperature (163~K). The results from this study are used to provide updated estimates of the achievable energy resolution at the decay $Q$-value for the nEXO design.

Published
2022
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106. Multipole expansion for 21cm Intensity Mapping power spectrum: forecasted cosmological parameters estimation for the SKA Observatory

Author

Berti, Maria, Spinelli, Marta, and Viel, Matteo

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The measurement of the large scale distribution of neutral hydrogen in the late Universe, obtained with radio telescopes through the hydrogen 21cm line emission, has the potential to become a key cosmological probe in the upcoming years. We explore the constraining power of 21cm intensity mapping observations on the full set of cosmological parameters that describe the $\Lambda$CDM model. We assume a single-dish survey for the SKA Observatory and simulate the 21cm linear power spectrum monopole and quadrupole within six redshift bins in the range $z=0.25-3$. Forecasted constraints are computed numerically through Markov Chain Monte Carlo techniques. We extend the sampler \texttt{CosmoMC} by implementing the likelihood function for the 21cm power spectrum multipoles. We assess the constraining power of the mock data set alone and combined with Planck 2018 CMB observations. We include a discussion on the impact of extending measurements to non-linear scales in our analysis. We find that 21cm multipoles observations alone are enough to obtain constraints on the cosmological parameters comparable with other probes. Combining the 21cm data set with CMB observations results in significantly reduced errors on all the cosmological parameters. The strongest effect is on $\Omega_ch^2$ and $H_0$, for which the error is reduced by almost a factor four. The percentage errors we estimate are $\sigma_{\Omega_ch^2} = 0.25\%$ and $\sigma_{H_0} = 0.16\%$, to be compared with the Planck only results $\sigma_{\Omega_ch^2} = 0.99\%$ and $\sigma_{H_0} = 0.79\%$. We conclude that 21cm SKAO observations will provide a competitive cosmological probe, complementary to CMB and, thus, pivotal for gaining statistical significance on the cosmological parameters constraints, allowing a stress test for the current cosmological model., Comment: 16 pages, 9 figures

Published
2022
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107. Sensitivity projections for a dual-phase argon TPC optimized for light dark matter searches through the ionization channel

Author

Agnes, P., Ahmad, I., Albergo, S., Albuquerque, I. F. M., Alexander, T., Alton, A. K., Amaudruz, P., Corona, M. Atzori, Auty, D. J., Ave, M., Avetisov, I. Ch., Avetisov, R. I., Azzolini, O., Back, H. O., Balmforth, Z., Barbarian, V., Olmedo, A. Barrado, Barrillon, P., Basco, A., Batignani, G., Berzin, E., Bondar, A., Bonivento, W. M., Borisova, E., Bottino, B., Boulay, M. G., Buccino, G., Bussino, S., Busto, J., Buzulutskov, A., Cadeddu, M., Cadoni, M., Caminata, A., Canci, N., Capra, A., Caprioli, S., Caravati, M., Cárdenas-Montes, M., Cargioli, N., Carlini, M., Castello, P., Cataudella, V., Cavalcante, P., Cavuoti, S., Cebrian, S., Ruiz, J. M. Cela, Chashin, S., Chepurnov, A., Chyhyrynets, E, Cicalò, C., Cifarelli, L., Cintas, D., Cocco, V., Vilda, E. Conde, Consiglio, L., Copello, S., Covone, G., Cross, S., Czudak, P., D'Aniello, M., D'Auria, S., Rolo, M. D. Da Rocha, Dadoun, O., Daniel, M., Davini, S., De Candia, A., De Cecco, S., De Falco, A., De Filippis, G., De Gruttola, D., De Pasquale, S., De Rosa, G., Dellacasa, G., Derbin, A. V., Devoto, A., Di Capua, F., Di Noto, L., Di Stefano, P., Dionisi, C., Dolganov, G., Dordei, F., Doria, L., Erjavec, T., Diaz, M. Fernandez, Fiorillo, G., Franceschi, A., Franchini, P., Franco, D., Frolov, E., Funicello, N., Gabriele, F., Gahan, D., Galbiati, C., Gallina, G., Gallus, G., Garbini, M., Abia, P. Garcia, Gendotti, A., Ghiano, C., Giampaolo, R. A., Giganti, C., Giorgi, M. A., Giovanetti, G. K., Casanueva, V. Goicoechea, Gola, A., Gorman, D., Diaz, R. Graciani, Grauso, G., di Cortona, G. Grilli, Grobov, A., Gromov, M., Guan, M., Guerzoni, M., Gulino, M., Guo, C., Hackett, B. R., Hall, J. B., Hallin, A. L., Hamer, A., Helton, H., Haranczyk, M., Hessel, T., Hill, S., Horikawa, S., Hubaut, F., Hugues, T., Hungerford, E. V., Ianni, An., Ippolito, V., Jillings, C., Kachru, P., Kemp, A. A., Kendziora, C. L., Keppel, G., Khomyakov, A. V., Kimura, M., Kochanek, I., Kondo, K., Korga, G., Koulosousas, S., Kubankin, A., Kuss, M., Kuźniak, M., La Commara, M., Lai, M., Guirriec, E. Le, Leason, E., Li, X., Lidey, L., Lipp, J., Lissia, M., Longo, G., Luzzi, L., Macfadyen, O., Machulin, I. N., Manthos, I., Mapelli, L., Margotti, A., Mari, S. M., Mariani, C., Maricic, J., Marini, A., Martínez, M., Martoff, C. J., Masoni, A., Mavrokoridis, K., Mazzi, A., McDonald, A. B., Messina, A., Milincic, R., Moggi, A., Moharana, A., Monroe, J., Morrocchi, M., Mozhevitina, E. N., Mróz, T., Muratova, V. N., Muscas, C., Musico, P., Nania, R., Napolitano, T., Nessi, M., Nieradka, G., Nikolopoulos, K., Nikulin, I., Nowak, J., Olchansky, K., Oleinik, A., Oleynikov, V., Organtini, P., de Solórzano, A. Ortiz, Pagani, L., Pallavicini, M., Pandola, L., Pantic, E., Paoloni, E., Paternoster, G., Pegoraro, P. A., Pelczar, K., Pellegrino, C., Perotti, F., Pesudo, V., Piacentini, S., Pietropaolo, F., Pino, N., Pira, C., Pocar, A., Poehlmann, D. M., Pordes, S., Pralavorio, P., Price, D., Raffaelli, F., Ragusa, F., Ramachers, Y., Ramirez, A., Razeti, M., Razeto, A., Renshaw, A. L., Rescigno, M., Resnati, F., Retiere, F., Rignanese, L. P., Ripoli, C., Rivetti, A., Roberts, A., Roberts, C., Rode, J., Rogers, G., Romero, L., Rossi, M., Rubbia, A., Sadashivajois, S., Saffold, T. R., Samoylov, O., Sandford, E., Sanfilippo, S., Santone, D., Santorelli, R., Savarese, C., Scapparone, E., Scioli, G., Semenov, D. A., Shchagin, A., Sheshukov, A., Simeone, M., Skensved, P., Skorokhvatov, M. D., Smirnov, O., Smirnova, T., Smith, B., Sokolov, A., Spangenberg, M., Stefanizzi, R., Steri, A., Stracka, S., Strickland, V., Stringer, M., Sulis, S., Sung, A., Suvorov, Y., Szelc, A. M., Türkoğ, C., Tartaglia, R., Taylor, A., Taylor, J., Tedesco, S., Testera, G., Thieme, K., Thorpe, T. N., Tonazzo, A., Torres-Lara, S., Tricomi, A., Unzhakov, E. V., John, T. Vallivilayil, Van Uffelen, M., Viant, T., Viel, S., Vishneva, A., Vogelaar, R. B., Vossebeld, J., Wada, M., Walczak, M. B., Wang, Y., Westerdale, S., Wheadon, R. J., Williams, L., Wingerter-Seez, I., Wojaczyński, R., Wojcik, Ma. M., Wojcik, Ma., Wright, T., Xie, Y., Yang, C., Zabihi, A., Zakhary, P., Zani, A., Zichichi, A., Zuzel, G., and Zykova, M. P.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract

Dark matter lighter than 10 GeV/c$^2$ encompasses a promising range of candidates. A conceptual design for a new detector, DarkSide-LowMass, is presented, based on the DarkSide-50 detector and progress toward DarkSide-20k, optimized for a low-threshold electron-counting measurement. Sensitivity to light dark matter is explored for various potential energy thresholds and background rates. These studies show that DarkSide-LowMass can achieve sensitivity to light dark matter down to the solar neutrino floor for GeV-scale masses and significant sensitivity down to 10 MeV/c$^2$ considering the Migdal effect or interactions with electrons. Requirements for optimizing the detector's sensitivity are explored, as are potential sensitivity gains from modeling and mitigating spurious electron backgrounds that may dominate the signal at the lowest energies.

Published
2022
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108. Studying the Warm Hot Intergalactic Medium in emission: a reprise

Author

Parimbelli, G., Branchini, E., Viel, M., Villaescusa-Navarro, F., and ZuHone, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Warm-Hot Intergalactic Medium (WHIM) is believed to host a significant fraction of the ``missing baryons'' in the nearby Universe. Its signature has been detected in the X-ray absorption spectra of distant quasars. However, its detection in emission, that would allow us to study the WHIM in a systematic way, is still lacking. Motivated by the possibility to perform these studies with next generation integral field spectrometers, and thanks to the availability of a large suite of state-of-the-art hydrodynamic simulations -- the CAMELS suite -- we study here in detail the emission properties of the WHIM and the possibility to infer its physical properties with upcoming X-ray missions like Athena. We focused on the two most prominent WHIM emission lines, the OVII triplet and the OVIII singlet, and build line surface brightness maps in a lightcone, mimicking a data cube generated through integral field spectroscopy. We confirm that detectable WHIM emission, even with next generation instruments, is largely associated to galaxy-size dark matter halos and that the WHIM properties evolve little from $z\simeq0.5$ to now. Some characteristics of the WHIM, like the line number counts as a function of their brightness, depend on the specific hydrodynamic simulation used, while others, like the WHIM clustering properties, are robust to this aspect. The large number of simulations available in the CAMELS datasets allows us to assess the sensitivity of the WHIM properties to the background cosmology and to the energy feedback mechanisms regulated by AGN and stellar activity. [ABRIDGED], Comment: 23 pages, 17 figures, 3 tables

Published
2022
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109. Euclid preparation. XXIV. Calibration of the halo mass function in $\Lambda(\nu)$CDM cosmologies

Author

Euclid Collaboration, Castro, T., Fumagalli, A., Angulo, R. E., Bocquet, S., Borgani, S., Carbone, C., Dakin, J., Dolag, K., Giocoli, C., Monaco, P., Ragagnin, A., Saro, A., Sefusatti, E., Costanzi, M., Brun, A. M. C. Le, Corasaniti, P. -S., Amara, A., Amendola, L., Baldi, M., Bender, R., Bodendorf, C., Branchini, E., Brescia, M., Camera, S., Capobianco, V., Carretero, J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Galeotta, S., Garilli, B., Gillis, B., Grazian, A., Grupp, F., Haugan, S. V. H., Hormuth, F., Hornstrup, A., Hudelot, P., Jahnke, K., Kermiche, S., Kitching, T., Kunz, M., Kurki-Suonio, H., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Marulli, F., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Saglia, R., Sapone, D., Sartoris, B., Schneider, P., Seidel, G., Sirri, G., Stanco, L., Crespí, P. Tallada, Taylor, A. N., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Vassallo, T., Wang, Y., Weller, J., Zacchei, A., Zamorani, G., Andreon, S., Bardelli, S., Bozzo, E., Colodro-Conde, C., Di Ferdinando, D., Farina, M., Graciá-Carpio, J., Lindholm, V., Neissner, C., Scottez, V., Tenti, M., Zucca, E., Baccigalupi, C., Balaguera-Antolínez, A., Ballardini, M., Bernardeau, F., Biviano, A., Blanchard, A., Borlaff, A. S., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Cooray, A., Coupon, J., Courtois, H. M., Davini, S., De Lucia, G., Desprez, G., Dole, H., Escartin, J. A., Escoffier, S., Finelli, F., Ganga, K., Garcia-Bellido, J., George, K., Gozaliasl, G., Hildebrandt, H., Hook, I., Ilić, S., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Loureiro, A., Macias-Perez, J., Magliocchetti, M., Maoli, R., Marcin, S., Martinelli, M., Martinet, N., Matthew, S., Maturi, M., Metcalf, R. B., Morgante, G., Nadathur, S., Nucita, A. A., Patrizii, L., Peel, A., Popa, V., Porciani, C., Potter, D., Pourtsidou, A., Pöntinen, M., Sánchez, A. G., Sakr, Z., Schirmer, M., Sereno, M., Mancini, A. Spurio, Teyssier, R., Valiviita, J., Veropalumbo, A., and Viel, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Euclid's photometric galaxy cluster survey has the potential to be a very competitive cosmological probe. The main cosmological probe with observations of clusters is their number count, within which the halo mass function (HMF) is a key theoretical quantity. We present a new calibration of the analytic HMF, at the level of accuracy and precision required for the uncertainty in this quantity to be subdominant with respect to other sources of uncertainty in recovering cosmological parameters from Euclid cluster counts. Our model is calibrated against a suite of N-body simulations using a Bayesian approach taking into account systematic errors arising from numerical effects in the simulation. First, we test the convergence of HMF predictions from different N-body codes, by using initial conditions generated with different orders of Lagrangian Perturbation theory, and adopting different simulation box sizes and mass resolution. Then, we quantify the effect of using different halo-finder algorithms, and how the resulting differences propagate to the cosmological constraints. In order to trace the violation of universality in the HMF, we also analyse simulations based on initial conditions characterised by scale-free power spectra with different spectral indexes, assuming both Einstein--de Sitter and standard $\Lambda$CDM expansion histories. Based on these results, we construct a fitting function for the HMF that we demonstrate to be sub-percent accurate in reproducing results from 9 different variants of the $\Lambda$CDM model including massive neutrinos cosmologies. The calibration systematic uncertainty is largely sub-dominant with respect to the expected precision of future mass-observation relations; with the only notable exception of the effect due to the halo finder, that could lead to biased cosmological inference., Comment: 25 pages, 21 figures, 5 tables, 3 appendixes; v2 matches published version

Published
2022
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110. The Sherwood-Relics simulations: overview and impact of patchy reionization and pressure smoothing on the intergalactic medium

Author

Puchwein, Ewald, Bolton, James S., Keating, Laura C., Molaro, Margherita, Gaikwad, Prakash, Kulkarni, Girish, Haehnelt, Martin G., Iršič, Vid, Šoltinský, Tomáš, Viel, Matteo, Aubert, Dominique, Becker, George D., and Meiksin, Avery

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the Sherwood-Relics simulations, a new suite of large cosmological hydrodynamical simulations aimed at modelling the intergalactic medium (IGM) during and after the cosmic reionization of hydrogen. The suite consists of over 200 simulations that cover a wide range of astrophysical and cosmological parameters. It also includes simulations that use a new lightweight hybrid scheme for treating radiative transfer effects. This scheme follows the spatial variations in the ionizing radiation field, as well as the associated fluctuations in IGM temperature and pressure smoothing. It is computationally much cheaper than full radiation hydrodynamics simulations and circumvents the difficult task of calibrating a galaxy formation model to observational constraints on cosmic reionization. Using this hybrid technique, we study the spatial fluctuations in IGM properties that are seeded by patchy cosmic reionization. We investigate the relevant physical processes and assess their impact on the z > 4 Lyman-alpha forest. Our main findings are: (i) Consistent with previous studies patchy reionization causes large scale temperature fluctuations that persist well after the end of reionization, (ii) these increase the Lyman-alpha forest flux power spectrum on large scales, and (iii) result in a spatially varying pressure smoothing that correlates well with the local reionization redshift. (iv) Structures evaporated or puffed up by photoheating cause notable features in the Lyman-alpha forest, such as flat-bottom or double-dip absorption profiles., Comment: Version accepted for publication in MNRAS, some discussions added, data added to Fig. 8. 24 pages, 15 figures. Images and movies may be viewed at https://www.nottingham.ac.uk/astronomy/sherwood-relics/

Published
2022
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112. Euclid preparation: XXIII. Derivation of galaxy physical properties with deep machine learning using mock fluxes and H-band images

Author

Euclid Collaboration, Bisigello, L., Conselice, C. J., Baes, M., Bolzonella, M., Brescia, M., Cavuoti, S., Cucciati, O., Humphrey, A., Hunt, L. K., Maraston, C., Pozzetti, L., Tortora, C., van Mierlo, S. E., Aghanim, N., Auricchio, N., Baldi, M., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brinchmann, J., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Castellano, M., Cimatti, A., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Guzzo, L., Haugan, S. V. H., Holmes, W., Hormuth, F., Hornstrup, A., Jahnke, K., Kümmel, M., Kermiche, S., Kiessling, A., Kilbinger, M., Kohley, R., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Medinaceli, E., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Polenta, G., Poncet, M., Popa, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Rix, H. -W., Romelli, E., Roncarelli, M., Rosset, C., Rossetti, E., Saglia, R., Sapone, D., Sartoris, B., Schneider, P., Scodeggio, M., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespí, P., Tavagnacco, D., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Vassallo, T., Wang, Y., Zacchei, A., Zamorani, G., Zoubian, J., Andreon, S., Boucaud, S. Bardelli A., Colodro-Conde, C., Di Ferdinando, D., Graciá-Carpio, J., Lindholm, V., Maino, D., Mei, S., Scottez, V., Sureau, F., Tenti, M., Zucca, E., Borlaff, A. S., Ballardini, M., Biviano, A., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Cooray, A., Coupon, J., Courtois, H. M., Cuby, J., Davini, S., De Lucia, G., Desprez, G., Dole, H., Escartin, J. A., Escoffier, S., Farina, M., Fotopoulou, S., Ganga, K., Garcia-Bellido, J., George, K., Giacomini, F., Gozaliasl, G., Hildebrandt, H., Hook, I., Huertas-Company, M., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Loureiro, A., Macías-Pérez, J. F., Magliocchetti, M., Mainetti, G., Marcin, S., Martinelli, M., Martinet, N., Metcalf, R. B., Monaco, P., Morgante, G., Nadathur, S., Nucita, A. A., Patrizii, L., Peel, A., Potter, D., Pourtsidou, A., Pöntinen, M., Reimberg, P., Sánchez, A. G., Sakr, Z., Schirmer, M., Sefusatti, E., Sereno, M., Stadel, J., Teyssier, R., Valieri, C., Valiviita, J., and Viel, M.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Next generation telescopes, like Euclid, Rubin/LSST, and Roman, will open new windows on the Universe, allowing us to infer physical properties for tens of millions of galaxies. Machine learning methods are increasingly becoming the most efficient tools to handle this enormous amount of data, because they are often faster and more accurate than traditional methods. We investigate how well redshifts, stellar masses, and star-formation rates (SFR) can be measured with deep learning algorithms for observed galaxies within data mimicking the Euclid and Rubin/LSST surveys. We find that Deep Learning Neural Networks and Convolutional Neutral Networks (CNN), which are dependent on the parameter space of the training sample, perform well in measuring the properties of these galaxies and have a better accuracy than methods based on spectral energy distribution fitting. CNNs allow the processing of multi-band magnitudes together with $H_{\scriptscriptstyle\rm E}$-band images. We find that the estimates of stellar masses improve with the use of an image, but those of redshift and SFR do not. Our best results are deriving i) the redshift within a normalised error of less than 0.15 for 99.9$\%$ of the galaxies with S/N>3 in the $H_{\scriptscriptstyle\rm E}$-band; ii) the stellar mass within a factor of two ($\sim0.3 \rm dex$) for 99.5$\%$ of the considered galaxies; iii) the SFR within a factor of two ($\sim0.3 \rm dex$) for $\sim$70$\%$ of the sample. We discuss the implications of our work for application to surveys as well as how measurements of these galaxy parameters can be improved with deep learning., Comment: accepted for publication in MNRAS, 21 pages, 22 figures, 6 tables

Published
2022

113. Hints of dark photon dark matter from observations and hydrodynamical simulations of the low-redshift Lyman-$\alpha$ forest

Author

Bolton, James S., Caputo, Andrea, Liu, Hongwan, and Viel, Matteo

Subjects
High Energy Physics - Phenomenology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Recent work has suggested that an additional $\lesssim 6.9 \rm{\, eV}$ per baryon of heating in the intergalactic medium is needed to reconcile hydrodynamical simulations with Lyman-$\alpha$ forest absorption line widths at redshift $z\simeq 0.1$. Resonant conversion of dark photon dark matter into low frequency photons is a viable source of such heating. We perform the first hydrodynamical simulations including dark photon heating and show that dark photons with mass $m_{A'}\sim 8\times 10^{-14}\rm\,eV\,c^{-2}$ and kinetic mixing $\epsilon \sim 5\times 10^{-15}$ can alleviate the heating excess. A prediction of this model is a non-standard thermal history for underdense gas at $z \gtrsim 3$., Comment: 5+1 pages, 2+1 figures

Published
2022
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114. One likelihood to bind them all: Lyman-$\alpha$ constraints on non-standard dark matter

Author

Hooper, Deanna C., Schöneberg, Nils, Murgia, Riccardo, Archidiacono, Maria, Lesgourgues, Julien, and Viel, Matteo

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology
Abstract

Recent cosmological tensions have rekindled the search for models beyond $\Lambda$CDM that cause a suppression of the matter power spectrum. Due to the small scales accessible to Lyman-$\alpha$ data they are an excellent additional tool to probe such models. In this work we extend a recently-developed approach for using Lyman-$\alpha$ data to constrain the power spectrum suppression caused by almost any mixture of cold and non-standard dark matter. We highlight the steps involved in the development of a corresponding likelihood that will be publicly released upon publication of this work. We study three examples of models suppressing the power spectrum, namely feebly interacting dark matter, dark matter interacting with baryons, and mixed cold+warm dark matter. The latter two can be well constrained from Lyman-$\alpha$ data, and we derive novel conclusions on the cosmologically allowed parameter spaces, including finding a mild preference for non-zero interactions between dark matter and baryons. The consistency of the constraints obtained on these models highlight the robustness and flexibility of the likelihood developed here., Comment: 34 pages, 10 figures, and one table. Comments are welcome!

Published
2022
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115. Euclid preparation: XX. The Complete Calibration of the Color-Redshift Relation survey: LBT observations and data release

Author

Euclid Collaboration, Saglia, R., De Nicola, S., Fabricius, M., Guglielmo, V., Snigula, J., Zöller, R., Bender, R., Heidt, J., Masters, D., Stern, D., Paltani, S., Amara, A., Auricchio, N., Baldi, M., Bodendorf, C., Bonino, D., Branchini, E., Brescia, M., Brinchmann, J., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Castellano, M., Cavuoti, S., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Frailis, M., Franceschi, E., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hornstrup, A., Jahnke, K., Kümmel, M., Kermiche, S., Kiessling, A., Kunz, M., Kurki-Suonio, H., Laureijs, R., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Marggraf, O., Markovic, K., Marulli, F., Massey, R., McCracken, H. J., Melchior, M., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Pasian, F., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Rossetti, E., Sapone, D., Sartoris, B., Schneider, P., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespí, P., Tavagnacco, D., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Vassallo, T., Wang, Y., Zacchei, A., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Graciá-Carpio, J., Maino, D., Mauri, N., Tramacere, A., Zucca, E., Ayllon, A. Alvarez, Aussel, H., Baccigalupi, C., Balaguera-Antolínez, A., Ballardini, M., Biviano, A., Bolzonella, M., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Cooray, A., Coupon, J., Courtois, H. M., Davini, S., Desprez, G., Dole, H., Escartin, J. A., Escoffier, S., Farina, M., Fotopoulou, S., Ganga, K., Garcia-Bellido, J., George, K., Giacomini, F., Gozaliasl, G., Hildebrandt, H., Hook, I., Ilbert, O., Kansal, V., Kashlinsky, A., Keihanen, E., Kirkpatrick, C. C., Loureiro, A., Macías-Pérez, J., Magliocchetti, M., Mainetti, G., Maoli, R., Martinelli, M., Martinet, N., Metcalf, R. B., Morgante, G., Nadathur, S., Nucita, A. A., Patrizii, L., Popa, V., Porciani, C., Potter, D., Pourtsidou, A., Reimberg, P., Sánchez, A. G., Sakr, Z., Schirmer, M., Sefusatti, E., Sereno, M., Stadel, J., Teyssier, R., Valieri, C., Valiviita, J., Veropalumbo, A., and Viel, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Complete Calibration of the Color-Redshift Relation survey (C3R2) is a spectroscopic programme designed to empirically calibrate the galaxy color-redshift relation to the Euclid depth (I_E=24.5), a key ingredient for the success of Stage IV dark energy projects based on weak lensing cosmology. A spectroscopic calibration sample as representative as possible of the galaxies in the Euclid weak lensing sample is being collected, selecting galaxies from a self-organizing map (SOM) representation of the galaxy color space. Here, we present the results of a near-infrared H- and K-bands spectroscopic campaign carried out using the LUCI instruments at the LBT. For a total of 251 galaxies, we present new highly-reliable redshifts in the 1.3<= z <=1.7 and 2<= z<=2.7 ranges. The newly-determined redshifts populate 49 SOM cells which previously contained no spectroscopic measurements and almost double the occupation numbers of an additional 153 SOM cells. A final optical ground-based observational effort is needed to calibrate the missing cells in particular in the redshift range 1.7<= z<=2.7 that lack spectroscopic calibration. In the end, Euclid itself will deliver telluric-free NIR spectra that can complete the calibration., Comment: A&A language edited version

Published
2022
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116. A validation of the short-form classroom community scale for undergraduate mathematics and statistics students

Author

Tackett, Maria, Viel, Shira, and Manturuk, Kim

Subjects
Statistics - Other Statistics
Abstract

This study examines Cho and Demmans Epp's short-form adaptation of Rovai's well-known Classroom Community Scale (CCS-SF) as a measure of classroom community among introductory undergraduate math and statistics students. A series of statistical analyses were conducted to investigate the validity of the CCS-SF for this new population. Data were collected from 351 students enrolled in 21 online classes, offered for credit in Fall 2020 and Spring 2021 at a private university in the United States. Further confirmatory analysis was conducted with data from 128 undergraduates enrolled in 13 in-person and hybrid classes, offered for credit in Fall 2021 at the same institution. Following Rovai's original 20-item CCS, the 8-item CCS-SF yields two interpretable factors, connectedness and learning. This study confirms the two-factor structure of the CCS-SF, and concludes that it is a valid measure of classroom community among undergraduate students enrolled in remote, hybrid, and in-person introductory mathematics and statistics courses.

Published
2022
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117. Euclid preparation. XXI. Intermediate-redshift contaminants in the search for $z>6$ galaxies within the Euclid Deep Survey

Author

Euclid Collaboration, van Mierlo, S. E., Caputi, K. I., Ashby, M., Atek, H., Bolzonella, M., Bowler, R. A. A., Brammer, G., Conselice, C. J., Cuby, J., Dayal, P., Díaz-Sánchez, A., Finkelstein, S. L., Hoekstra, H., Humphrey, A., Ilbert, O., McCracken, H. J., Milvang-Jensen, B., Oesch, P. A., Pello, R., Rodighiero, G., Schirmer, M., Toft, S., Weaver, J. R., Wilkins, S. M., Willott, C. J., Zamorani, G., Amara, A., Auricchio, N., Baldi, M., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brescia, M., Brinchmann, J., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Hornstrup, A., Jahnke, K., Kümmel, M., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kunz, M., Kurki-Suonio, H., Laureijs, R., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Medinaceli, E., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Rossetti, E., Saglia, R., Sapone, D., Sartoris, B., Schneider, P., Secroun, A., Sirignano, C., Sirri, G., Stanco, L., Starck, J. -L., Surace, C., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Vassallo, T., Wang, Y., Zacchei, A., Zoubian, J., Andreon, S., Bardelli, S., Boucaud, A., Graciá-Carpio, J., Maino, D., Mauri, N., Mei, S., Sureau, F., Zucca, E., Aussel, H., Baccigalupi, C., Balaguera-Antolínez, A., Biviano, A., Blanchard, A., Borgani, S., Bozzo, E., Burigana, C., Cabanac, R., Calura, F., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Cooray, A. R., Coupon, J., Courtois, H. M., Crocce, M., Cucciati, O., Davini, S., Dole, H., Escartin, J. A., Escoffier, S., Fabricius, M., Farina, M., Ganga, K., García-Bellido, J., George, K., Giacomini, F., Gozaliasl, G., Gwyn, S., Hook, I., Huertas-Company, M., Kansal, V., Kashlinsky, A., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., Monaco, P., Morgante, G., Nucita, A. A., Patrizii, L., Peel, A., Pollack, J., Popa, V., Porciani, C., Potter, D., Reimberg, P., Sánchez, A. G., Scottez, V., Sefusatti, E., Stadel, J., Teyssier, R., Valiviita, J., and Viel, M.

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

(Abridged) The Euclid mission is expected to discover thousands of z>6 galaxies in three Deep Fields, which together will cover a ~40 deg2 area. However, the limited number of Euclid bands and availability of ancillary data could make the identification of z>6 galaxies challenging. In this work, we assess the degree of contamination by intermediate-redshift galaxies (z=1-5.8) expected for z>6 galaxies within the Euclid Deep Survey. This study is based on ~176,000 real galaxies at z=1-8 in a ~0.7 deg2 area selected from the UltraVISTA ultra-deep survey, and ~96,000 mock galaxies with 25.3$\leq$H<27.0, which altogether cover the range of magnitudes to be probed in the Euclid Deep Survey. We simulate Euclid and ancillary photometry from the fiducial, 28-band photometry, and fit spectral energy distributions (SEDs) to various combinations of these simulated data. Our study demonstrates that identifying z>6 with Euclid data alone will be very effective, with a z>6 recovery of 91(88)% for bright (faint) galaxies. For the UltraVISTA-like bright sample, the percentage of z=1-5.8 contaminants amongst apparent z>6 galaxies as observed with Euclid alone is 18%, which is reduced to 4(13)% by including ultra-deep Rubin (Spitzer) photometry. Conversely, for the faint mock sample, the contamination fraction with Euclid alone is considerably higher at 39%, and minimized to 7% when including ultra-deep Rubin data. For UltraVISTA-like bright galaxies, we find that Euclid (I-Y)>2.8 and (Y-J)<1.4 colour criteria can separate contaminants from true z>6 galaxies, although these are applicable to only 54% of the contaminants, as many have unconstrained (I-Y) colours. In the most optimistic scenario, these cuts reduce the contamination fraction to 1% whilst preserving 81% of the fiducial z>6 sample. For the faint mock sample, colour cuts are infeasible., Comment: 27 pages, 14 figures, 9 tables; version accepted for publication by A&A

Published
2022
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123. Euclid preparation. XVIII. The NISP photometric system

Author

Euclid Collaboration, Schirmer, M., Jahnke, K., Seidel, G., Aussel, H., Bodendorf, C., Grupp, F., Hormuth, F., Wachter, S., Appleton, P. N., Barbier, R., Brinchmann, J., Carrasco, J. M., Castander, F. J., Coupon, J., De Paolis, F., Franco, A., Ganga, K., Hudelot, P., Jullo, E., Lancon, A., Nucita, A. A., Paltani, S., Smadja, G., Venancio, L. M. G., Strafella, F., Weiler, M., Amara, A., Auphan, T., Auricchio, N., Balestra, A., Bender, R., Bonino, D., Branchini, E., Brescia, M., Capobianco, V., Carbone, C., Carretero, J., Casas, R., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Courbin, F., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Dupac, X., Dusini, S., Ealet, A., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Guzzo, L., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hornstrup, A., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kümmel, M., Kunz, M., Kurki-Suonio, H., Laureijs, R., Ligori, S., Lilje, P. B., Lloro, I., Maciaszek, T., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Mellier, Y., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Nakajima, R., Nichol, R. C., Niemi, S. M., Padilla, C., Pasian, F., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Prieto, E., Raison, F., Rhodes, J., Rix, H. -W., Roncarelli, M., Rossetti, E., Saglia, R., Sartoris, B., Scaramella, R., Schneider, P., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespí, P., Taylor, A. N., Teplitz, H. I., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Trifoglio, M., Valentijn, E. A., Valenziano, L., Wang, Y., Weller, J., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Boucaud, A., Camera, S., Farinelli, R., Graciá-Carpio, J., Maino, D., Medinaceli, E., Mei, S., Morisset, N., Polenta, G., Renzi, A., Romelli, E., Tenti, M., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antolínez, A., Biviano, A., Blanchard, A., Borgani, S., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Cooray, A. R., Courtois, H. M., Crocce, M., Cuby, J. -G., Davini, S., de la Torre, S., Di Ferdinando, D., Escartin, J. A., Farina, M., Ferreira, P. G., Finelli, F., Fotopoulou, S., Galeotta, S., Garcia-Bellido, J., Gaztanaga, E., George, K., Gozaliasl, G., Hook, I. M., Ilić, S., Kansal, V., Kashlinsky, A., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Mauri, N., McCracken, H. J., Metcalf, R. B., Monaco, P., Morgante, G., Nightingale, J., Patrizii, L., Peel, A., Popa, V., Porciani, C., Potter, D., Reimberg, P., Riccio, G., Sánchez, A. G., Sapone, D., Scottez, V., Sefusatti, E., Teyssier, R., Tutusaus, I., Valieri, C., Valiviita, J., Viel, M., and Hildebrandt, H.

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

Euclid will be the first space mission to survey most of the extragalactic sky in the 0.95-2.02 $\mu$m range, to a 5$\sigma$ point-source median depth of 24.4 AB mag. This unique photometric data set will find wide use beyond Euclid's core science. In this paper, we present accurate computations of the Euclid Y_E, J_E and H_E passbands used by the Near-Infrared Spectrometer and Photometer (NISP), and the associated photometric system. We pay particular attention to passband variations in the field of view, accounting among others for spatially variable filter transmission, and variations of the angle of incidence on the filter substrate using optical ray tracing. The response curves' cut-on and cut-off wavelengths - and their variation in the field of view - are determined with 0.8 nm accuracy, essential for the photometric redshift accuracy required by Euclid. After computing the photometric zeropoints in the AB mag system, we present linear transformations from and to common ground-based near-infrared photometric systems, for normal stars, red and brown dwarfs, and galaxies separately. A Python tool to compute accurate magnitudes for arbitrary passbands and spectral energy distributions is provided. We discuss various factors from space weathering to material outgassing that may slowly alter Euclid's spectral response. At the absolute flux scale, the Euclid in-flight calibration program connects the NISP photometric system to Hubble Space Telescope spectrophotometric white dwarf standards; at the relative flux scale, the chromatic evolution of the response is tracked at the milli-mag level. In this way, we establish an accurate photometric system that is fully controlled throughout Euclid's lifetime., Comment: 33 pages, 25 figures, accepted for publication in A&A

Published
2022
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124. Weighing Cosmic Structures with Clusters of Galaxies and the Intergalactic Medium

Author

Esposito, Matteo, Iršič, Vid, Costanzi, Matteo, Borgani, Stefano, Saro, Alexandro, and Viel, Matteo

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Theory
Abstract

We present an analysis aimed at combining cosmological constraints from number counts of galaxy clusters identified through the Sunyaev-Zeldovich effect, obtained with the South Pole Telescope (SPT), and from Lyman-$\alpha$ spectra obtained with the MIKE/HIRES and X-shooter spectrographs. The SPT cluster analysis relies on mass calibration based on weak lensing measurements, while the Lyman-$\alpha$ analysis is built over a suite of hydrodynamical simulations for the extraction of mock spectra. The resulting constraints exhibit a tension ($\sim 3.3\sigma$) between the low $\sigma_8$ values preferred by the low-redshift cluster data, $\sigma_8=0.74 ^{+0.03}_{-0.04}$, and the higher one preferred by the high-redshift Lyman-$\alpha$ data, $\sigma_8=0.91 ^{+0.03}_{-0.03}$. We present a detailed analysis in order to understand the origin of this tension and, in particular, to establish whether it arises from systematic uncertainties related to the assumptions underlying the analyses of cluster counts and/or Lyman-$\alpha$ forest. We found this tension to be robust with respect to the choice of modeling of the IGM, even when including possible systematics from unaccounted sub-Damped Lyman-$\alpha$ (DLA) and Lyman-limit systems (LLS) in the Lyman-$\alpha$ data. We conclude that to solve this tension from the SPT side would require a large bias on the cluster mass estimate, or from the Lyman-$\alpha$ side large unaccounted errors on the Lyman-$\alpha$ mean fluxes, respectively. Our results have important implications for future analyses based on cluster number counts from future large photometric surveys (e.g. Euclid and LSST) and on larger samples of high-redshift quasar spectra (e.g. DESI and WEAVE surveys). If confirmed at the much higher statistical significance reachable by such surveys, this tension could represent a significant challenge for the standard $\Lambda$CDM paradigm., Comment: 14 pages, 8 figures

Published
2022
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125. Development of a $^{127}$Xe calibration source for nEXO

Author

Lenardo, B. G., Hardy, C. A., Tsang, R. H. M., Ondze, J. C. Nzobadila, Piepke, A., Triambak, S., Jamil, A., Adhikari, G., Kharusi, S. Al, Angelico, E., Arnquist, I. J., Belov, V., Bernard, E. P., Bhat, A., Bhatta, T., Bolotnikov, A., Breur, P. A., Brodsky, J. P., Brown, E., Brunner, T., Caden, E., Cao, G. F., Cao, L., Chana, B., Charlebois, S. A., Chernyak, D., Chiu, M., Cohen, J. R., Collister, R., Dalmasson, J., Daniels, T., Darroch, L., DeVoe, R., di Vacri, M. L., Ding, Y. Y., Dolinski, M. J., Echevers, J., Eckert, B., Elbeltagi, M., Fabris, L., Fairbank, D., Fairbank, W., Farine, J., Fu, Y. S., Gallina, G., Gautam, P., Giacomini, G., Gillis, W., Gingras, C., Gornea, R., Gratta, G., Harouaka, K., Heffner, M., Hein, E., Hößl, J., House, A., Iverson, A., Jiang, X. S., Karelin, A., Kaufman, L. J., Krücken, R., Kuchenkov, A., Kumar, K. S., Larson, A., Leach, K. G., Leonard, D. S., Li, G., Li, S., Li, Z., Licciardi, C., Lindsay, R., MacLellan, R., Masbou, J., McMichael, K., Peregrina, M. Medina, Mong, B., Moore, D. C., Murray, K., Nattress, J., Natzke, C. R., Ngwadla, X. E., Ni, K., Ning, Z., Orrell, J. L., Ortega, G. S., Ostrovskiy, I., Overman, C. T., Perna, A., Franco, T. Pinto, Pocar, A., Pratte, J. F., Priel, N., Raguzin, E., Ramonnye, G. J., Rasiwala, H., Raymond, K., Richardson, G., Richman, M., Ringuette, J., Rowson, P. C., Saldanha, R., Sangiorgio, S., Shang, X., Soma, A. K., Spadoni, F., Stekhanov, V., Sun, X. L., Thibado, S., Tidball, A., Todd, J., Totev, T., Tyuka, O. A., Vachon, F., Veeraraghavan, V., Viel, S., Wamba, K., Wang, Y., Wang, Q., Wei, W., Wen, L. J., Wichoski, U., Wilde, S., Wu, W. H., Yan, W., Yang, L., Zeldovich, O., Zhao, J., and Ziegler, T.

Subjects
Physics - Instrumentation and Detectors, Nuclear Experiment
Abstract

We study a possible calibration technique for the nEXO experiment using a $^{127}$Xe electron capture source. nEXO is a next-generation search for neutrinoless double beta decay ($0\nu\beta\beta$) that will use a 5-tonne, monolithic liquid xenon time projection chamber (TPC). The xenon, used both as source and detection medium, will be enriched to 90% in $^{136}$Xe. To optimize the event reconstruction and energy resolution, calibrations are needed to map the position- and time-dependent detector response. The 36.3 day half-life of $^{127}$Xe and its small $Q$-value compared to that of $^{136}$Xe $0\nu\beta\beta$ would allow a small activity to be maintained continuously in the detector during normal operations without introducing additional backgrounds, thereby enabling in-situ calibration and monitoring of the detector response. In this work we describe a process for producing the source and preliminary experimental tests. We then use simulations to project the precision with which such a source could calibrate spatial corrections to the light and charge response of the nEXO TPC., Comment: 24 pages, 16 figures

Published
2022
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126. The CAMELS project: public data release

Author

Villaescusa-Navarro, Francisco, Genel, Shy, Anglés-Alcázar, Daniel, Perez, Lucia A., Villanueva-Domingo, Pablo, Wadekar, Digvijay, Shao, Helen, Mohammad, Faizan G., Hassan, Sultan, Moser, Emily, Lau, Erwin T., Valle, Luis Fernando Machado Poletti, Nicola, Andrina, Thiele, Leander, Jo, Yongseok, Philcox, Oliver H. E., Oppenheimer, Benjamin D., Tillman, Megan, Hahn, ChangHoon, Kaushal, Neerav, Pisani, Alice, Gebhardt, Matthew, Delgado, Ana Maria, Caliendo, Joyce, Kreisch, Christina, Wong, Kaze W. K., Coulton, William R., Eickenberg, Michael, Parimbelli, Gabriele, Ni, Yueying, Steinwandel, Ulrich P., La Torre, Valentina, Dave, Romeel, Battaglia, Nicholas, Nagai, Daisuke, Spergel, David N., Hernquist, Lars, Burkhart, Blakesley, Narayanan, Desika, Wandelt, Benjamin, Somerville, Rachel S., Bryan, Greg L., Viel, Matteo, Li, Yin, Irsic, Vid, Kraljic, Katarina, and Vogelsberger, Mark

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, Computer Science - Artificial Intelligence, Computer Science - Machine Learning
Abstract

The Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS) project was developed to combine cosmology with astrophysics through thousands of cosmological hydrodynamic simulations and machine learning. CAMELS contains 4,233 cosmological simulations, 2,049 N-body and 2,184 state-of-the-art hydrodynamic simulations that sample a vast volume in parameter space. In this paper we present the CAMELS public data release, describing the characteristics of the CAMELS simulations and a variety of data products generated from them, including halo, subhalo, galaxy, and void catalogues, power spectra, bispectra, Lyman-$\alpha$ spectra, probability distribution functions, halo radial profiles, and X-rays photon lists. We also release over one thousand catalogues that contain billions of galaxies from CAMELS-SAM: a large collection of N-body simulations that have been combined with the Santa Cruz Semi-Analytic Model. We release all the data, comprising more than 350 terabytes and containing 143,922 snapshots, millions of halos, galaxies and summary statistics. We provide further technical details on how to access, download, read, and process the data at \url{https://camels.readthedocs.io}., Comment: 18 pages, 3 figures. More than 350 Tb of data from thousands of simulations publicly available at https://www.camel-simulations.org

Published
2022
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128. Paediatric inflammatory multisystem syndrome in Canada: population-based surveillance and role of SARS-CoV-2 linkage

Author

El Tal, Tala, Morin, Marie-Paule, Morris, Shaun K., Farrar, Daniel S., Berard, Roberta A., Kakkar, Fatima, Moore Hepburn, Charlotte, Baerg, Krista, Beaufils, Camille, Bennett, Terri-Lyn, Benseler, Susanne M., Beaudoin-Bussières, Guillaume, Chan, Kevin, Cyr, Claude, Dahdah, Nagib, Donner, Elizabeth J., Drouin, Olivier, Edjoc, Rojiemiahd, Eljaouhari, Maryem, Embree, Joanne E., Farrell, Catherine, Finzi, Andrés, Forgie, Sarah, Giroux, Ryan, Kang, Kristopher T., King, Melanie, Laffin Thibodeau, Melanie, Lang, Bianca, Laxer, Ronald M., Luu, Thuy Mai, McCrindle, Brian W., Orkin, Julia, Papenburg, Jesse, Pound, Catherine M., Price, Victoria E., Proulx-Gauthier, Jean-Philippe, Purewal, Rupeena, Sadarangani, Manish, Salvadori, Marina I., Thibeault, Roseline, Top, Karina A., Viel-Thériault, Isabelle, Haddad, Elie, Scuccimarri, Rosie, and Yeung, Rae S. M.

Published
2023
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129. Hydrogen–iodine scattering. II. Rovibronic analysis and collisional dynamics.

Author

Weike, Nicole, Eisfeld, Wolfgang, Dunseath, Kevin M., and Viel, Alexandra

Subjects
ANGULAR momentum (Mechanics), QUASI bound states, BOUND states, EXCITED states, BRANCHING ratios, IODINE, ELASTIC scattering, INELASTIC scattering
Abstract

Our recently published [Weike et al., J. Chem. Phys. 159, 244119 (2023)] spin–orbit coupled diabatic potential energy model for HI is used in a thorough analysis of bound and quasi-bound states as well as elastic and inelastic processes in H + I collisions. The potential energy model, designed explicitly for studying scattering, accurately describes the various couplings in the system, which lead to complex dynamics. Ro-vibronic bound and quasi-bound states related to the adiabatic electronic ground state and an excited electronic state are analyzed. Calculations using the full 104 × 104 diabatic matrix model or a single adiabatic state are compared in order to investigate approximations in the latter. Elastic and inelastic scattering cross sections as well as thermal rates between the ground and first excited fine structure levels of iodine are computed for collision energies up to 12 500 cm−1. Resonances related to the quasi-bound states are analyzed in terms of their energy, width, lifetime, and decay probabilities. The effect of different resonances on the thermal rates is discussed. Resonances between 30 000 and 40 000 cm−1 are also studied for selected values of the total angular momentum, in particular their decay probabilities into different final states of iodine and hence their potential effect on branching ratios in photodissociation of HI. [ABSTRACT FROM AUTHOR]

Published
2024
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130. Utilizing a Blended + Flipped Learning Approach in a Calculus for Life and Management Sciences Classroom

Author

Spencer, Dan, Willis, Chris, Shen, Yan, Fenn, Molly, and Viel, Shira

Abstract

The current study evaluated the success of implementing a blended + flipped structure in a Calculus for Life and Management Sciences course. By reimagining two of the three weekly instructional hours as online asynchronous lessons, we redesigned a 200-person section into 30-person sections, with minimal additional instructor resources. Findings indicated that students viewed the course positively, with perceptions positively correlating with course outcomes. Further, students reported more positive beliefs relating to their ability to accomplish course learning outcomes, comfort with math, and perceptions of in-class readiness compared to those in the traditional course format. Significant differences in grade distributions were also observed.

Published
2023
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131. Limits on non-canonical heating and turbulence in the intergalactic medium from the low redshift Lyman-alpha forest

Author

Bolton, James S., Gaikwad, Prakash, Haehnelt, Martin G., Kim, Tae-Sun, Nasir, Fahad, Puchwein, Ewald, Viel, Matteo, and Wakker, Bart P.

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

We examine the column density distribution function (CDDF) and Doppler parameter distribution from hydrodynamical simulations and Cosmic Origins Spectrograph (COS) observations of the Lyman-alpha forest at redshift $0\leq z\leq 0.2$. Allowing for a factor of two uncertainty in the metagalactic HI photoionisation rate, our hydrodynamical simulations are in good agreement ($1$-$1.5\sigma$) with the shape and amplitude of the observed CDDF at HI column densities $10^{13.3}\rm\,cm^{-2}\leq N_{\rm HI}\leq 10^{14.5}\rm\,cm^{-2}$. However, the Doppler widths of the simulated lines remain too narrow with respect to the COS data. We argue that invoking AGN feedback does not resolve this discrepancy. We also disfavour enhanced photoheating rates as a potential solution, as this requires an unphysically hard UV background spectrum. If instead appealing to a non-canonical source of heating, an additional specific heat injection of $u \lesssim 6.9\rm\,eV\,m_{\rm p}^{-1}$ is required at $z\lesssim 2.5$ for gas that has $N_{\rm HI}\simeq 10^{13.5}\rm\,cm^{-2}$ by $z=0.1$. Alternatively, there may be an unresolved line of sight turbulent velocity component of $v_{\rm turb}\lesssim 8.5\rm\,km\,s^{-1}(N_{\rm HI}/10^{13.5}\rm\,cm^{-2})^{0.21}$ for the coldest gas in the diffuse IGM., Comment: 21 pages, 13 figures, MNRAS accepted following revision. The accepted version includes an extra panel in figure 2 and some additional clarifications on the line broadening within the models. Conclusions unchanged

Published
2021
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132. Euclid preparation: XVIII. Cosmic Dawn Survey. Spitzer observations of the Euclid deep fields and calibration fields

Author

Moneti, Andrea, McCracken, H. J., Shuntov, M., Kauffmann, O. B., Capak, P., Davidzon, I., Ilbert, O., Scarlata, C., Toft, S., Weaver, J., Chary, R., Cuby, J., Faisst, A. L., Masters, D. C., McPartland, C., Mobasher, B., Sanders, D. B., Scaramella, R., Stern, D., Szapudi, I., Teplitz, H., Zalesky, L., Amara, A., Auricchio, N., Bodendorf, C., Bonino, D., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Gillis, B., Giocoli, C., Granett, B. R., Grazian, A., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kuemmel, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Rix, H., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespi, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Camera, S., Gracia-Carpio, J., Medinaceli, E., Mei, S., Polenta, G., Romelli, E., Sureau, F., Tenti, M., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antolinez, A., Bernardeau, F., Biviano, A., Bolzonella, M., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Di Ferdinando, D., Farina, M., Finelli, F., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I., Joachimi, B., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., Morgante, G., Morisset, N., Nucita, A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., Sanchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Teyssier, R., Tubio, O., Tutusaus, I., Valiviita, J., Viel, M., and Hildebrandt, H.

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

We present a new infrared survey covering the three Euclid deep fields and four other Euclid calibration fields using Spitzer's Infrared Array Camera (IRAC). We have combined these new observations with all relevant IRAC archival data of these fields in order to produce the deepest possible mosaics of these regions. In total, these observations represent nearly 11% of the total Spitzer mission time. The resulting mosaics cover a total of approximately 71.5deg$^2$ in the 3.6 and 4.5um bands, and approximately 21.8deg$^2$ in the 5.8 and 8um bands. They reach at least 24 AB magnitude (measured to sigma, in a 2.5 arcsec aperture) in the 3.6um band and up to ~ 5 mag deeper in the deepest regions. The astrometry is tied to the Gaia astrometric reference system, and the typical astrometric uncertainty for sources with 16<[3.6]<19 is <0.15 arcsec. The photometric calibration is in excellent agreement with previous WISE measurements. We have extracted source number counts from the 3.6um band mosaics and they are in excellent agreement with previous measurements. Given that the Spitzer Space Telescope has now been decommissioned these mosaics are likely to be the definitive reduction of these IRAC data. This survey therefore represents an essential first step in assembling multi-wavelength data on the Euclid deep fields which are set to become some of the premier fields for extragalactic astronomy in the 2020s., Comment: 15 pages with 11 figures, approved by Euclid Consortium Publication Board and submitted to Astronomy and Astrophysics. Data products will become available via the IRSA website once the paper is accepted. This paper is a companion to "COSMOS2020: A panchromatic view of the Universe to z~10 from two complementary catalogs" by John Weaver et al., which is being posted in parallel

Published
2021
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133. Euclid preparation: XIX. Impact of magnification on photometric galaxy clustering

Author

Lepori, F., Tutusaus, I., Viglione, C., Bonvin, C., Camera, S., Castander, F. J., Durrer, R., Fosalba, P., Jelic-Cizmek, G., Kunz, M., Adamek, J., Casas, S., Martinelli, M., Sakr, Z., Sapone, D., Amara, A., Auricchio, N., Bodendorf, C., Bonino, D., Branchini, E., Brescia, M., Brinchmann, J., Capobianco, V., Carbone, C., Carretero, J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Dupac, X., Dusini, S., Ealet, A., Farrens, S., Ferriol, S., Franceschi, E., Fumana, M., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Guzzo, L., Haugan, S. V. H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kümmel, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Melchior, M., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Nakajima, R., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J. -L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., Valenziano, L., Wang, Y., Weller, J., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Fabbian, G., Graciá-Carpio, J., Maino, D., Medinaceli, E., Mei, S., Renzi, A., Romelli, E., Sureau, F., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antolínez, A., Bernardeau, F., Biviano, A., Blanchard, A., Bolzonella, M., Borgani, S., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J. -G., Davini, S., de la Torre, S., Di Ferdinando, D., Farina, M., Ferreira, P. G., Finelli, F., Galeotta, S., Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I. M., Ilić, S., Joachimi, B., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maoli, R., Martinet, N., Maturi, M., Metcalf, R. B., Monaco, P., Morgante, G., Nightingale, J., Nucita, A., Patrizii, L., Popa, V., Potter, D., Riccio, G., Sánchez, A. G, Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Tramacere, A., Valiviita, J., Viel, M., and Hildebrandt, H.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the importance of lensing magnification for estimates of galaxy clustering and its cross-correlation with shear for the photometric sample of Euclid. Using updated specifications, we study the impact of lensing magnification on the constraints and the shift in the estimation of the best fitting cosmological parameters that we expect if this effect is neglected. We follow the prescriptions of the official Euclid Fisher matrix forecast for the photometric galaxy clustering analysis and the combination of photometric clustering and cosmic shear. The slope of the luminosity function (local count slope), which regulates the amplitude of the lensing magnification, and the galaxy bias have been estimated from the Euclid Flagship simulation.We find that magnification significantly affects both the best-fit estimation of cosmological parameters and the constraints in the galaxy clustering analysis of the photometric sample. In particular, including magnification in the analysis reduces the 1$\sigma$ errors on $\Omega_{\text{m},0}, w_{0}, w_a$ at the level of 20-35%, depending on how well we will be able to independently measure the local count slope. In addition, we find that neglecting magnification in the clustering analysis leads to shifts of up to 1.6$\sigma$ in the best-fit parameters. In the joint analysis of galaxy clustering, cosmic shear, and galaxy-galaxy lensing, magnification does not improve precision, but it leads to an up to 6$\sigma$ bias if neglected. Therefore, for all models considered in this work, magnification has to be included in the analysis of galaxy clustering and its cross-correlation with the shear signal ($3\times2$pt analysis) for an accurate parameter estimation., Comment: 26 pages, 11 figures. Version accepted for publication in A&A

Published
2021
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134. Lack of association between classical HLA genes and asymptomatic SARS-CoV-2 infection

Author

Abel, Laurent, Aiuti, Alessandro, Al-Muhsen, Saleh, Al-Mulla, Fahd, Amara, Ali, Anderson, Mark S., Andreakos, Evangelos, Arias, Andrés A., Arkin, Lisa M., Feldman, Hagit Baris, Bastard, Paul, Belot, Alexandre, Biggs, Catherine M., Bogunovic, Dusan, Bolze, Alexandre, Bondarenko, Anastasiia, Borghesi, Alessandro, Bousfiha, Ahmed A., Brodin, Petter, Bryceson, Yenan, Butte, Manish J., Casanova, Jean-Laurent, Casari, Giorgio, Christodoulou, John, Cobat, Aurélie, Colobran, Roger, Condino-Neto, Antonio, Constantinescu, Stefan N., Cooper, Megan A., Dalgard, Clifton L., Desai, Murkesh, Drolet, Beth A., Duval, Xavier, El Baghdadi, Jamila, Eloy, Philippine, Espinosa-Padilla, Sara, Fellay, Jacques, Flores, Carlos, Franco, José Luis, Froidure, Antoine, Gorochov, Guy, Gregersen, Peter K., Grimbacher, Bodo, Haerynck, Filomeen, Hagin, David, Halwani, Rabih, Hammarström, Lennart, Heath, James R., Hsieh, Elena W.Y., Husebye, Eystein, Imai, Kohsuke, Itan, Yuval, Jouanguy, Emmanuelle, Kaja, Elżbieta, Karamitros, Timokratis, Kisand, Kai, Ku, Cheng-Lung, Lau, Yu-Lung, Ling, Yun, Lucas, Carrie L., Maniatis, Tom, Mansouri, Davood, Maródi, László, Mentré, France, Meyts, Isabelle, Milner, Joshua D., Mironska, Kristina, Mogensen, Trine H., Morio, Tomohiro, Ng, Lisa F.P., Notarangelo, Luigi D., Novelli, Antonio, Novelli, Giuseppe, O'Farrelly, Cliona, Okada, Satoshi, Okamoto, Keisuke, Ozcelik, Tayfun, Pan-Hammarström, Qiang, Pape, Jean W., Perez de Diego, Rebeca, Perez-Tur, Jordi, Perlin, David S., Pesole, Graziano, Planas, Anna M., Prando, Carolina, Pujol, Aurora, Puel, Anne, Quintana-Murci, Lluis, Ramaswamy, Sathishkumar, Renia, Laurent, Resnick, Igor, Rodríguez-Gallego, Carlos, Sancho-Shimizu, Vanessa, Sediva, Anna, Seppänen, Mikko R.J., Shahrooei, Mohammad, Shcherbina, Anna, Slaby, Ondrej, Snow, Andrew L., Soler-Palacín, Pere, Soumelis, Vassili, Spaan, András N., Tancevski, Ivan, Tangye, Stuart G., Tayoun, Ahmad Abou, Temel, Şehime Gülsün, Thorball, Christian, Tiberghien, Pierre, Trouillet-Assant, Sophie, Turvey, Stuart E., Uddin, K. M. Furkan, Uddin, Mohammed J., van de Beek, Diederik, Vinh, Donald C., von Bernuth, Horst, Wauters, Joost, Zatz, Mayana, Zawadzki, Pawel, Zhang, Qian, Zhang, Shen-Ying, Bureau, Serge, Vacher, Yannick, Gysembergh-Houal, Anne, Demerville, Lauren, Benleulmi-Chaachoua, Abla, Abad, Sebastien, Abassi, Radhiya, Abdellaoui, Abdelrafie, Abdelmalek, Abdelkrim, Abdoul, Hendy, Abergel, Helene, Abeud, Fariza, Abgrall, Sophie, Abisror, Noemie, Adechian, Marylise, Aderdour, Nordine, Admane, Hakeem Farid, Adnet, Frederic, Afritt, Sara, Agostini, Helene, Aguilar, Claire, Agut, Sophie, Aiello, Tommaso Francesco, Kaci, Marc Ait, Oufella, Hafid Ait, Ajeenthiravasan, Gokula, Alauzy, Virginie, Alby-Laurent, Fanny, Allard, Lucie, Alyanakian, Marie-Alexandra, Borrero, Blanca Amador, Amam, Sabrina, Amrouche, Lucile, Andronikof, Marc, Anglicheau, Dany, Anguel, Nadia, Annane, Djillali, Aounzou, Mohammed, Aparicio, Caroline, Aratus, Gladys, Arlet, Jean-Benoit, Arzoine, Jeremy, Aslangul, Elisabeth, Assefi, Mona, Aubry, Adeline, Audiffred, Laetitia, Audureau, Etienne, Auger, Christelle Nathalie, Auregan, Jean-Charles, Awotar, Celine, Milla, Sonia Ayllon, Azan, Delphine, Azemar, Laurene, Azzouguen, Billal, Elrufaai, Marwa Bachir, Badsi, Aïda, Bakouboula, Prissile, Balcerowiak, Coline, Balde, Fanta, Baldivia, Elodie, Bangamingo, Eliane-Flore, Baptiste, Amandine, Baran-Marszak, Fanny, Barau, Caroline, Barget, Nathalie, Baronnet, Flore, Barthelemy, Romain, Baudel, Jean-Luc, Baudry, Camille, Baudry, Elodie, Beaugerie, Laurent, Belamri, Adel, Belaube, Nicolas, Belilita, Rhida, Bellassen, Pierre, Belmokhtar, Rawan, Beltran, Isabel, Benainous, Ruben, Benallaoua, Mourad, Benamouzig, Robert, Benbara, Amélie, Benhida, Jaouad, Benkhelouf, Anis, Benlagha, Jihene, Benmostafa, Chahinez, Benothmane, Skander, Bentifraouine, Miassa, Berard, Laurence, Bernier, Quentin, Berti, Enora, Bertier, Astrid, Berton, Laure, Bessis, Simon, Beurton, Alexandra, Bianco, Celine, Bianquis, Clara, Bidar, Frank, Blanche, Philippe, Blayau, Clarisse, Bleibtreu, Alexandre, Blin, Emmanuelle, Bloch-Queyrat, Coralie, Boissier, Marie-Christophe, Bollens, Diane, Bolzoni, Marion, Bompard, Rudy pierre, Bonnet, Nicolas, Bonnouvrier, Justine, Botha, Shirmonecrystal, Boucenna, Wissam, Bouchama, Fatiha, Bouchaud, Olivier, Bouchghoul, Hanane, Boudjebla, Taoueslylia, Boudjema, Noel, Bouffard, Catherine, Bougle, Adrien, Bouguerra, Meriem, Bouras, Leila, Bourcier, Agnes, Durand, Anne Bourgarit, Bourrier, Anne, Bouscarat, Fabrice, Bouvry, Diane, Bouziri, Nesrine, Bouzrara, Ons, Bribier, Sarah, Brugier, Delphine, Brunel, Melanie, Bui, Eida, Buisson, Anne, Bukreyeva, Iryna, Bureau, Côme, Cadranel, Jacques, Cailhol, Johann, Calin, Ruxandra, Vega, Clara Campos, Canavaggio, Pauline, Cancella, Marta, Cantin, Delphine, Cao, Albert, Carbillon, Lionel, Carlier, Nicolas, Cassard, Clementine, Castor, Guylaine, Cauchy, Marion, Cha, Olivier, Chaigne, Benjamin, Challal, Salima, Champion, Karine, Chariot, Patrick, Chas, Julie, Chauveau, Simon, Chauvin, Anthony, Chauvin, Clement, Chavarot, Nathalie, Chebbout, Kamélia, Cherai, Mustapha, Cherubini, Ilaria, Chevalier, Amelie, Chiarabini, Thibault, Chinet, Thierry, Chocron, Richard, Choinier, Pascaline, Chommeloux, Juliette, Choquet, Christophe, Choupeaux, Laure, Chousterman, Benjamin, Ciocan, Dragosmarius, Clarke, Ada, Clavere, Gaëlle, Clavier, Florian, Clement, Karine, Clerc, Sebastien, Cohen, Yves, Cohen, Fleur, Cohen, Adrien, Coilly, Audrey, Colboc, Hester, Colin, Pauline, Collet, Magalie, Comarmond, Chloé, Combacon, Emeline, Combes, Alain, Comparon, Celine, Constantin, Jean-Michel, Cordel, Hugues, Cordier, Anne-Gael, Costantini, Adrien, Chalumeau, Nathalie Costedoat, Couffignal, Camille, Coupeau, Doriane, Creange, Alain, Lamarre, Yannie Cuvillier, Da Silveira, Charlène, Guibal El Kayani, Sandrine Dautheville, De Castro, Nathalie, De Rycke, Yann, Del Pozo, Lucie, Delannoy, Quentin, Delay, Mathieu, Deleris, Robin, Delforge, Juliette, Delphine, Laëtitia, Demare, Noemie, Demeret, Sophie, Demoule, Alexandre, Deniau, Aurore, Depret, François, Derolez, Sophie, Derradji, Ouda, Derridj, Nawal, Descamps, Vincent, Deschamps, Lydia, Desconclois, Celine, Desnos, Cyrielle, Desongins, Karine, Dhote, Robin, Diallo, Benjamin, Didier, Morgane, Diemer, Myriam, Diez, Stephane, Djadi-Prat, Juliette, Djamouri Monnory, Fatima-Zohra, Djebara, Siham, Djebra, Naoual, Djietcheu, Minette, Djillali, Hadjer, Djouadi, Nouara, Donneger, Severine, Santos, Catarina Dos, Dournon, Nathalie, Dres, Martin, Droctove, Laura, Drogrey, Marie, Dropy, Margot, Drouet, Elodie, Dubosq, Valérie, Dubreucq, Evelyne, Dubus, Estelle, Duchemann, Boris, Duchenoy, Thibault, Dudoignon, Emmanuel, Dufau, Romain, Dumas, Florence, Duran, Clara, Duron, Emmanuelle, Durrbach, Antoine, Duvivier, Claudine, Ebstein, Nathan, El Khalifa, Jihane, Elabbadi, Alexandre, Elie, Caroline, Ernotte, Gabriel, Esling, Anne, Etienne, Martin, Eyer, Xavier, Fartoukh, Muriel Sarah, Fayali, Takoua, Fermaut, Marion, Fiorentino, Arianna, Fliss, Souha, Fournier, Marie-Céline, Fournier, Benjamin, Francois, Hélène, Freynet, Olivia, Frigout, Yvann, Fromont, Isaure, Fuentes, Axelle, Furet, Thomas, Galand, Joris, Garnier, Marc, Gaubert, Agnes, Gaudry, Stéphane, Gaugain, Samuel, Gauthier, Damien, Gautier, Maxime, Georgin-Lavialle, Sophie, Geromin, Daniela, Ghalayini, Mohamed, Ghaleh, Bijan, Ghezal, Myriam, Gibelin, Aude, Gimeno, Linda, Girard, Benoit, Leprieur, Bénédicte Giroux, Gomes, Doryan, Gomes-Pires, Elisabete, Gouge, Anne, Gouja, Amel, Goulet, Helene, Goupil, Sylvain, De Bouille, Jeanne Goupil, Gras, Julien, Greffe, Segolene, Grimaldi, Lamiae, Guedeney, Paul, Guidet, Bertrand, Guillo, Matthias, Gulczynski, Mariechristelle, Hadjam, Tassadit, Haguenauer, Didier, Hammal, Soumeya, Hammoudi, Nadjib, Hanon, Olivier, Harrois, Anarole, Hausfater, Pierre, Hautem, Coraline, Hekimian, Guillaume, Heming, Nicholas, Hermine, Olivier, Ho, Sylvie, Houllier, Marie, Huot, Benjamin, Huscenot, Tessa, Saied, Wafa Ibn, Ikherbane, Ghilas, Imarazene, Meriem, Ingiliz, Patrick, Iratni, Lina, Jaureguiberry, Stephane, Jean-Marc, Jean-Francois, Jeyarajasingham, Deleena, Jouany, Pauline, Jouis, Veronique, Jourdaine, Clement, Kafif, Ouifiya, Kallala, Rim, Katsahian, Sandrine, Kelesyan, Lilit, Keo, Vixra, Ketz, Flora, Khamis, Warda, Khelili, Enfel, Khellaf, Mehdi, Kotokpo Youkou, Christy Gaëlla, Kounis, Ilias, Kpalma, Gaelle, Krause, Jessica, Labbe, Vincent, Lacombe, Karine, Lacorte, Jean-Marc, Lafont, Anne Gaelle, Lafont, Emmanuel, Lagha, Lynda, Lamhaut, Lionel, Lancelot, Aymeric, Landman, Cecilia, Lanternier, Fanny, Larcheveque, Cecile, Combe, Caroline Lascoux, Lassel, Ludovic, Laverdant, Benjamin, Lavergne, Christophe, Lavillegrand, Jean-Rémi, Lazureanu, Pompilia, Le Guennec, Loïc, Leberre, Lamia, Leblanc, Claire, Leboyer, Marion, Lecomte, Francois, Lecorre, Marine, Leenhardt, Romain, Lefebvre, Marylou, Lefebvre, Bénédicte, Legendre, Paul, Leger, Anne, Legros, Laurence, Legrosse, Justyna, Lehuunghia, Sébastien, Lemarec, Julien, Leporrier-Ext, Jeremie, Lesein, Manon, Lesur, Hubert, Levy, Vincent, Levy, Albert, Lopes, Edwige, Lopes, Amanda, Lopez, Vanessa, Lopinto, Julien, Lortholary, Olivier, Louadah, Badr, Loze, Bénédicte, Lucas, Marie-Laure, Lucasamichi, Axelle, Luong, Liem Binh, Magazimama-Ext, Arouna, Maingret, David, Mameri, Lakhdar, Manivet, Philippe, Mansouri, Cylia, Marcault, Estelle, Marey, Jonathan, Marin, Nathalie, Marois, Clémence, Martin, Olivier, Martineau, Lou, Martinez-Lopez, Cannelle, Martyniuck, Pierre, De Farcy, Pauline Mary, Marzouk, Nessrine, Masmoudi, Rafik, Mebazaa, Alexandre, Mechai, Frédéric, Mecozzi, Fabio, Mediouni, Chamseddine, Megarbane, Bruno, Meghadecha, Mohamed, Mejean, Élodie, Mekinian, Arsene, Abdelhadi, Nour Mekki, Mekni, Rania, Meliti, Thinhinan Sabrina, Lima, Breno Melo, Meng, Paris, Merbah, Soraya, Messani, Fadhila, Messaoudi, Yasmine, Mewasing, Baboo-Irwinsingh, Meziane, Lydia, Michelot-Burger, Carole, Mignot, Françoise, Minka, Fadi Hillary, Miyara, Makoto, Moine, Pierre, Molina, Jean-Michel, Montegnies-Boulet, Anaïs, Monti, Alexandra, Montlahuc, Claire, Montout, Anne-Lise, Moores, Alexandre, Morbieu, Caroline, Mortelette, Helene, Mouly, Stéphane, Muzaffar, Rosita, Nacerddine, Cherifa Iness, Nadal, Marine, Nadif, Hajer, Nassarmadji, Kladoum, Natella, Pierre, Ndingamondze, Sandrine, Neraal, Stefan, Nguyen, Caroline, N'Guyen, Bao, Larmurier, Isabelle Nion, Nlomenyengue, Luc, Noel, Nicolas, Nunes, Hilario, Omar, Edris, Ouazene, Zineb, Ouedraogo, Elise, Ouelaa, Wassila, Oukhedouma, Anissa, Amara, Yasmina Ould, Oya, Herve, Oziel, Johanna, Padilla, Thomas, Paillaud, Elena, Paiva, Solenne, Parfait, Beatrice, Parize, Perrine, Parizot, Christophe, Parrot, Antoine, Pavot, Arthur, Peaudecerf, Laetitia, Pene, Frédéric, Pepin, Marion, Pernet, Julie, Pernin, Claire, Petit, Mylène, Peyrony, Olivier, Pietri, Marie-Pierre, Pietri, Olivia, De Chambrun, Marc Pineton, Pinson, Michelle, Pintado, Claire, Piquard, Valentine, Pires, Christine, Planquette, Benjamin, Poirier, Sandrine, Pomel, Anne-Laure, Pons, Stéphanie, Ponscarme, Diane, Pourcelot, Annegaelle, Pourcher, Valérie, Pouvaret, Anne, Prever, Florian, Previlon, Miresta, Prevost, Margot, Provoost, Marie-Julie, Quemeneur, Cyril, Rafat, Cédric, Rami, Agathe, Ranque, Brigitte, Raphael, Maurice, Raphalen, Jean Herle, Rastoin, Anna, Raux, Mathieu, Rebai, Amani, Reby, Michael, Regent, Alexis, Regrag, Asma, Resche-Rigon, Matthieu, Ressaire, Quentin, Richard, Christian, Richard, Mariecaroline, Robert, Maxence, Rohaut, Benjamin, Rolland-Debord, Camille, Ropers, Jacques, Roque-Afonso, Anne-Marie, Rosso, Charlotte, Rousseaux, Mélanie, Rousseaux, Nabila, Roux, Swasti, Roux, Lorène, Rouzaud, Claire, Rozes, Antoine, Rubenstein, Emma, Sabate, Jean-Marc, Sabet, Sheila, Sacleux, Sophie-Caroline, Kermanach, Nathalie Saidenberg, Saliba, Faouzi, Salmon, Dominique, Savale, Laurent, Savary, Guillaume, Sberro, Rebecca, Scemla, Anne, Schlemmer, Frederic, Schwartz, Mathieu, Sedfi, Saïd, Sefir-Kribel, Samia, Seksik, Philippe, Sellier, Pierre, Selves, Agathe, Sembach, Nicole, Semerano, Luca, Senat, Marie-Victoire, Sene, Damien, Serris, Alexandra, Sese, Lucile, Sghiouar, Naima, Sigaux, Johanna, Siguier, Martin, Silvain, Johanne, Simon, Noémie, Simon, Tabassome, Skandri, Lina Innes, Slimani, Miassa, Snauwaert, Aurélie, Sokol, Harry, Soliman, Heithem, Soltani, Nisrine, Soyer, Benjamin, Steg, Gabriel, Suarez, Lydia, Szwebel, Tali-Anne, Taffame, Kossi, Tandjaoui-Lambiotte, Yacine, Tantet, Claire, Tateo, Mariagrazia, Theodose, Igor, Thiebaud, Pierre clement, Thomas, Caroline, Tiercelet, Kelly, Tisserand, Julie, Tomczak, Carole, Torelino, Krystel, Touam-Ext, Fatima, Toumi, Lilia, Toury, Gustave, Toy-Miou, Mireille, Dinh Thanh Lien, Olivia Tran, Trandinh, Alexy, Treluyer, Jean-Marc, Trinque, Baptiste, Truchot, Jennifer, Tubach, Florence, Tubiana, Sarah, Tunesi, Simone, Turpin, Matthieu, Turpin, Agathe, Urbina, Tomas, Narvaez, Rafael Usubillaga, Uzunhan, Yurdagul, Vaittinadaayar, Prabakar, Valent, Arnaud, Valentian, Maelle, Valin, Nadia, Vallet, Hélène, Vaz, Marina, Vazquezibarra, Miguel-Alejandro, Vedie, Benoit, Velly, Laetitia, Verstuyft, Celine, Viallette, Cedric, Vicaut, Eric, Vignes, Dorothee, Vimpere, Damien, Virlouvet, Myriam, Voiriot, Guillaume, Voisot, Lena, Weiss, Emmanuel, Weiss, Nicolas, Winchenne, Anaïs, Yordanov, Youri, Zafrani, Lara, Zaidan, Mohamad, Zaidi, Wissem, Zak, Cathia, Zarhrate-Ghoul, Aida, Zatout, Ouassila, Zeino, Suzanne, Zeitouni, Michel, Zemirli, Naïma, Zerah, Lorene, Zia, Ounsa, Ziol, Marianne, Zolario, Oceane, Zuber, Julien, Andrejak, Claire, Angoulvant, François, Bachelet, Delphine, Bartoli, Marie, Basmaci, Romain, Behillil, Sylvie, Beluze, Marine, Benkerrou, Dehbia, Bhavsar, Krishna, Bouadma, Lila, Bouchez, Sabelline, Bouscambert, Maude, Cervantes-Gonzalez, Minerva, Chair, Anissa, Chirouze, Catherine, Coelho, Alexandra, Couffin-Cadiergues, Sandrine, d’Ortenzio, Eric, Debray, Marie-Pierre, Deconinck, Laurene, 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Huong, Picone, Olivier, Puéchal, Oriane, Rabaud, Christian, Rosa-Calatrava, Manuel, Rossignol, Bénédicte, Rossignol, Patrick, Roy, Carine, Schneider, Marion, Su, Richa, Tardivon, Coralie, Tellier, Marie-Capucine, Téoulé, François, Terrier, Olivier, Timsit, Jean-François, Tual, Christelle, Van Der Werf, Sylvie, Vanel, Noémie, Veislinger, Aurélie, Visseaux, Benoit, Wiedemann, Aurélie, Yazdanpanah, Yazdan, Alavoine, Loubna, Burdet, Charles, Charpentier, Charlotte, Dechanet, Aline, Ecobichon, Jean-Luc, Frezouls, Wahiba, Houhou, Nadhira, Lehacaut, Jonathan, Manchon, Pauline, Nouroudine, Mariama, Quintin, Caroline, Thy, Michael, van der Werf, Sylvie, Vignali, Valérie, Chahine, Abir, Waucquier, Nawal, Migaud, Maria-Claire, Djossou, Félix, Mergeay-Fabre, Mayka, Lucarelli, Aude, Demar, Magalie, Bruneau, Léa, Gérardin, Patrick, Maillot, Adrien, Payet, Christine, Laviolle, Bruno, Laine, Fabrice, Paris, Christophe, Desille-Dugast, Mireille, Fouchard, Julie, Pistone, Thierry, Perreau, Pauline, Gissot, Valérie, Goas, Carole L.E., Montagne, Samatha, Richard, Lucie, Bouiller, Kévin, Desmarets, Maxime, Meunier, Alexandre, Bourgeon, Marilou, Lefévre, Benjamin, Jeulin, Hélène, Legrand, Karine, Lomazzi, Sandra, Tardy, Bernard, Gagneux-Brunon, Amandine, Bertholon, Frédérique, Botelho-Nevers, Elisabeth, Kouakam, Christelle, Nicolas, Leturque, Roufai, Layidé, Amat, Karine, Espérou, Hélène, Hendou, Samia, Foti, Giuseppe, Citerio, Giuseppe, Contro, Ernesto, Pesci, Alberto, Valsecchi, Maria Grazia, Cazzaniga, Marina, Bellani, Giacomo, Abad, Jorge, Accordino, Giulia, Angelini, Micol, Aguilera-Albesa, Sergio, Aguiló-Cucurull, Aina, Özkan, Esra Akyüz, Darazam, Ilad Alavi, Roblero Albisures, Jonathan Antonio, Aldave, Juan C., Ramos, Miquel Alfonso, Khan, Taj Ali, Aliberti, Anna, Nadji, Seyed Alireza, Alkan, Gulsum, AlKhater, Suzan A., Allardet-Servent, Jerome, Allende, Luis M., Alonso-Arias, Rebeca, Alshahrani, Mohammed S., Alsina, Laia, Amoura, Zahir, Antolí, Arnau, Arrestier, Romain, Aubart, Mélodie, Auguet, Teresa, Avramenko, Iryna, Aytekin, Gökhan, Azot, Axelle, Bahram, Seiamak, Bajolle, Fanny, Baldanti, Fausto, Baldolli, Aurélie, Ballester, Maite, Barrou, Benoit, Barzaghi, Federica, Basso, Sabrina, Bayhan, Gulsum Iclal, Bezrodnik, Liliana, Bilbao, Agurtzane, Blanchard-Rohner, Geraldine, Blanco, Ignacio, Blandinières, Adeline, Blázquez-Gamero, Daniel, Bloomfield, Marketa, Bolivar-Prados, Mireia, Borie, Raphael, Botdhlo-Nevers, Elisabeth, Bousquet, Aurore, Boutolleau, David, Bouvattier, Claire, Boyarchuk, Oksana, Bravais, Juliette, Briones, M. Luisa, Brunner, Marie-Eve, Bruno, Raffaele, Bueno, Maria Rita P., Bukhari, Huda, Bustamante, Jacinta, Cáceres Agra, Juan José, Capra, Ruggero, Carapito, Raphael, Carrabba, Maria, Casasnovas, Carlos, Caseris, Marion, Cassaniti, Irene, Castelle, Martin, Castelli, Francesco, Castillo de Vera, Martín, Castro, Mateus V., Catherinot, Emilie, Celik, Jale Bengi, Ceschi, Alessandro, Chalumeau, Martin, Charbit, Bruno, Boulanger, Cécile, Clavé, Père, Clotet, Bonaventura, Codina, Anna, Comarmond, Cloé, Comoli, Patrizia, Corsico, Angelo G., Coşkuner, Taner, Cvetkovski, Aleksandar, Cyrus, Cyril, Dalmau, David, Danion, François, Darley, David Ross, Das, Vincent, Dauby, Nicolas, Dauger, Stéphane, De Munte, Paul, de Pontual, Loic, Dehban, Amin, Delplancq, Geoffroy, Desguerre, Isabelle, Di Sabatino, Antonio, Diehl, Jean-Luc, Dobbelaere, Stephanie, Domínguez-Garrido, Elena, Dubost, Clément, Ekwall, Olov, Bozdemir, Şefika Elmas, Elnagdy, Marwa H., Emiroglu, Melike, Endo, Akifumi, Erdeniz, Emine Hafize, Aytekin, Selma Erol, Etxart Lasa, Maria Pilar, Euvrard, Romain, Fabio, Giovanna, Faivre, Laurence, Falck, Antonin, Fartoukh, Muriel, Faure, Morgane, Arquero, Miguel Fernandez, Ferrer, Ricard, Ferreres, Jose, Francois, Bruno, Fumadó, Victoria, Fung, Kitty S.C., Fusco, Francesca, Gagro, Alenka, Solis, Blanca Garcia, Garçon, Pierre, Gaussem, Pascale, Gayretli, Zeynep, Gil-Herrera, Juana, Gilardin, Laurent, Gatineau, Audrey Giraud, Girona-Alarcón, Mònica, Cifuentes Godínez, Karen Alejandra, Goffard, Jean-Christophe, Gonzales, Nacho, Gonzalez-Granado, Luis I., González-Montelongo, Rafaela, Guerder, Antoine, Gülhan, Belgin, Gumucio, Victor Daniel, Hanitsch, Leif Gunnar, Gunst, Jan, Gut, Marta, Hadjadj, Jérôme, Hancerli, Selda, Hariyan, Tetyana, Hatipoglu, Nevin, Heppekcan, Deniz, Hernandez-Brito, Elisa, Ho, Po-ki, Holanda-Peña, María Soledad, Horcajada, Juan P., Hraiech, Sami, Humbert, Linda, Hung, Ivan F.N., Iglesias, Alejandro D., Íñigo-Campos, Antonio, Jamme, Matthieu, Arranz, María Jesús, Jimeno, Marie-Thérèse, Jordan, Iolanda, Kanık-Yüksek, Saliha, Kara, Yalcin, Karahan, Aydın, Karbuz, Adem, Yasar, Kadriye Kart, Kasapcopur, Ozgur, Kashimada, Kenichi, Keles, Sevgi, Demirkol, Yasemin Kendir, Kido, Yasutoshi, Kizil, Can, Kılıç, Ahmet Osman, Klocperk, Adam, Koutsoukou, Antonia, Król, Zbigniew J., Ksouri, Hatem, Kuentz, Paul, Kwan, Arthur M.C., Kwan, Yat Wah M., Kwok, Janette S.Y., Lagier, Jean-Christophe, Lam, David S.Y., Lampropoulou, Vicky, Le Bourgeois, Fleur, Leo, Yee-Sin, Lopez, Rafael Leon, Leung, Daniel, Levin, Michael, Levy, Michael, Lévy, Romain, Li, Zhi, Lilleri, Daniele, Adrian Bolanos Lima, Edson Jose, Linglart, Agnes, López-Collazo, Eduardo, Lorenzo-Salazar, José M., Louapre, Céline, Lubetzki, Catherine, Lung, Kwok-Cheung, Luyt, Charles-Edouard, Lye, David C., Magnone, Cinthia, Marchioni, Enrico, Marioli, Carola, Marjani, Majid, Marques, Laura, Pereira, Jesus Marquez, Martín-Nalda, Andrea, Pueyo, David Martínez, Martinez-Picado, Javier, Marzana, Iciar, Mata-Martínez, Carmen, Mathian, Alexis, Matos, Larissa R.B., Matthews, Gail V., Mayaux, Julien, McLaughlin-Garcia, Raquel, Meersseman, Philippe, Mège, Jean-Louis, Mekontso-Dessap, Armand, Melki, Isabelle, Meloni, Federica, Meritet, Jean-François, Merlani, Paolo, Akcan, Özge Metin, Mezidi, Mehdi, Migeotte, Isabelle, Millereux, Maude, Million, Matthieu, Mirault, Tristan, Mircher, Clotilde, Mirsaeidi, Mehdi, Mizoguchi, Yoko, Modi, Bhavi P., Mojoli, Francesco, Moncomble, Elsa, Melián, Abián Montesdeoca, Martinez, Antonio Morales, Morandeira, Francisco, Morange, Pierre-Emmanuel, Mordacq, Clémence, Morelle, Guillaume, Mouly, Stéphane J., Muñoz-Barrera, Adrián, Nafati, Cyril, Nagashima, Shintaro, Nakagama, Yu, Neven, Bénédicte, Neves, João Farela, Ng, Yuk-Yung, Hubert Nielly, Medina, Yeray Novoa, Cuadros, Esmeralda Nuñez, Karabela, Semsi Nur, Ocejo-Vinyals, J. Gonzalo, Oualha, Mehdi, Ouedrani, Amani, Özçelik, Tayfun, Ozkaya-Parlakay, Aslinur, Pagani, Michele, Papadaki, Maria, Parola, Philippe, Pascreau, Tiffany, Paul, Stéphane, Paz-Artal, Estela, Pedraza, Sigifredo, González Pellecer, Nancy Carolina, Pellegrini, Silvia, Pérez de Diego, Rebeca, Pérez-Fernández, Xosé Luis, Philippe, Aurélien, Philippot, Quentin, Picod, Adrien, Pineton de Chambrun, Marc, Piralla, Antonio, Planas-Serra, Laura, Ploin, Dominique, Poissy, Julien, Poncelet, Géraldine, Poulakou, Garyphallia, Pouletty, Marie S., Pourshahnazari, Persia, Qiu-Chen, Jia Li, Quentric, Paul, Rambaud, Thomas, Raoult, Didier, Raoult, Violette, Rebillat, Anne-Sophie, Redin, Claire, Resmini, Léa, Ricart, Pilar, Richard, Jean-Christophe, Rigo-Bonnin, Raúl, Rivet, Nadia, Rivière, Jacques G., Rocamora-Blanch, Gemma, Rodero, Mathieu P., Rodrigo, Carlos, Rodriguez, Luis Antonio, Rodriguez-Gallego, Carlos, Rodriguez-Palmero, Agustí, Romero, Carolina Soledad, Rothenbuhler, Anya, Roux, Damien, Rovina, Nikoletta, Rozenberg, Flore, Ruch, Yvon, Ruiz, Montse, Ruiz del Prado, Maria Yolanda, Ruiz-Rodriguez, Juan Carlos, Sabater-Riera, Joan, Saks, Kai, Salagianni, Maria, Sanchez, Oliver, Sánchez-Montalvá, Adrián, Sánchez-Ramón, Silvia, Schidlowski, Laire, Schluter, Agatha, Schmidt, Julien, Schmidt, Matthieu, Schuetz, Catharina, Schweitzer, Cyril E., Scolari, Francesco, Seijo, Luis, Seminario, Analia Gisela, Seng, Piseth, Senoglu, Sevtap, Seppänen, Mikko, Llovich, Alex Serra, Siguret, Virginie, Siouti, Eleni, Smadja, David M., Smith, Nikaia, Sobh, Ali, Solanich, Xavier, Solé-Violán, Jordi, Soler, Catherine, Sözeri, Betül, Stella, Giulia Maria, Stepanovskiy, Yuriy, Stoclin, Annabelle, Taccone, Fabio, Taupin, Jean-Luc, Tavernier, Simon J., Tello, Loreto Vidaur, Terrier, Benjamin, Thiery, Guillaume, Thorn, Karolina, Thumerelle, Caroline, Tipu, Imran, Tolstrup, Martin, Tomasoni, Gabriele, Toubiana, Julie, Alvarez, Josep Trenado, Triantafyllia, Vasiliki, Troya, Jesús, Tsang, Owen T.Y., Tserel, Liina, Tso, Eugene Y.K., Tucci, Alessandra, Tüter Öz, Şadiye Kübra, Ursini, Matilde Valeria, Utsumi, Takanori, Vabres, Pierre, Valencia-Ramos, Juan, Van Den Rym, Ana Maria, Vandernoot, Isabelle, Velez-Santamaria, Valentina, Zuniga Veliz, Silvia Patricia, Vidigal, Mateus C., Viel, Sébastien, Villain, Cédric, Vilaire-Meunier, Marie E., Villar-García, Judit, Vincent, Audrey, Van der Linden, Dimitri, Volokha, Alla, Vuotto, Fanny, Wauters, Els, Wu, Alan K.L., Wu, Tak-Chiu, Yahşi, Aysun, Yesilbas, Osman, Yildiz, Mehmet, Young, Barnaby E., Yükselmiş, Ufuk, Zecca, Marco, Zuccaro, Valentina, Van Praet, Jens, Lambrecht, Bart N., Van Braeckel, Eva, Bosteels, Cédric, Hoste, Levi, Hoste, Eric, Bauters, Fré, De Clercq, Jozefien, Heijmans, Catherine, Slabbynck, Hans, Naesens, Leslie, Florkin, Benoit, Young, Mary-Anne, Willis, Amanda, Lapuente-Suanzes, Paloma, de Andrés-Martín, Ana, Berkell, Matilda, Carelli, Valerio, Fiorentino, Alessia, Malhotra, Surbhi, Mattiaccio, Alessandro, Pippucci, Tommaso, Seri, Marco, Tacconelli, Evelina, van Agtmael, Michiel, Algera, Anne Geke, Appelman, Brent, van Baarle, Frank, Bax, Diane, Beudel, Martijn, Bogaard, Harm Jan, Bomers, Marije, Bonta, Peter, Bos, Lieuwe, Botta, Michela, de Brabander, Justin, de Bree, Godelieve, de Bruin, Sanne, Buis, David T.P., Bugiani, Marianna, Bulle, Esther, Chouchane, Osoul, Cloherty, Alex, Dijkstra, Mirjam, Dongelmans, Dave A., Dujardin, Romein W.G., Elbers, Paul, Fleuren, Lucas, Geerlings, Suzanne, Geijtenbeek, Theo, Girbes, Armand, Goorhuis, Bram, Grobusch, Martin P., Hafkamp, Florianne, Hagens, Laura, Hamann, Jorg, Harris, Vanessa, Hemke, Robert, Hermans, Sabine M., Heunks, Leo, Hollmann, Markus, Horn, Janneke, Hovius, Joppe W., de Jong, Menno D., Koning, Rutger, Lim, Endry H.T., van Mourik, Niels, Nellen, Jeaninne, Nossent, Esther J., Paulus, Frederique, Peters, Edgar, Pina-Fuentes, Dan A.I., van der Poll, Tom, Preckel, Bennedikt, Prins, Jan M., Raasveld, Jorinde, Reijnders, Tom, de Rotte, Maurits C.F. J., Schinkel, Michiel, Schultz, Marcus J., Schrauwen, Femke A.P., Schuurmans, Alex, Schuurmans, Jaap, Sigaloff, Kim, Slim, Marleen A., Smeele, Patrick, Smit, Marry, Stijnis, Cornelis S., Stilma, Willemke, Teunissen, Charlotte, Thoral, Patrick, Tsonas, Anissa M., Tuinman, Pieter R., van der Valk, Marc, Veelo, Denise P., Volleman, Carolien, de Vries, Heder, Vught, Lonneke A., van Vugt, Michèle, Wouters, Dorien, Zwinderman, A.H., Brouwer, Matthijs C., Wiersinga, W. Joost, Vlaar, Alexander P.J., Tompkins, Miranda F., Alba, Camille, Hupalo, Daniel N., Rosenberger, John, Sukumar, Gauthaman, Wilkerson, Matthew D., Zhang, Xijun, Lack, Justin, Oler, Andrew J., Dobbs, Kerry, Delmonte, Ottavia M., Danielson, Jeffrey J., Biondi, Andrea, Bettini, Laura Rachele, D’Angiò, Mariella, Beretta, Ilaria, Imberti, Luisa, Sottini, Alessandra, Quaresima, Virginia, Quiros-Roldan, Eugenia, Rossi, Camillo, Castagnoli, Riccardo, Montagna, Daniela, Licari, Amelia, Marseglia, Gian Luigi, Marchal, Astrid, Cirulli, Elizabeth T., Neveux, Iva, Bellos, Evangelos, Thwaites, Ryan S., Schiabor Barrett, Kelly M., Zhang, Yu, Nemes-Bokun, Ivana, Kalinova, Mariya, Catchpole, Andrew, Lack, Justin B., Chiu, Christopher, and Grzymski, Joseph J.

Published
2024
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137. The effect of inhomogeneous reionisation on the Lyman-$\alpha$ forest power spectrum at redshift $z>4$: implications for thermal parameter recovery

Author

Molaro, Margherita, Iršič, Vid, Bolton, James S., Keating, Laura C., Puchwein, Ewald, Gaikwad, Prakash, Haehnelt, Martin G., Kulkarni, Girish, and Viel, Matteo

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use the Sherwood-Relics suite of hybrid hydrodynamical and radiative transfer simulations to model the effect of inhomogeneous reionisation on the 1D power spectrum of the \Lya forest transmitted flux at redshifts $4.2\leq z \leq 5$. Relative to models that assume a homogeneous UV background, reionisation suppresses the power spectrum at small scales, $k \sim 0.1\rm\,km^{-1}\,s$ by $\sim 10$ per cent because of spatial variations in the thermal broadening kernel and the divergent peculiar velocity field associated with over-pressurised intergalactic gas. On larger scales, $k<0.03\rm\,km^{-1}\,s$, the power spectrum is instead enhanced by $10$--$50$ per cent by large scale spatial variations in the neutral hydrogen fraction. The effect of inhomogeneous reionisation must therefore be accounted for in analyses of forthcoming high precision measurements. We provide a correction for the Ly$\alpha$ forest power spectrum at $4.1\leq z \leq 5.4$ that can be easily applied within other parameter inference frameworks using similar reionisation models. We perform a Bayesian analysis of mock data to assess the extent of systematic biases that may arise in measurements of the intergalactic medium if ignoring this correction. At the scales probed by current high resolution Ly$\alpha$ forest data at $z>4$, $0.006 \rm \,km^{-1}\,s\leq k \leq 0.2 \rm\, km^{-1}\,s$, we find inhomogeneous reionisation does not introduce any significant bias in thermal parameter recovery for the current measurement uncertainties of $\sim 10$ per cent. However, for $5$ per cent uncertainties, $\sim 1\sigma$ shifts between the estimated and true parameters occur., Comment: Accepted by MNRAS (21 November 2021), 20 pages, 11 figures

Published
2021
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138. Constraining beyond $\Lambda$CDM models with 21cm intensity mapping forecast observations combined with latest CMB data

Author

Berti, Maria, Spinelli, Marta, Haridasu, Balakrishna S., Viel, Matteo, and Silvestri, Alessandra

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We explore constraints on dark energy and modified gravity with forecast 21cm intensity mapping measurements using the Effective Field Theory approach. We construct a realistic mock data set forecasting a low redshift 21cm signal power spectrum $P_{21}(z,k)$ measurement from the MeerKAT radio-telescope. We compute constraints on cosmological and model parameters through Monte Carlo Markov chain techniques, testing both the constraining power of $P_{21}(k)$ alone and its effect when combined with the latest Planck 2018 CMB data. We complement our analysis by testing the effects of tomography from an ideal mock data set of observations in multiple redshift bins. We conduct our analysis numerically with the codes EFTCAMB/EFTCosmoMC, which we extend by implementing a likelihood module fully integrated with original codes. We find that adding $P_{21}(k)$ to CMB data provides significantly tighter constraints on $\Omega_ch^2$ and $H_0$, with a reduction of the error with respect to Planck results at the level of more than $60\%$. For the parameters describing beyond $\Lambda$CDM theories, we observe a reduction in the error with respect to the Planck constraints at the level of $\lesssim 10\%$. The improvement increases up to $\sim 35\%$ when we constrain the parameters using ideal, tomographic mock observations. We conclude that the power spectrum of the 21cm signal is sensitive to variations of the parameters describing the examined beyond $\Lambda$CDM models and, thus, $P_{21}(k)$ observations could help to constrain dark energy. The constraining power on such theories is improved significantly by tomography., Comment: 38 pages, 16 figures, 12 tables, prepared for submission to JCAP

Published
2021
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139. Cosmic voids and BAO with relative baryon-CDM perturbations

Author

Khoraminezhad, Hasti, Vielzeuf, Pauline, Lazeyras, Titouan, Baccigalupi, Carlo, and Viel, Matteo

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the statistics of various large-scale structure tracers in gravity-only cosmological simulations including baryons and cold dark matter (CDM) initialized with two different transfer functions, and simulated as two distinct fluids. This allows us to study the impact of baryon-CDM relative perturbations on these statistics. In particular, we focus on the statistics of cosmic voids, as well as on the matter and halo real-space 2-point correlation function and baryon acoustic oscillations (BAO) peak. We find that the void size function is affected at the 1-2% level at maximum, and that the impact is more important at higher redshift, while the void density profile and void bias are roughly unaffected. We do not detect a sizeable impact of relative baryon-CDM perturbations on the real-space correlation functions of matter and halos or the BAO peak, which is in line with results from previous works. Our results imply that it would be hard to use voids or real-space correlation functions to constrain baryon-CDM relative perturbations, but also that we might not have to include them in models for the analysis of future cosmological surveys data., Comment: 17 pages, 12 figures, v2: version published in MNRAS

Published
2021
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140. Euclid preparation: XVI. Exploring the ultra low-surface brightness Universe with Euclid/VIS

Author

Borlaff, A. S., Gómez-Alvarez, P., Altieri, B., Marcum, P. M., Vavrek, R., Laureijs, R., Kohley, R., Buitrago, F., Cuillandre, J. C., Duc, P. A., Venancio, L. M. Gaspar, Amara, A., Andreon, S., Auricchio, N., Azzollini, R., Baccigalupi, C., Balaguera-Antolínez, A., Baldi, M., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Bozzo, E., Branchini, E., Brescia, M., Brinchmann, J., Burigana, C., Cabanac, R., Camera, S., Candini, G. P., Capobianco, V., Cappi, A., Carbone, C., Carretero, J., Carvalho, C. S., Casas, S., Castander, F. J., Castellano, M., Castignani, G., Cavuoti, S., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Coupon, J., Courtois, H. M., Cropper, M., Da Silva, A., Degaudenzi, H., Di Ferdinando, D., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Ealet, A., Fabricius, M., Farina, M., Farrens, S., Ferreira, P. G., Ferriol, S., Finelli, F., Flose-Reimberg, P., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Galeotta, S., Ganga, K., Garilli, B., Gillis, B., Giocoli, C., Gozaliasl, G., Graciá-Carpio, J., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Jahnke, K., Keihanen, E., Kermiche, S., Kiessling, A., Kilbinger, M., Kirkpatrick, C. C., Kitching, T., Knapen, J. H., Kubik, B., Kümmel, M., Kunz, M., Kurki-Suonio, H., Liebing, P., Ligori, S., Lilje, P. B., Lindholm, V., Lloro, I., Mainetti, G., Maino, D., Mansutti, O., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Martínez-Delgado, D., Marulli, F., Massey, R., Maturi, M., Maurogordato, S., Medinaceli, E., Mei, S., Meneghetti, M., Merlin, E., Metcalf, R. B., Meylan, G., Moresco, M., Morgante, G., Moscardini, L., Munari, E., Nakajima, R., Neissner, C., Niemi, S. M., Nightingale, J. W., Nucita, A., Padilla, C., Paltani, S., Pasian, F., Patrizii, L., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rosset, C., Rossetti, E., Saglia, R., Sánchez, A. G., Sapone, D., Sauvage, M., Schneider, P., Scottez, V., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Skottfelt, J., Stanco, L., Starck, J. L., Sureau, F., Tallada-Crespí, P., Taylor, A. N., Tenti, M., Tereno, I., Teyssier, R., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Valiviita, J., Vassallo, T., Viel, M., Wang, Y., Weller, J., Whittaker, L., Zacchei, A., Zamorani, G., and Zucca, E.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

While Euclid is an ESA mission specifically designed to investigate the nature of Dark Energy and Dark Matter, the planned unprecedented combination of survey area ($\sim15\,000$ deg$^2$), spatial resolution, low sky-background, and depth also make Euclid an excellent space observatory for the study of the low surface brightness Universe. Scientific exploitation of the extended low surface brightness structures requires dedicated calibration procedures yet to be tested. We investigate the capabilities of Euclid to detect extended low surface brightness structure by identifying and quantifying sky background sources and stray-light contamination. We test the feasibility of generating sky flat-fields to reduce large-scale residual gradients in order to reveal the extended emission of galaxies observed in the Euclid Survey. We simulate a realistic set of Euclid/VIS observations, taking into account both instrumental and astronomical sources of contamination, including cosmic rays, stray-light, zodiacal light, ISM, and the CIB, while simulating the effects of the presence of background sources in the FOV. We demonstrate that a combination of calibration lamps, sky flats and self-calibration would enable recovery of emission at a limiting surface brightness magnitude of $\mu=29.5^{+0.08}_{-0.27} $ mag arcsec$^{-2}$ ($3\sigma$, $10\times10$ arcsec$^2$) in the Wide Survey, reaching regions 2 magnitudes deeper in the Deep Surveys. Euclid/VIS has the potential to be an excellent low surface brightness observatory. Covering the gap between pixel-to-pixel calibration lamp flats and self-calibration observations for large scales, the application of sky flat-fielding will enhance the sensitivity of the VIS detector at scales of larger than 1 degree, up to the size of the FOV, enabling Euclid to detect extended surface brightness structures below $\mu=31$ mag arcsec$^{-2}$ and beyond., Comment: 23 pages, 13 figures, Euclid Consortium Key Project, accepted for publication in Astronomy & Astrophysics

Published
2021
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141. First direct detection constraints on Planck-scale mass dark matter with multiple-scatter signatures using the DEAP-3600 detector

Author

Adhikari, P., Ajaj, R., Alpízar-Venegas, M., Auty, D. J., Benmansour, H., Bina, C. E., Bonivento, W., Boulay, M. G., Cadeddu, M., Cai, B., Cárdenas-Montes, M., Cavuoti, S., Chen, Y., Cleveland, B. T., Corning, J. M., Daugherty, S., DelGobbo, P., Di Stefano, P., Doria, L., Dunford, M., Ellingwood, E., Erlandson, A., Farahani, S. S., Fatemighomi, N., Fiorillo, G., Gallacher, D., Abia, P. García, Garg, S., Giampa, P., Goeldi, D., Gorel, P., Graham, K., Grobov, A., Hallin, A. L., Hamstra, M., Hugues, T., Ilyasov, A., Joy, A., Jigmeddorj, B., Jillings, C. J., Kamaev, O., Kaur, G., Kemp, A., Kochanek, I., Ku{ź}niak, M., Lai, M., Langrock, S., Lehnert, B., Leonhardt, A., Levashko, N., Li, X., Lissia, M., Litvinov, O., Lock, J., Longo, G., Machulin, I., McDonald, A. B., McElroy, T., McLaughlin, J. B., Mielnichuk, C., Mirasola, L., Monroe, J., Oliviéro, G., Pal, S., Peeters, S. J. M., Perry, M., Pesudo, V., Picciau, E., Piro, M. -C., Pollmann, T. R., Raj, N., Rand, E. T., Rethmeier, C., Retière, F., Rodríguez-García, I., Roszkowski, L., Ruhland, J. B., García, E. Sanchez, Sánchez-Pastor, T., Santorelli, R., Seth, S., Sinclair, D., Skensved, P., Smith, B., Smith, N. J. T., Sonley, T., Stainforth, R., Stringer, M., Sur, B., Vázquez-Jáuregui, E., Viel, S., Walding, J., Waqar, M., Ward, M., Westerdale, S., Willis, J., and Zuñiga-Reyes, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract

Dark matter particles with Planck-scale mass ($\simeq10^{19}\text{GeV}/c^2$) arise in well-motivated theories and could be produced by several cosmological mechanisms. Using a blind analysis of data collected over a 813 d live time with DEAP-3600, a 3.3 t single-phase liquid argon-based dark matter experiment at SNOLAB, a search for supermassive dark matter was performed, looking for multiple-scatter signals. No candidate signal events were observed, leading to the first direct detection constraints on Planck-scale mass dark matter. Leading limits constrain dark matter masses between $8.3\times10^{6}$ and $1.2\times10^{19} \text{GeV}/c^2$, and cross sections for scattering on $^{40}$Ar between $1.0\times10^{-23}$ and $2.4\times10^{-18} \text{cm}^2$. These are used to constrain two composite dark matter models.

Published
2021
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142. Euclid preparation: I. The Euclid Wide Survey

Author

Scaramella, R., Amiaux, J., Mellier, Y., Burigana, C., Carvalho, C. S., Cuillandre, J. -C., Da Silva, A., Derosa, A., Dinis, J., Maiorano, E., Maris, M., Tereno, I., Laureijs, R., Boenke, T., Buenadicha, G., Dupac, X., Venancio, L. M. Gaspar, Gómez-Álvarez, P., Hoar, J., Alvarez, J. Lorenzo, Racca, G. D., Saavedra-Criado, G., Schwartz, J., Vavrek, R., Schirmer, M., Aussel, H., Azzollini, R., Cardone, V. F., Cropper, M., Ealet, A., Garilli, B., Gillard, W., Granett, B. R., Guzzo, L., Hoekstra, H., Jahnke, K., Kitching, T., Meneghetti, M., Miller, L., Nakajima, R., Niemi, S. M., Pasian, F., Percival, W. J., Sauvage, M., Scodeggio, M., Wachter, S., Zacchei, A., Aghanim, N., Amara, A., Auphan, T., Auricchio, N., Awan, S., Balestra, A., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brau-Nogue, S., Brescia, M., Candini, G. P., Capobianco, V., Carbone, C., Carlberg, R. G., Carretero, J., Casas, R., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Courbin, F., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., Fourmanoit, N., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Hudelot, P., Kermiche, S., Kiessling, A., Kilbinger, M., Kohley, R., Kubik, B., Kümmel, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Melchior, M., Merlin, E., Meylan, G., Mohr, J. J., Moresco, M., Morin, B., Moscardini, L., Munari, E., Nichol, R. C., Padilla, C., Paltani, S., Peacock, J., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Rix, H. -W., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Schrabback, T., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Skottfelt, J., Stanco, L., Starck, J. L., Tallada-Crespí, P., Tavagnacco, D., Taylor, A. N., Teplitz, H. I., Toledo-Moreo, R., Torradeflot, F., Trifoglio, M., Valentijn, E. A., Valenziano, L., Kleijn, G. A. Verdoes, Wang, Y., Welikala, N., Weller, J., Wetzstein, M., Zamorani, G., Zoubian, J., Andreon, S., Baldi, M., Bardelli, S., Boucaud, A., Camera, S., Fabbian, G., Farinelli, R., Graciá-Carpio, J., Maino, D., Medinaceli, E., Mei, S., Neissner, C., Polenta, G., Renzi, A., Romelli, E., Rosset, C., Sureau, F., Tenti, M., Vassallo, T., Zucca, E., Baccigalupi, C., Balaguera-Antolínez, A., Battaglia, P., Biviano, A., Borgani, S., Bozzo, E., Cabanac, R., Cappi, A., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J., de la Torre, S., Desai, S., Di Ferdinando, D., Dole, H., Fabricius, M., Farina, M., Ferreira, P. G., Finelli, F., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Gozaliasl, G., Hook, I. M., Keihanen, E., Kirkpatrick, C. C., Liebing, P., Lindholm, V., Mainetti, G., Martinelli, M., Martinet, N., Maturi, M., McCracken, H. J., Metcalf, R. B., Morgante, G., Nightingale, J., Nucita, A., Patrizii, L., Potter, D., Riccio, G., Sánchez, A. G., Sapone, D., Schewtschenko, J. A., Schultheis, M., Scottez, V., Teyssier, R., Tutusaus, I., Valiviita, J., Viel, M., Vriend, W., and Whittaker, L.

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

Euclid is an ESA mission designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (EWS) in visible and near-infrared, covering roughly 15,000 square degrees of extragalactic sky on six years. The wide-field telescope and instruments are optimized for pristine PSF and reduced straylight, producing very crisp images. This paper presents the building of the Euclid reference survey: the sequence of pointings of EWS, Deep fields, Auxiliary fields for calibrations, and spacecraft movements followed by Euclid as it operates in a step-and-stare mode from its orbit around the Lagrange point L2. Each EWS pointing has four dithered frames; we simulate the dither pattern at pixel level to analyse the effective coverage. We use up-to-date models for the sky background to define the Euclid region-of-interest (RoI). The building of the reference survey is highly constrained from calibration cadences, spacecraft constraints and background levels; synergies with ground-based coverage are also considered. Via purposely-built software optimized to prioritize best sky areas, produce a compact coverage, and ensure thermal stability, we generate a schedule for the Auxiliary and Deep fields observations and schedule the RoI with EWS transit observations. The resulting reference survey RSD_2021A fulfills all constraints and is a good proxy for the final solution. Its wide survey covers 14,500 square degrees. The limiting AB magnitudes ($5\sigma$ point-like source) achieved in its footprint are estimated to be 26.2 (visible) and 24.5 (near-infrared); for spectroscopy, the H$_\alpha$ line flux limit is $2\times 10^{-16}$ erg cm$^{-2}$ s$^{-1}$ at 1600 nm; and for diffuse emission the surface brightness limits are 29.8 (visible) and 28.4 (near-infrared) mag arcsec$^{-2}$., Comment: 43 pages, 51 figures, submitted to A&A

Published
2021
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144. Titanium dioxide nanotubes applied to conventional glass ionomer cement influence the expression of immunoinflammatory markers: An in vitro study

Author

Rangel-Coelho, João Pedro, Gogolla, Pedro Viel, Meyer, Maria Davoli, Simão, Lucas Carvalho, Costa, Bruna Carolina, Casarin, Renato Côrrea Viana, Santamaria, Mauro Pedrine, Teixeira, Lucas Novaes, Peruzzo, Daiane Cristina, Lisboa-Filho, Paulo Noronha, Nociti-Jr, Francisco Humberto, and Kantovitz, Kamila Rosamilia

Published
2024
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145. Genetically corrected RAG2-SCID human hematopoietic stem cells restore V(D)J-recombinase and rescue lymphoid deficiency

Author

Pavel-Dinu, Mara, Gardner, Cameron L., Nakauchi, Yusuke, Kawai, Tomoki, Delmonte, Ottavia M., Palterer, Boaz, Bosticardo, Marita, Pala, Francesca, Viel, Sebastien, Malech, Harry L., Ghanim, Hana Y., Bode, Nicole M., Kurgan, Gavin L., Detweiler, Angela M., Vakulskas, Christopher A., Neff, Norma F., Sheikali, Adam, Menezes, Sherah T., Chrobok, Jade, Hernández González, Elaine M., Majeti, Ravindra, Notarangelo, Luigi D., and Porteus, Matthew H.

Published
2024
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146. NEXO: Neutrinoless double beta decay search beyond $10^{28}$ year half-life sensitivity

Author

nEXO Collaboration, Adhikari, G., Kharusi, S. Al, Angelico, E., Anton, G., Arnquist, I. J., Badhrees, I., Bane, J., Belov, V., Bernard, E. P., Bhatta, T., Bolotnikov, A., Breur, P. A., Brodsky, J. P., Brown, E., Brunner, T., Caden, E., Cao, G. F., Cao, L., Chambers, C., Chana, B., Charlebois, S. A., Chernyak, D., Chiu, M., Cleveland, B., Collister, R., Czyz, S. A., Dalmasson, J., Daniels, T., Darroch, L., DeVoe, R., Di Vacri, M. L., Dilling, J., Ding, Y. Y., Dolgolenko, A., Dolinski, M. J., Dragone, A., Echevers, J., Elbeltagi, M., Fabris, L., Fairbank, D., Fairbank, W., Farine, J., Ferrara, S., Feyzbakhsh, S., Fu, Y. S., Gallina, G., Gautam, P., Giacomini, G., Gingras, W. Gillis C., Goeldi, D., Gornea, R., Gratta, G., Hardy, C. A., Harouaka, K., Heffner, M., Hoppe, E. W., House, A., Iverson, A., Jamil, A., Jewell, M., Jiang, X. S., Karelin, A., Kaufman, L. J., Kotov, I., Krücken, R., Kuchenkov, A., Kumar, K. S., Lan, Y., Larson, A., Leach, K. G., Lenardo, B. G., Leonard, D. S., Li, G., Li, S., Li, Z., Licciardi, C., Lindsay, R., MacLellan, R., Mahtab, M., Martel-Dion, P., Masbou, J., Massacret, N., McElroy, T., McMichael, K., Peregrina, M. Medina, Michel, T., Mong, B., Moore, D. C., Murray, K., Nattress, J., Natzke, C. R., Newby, R. J., Ni, K., Nolet, F., Nusair, O., Ondze, J. C. Nzobadila, Odgers, K., Odian, A., Orrell, J. L., Ortega, G. S., Overman, C. T., Parent, S., Perna, A., Piepke, A., Pocar, A., Pratte, J-F., Priel, N., Radeka, V., Raguzin, E., Ramonnye, G. J., Rao, T., Rasiwala, H., Rescia, S., Retière, F., Ringuette, J., Riot, V., Rossignol, T., Rowson, P. C., Roy, N., Saldanha, R., Sangiorgio, S., Shang, X., Soma, A. K., Spadoni, F., Stekhanov, V., Sun, X. L., Tarka, M., Thibado, S., Tidball, A., Todd, J., Totev, T., Triambak, S., Tsang, R. H. M., Tsang, T., Vachon, F., Veeraraghavan, V., Viel, S., Vivo-Vilches, C., Vogel, P., Vuilleumier, J-L., Wagenpfeil, M., Wager, T., Walent, M., Wamba, K., Wang, Q., Wei, W., Wen, L. J., Wichoski, U., Wilde, S., Worcester, M., Wu, S. X., Wu, W. H., Wu, X., Xia, Q., Yan, W., Yang, H., Yang, L., Zeldovich, O., Zhao, J., and Ziegler, T.

Subjects
Nuclear Experiment, Physics - Instrumentation and Detectors
Abstract

The nEXO neutrinoless double beta decay experiment is designed to use a time projection chamber and 5000 kg of isotopically enriched liquid xenon to search for the decay in $^{136}$Xe. Progress in the detector design, paired with higher fidelity in its simulation and an advanced data analysis, based on the one used for the final results of EXO-200, produce a sensitivity prediction that exceeds the half-life of $10^{28}$ years. Specifically, improvements have been made in the understanding of production of scintillation photons and charge as well as of their transport and reconstruction in the detector. The more detailed knowledge of the detector construction has been paired with more assays for trace radioactivity in different materials. In particular, the use of custom electroformed copper is now incorporated in the design, leading to a substantial reduction in backgrounds from the intrinsic radioactivity of detector materials. Furthermore, a number of assumptions from previous sensitivity projections have gained further support from interim work validating the nEXO experiment concept. Together these improvements and updates suggest that the nEXO experiment will reach a half-life sensitivity of $1.35\times 10^{28}$ yr at 90% confidence level in 10 years of data taking, covering the parameter space associated with the inverted neutrino mass ordering, along with a significant portion of the parameter space for the normal ordering scenario, for almost all nuclear matrix elements. The effects of backgrounds deviating from the nominal values used for the projections are also illustrated, concluding that the nEXO design is robust against a number of imperfections of the model., Comment: 26 pages, 19 figures, version accepted by Journal of Phys. G

Published
2021
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147. Euclid Preparation: XIV. The Complete Calibration of the Color-Redshift Relation (C3R2) Survey: Data Release 3

Author

Euclid Collaboration, Stanford, S. A., Masters, D., Darvish, B., Stern, D., Cohen, J. G., Capak, P., Hernitschek, N., Davidzon, I., Rhodes, J., Sanders, D. B., Mobasher, B., Castander, F. J., Paltani, S., Aghanim, N., Amara, A., Auricchio, N., Balestra, A., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brinchmann, J., Capobianco, V., Carbone, C., Carretero, J., Casas, R., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Conselice, C. J., Corcione, L., Costille, A., Cropper, M., Degaudenzi, H., Douspis, M., Dubath, F., Dusini, S., Fosalba, P., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Garilli, B., Giocoli, C., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kiessling, A., Kilbinger, M., Kitching, T., Kubik, B., Kummel, M., Kunz, M., Kurki-Suonio, H., Laureijs, R., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Marggraf, O., Markovic, K., Massey, R., Meneghetti, M., Meylan, G., Moscardini, L., Niemi, S. M., Padilla, C., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Roncarelli, M., Rossetti, E., Saglia, R., Scaramella, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Taylor, A. N., Teplitz, H. I., Tereno, I., Toledo-Moreo, R., Valentijn, E. A., Valenziano, L., Kleijn, G. A. Verdoes, Wang, Y., Zamorani, G., Zoubian, J., Brescia, M., Congedo, G., Conversi, L., Copin, Y., Kermiche, S., Kohley, R., Medinaceli, E., Mei, S., Moresco, M., Morin, B., Munari, E., Polenta, G., Sureau, F., Crespí, P. Tallada, Vassallo, T., Zacchei, A., Andreon, S., Aussel, H., Baccigalupi, C., Balaguera-Antolínez, A., Baldi, M., Bardelli, S., Biviano, A., Borsato, E., Bozzo, E., Burigana, C., Cabanac, R., Camera, S., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J. -G., Da Silva, A., de la Torre, S., Di Ferdinando, D., Duncan, C. A. J., Dupac, X., Fabricius, M., Farina, M., Farrens, S., Ferreira, P. G., Finelli, F., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Gillard, W., Gozaliasl, G., Graciá-Carpio, J., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Martinet, N., Marulli, F., Maturi, M., Maurogordato, S., Metcalf, R. B., Nakajima, R., Neissner, C., Nightingale, J. W., Nucita, A. A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., Romelli, E., Sanchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Stanco, L., Tenti, M., Teyssier, R., Torradeflot, F., Valiviita, J., Viel, M., Whittaker, L., and Zucca, E.

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

The Complete Calibration of the Color-Redshift Relation (C3R2) survey is obtaining spectroscopic redshifts in order to map the relation between galaxy color and redshift to a depth of i ~ 24.5 (AB). The primary goal is to enable sufficiently accurate photometric redshifts for Stage IV dark energy projects, particularly Euclid and the Roman Space Telescope, which are designed to constrain cosmological parameters through weak lensing. We present 676 new high-confidence spectroscopic redshifts obtained by the C3R2 survey in the 2017B-2019B semesters using the DEIMOS, LRIS, and MOSFIRE multi-object spectrographs on the Keck telescopes. Combined with the 4454 redshifts previously published by this project, the C3R2 survey has now obtained and published 5130 high-quality galaxy spectra and redshifts. If we restrict consideration to only the 0.2 < z(phot) < 2.6 range of interest for the Euclid cosmological goals, then with the current data release C3R2 has increased the spectroscopic redshift coverage of the Euclid color space from 51% (as reported by Masters et al. 2015) to the current 91%. Once completed and combined with extensive data collected by other spectroscopic surveys, C3R2 should provide the spectroscopic calibration set needed to enable photometric redshifts to meet the cosmology requirements for Euclid, and make significant headway toward solving the problem for Roman., Comment: 14 pages, 7 figures, 4 tables. Accepted for publication in The Astrophysical Journal Supplement. Survey website with links to the C3R2 redshift catalog and the spectroscopic data hosted by the Keck Observatory Archive can be found at https://sites.google.com/view/c3r2-survey/home

Published
2021
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148. Gravitational waves $\times$ HI intensity mapping: cosmological and astrophysical applications

Author

Scelfo, Giulio, Spinelli, Marta, Raccanelli, Alvise, Boco, Lumen, Lapi, Andrea, and Viel, Matteo

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology
Abstract

Two of the most rapidly growing observables in cosmology and astrophysics are gravitational waves (GW) and the neutral hydrogen (HI) distribution. In this work, we investigate the cross-correlation between resolved gravitational wave detections and HI signal from intensity mapping (IM) experiments. By using a tomographic approach with angular power spectra, including all projection effects, we explore possible applications of the combination of the Einstein Telescope and the SKAO intensity mapping surveys. We focus on three main topics: \textit{(i)} statistical inference of the observed redshift distribution of GWs; \textit{(ii)} constraints on dynamical dark energy models as an example of cosmological studies; \textit{(iii)} determination of the nature of the progenitors of merging binary black holes, distinguishing between primordial and astrophysical origin. Our results show that: \textit{(i)} the GW redshift distribution can be calibrated with good accuracy at low redshifts, without any assumptions on cosmology or astrophysics, potentially providing a way to probe astrophysical and cosmological models; \textit{(ii)} the constrains on the dynamical dark energy parameters are competitive with IM-only experiments, in a complementary way and potentially with less systematics; \textit{(iii)} it will be possible to detect a relatively small abundance of primordial black holes within the gravitational waves from resolved mergers. Our results extend towards $\mathrm{GW \times IM}$ the promising field of multi-tracing cosmology and astrophysics, which has the major advantage of allowing scientific investigations in ways that would not be possible by looking at single observables separately., Comment: 36 pages, 7 figures, 1 table. Matches the published version

Published
2021
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149. $Euclid$ preparation: XV. Forecasting cosmological constraints for the $Euclid$ and CMB joint analysis

Author

Euclid Collaboration, Ilić, S., Aghanim, N., Baccigalupi, C., Bermejo-Climent, J. R., Fabbian, G., Legrand, L., Paoletti, D., Ballardini, M., Archidiacono, M., Douspis, M., Finelli, F., Ganga, K., Hernández-Monteagudo, C., Lattanzi, M., Marinucci, D., Migliaccio, M., Carbone, C., Casas, S., Martinelli, M., Tutusaus, I., Natoli, P., Ntelis, P., Pagano, L., Wenzl, L., Gruppuso, A., Kitching, T., Langer, M., Mauri, N., Patrizii, L., Renzi, A., Sirri, G., Stanco, L., Tenti, M., Vielzeuf, P., Lacasa, F., Polenta, G., Yankelevich, V., Blanchard, A., Sakr, Z., Pourtsidou, A., Camera, S., Cardone, V. F., Kilbinger, M., Kunz, M., Markovic, K., Pettorino, V., Sánchez, A. G., Sapone, D., Amara, A., Auricchio, N., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brescia, M., Brinchmann, J., Capobianco, V., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Ealet, A., Farrens, S., Fosalba, P., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Guzzo, L., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kohley, R., Kubik, B., Kümmel, M., Kurki-Suonio, H., Laureijs, R., Ligori, S., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Marulli, F., Massey, R., Maurogordato, S., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Percival, W., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Scaramella, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Starck, J. L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., Valenziano, L., Kleijn, G. A. Verdoes, Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Medinaceli, E., Mei, S., Rosset, C., Sureau, F., Vassallo, T., Zacchei, A., Andreon, S., Balaguera-Antolínez, A., Baldi, M., Bardelli, S., Biviano, A., Borgani, S., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J., de la Torre, S., Di Ferdinando, D., Dole, H., Farina, M., Ferreira, P. G., Flose-Reimberg, P., Galeotta, S., Gozaliasl, G., Graciá-Carpio, J., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Martinet, N., Maturi, M., Metcalf, R. B., Morgante, G., Neissner, C., Nightingale, J., Nucita, A. A., Potter, D., Riccio, G., Romelli, E., Schirmer, M., Schultheis, M., Scottez, V., Teyssier, R., Tramacere, A., Valiviita, J., Viel, M., Whittaker, L., and Zucca, E.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The combination and cross-correlation of the upcoming $Euclid$ data with cosmic microwave background (CMB) measurements is a source of great expectation since it will provide the largest lever arm of epochs, ranging from recombination to structure formation across the entire past light cone. In this work, we present forecasts for the joint analysis of $Euclid$ and CMB data on the cosmological parameters of the standard cosmological model and some of its extensions. This work expands and complements the recently published forecasts based on $Euclid$-specific probes, namely galaxy clustering, weak lensing, and their cross-correlation. With some assumptions on the specifications of current and future CMB experiments, the predicted constraints are obtained from both a standard Fisher formalism and a posterior-fitting approach based on actual CMB data. Compared to a $Euclid$-only analysis, the addition of CMB data leads to a substantial impact on constraints for all cosmological parameters of the standard $\Lambda$-cold-dark-matter model, with improvements reaching up to a factor of ten. For the parameters of extended models, which include a redshift-dependent dark energy equation of state, non-zero curvature, and a phenomenological modification of gravity, improvements can be of the order of two to three, reaching higher than ten in some cases. The results highlight the crucial importance for cosmological constraints of the combination and cross-correlation of $Euclid$ probes with CMB data., Comment: 20 pages, 8 figures, 5 tables, 1 appendix; updated to match version accepted by journal

Published
2021
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150. Mixed dark matter: matter power spectrum and halo mass function

Author

Parimbelli, G., Scelfo, G., Giri, S. K., Schneider, A., Archidiacono, M., Camera, S., and Viel, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate and quantify the impact of mixed (cold and warm) dark matter models on large-scale structure observables. In this scenario, dark matter comes in two phases, a cold one (CDM) and a warm one (WDM): the presence of the latter causes a suppression in the matter power spectrum which is allowed by current constraints and may be detected in present-day and upcoming surveys. We run a large set of $N$-body simulations in order to build an efficient and accurate emulator to predict the aforementioned suppression with percent precision over a wide range of values for the WDM mass, $M_\mathrm{wdm}$, and its fraction with respect to the totality of dark matter, $f_\mathrm{wdm}$. The suppression in the matter power spectrum is found to be independent of changes in the cosmological parameters at the 2% level for $k\lesssim 10 \ h/$Mpc and $z\leq 3.5$. In the same ranges, by applying a baryonification procedure on both $\Lambda$CDM and CWDM simulations to account for the effect of feedback, we find a similar level of agreement between the two scenarios. We examine the impact that such suppression has on weak lensing and angular galaxy clustering power spectra. Finally, we discuss the impact of mixed dark matter on the shape of the halo mass function and which analytical prescription yields the best agreement with simulations. We provide the reader with an application to galaxy cluster number counts., Comment: 27 pages, 10 figures, minor changes after peer review

Published
2021
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