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We describe updated scientific goals for the wide-field, millimeter-wave survey that will be produced by the Simons Observatory (SO). Significant upgrades to the 6-meter SO Large Aperture Telescope (LAT) are expected to be complete by 2028, and will include a doubled mapping speed with 30,000 new detectors and an automated data reduction pipeline. In addition, a new photovoltaic array will supply most of the observatory’s power. The LAT survey will cover about 60% of the sky at a regular observing cadence, with five times the angular resolution and ten times the map depth of the Planck satellite. The science goals are to: (1) determine the physical conditions in the early universe and constrain the existence of new light particles; (2) measure the integrated distribution of mass, electron pressure, and electron momentum in the late-time universe, and, in combination with optical surveys, determine the neutrino mass and the effects of dark energy via tomographic measurements of the growth of structure at redshifts z ≲ 3; (3) measure the distribution of electron density and pressure around galaxy groups and clusters, and calibrate the effects of energy input from galaxy formation on the surrounding environment; (4) produce a sample of more than 30,000 galaxy clusters, and more than 100,000 extragalactic millimeter sources, including regularly sampled AGN light-curves, to study these sources and their emission physics; (5) measure the polarized emission from magnetically aligned dust grains in our Galaxy, to study the properties of dust and the role of magnetic fields in star formation; (6) constrain asteroid regoliths, search for Trans-Neptunian Objects, and either detect or eliminate large portions of the phase space in the search for Planet 9; and (7) provide a powerful new window into the transient universe on time scales of minutes to years, concurrent with observations from the Vera C. Rubin Observatory of overlapping sky.
The Simons Observatory: science goals and forecasts for the enhanced Large Aperture Telescope / Abitbol, M., Abril-Cabezas, I., Adachi, S., Ade, P., Adler, A.E., Agrawal, P., Aguirre, J., Ahmed, Z., Aiola, S., Alford, T., Ali, A., Alonso, D., Alvarez, M.A., An, R., Arnold, K., Ashton, P., Atkins, Z., Austermann, J., Azzoni, S., Baccigalupi, C., et al.. - In: JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS. - ISSN 1475-7516. - 2025:08(2025), pp. 1-45. [10.1088/1475-7516/2025/08/034]
The Simons Observatory: science goals and forecasts for the enhanced Large Aperture Telescope
Abitbol, M.;Abril-Cabezas, I.;Adachi, S.;Ade, P.;Adler, A. E.;Agrawal, P.;Aguirre, J.;Ahmed, Z.;Aiola, S.;Alford, T.;Ali, A.;Alonso, D.;Alvarez, M. A.;An, R.;Arnold, K.;Ashton, P.;Atkins, Z.;Austermann, J.;Azzoni, S.;Baccigalupi, C.;Baleato Lizancos, A.;Barron, D.;Barry, P.;Bartlett, J.;Battaglia, N.;Battye, R.;Baxter, E.;Bazarko, A.;Beall, J. A.;Bean, R.;Beck, D.;Beckman, S.;Begin, J.;Beheshti, A.;Beringue, B.;Bhandarkar, T.;Bhimani, S.;Bianchini, F.;Biermann, E.;Biquard, S.;Bixler, B.;Boada, S.;Boettger, D.;Bolliet, B.;Bond, J. R.;Borrill, J.;Borrow, J.;Braithwaite, C.;Brien, T. L. R.;Brown, M. L.;Bruno, S. M.;Bryan, S.;Bustos, R.;Cai, H.;Calabrese, E.;Calafut, V.;Carl, F. M.;Carones, A.;Carron, J.;Challinor, A.;Chanial, P.;Chen, N.;Cheung, K.;Chiang, B.;Chinone, Y.;Chluba, J.;Cho, H. S.;Choi, S. K.;Chu, M.;Clancy, J.;Clark, S. E.;Clarke, P.;Cleary, J.;Clements, D. L.;Connors, J.;Contaldi, C.;Coppi, G.;Corbett, L.;Cothard, N. F.;Coulton, W.;Crowley, K. D.;Crowley, K. T.;Cukierman, A.;D'Ewart, J. M.;Dachlythra, K.;Datta, R.;Day-Weiss, S.;de Haan, T.;Devlin, M.;Di Mascolo, L.;Dicker, S.;Dober, B.;Doux, C.;Dow, P.;Doyle, S.;Duell, C. J.;Duff, S. M.;Duivenvoorden, A. J.;Dunkley, J.;Dutcher, D.;Dünner, R.;Edenton, M.;El Bouhargani, H.;Errard, J.;Fabbian, G.;Fanfani, V.;Farren, G. S.;Fergusson, J.;Ferraro, S.;Flauger, R.;Foster, A.;Freese, K.;Frisch, J. C.;Frolov, A.;Fuller, G.;Galitzki, N.;Gallardo, P. A.;Galvez Ghersi, J. T.;Ganga, K.;Gao, J.;Garrido, X.;Gawiser, E.;Gerbino, M.;Gerras, R.;Giardiello, S.;Gill, A.;Gilles, V.;Giri, U.;Gleave, E.;Gluscevic, V.;Goeckner-Wald, N.;Golec, J. E.;Gordon, S.;Gralla, M.;Gratton, S.;Green, D.;Groh, J. C.;Groppi, C.;Guan, Y.;Gupta, N.;Gudmundsson, J. E.;Hagstotz, S.;Hargrave, P.;Haridas, S.;Harrington, K.;Harrison, I.;Hasegawa, M.;Hasselfield, M.;Haynes, V.;Hazumi, M.;He, A.;Healy, E.;Henderson, S. W.;Hensley, B. S.;Hertig, E.;Hervías-Caimapo, C.;Higuchi, M.;Hill, C. A.;Hill, J. C.;Hilton, G.;Hilton, M.;Hincks, A. D.;Hinshaw, G.;Hložek, R.;Ho, A. Y. Q.;Ho, S.;Ho, S. P.;Hoang, T. D.;Hoh, J.;Hornecker, E.;Hornsby, A. L.;Hotinli, S. C.;Huang, Z.;Huber, Z. B.;Hubmayr, J.;Huffenberger, K.;Hughes, J. P.;Idicherian Lonappan, A.;Ikape, M.;Irwin, K.;Iuliano, J.;Jaffe, A. H.;Jain, B.;Jense, H. T.;Jeong, O.;Johnson, A.;Johnson, B. R.;Johnson, M.;Jones, M.;Jost, B.;Kaneko, D.;Karpel, E. D.;Kasai, Y.;Katayama, N.;Keating, B.;Keller, B.;Keskitalo, R.;Kim, J.;Kisner, T.;Kiuchi, K.;Klein, J.;Knowles, K.;Kofman, A. M.;Koopman, B. J.;Kosowsky, A.;Kou, R.;Krachmalnicoff, N.;Kramer, D.;Krishak, A.;Krolewski, A.;Kusaka, A.;Kusiak, A.;La Plante, P.;La Posta, A.;Laguë, A.;Lashner, J.;Lattanzi, M.;Lee, A.;Lee, E.;Leech, J.;Lessler, C.;Leung, J. S.;Lewis, A.;Li, Y.;Li, Z.;Limon, M.;Lin, L.;Link, M.;Liu, J.;Liu, Y.;Lonergan, J.;Louis, T.;Lucas, T.;Ludlam, M.;Lungu, M.;Lyons, M.;MacCrann, N.;MacInnis, A.;Madhavacheril, M.;Mak, D.;Maldonado, F.;Mallaby-Kay, M.;Manduca, A.;Mangu, A.;Mani, H.;Maniyar, A. S.;Marques, G. A.;Mates, J.;Matsumura, T.;Mauskopf, P.;May, A.;McCallum, N.;McCarrick, H.;McCarthy, F.;McCulloch, M.;McMahon, J.;Meerburg, P. D.;Mehta, Y.;Melin, J.;Meyers, J.;Middleton, A.;Miller, A.;Mirmelstein, M.;Moodley, K.;Moore, J.;Morshed, M.;Morton, T.;Moser, E.;Mroczkowski, T.;Murata, M.;Münchmeyer, M.;Naess, S.;Nakata, H.;Namikawa, T.;Nashimoto, M.;Nati, F.;Natoli, P.;Negrello, M.;Nerval, S. K.;Newburgh, L.;Nguyen, D. V.;Nicola, A.;Niemack, M. D.;Nishino, H.;Nishinomiya, Y.;Orlando, A.;Orlowski-Scherer, J.;Pagano, L.;Page, L. A.;Pandey, S.;Papageorgiou, A.;Paraskevakos, I.;Partridge, B.;Patki, R.;Peel, M.;Perez Sarmiento, K.;Perrotta, F.;Phakathi, P.;Piccirillo, L.;Pierpaoli, E.;Pinsonneault-Marotte, T.;Pisano, G.;Poletti, D.;Puddu, R.;Puglisi, G.;Qu, F. J.;Randall, M. J.;Ranucci, C.;Raum, C.;Reeves, R.;Reichardt, C. L.;Remazeilles, M.;Rephaeli, Y.;Riechers, D.;Robe, J.;Robertson, M. F.;Robertson, N.;Rogers, K.;Rojas, F.;Romero, A.;Rosenberg, E.;Rotti, A.;Rowe, S.;Roy, A.;Sadeh, S.;Sailer, N.;Sakaguri, K.;Sakuma, T.;Sakurai, Y.;Salatino, M.;Sanders, G. H.;Sasaki, D.;Sathyanarayana Rao, M.;Satterthwaite, T. P.;Saunders, L.;Scalcinati, L.;Schaan, E.;Schmitt, B.;Schmittfull, M.;Sehgal, N.;Seibert, J.;Seino, Y.;Seljak, U.;Shaikh, S.;Shaw, E.;Shellard, P.;Sherwin, B.;Shimon, M.;Shroyer, J. E.;Sierra, C.;Sievers, J.;Sifón, C.;Sikhosana, P.;Silva-Feaver, M.;Simon, S. M.;Sinclair, A.;Smith, K.;Sohn, W.;Song, X.;Sonka, R. F.;Spergel, D.;Spisak, J.;Staggs, S. T.;Stein, G.;Stevens, J. R.;Stompor, R.;Storer, E.;Sudiwala, R.;Sugiyama, J.;Surrao, K. M.;Sutariya, S.;Suzuki, A.;Suzuki, J.;Tajima, O.;Takakura, S.;Takeuchi, A.;Tansieri, I.;Taylor, A. C.;Teply, G.;Terasaki, T.;Thomas, A.;Thomas, D. B.;Thornton, R.;Trac, H.;Tsan, T.;Tsang King Sang, E.;Tucker, C.;Ullom, J.;Vacher, L.;Vale, L.;van Engelen, A.;Van Lanen, J.;van Marrewijk, J.;Van Winkle, D. D.;Vargas, C.;Vavagiakis, E. M.;Veenendaal, I.;Vergès, C.;Vissers, M.;Viña, M.;Wagoner, K.;Walker, S.;Walters, L.;Wang, Y.;Westbrook, B.;Williams, J.;Williams, P.;Winch, H.;Wollack, E. J.;Wolz, K.;Wong, J.;Xu, Z.;Yamada, K.;Young, E.;Yu, B.;Yu, C.;Zannoni, M.;Zheng, K.;Zhu, N.;Zonca, A.;Zubeldia, I.;null, null
2025-01-01
Abstract
We describe updated scientific goals for the wide-field, millimeter-wave survey that will be produced by the Simons Observatory (SO). Significant upgrades to the 6-meter SO Large Aperture Telescope (LAT) are expected to be complete by 2028, and will include a doubled mapping speed with 30,000 new detectors and an automated data reduction pipeline. In addition, a new photovoltaic array will supply most of the observatory’s power. The LAT survey will cover about 60% of the sky at a regular observing cadence, with five times the angular resolution and ten times the map depth of the Planck satellite. The science goals are to: (1) determine the physical conditions in the early universe and constrain the existence of new light particles; (2) measure the integrated distribution of mass, electron pressure, and electron momentum in the late-time universe, and, in combination with optical surveys, determine the neutrino mass and the effects of dark energy via tomographic measurements of the growth of structure at redshifts z ≲ 3; (3) measure the distribution of electron density and pressure around galaxy groups and clusters, and calibrate the effects of energy input from galaxy formation on the surrounding environment; (4) produce a sample of more than 30,000 galaxy clusters, and more than 100,000 extragalactic millimeter sources, including regularly sampled AGN light-curves, to study these sources and their emission physics; (5) measure the polarized emission from magnetically aligned dust grains in our Galaxy, to study the properties of dust and the role of magnetic fields in star formation; (6) constrain asteroid regoliths, search for Trans-Neptunian Objects, and either detect or eliminate large portions of the phase space in the search for Planet 9; and (7) provide a powerful new window into the transient universe on time scales of minutes to years, concurrent with observations from the Vera C. Rubin Observatory of overlapping sky.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11767/152871
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