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The Dark Energy Survey Supernova Program: Light Curves and 5 Yr Data Release

The Astrophysical Journal American Astronomical Society 975:1 (2024) 5

Authors:

BO Sánchez, D Brout, M Vincenzi, M Sako, K Herner, R Kessler, TM Davis, D Scolnic, M Acevedo, J Lee, A Möller, H Qu, L Kelsey, P Wiseman, P Armstrong, B Rose, R Camilleri, R Chen, L Galbany, E Kovacs, C Lidman, B Popovic, M Smith, P Shah, M Sullivan, M Toy, TMC Abbott, M Aguena, S Allam, O Alves, J Annis, J Asorey, S Avila, D Bacon, D Brooks, DL Burke, A Carnero Rosell, D Carollo, J Carretero, LN da Costa, FJ Castander, S Desai, HT Diehl, J Duarte, S Everett, I Ferrero, B Flaugher, J Frieman, J García-Bellido, M Gatti, E Gaztanaga, G Giannini, K Glazebrook, S González-Gaitán, RA Gruendl, G Gutierrez, SR Hinton, DL Hollowood, K Honscheid, DJ James, K Kuehn, O Lahav, S Lee, GF Lewis, H Lin, JL Marshall, J Mena-Fernández, R Miquel, J Myles, RC Nichol, RLC Ogando, A Palmese, MES Pereira, A Pieres, AA Plazas Malagón, A Porredon, AK Romer, E Sanchez, D Sanchez Cid, I Sevilla-Noarbe, E Suchyta, MEC Swanson, G Tarle, BE Tucker, DL Tucker, V Vikram, AR Walker, N Weaverdyck
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The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties

The Astrophysical Journal American Astronomical Society 975:1 (2024) 86

Authors:

M Vincenzi, D Brout, P Armstrong, B Popovic, G Taylor, M Acevedo, R Camilleri, R Chen, TM Davis, J Lee, C Lidman, SR Hinton, L Kelsey, R Kessler, A Möller, H Qu, M Sako, B Sanchez, D Scolnic, M Smith, M Sullivan, P Wiseman, J Asorey, BA Bassett, D Carollo, A Carr, RJ Foley, C Frohmaier, L Galbany, K Glazebrook, O Graur, E Kovacs, K Kuehn, U Malik, RC Nichol, B Rose, BE Tucker, M Toy, DL Tucker, F Yuan, TMC Abbott, M Aguena, O Alves, SS Allam, F Andrade-Oliveira, J Annis, D Bacon, K Bechtol, GM Bernstein, D Brooks, DL Burke, A Carnero Rosell, J Carretero, FJ Castander, C Conselice, LN da Costa, MES Pereira, S Desai, HT Diehl, P Doel, I Ferrero, B Flaugher, D Friedel, J Frieman, J García-Bellido, M Gatti, G Giannini, D Gruen, RA Gruendl, DL Hollowood, K Honscheid, D Huterer, DJ James, N Kuropatkin, O Lahav, S Lee, H Lin, JL Marshall, J Mena-Fernández, F Menanteau, R Miquel, A Palmese, A Pieres, AA Plazas Malagón, A Porredon, AK Romer, A Roodman, E Sanchez, D Sanchez Cid, M Schubnell, I Sevilla-Noarbe, E Suchyta, MEC Swanson, G Tarle, C To, AR Walker, N Weaverdyck, M Yamamoto
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Euclid preparation

Astronomy & Astrophysics EDP Sciences 691 (2024) a319

Authors:

G Congedo, L Miller, AN Taylor, N Cross, CAJ Duncan, T Kitching, N Martinet, S Matthew, T Schrabback, M Tewes, N Welikala, N Aghanim, A Amara, S Andreon, N Auricchio, M Baldi, S Bardelli, R Bender, C Bodendorf, D Bonino, E Branchini, M Brescia, J Brinchmann, S Camera, V Capobianco, C Carbone, VF Cardone, J Carretero, S Casas, FJ Castander, M Castellano, S Cavuoti, A Cimatti, CJ Conselice, L Conversi, Y Copin, F Courbin, HM Courtois, M Cropper, A Da Silva, H Degaudenzi, AM Di Giorgio, J Dinis, F Dubath, X Dupac, M Farina, S Farrens, S Ferriol, P Fosalba, M Frailis, E Franceschi, S Galeotta, B Garilli, B Gillis, C Giocoli, A Grazian, F Grupp, SVH Haugan, MS Holliman, W Holmes, F Hormuth, A Hornstrup, P Hudelot, K Jahnke, E Keihänen, S Kermiche, A Kiessling, M Kilbinger, B Kubik, K Kuijken, M Kümmel, M Kunz, H Kurki-Suonio, S Ligori, PB Lilje, V Lindholm, I Lloro, D Maino, E Maiorano, O Mansutti, O Marggraf, K Markovic, F Marulli, R Massey, S Maurogordato, HJ McCracken, E Medinaceli, S Mei, M Melchior, M Meneghetti, E Merlin, G Meylan, M Moresco, B Morin, L Moscardini, E Munari, S-M Niemi, JW Nightingale, C Padilla, S Paltani, F Pasian, K Pedersen, WJ Percival, V Pettorino, S Pires, G Polenta, M Poncet, LA Popa, L Pozzetti, F Raison, R Rebolo, A Renzi, J Rhodes, G Riccio, E Romelli, M Roncarelli, E Rossetti, R Saglia, D Sapone, B Sartoris, P Schneider, A Secroun, G Seidel, S Serrano, C Sirignano, G Sirri, L Stanco, P Tallada-Crespí, D Tavagnacco, I Tereno, R Toledo-Moreo, F Torradeflot, I Tutusaus, EA Valentijn, L Valenziano, T Vassallo, A Veropalumbo, Y Wang, J Weller, G Zamorani, J Zoubian, E Zucca, A Biviano, M Bolzonella, A Boucaud, E Bozzo, C Burigana, C Colodro-Conde, D Di Ferdinando, J Graciá-Carpio, N Mauri, C Neissner, AA Nucita, Z Sakr, V Scottez, M Tenti, M Viel, M Wiesmann, Y Akrami, V Allevato, S Anselmi, C Baccigalupi, M Ballardini, S Borgani, AS Borlaff, S Bruton, R Cabanac, A Cappi, CS Carvalho, G Castignani, T Castro, G Cañas-Herrera, KC Chambers, AR Cooray, J Coupon, S Davini, G De Lucia, G Desprez, S Di Domizio, H Dole, A Díaz-Sánchez, JA Escartin Vigo, S Escoffier, I Ferrero, F Finelli, L Gabarra, J García-Bellido, E Gaztanaga, F Giacomini, G Gozaliasl, D Guinet, A Hall, H Hildebrandt, S Ilić, A Jimenez Muñoz, S Joudaki, JJE Kajava, V Kansal, D Karagiannis, CC Kirkpatrick, L Legrand, J Macias-Perez, G Maggio, M Magliocchetti, R Maoli, M Martinelli, CJAP Martins, M Maturi, L Maurin, RB Metcalf, M Migliaccio, P Monaco, G Morgante, S Nadathur, L Patrizii, A Peel, A Pezzotta, V Popa, C Porciani, D Potter, M Pöntinen, P Reimberg, P-F Rocci, AG Sánchez, JA Schewtschenko, A Schneider, E Sefusatti, M Sereno, P Simon, A Spurio Mancini, J Stadel, J Steinwagner, G Testera, R Teyssier, S Toft, S Tosi, A Troja, M Tucci, C Valieri, J Valiviita, D Vergani
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Scant evidence for thawing quintessence

Physical Review D American Physical Society (APS) 110:8 (2024) 83528

Authors:

William J Wolf, Carlos García-García, Deaglan J Bartlett, Pedro G Ferreira

Abstract:

<jats:p>New constraints on the expansion rate of the Universe seem to favor evolving dark energy in the form of thawing quintessence models, i.e., models for which a canonical, minimally coupled scalar field has, at late times, begun to evolve away from potential energy domination. We scrutinize the evidence for thawing quintessence by exploring what it predicts for the equation of state. We show that, in terms of the usual Chevalier-Polarski-Linder parameters, (<a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mrow><a:msub><a:mrow><a:mi>w</a:mi></a:mrow><a:mrow><a:mn>0</a:mn></a:mrow></a:msub></a:mrow></a:math>, <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:msub><c:mi>w</c:mi><c:mi>a</c:mi></c:msub></c:math>), thawing quintessence is, in fact, only marginally consistent with a compilation of the current data. Despite this, we embrace the possibility that thawing quintessence is dark energy and find constraints on the microphysics of this scenario. We do so in terms of the effective mass <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:msup><e:mi>m</e:mi><e:mn>2</e:mn></e:msup></e:math> and energy scale <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"><g:msub><g:mi>V</g:mi><g:mn>0</g:mn></g:msub></g:math> of the scalar field potential. We are particularly careful to enforce uninformative, flat priors on these parameters so as to minimize their effect on the final posteriors. While the current data favors a large and negative value of <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:msup><i:mi>m</i:mi><i:mn>2</i:mn></i:msup></i:math>, when we compare these models to the standard <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:mi mathvariant="normal">Λ</k:mi><k:mi>CDM</k:mi></k:math> model we find that there is scant evidence for thawing quintessence.</jats:p> <jats:sec> <jats:title/> <jats:supplementary-material> <jats:permissions> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2024</jats:copyright-year> </jats:permissions> </jats:supplementary-material> </jats:sec>
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syren-new: Precise formulae for the linear and nonlinear matter power spectra with massive neutrinos and dynamical dark energy

(2024)

Authors:

Ce Sui, Deaglan J Bartlett, Shivam Pandey, Harry Desmond, Pedro G Ferreira, Benjamin D Wandelt
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