论文标题

宇宙边界的光谱路线图:Desi,Desi-II,第5阶段

A Spectroscopic Road Map for Cosmic Frontier: DESI, DESI-II, Stage-5

论文作者

Schlegel, David J., Ferraro, Simone, Aldering, Greg, Baltay, Charles, BenZvi, Segev, Besuner, Robert, Blanc, Guillermo A., Bolton, Adam S., Bonaca, Ana, Brooks, David, Buckley-Geer, Elizabeth, Cai, Zheng, DeRose, Joseph, Dey, Arjun, Doel, Peter, Drlica-Wagner, Alex, Fan, Xiaohui, Gutierrez, Gaston, Green, Daniel, Guy, Julien, Huterer, Dragan, Infante, Leopoldo, Jelinsky, Patrick, Karagiannis, Dionysios, Kent, Stephen M., Kim, Alex G., Kneib, Jean-Paul, Kollmeier, Juna A., Kremin, Anthony, Lahav, Ofer, Landriau, Martin, Lang, Dustin, Leauthaud, Alexie, Levi, Michael E., Linder, Eric V., Magneville, Christophe, Martini, Paul, McDonald, Patrick, Miller, Christopher J., Myers, Adam D., Newman, Jeffrey A., Nugent, Peter E., Palanque-Delabrouille, Nathalie, Padmanabhan, Nikhil, Palmese, Antonella, Poppett, Claire, Prochaska, Jason X., Raichoor, Anand, Ramirez, Solange, Sailer, Noah, Schaan, Emmanuel, Schubnell, Michael, Seljak, Uros, Seo, Hee-Jong, Silber, Joseph, Simon, Joshua D., Slepian, Zachary, Soares-Santos, Marcelle, Tarle, Greg, Valluri, Monica, Weaverdyck, Noah J., Wechsler, Risa H., White, Martin, Yeche, Christophe, Zhou, Rongpu

论文摘要

在这份白皮书中,我们提出了DESI以外的光谱实验的实验路线图。 DESI将是2020年代的变革性宇宙学调查,绘制了4000万个星系和类星体,并捕获了最大的可用线性模式的很大一部分,最高为Z = 1.2。 DESI-II将在更高的密度和延伸到更高的红移时对星系进行试验观察。第5阶段实验将建立那些高密度和高红移观察结果,在三个维度上绘制数亿颗恒星和星系,以解决通货膨胀,暗能量,光相对论物种和深色物质的问题。这些光谱数据还将补充下一代弱透镜,线强度映射和CMB实验,并允许它们发挥其全部潜力。

In this white paper, we present an experimental road map for spectroscopic experiments beyond DESI. DESI will be a transformative cosmological survey in the 2020s, mapping 40 million galaxies and quasars and capturing a significant fraction of the available linear modes up to z=1.2. DESI-II will pilot observations of galaxies both at much higher densities and extending to higher redshifts. A Stage-5 experiment would build out those high-density and high-redshift observations, mapping hundreds of millions of stars and galaxies in three dimensions, to address the problems of inflation, dark energy, light relativistic species, and dark matter. These spectroscopic data will also complement the next generation of weak lensing, line intensity mapping and CMB experiments and allow them to reach their full potential.

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