The Cosmic Energy Inventory : Construction and Consistency Investigations

宇宙能量清单：构建和一致性调查

• 批准号: 20540255
• 负责人: FUKUGITA Masataka
• 金额: $ 2.33万
• 依托单位: The University of Tokyo
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (C)
• 财政年份: 2008
• 资助国家: 日本
• 起止时间: 2008 至 2010
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-20540255/
• 关键词: 宇宙物理(理論); 宇宙論; 銀河の質量分布; 弱重力レンズ; 宇宙シミュレーション; ヴィリアル半徑; Sloan Digital Sky Survey; 宇宙論パラメター; 重力レンズ頻度; 宇宙エネルギー型録; 星生成率; SDSS測光標準系; 宇宙塵(dust); 円盤・バルヂ分解; 宇宙背景輻射; 宇宙塵; 超新星生起率; 銀河合體

The two noteworthy findings, among others, are that(i) the mass of galaxies is distributed far away to the distance beyond the gravitational binding radius(virial radius), and(ii) a significant amount of dust is present outside galaxies, i. e., dust produced in stars in galaxies is blown out even to the distance beyond the galactic haloes. These mean that the universe is not empty anywhere.Weak gravitational lensing, when applied to large galaxy-quasar samples, leads us to estimate the column mass density. When plotted as a function of the distance from galaxies, it gives us mass distribution of galaxies as a function of the distance with the aid of N body simulations(dark matter only) which are constrained by the observed mass distribution. The result is that the mass associated with galaxies is extended to the middle to the neibouring galaxy, far beyond the virial radius, and the mass contained in the virial radius is only 25% of the total. This result applies both dark matter that is the main component of the galaxy and baryons. This also explains the discrepancy between the two mass density estimates, one using the luminosity density times the average mass-to-light ratio of galaxies and the other the global estimate using such as the cosmic microwave background fluctuation.The other conspicuous result is that dust is present not only in HI regions of galactic discs but also outside the galaxy, even beyond the virial radius, while dust is supposed to be produced by stars in galactic discs. The integrated amount of dust present outside galactic discs is as much as, or even more than, that in galactic discs. When added both component the amount of dust in the universe becomes consistent with the accumulated amount expected from the star formation history over the cosmic time. The extragalactic component accounts for missing dust in the cosmic energy inventory and it now closes.

其中两个值得注意的发现是：（i）星系的质量分布在远离引力束缚半径（维里半径）的地方，以及（ii）星系外部存在大量的尘埃，即。例如，星系中恒星产生的尘埃甚至被吹到银晕之外的距离。这意味着宇宙在任何地方都不是空的。当弱引力透镜应用于大型星系-类星体样本时，我们可以估计柱质量密度。当绘制为距星系距离的函数时，它借助受观测到的质量分布约束的 N 体模拟（仅限暗物质），为我们提供了作为距离函数的星系质量分布。其结果是，与星系相关的质量延伸到了邻近星系的中部，远远超出了维里半径，而维里半径所包含的质量仅占总量的25%。这一结果同时适用于作为星系主要成分的暗物质和重子。这也解释了两种质量密度估计之间的差异，一种使用光度密度乘以星系的平均质光比，另一种使用宇宙微波背景波动等全局估计。另一个显着的结果是尘埃不仅存在于银盘的HI区域，而且还存在于星系之外，甚至超出维里半径，而尘埃应该是由银盘中的恒星产生的。银盘外部存在的尘埃总量与银盘内部的尘埃总量相当，甚至更多。当添加这两种成分时，宇宙中的尘埃量变得与宇宙时间内恒星形成历史中预期的累积量一致。河外部分解释了宇宙能量库存中缺失的尘埃，现在它已经结束了。

项目成果

The Sloan Digital Sky Survey quasar lens search. IV : Statistical lens sample from the fifth data release

斯隆数字巡天类星体镜头搜索。

• DOI: 10.1088/0004-6256/140/2/403
• 发表时间: 2010
• 期刊: Astron. J.
• 作者: N. Inada;M. Oguri;M. S. Shin;I. Kayo;M. A. Strauss;J. F. Hannawi;T. Morokuma;R. H. Becker;R. L. White;C. S. Kochanek;M. D. Gregg;K. Chiu;D. E. Johnston;A. Clocchiatti;G. T. Richards;D. P. Schneider;J. A. Frieman;M. Fukugita;R. J. Gott;P
• 通讯作者: P

Effects of massive neutrinos on the structure formation of the universe

大质量中微子对宇宙结构形成的影响

• 发表时间: 2009
• 作者: C.S. Chu;P. M. Ho;Y. Matsuo;S. Shiba;M.Fukugita
• 通讯作者: M.Fukugita

PHOTOMETRIC RESPONSE FUNCTIONS OF THE SLOAN DIGITAL SKY SURVEY IMAGER

• DOI: 10.1088/0004-6256/139/4/1628
• 发表时间: 2010-02
• 期刊: The Astronomical Journal
• 作者: M. Doi;Masayuki Tanaka;M. Fukugita;J. Gunn;N. Yasuda;Ž. Ivezić;J. Brinkmann;Ernst de Haars

Matter distribution around galaxies

星系周围的物质分布

• 发表时间: 2012
• 期刊: Astrophys.J.
• 作者: S.Masaki;M.Fukugita;N.Yoshida
• 通讯作者: N.Yoshida

Supernovae in the Subaru Deep Field: the rate and delay-time distribution of Type la supernovae out to redshift 2

斯巴鲁深场中的超新星：la型超新星到达红移2的速率和延迟时间分布

• 发表时间: 2011
• 期刊: Mon.Not.Roy.astr.Soc.
• 作者: O.Graur;D.Poznanski;D.Maoz;N.Yasuda;T.Totani;M.Fukugita;A.V.Filippenko;R.J.Foley;J.M.Silverman
• 通讯作者: J.M.Silverman