UltraVISTA: a new ultra-deep near-infrared survey in COSMOS
H. J. McCracken, B. Milvang-Jensen, J. Dunlop, M. Franx, J. P. U. Fynbo, O. Le Fèvre, J. Holt, K. I. Caputi, Y. Goranova, F. Buitrago, J. Emerson, W. Freudling,… 展开作者
H. J. McCracken, B. Milvang-Jensen, J. Dunlop, M. Franx, J. P. U. Fynbo, O. Le Fèvre, J. Holt, K. I. Caputi, Y. Goranova, F. Buitrago, J. Emerson, W. Freudling, P. Hudelot, C. López-Sanjuan, F. Magnard, Y. Mellier, P. Møller, K. K. Nilsson, W. Sutherland, L. Tasca, J. Zabl
备注：
11 pages, 15 figures, updated to match published version. Error in Fig. 15 in A&A version corrected
In this paper we describe the first data release of the UltraVISTA near-infrared imaging survey of the COSMOS field. We summarise the key goals and design of the survey and provide a detailed description of our data reduction techniques . We provide stacked, sky-subtracted images in $YJHK_{\rm s}$ and narrow-band filters constructed from data collected during the first year of UltraVISTA observations. Our stacked images reach $5σ$ $AB$ depths in an aperture of $2\arcsec$ diameter of $\sim 25$ in $Y$ and $\sim 24$ in $JHK_{\rm s}$ bands and all have sub-arcsecond seeing. To this $5σ$ limit, our $K_{\rm s}$ catalogue contains 216,268 sources. We carry out a series of quality assessment tests on our images and catalogues, comparing our stacks with existing catalogues. The $1σ$ astrometric RMS in both directions for stars selected with $17.0<K_{\rm s}\rm {(AB)} <19.5$ is $\sim 0.08\arcsec$ in comparison to the publicly-available COSMOS ACS catalogues. Our images are resampled to the same pixel scale and tangent point as the publicly available COSMOS data and so may be easily used to generate multi-colour catalogues using this data. All images and catalogues presented in this paper are publicly available through ESO's "phase 3" archiving and distribution system and from the UltraVISTA web site.
Spitzer Matching survey of the UltraVISTA ultra-deep Stripes (SMUVS): Full-mission IRAC Mosaics and Catalogs
本文介绍了新的深3.6和4.5微米成像的三个UltraVISTA近红外探测条纹内的COSMOS领域。这些观测是用斯皮策的红外线阵列相机（IRAC）进行的，用于斯皮策对Ultra-VISTA深条纹的匹配调查（SMUVS）。在这项工作中，我们提出了我们的数据减少技术，并记录所产生的马赛克，覆盖地图，目录在两个IRAC通带的三个最东端的UltraVISTA调查条纹，覆盖约0.66平方度的组合面积，其中0.45平方度至少有20小时的集成时间。SMUVS在3.6和4.5微米处达到约25.0 AB mag的点源灵敏度，具有4-sigma的显著性，占调查灵敏度和源混淆。在这个极限下，SMUVS星表总共包含大约350，000个源，每个源至少在一个IRAC波段中被显著检测到。由于其均匀和高灵敏度，相对较大的区域覆盖范围，以及COSMOS提供的广泛的辅助数据，SMUVS调查将有助于大量的宇宙学研究。我们将通过斯皮策科学中心公开提供本文所述的所有图像和目录。
A Strongly-Lensed Massive Ultra-Compact Quiescent Galaxy at z ~ 2.4 in the COSMOS/UltraVISTA Field
We report the discovery of a massive ultra-compact quiescent galaxy that has been strongly-lensed into multiple images by a foreground galaxy at z = 0.960. This system was serendipitously discovered as a set of extremely Ks-bright high-redshift galaxies with red J - Ks colors using new data from the UltraVISTA YJHKs near-infrared survey. The system was also previously identified as an optically-faint lens/source system using the COSMOS ACS imaging by Faure et al. (2008, 2011). Photometric redshifts for the three brightest images of the source galaxy determined from twenty-seven band photometry…
The Evolution of the Stellar Mass Functions of Star-Forming and Quiescent Galaxies to z = 4 from the COSMOS/UltraVISTA Survey
我们目前的恒星质量函数（SMF）的恒星形成和静止星系z = 4使用的样本中的95 675个星系的COSMOS/UltraVISTA字段的测量。从DR 1 UltraVISTA K_{s}波段成像中选择了源，该波段成像覆盖了宽区域（1.62 deg^2）到显著深度（K_{s,tot} = 23.4）的独特组合。合并后的星族的SMF与先前的测量结果非常一致，表明宇宙的恒星质量密度在z = 0.75、2.0和3.5时分别只有当前值的50%、10%和1%。静止的星族驱动了大部分的整体增长，这些星系的恒星质量密度从z = 3.5开始增加了2.71^{+0.93}_{-0.22} dex。在z > 2.5时，恒星形成星系在所有恒星质量的总SMF中占主导地位，尽管静止星系的非零种群持续到z = 4。K_{s}选择的恒星形成星系SMF与紫外选择的SMF在2.5 < z 3.5的比较< 4 show reasonable agreement and suggests UV-selected samples are representative of the majority of the stellar mass density at z >。我们估计的平均质量增长的个别星系选择星系在固定的累积数密度。在z = 0.3时Log（M_{*} / M_{sun}）= 11.5的星系，平均质量自z …
Spitzer bright, UltraVISTA faint sources in COSMOS: the contribution to the overall population of massive galaxies at z=3-7
我们分析了UltraVISTA超深COSMOS场上574个斯皮策4.5微米选择星系的样本，[4.5] <23 and Ks_auto>24（AB）。我们的目标是调查这些中红外明亮，近红外暗淡的来源是否对红移z>=3的大质量星系的总体人口有显着贡献。通过使用多达30个光度带进行光谱能量分布（SED）分析，我们已经确定了我们的样品峰的红移分布在红移z~2.5-3.0，约32%的星系位于z>=3。我们研究了在高红移下这些源对星系恒星质量函数（GSMF）的贡献。我们发现，[4.5]<23，Ks_auto>24的星系对先前在3=<z<4时Ks_auto<24的源所确定的GSMF产生的变化可以忽略不计，但在4=<z<5时它们的贡献更重要，占恒星质量Mst>~6 x 10^10 Msun的星系的>~50%。我们还将GSMF限制在z>=5时的最高质量端（Mst>~2 x 10^11 Msun）。根据它们在5=<z<6处的存在，以及在较高红移处的实际不存在，我们可以相当精确地确定第一个最大质量星系出现的时刻发生在z~6和z~5之间的约0.2 Gyr的时间内。或者，如果非常大的星系在宇宙时间的早期就存在，它们应该被大量的尘埃遮蔽，从而超出当前大面积深近红外探测的探测极限。
A search for ultra-light axions using precision cosmological data
Ultra-light axions (ULAs) with masses in the range 10^{-33} eV <m <10^{-20} eV are motivated by string theory and might contribute to either the dark-matter or dark-energy density of the Universe. ULAs could suppress the growth of structure on small scales, or lead to an enhanced integrated Sachs-Wolfe effect on large-scale cosmic microwave-background (CMB) anisotropies. In this work, cosmological observables over the full ULA mass range are computed, and then used to search for evidence of ULAs using CMB data from the Wilkinson Microwave Anisotropy Probe (WMAP), Planck satellite, Atacama Cosm…
