Unveiling the distant Universe: Characterizing $z\ge9$ Galaxies in the first epoch of COSMOS-Web
Maximilien Franco, Hollis B. Akins, Caitlin M. Casey, Steven L. Finkelstein, Marko Shuntov, Katherine Chworowsky, Andreas L. Faisst, Seiji Fujimoto, Olivier Ilb… 展开作者
Maximilien Franco, Hollis B. Akins, Caitlin M. Casey, Steven L. Finkelstein, Marko Shuntov, Katherine Chworowsky, Andreas L. Faisst, Seiji Fujimoto, Olivier Ilbert, Anton M. Koekemoer, Daizhong Liu, Christopher C. Lovell, Claudia Maraston, Henry Joy McCracken, Jed McKinney, Brant E. Robertson, Micaela B. Bagley, Jaclyn B. Champagne, Olivia R. Cooper, Xuheng Ding, Nicole E. Drakos, Andrea Enia, Steven Gillman, Christopher C. Hayward, Michaela Hirschmann, Vasily Kokorev, Clotilde Laigle, Arianna S. Long, Ghassem Gozaliasl, Santosh Harish, Shuowen Jin, Jeyhan S. Kartaltepe, Georgios Magdis, Guillaume Mahler, Crystal L. Martin, R. Michael Rich, Benny Trakhtenbrot, Bahram Mobasher, Louise Paquereau, Alvio Renzini, Jason Rhodes, Kartik Sheth, John D. Silverman, Martin Sparre, Margherita Talia, Francesco Valentino, Aswin P. Vijayan, Stephen M. Wilkins, Lilan Yang, Jorge A. Zavala
We report the identification of 15 galaxy candidates at $z\ge9$ using the initial COSMOS-Web JWST observations over 77 arcmin$^2$ through four NIRCam filters (F115W, F150W, F277W, F444W) with an overlap with MIRI (F770W) of 8.7 arcmin$^2$. We fit the sample using several publicly-available SED fitting and photometric redshift codes and determine their redshifts between $z=9.3$ and $z=10.9$ ($\langle z\rangle=10.0$), UV-magnitudes between M$_{\rm UV}$ = $-$21.2 and $-$19.5 (with $\langle $M$_{\rm UV}\rangle=-20.2$) and rest-frame UV slopes ($\langle β\rangle=-2.4$). These galaxies are, on average, more luminous than most $z\ge9$ candidates discovered by JWST so far in the literature, while exhibiting similar blue colors in their rest-frame UV. The rest-frame UV slopes derived from SED-fitting are blue ($β\sim$[$-$2.0, $-$2.7]) without reaching extremely blue values as reported in other recent studies at these redshifts. The blue color is consistent with models that suggest the underlying stellar population is not yet fully enriched in metals like similarly luminous galaxies in the lower redshift Universe. The derived stellar masses with $\langle \log_{\rm 10} ($M$_\star/$M$_\odot)\rangle\approx8-9$ are not in tension with the standard $Λ$CDM model and our measurement of the volume density of such UV luminous galaxies aligns well with previously measured values presented in the literature at $z\sim9-10$. Our sample of galaxies, although compact, are significantly resolved.
Small hosts, big appetites: unveiling rapid and early low-mass black hole growth in cosmological zoom-in simulations of dwarf galaxies
Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Kavli Institute for Cosmology, Cambridge, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire（赫特福德大学物理、天文与数学系天体物理研究中心）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）
Insights into Galaxy Morphology and Star Formation: Unveiling Filamentary Structures around an Extreme Overdensity at $z \sim 1.5$ Traced by [OII] Emitters
Unveiling the roles of thermal and nonthermal processes in the ISM & IGM structure formation and evolution of galaxies with SKAO
Institute for Research in Fundamental Sciences (IPM)（伊朗基础科学研究所）；Xinjiang Astronomical Observatory, CAS（中国科学院新疆天文台）；National Radio Astronomy Observatory（美国国家射电天文台）；Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；University of Groningen（格罗宁根大学）；SKA Observatory（平方公里阵列望远镜观测站）；Chalmers University of Technology（查尔姆斯理工大学）；University of Hamburg（汉堡大学）；University of Virginia（弗吉尼亚大学）
Predicting emission line fluxes and number counts of distant galaxies for cosmological surveys
我们结合光度学和光谱学估计了高红移线发射体的数目及其随宇宙时间的演化。我们预测的H $α$，H $β$，[OII]和[OIII]线通量超过$35,000$星系下降到恒星质量的$\sim10^9$ $M_{\odot}$在COSMOS和GOODS-S领域，应用标准转换和利用光谱覆盖的FMOS-COSMOS调查在$z\sim1.55$校准的预测。在FMOS-COSMOS巡天覆盖的范围$1.4 < z < 1.8$内，我们计算了H $α$、[OII]和[OIII]发射体的数量计数，直到$1\times10^{-17}$ erg cm $^{-2}$ s $^{-1}$的通量。我们模拟的差分和累积H $α$计数的时间演变，急剧下降，在最亮的通量。我们期望$\sim9,300-9,700$和$\sim2,300-2,900$星系deg $^{-2}$的流量$\geq1\times10^{-16}$和$\geq2\times10^{-16}$ erg cm $^{-2}$ s $^{-1}$在$0.9<z<1.8$范围内。我们发现，观测到的星系红移的主要序列的演变是足够的再现观测到的计数变化$0.2<z<2.5$。我们用通量$\geq2\times10^{-16}$ erg cm $^{-2}$ s $^{-1}$来表征H $α$辐射体的物理性质，包括它们的恒星质量、紫外线大小、[NII]/H…
