PPT-Understanding Metallicity

at High Redshift Universe KenTaro Motohara IoA Univsersity of Tokyo Gas Phase Metallicity Gas Phase Metallicity Oxygen Abundance is crucial to understand galaxy formationevolution as it traces the previous star formation history . Michael Hayden (NMSU), Jo . Bovy. (IAS), Steve . Majewski. (. UVa. ), Jennifer Johnson (OSU), Gail . Zasowski. (JHU), Leo . Girardi. (. Padova. ), Carlos Allende-. Prieto. (IAC), Ana Garcia-Perez (. Michael Hayden (NMSU), Jo . Bovy. (IAS), Steve . Majewski. (. UVa. ), Jennifer Johnson (OSU), Gail . Zasowski. (JHU), Leo . Girardi. (. Padova. ), Carlos Allende-. Prieto. (IAC), Ana Garcia-Perez (. “Education: That which discloses to the wise and disguises from the foolish their lack of understanding.”- Ambrose Pierce. Interpreted by Dr. Rich Hawkins and Dr. Deborah . DeLuca. Presented . By:Laura. Metallicity. Relation at High . Redshifts. Stellar-mass . Metallicity. Relation at . ｚ～. １．. 4. Kouji. OHTA. 　（. Kyoto University. ）. K. Yabe. , F. . Iwamuro. , S. Yuma, M. Akiyama, N. Tamura, FMOS team et al.. Q: in order to study the spatial distribution of the thin disk (which dominates the Milky Way luminosity) surface photometry in the K band from space has been used. What is the advantage of the K band? What sort of stars give off most of their light at 2 microns. metallicity. gradients . in disk galaxies from . integrated stellar populations. Patricia Sánchez-. Blázquez. . And the CALIFA collaboration. Evolution of the . metallicity. gradients in cosmological simulations. Lessons from the. Illustris Simulation . Shy . Genel. Hubble Fellow. Columbia University. Genel 2016, . ApJ. in press. (. arXiv:1602.02773. ). How Environment Affects Galaxy Metallicity:. Lessons from the. Dana . Balser. (NRAO) . Loren Anderson (WVU), Tom . Bania. (BU), & Trey Wenger (. UVa. ). Photo: Harry Morton. Key Capabilities of the GBT. Receivers cover 0.1 to 100 GHz . Excellent point-source sensitivity. Lisa Kewley. Australian National University. Thank you to the LOC and SOC. Jeff Rich. I-Ting Ho. Rebecca Davies. Anne . Medling. Credit . goes to. Elise Hampton. David Nicholls. Results in this talk are from:. David Spergel. What has changed?. Context:. Standard cosmological model. No galaxy is an island… (John Dunne vs. Immanuel Kant). Tools:. Statistical galactic astronomy. 100s of stars -> 100,000s -> 1e9 (GAIA +LSST). An X-ray/UV Perspective. Edmund Hodges-. Kluck. Joel . Bregman. . University of Michigan. How do baryons cycle in and out of galaxies, and how does this impact galaxy evolution?. What happened to the “missing” baryons?. Ultra Metal - Poor (UMP ; [Fe/H] - 4 . 0 ) stars hold the key to the nucleosynthesis processes associated with first - generation stars in the Universe . However, only about two dozen UMP stars have b SOFIA [C . II. ]158 . μ. m vs H . I, . and CO data to decompose the [C . II. ] line. Results:. 46% of [C . II. ] associated with H . I. ~9% of [C . II. ] with CNM. 79% of H. 2. not traced by CO. /Fe]. SNII . release. . most. . alpha. –. elements. . SNIa. . release. . most. Fe-. peak. . elements. Other. . proposed. . possibilities. (1) A variable IMF. (2) . Differential. . retention.