PPT-The Slit-Less Spectroscopic Survey of Galaxies (SPICY) with

AKARIIRC perspective to SPICA T Wada Y Ohyama H Matsuhara M Malkan T Goto E Egami JH Kim C Pearson H Inami D Burgarella T . Patricia . Sánchez-Blázquez. (UAM). Jairo. Mendez-Abreu (IAC). Sebastian F Sánchez (UNAM). Isabel Perez (UGR). Fabian Rosales-Ortega (UAM). And . the CALIFA collaboration. Resolved stellar . population. Li Jiang-Tao. 1. Service d’Astrophysique, CEA, Saclay, France. 2. . Department. of . Astronomy. , . University. of Michigan, Ann Arbor, USA. Outline. 1. Introduction. 2. Diffuse X-ray . observation. Lawrence Rudnick, University of Minnesota. Deep+wideband+polarization. ~30. m. Jy,800sq . deg. 700-1800. More science using subsamples. This is single project from large survey. Feasible with JVLA only: NVSS level investment. One Photon at a Time. By:. Kevin Masson. I then found positions of the slit blocker that would effect the double slit, there are five positions;. Far side with both slits blocked, allowing no light to pass.. ). Presentation to P. Hertz April 19, 2013. . Neil . Gehrels. (GSFC). SDT . Co-Chair. David . Spergel. (Princeton) . . SDT Co-Chair. Kevin Grady (GSFC) Study Manager . & . Project Team. An up-close view of turbulent, clumpy galaxies. David B Fisher . Swinburne University of Technology. Karl . Glazebrook. , Rob Bassett, Andy Green, Heidi White, . Ivana. . Damjanov. , Emily . Wisnioski. . Ste. llar. . P. opulations . at intermediate redshift . S. urvey. w. ith . WEAVE. Bianca Poggianti – Angela . Iovino. (co-. Leads. ). o. n . behalf. of the . StePS. team . A. Mercurio, M. . The Evolution of the Tully-Fisher Relation Since . z. ~ 1. KROSS . P.Is. : Richard Bower (. Dur. ), Martin Bureau (Ox). Oxford: Andy Bunker, Matt Jarvis, . Georgios . Magdis. , John Stott . Durham: Mark . HECTOR project scientist. Australian Astronomical Observatory. University of Sydney CAASTRO. With Joss Bland-Hawthorn, Jon Lawrence, Scott Croom and the Hector team. HECTOR . . - a . massive new . IFS instrument for . - Understand the basic origin of spectroscopic lines (homework).. - Understand how diffraction gratings work (homework).. - Determine the wavelength of particular spectroscopic lines.. - Identify a material based on it’s spectrum.. spectroscopy of Y . dwarfs. NIRSpec. MIRI LRS. In this hands-on session you will be asked to use:. The . Exposure Time Calculator. (ETC) for the . NIRSpec. fraction. The . Astronomer’s Proposal Tool. HOT DISHESCLASSICMatsuhisa ShrimpRock Shrimp Tempura with Creamy Spicy Sauce or PonzuSquid "Pasta" with Light Garlic SauceShrimp and Lobster with Spicy Lemon SauceSea Bass with Black Bean SauceBlack C Read March 21 1916 MICROSCoPze ACCB86OBY 131 which passes is limited to that which has traversed the crystal- structure in what is plctically one direction only and with the help of a nicol it may be GUViCS. ). IV. The role of the cluster environment on galaxy evolution. Speaker: Xinkai Chen. Sample. Sample:. Extended Source . Catalogue of Voyer+14. recessional . velocity < . 3500kms-1. , Virgo cluster region.