PPT-The Stellar Populations of Galaxies

HW Rix IMPRS Galaxies Course March 11 2011 Goal Determine n M t age Fe H R for a population of galaxies How many stars of what mass and metallicity formed when and where in galaxies. 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. The Cosmic Time Machine. Astronomical telescopes can’t help viewing the past.. . Distance and time are always mixed in astronomical observations.. The finite speed of light means that we always see things after they have happened–a delay of 8 minutes for the Sun and about 12 billion years for the most distant galaxies we can observe. In other words,. the full SED (. from. UV to . far-IR. ) of galaxies to put . constraints. on. dust. . attenuation. and star formation . determinations. , . from. z=0 to z=2. The CIGALE code and . its. application to Herschel . Giuseppina. . Battaglia. Instituto. de . Astrofisica. de Canarias, Tenerife. Credit. : ESO/. H.H.Heyer. Credit. : ESO/L. . Calçada. Karachentsev. et al. 2014. Individual . Red . Giant Branch . stars. Scott Croom. Julia Bryant. Joss Bland-Hawthorn. Disturbed Things Come in . small. packages. Jessica V. Bloom. Kinematics can uncover processes shaping galaxy evolution. Bloom et al., 2016 (submitted). metallicity. gradients . in disk galaxies from . integrated stellar populations. Patricia Sánchez-. Blázquez. . And the CALIFA collaboration. Evolution of the . metallicity. gradients in cosmological simulations. . 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. . diffuse X-ray emission – a survey of highly inclined disk galaxies. How is the emission correlated with galaxy properties?. How . are observations compared to simulations. ?. Nature of the emission – X-ray line spectroscopy. G. . Fabbiano. Harvard-Smithsonian Center for Astrophysics. What are these X-ray sources?. See . Fabbiano. 1989, 2006 ARAA. L. X. >10. 37. erg s. -1. Accreting NS and BH in . binary system (XRB). Astronomy C Event 2019. Stellar Evolution in Normal & Starburst Galaxies. Supported by NASA’s Universe of Learning STEM Network. . NASA’s Universe of Learning Network/CXC/NSO . Astronomy 2019 (Division C). Stellar Evolution in Normal & Starburst Galaxies. NASA Universe of Learning/CXC/NSO. https://www.universe-of-learning.org/. . . . . . . . . . http://chandra.harvard.edu/index.html. The astonishing variety of galaxies derived from a few structural types. Sec 1.3. Irregulars. = misfits in any class. Edwin Hubble . The Realm of the Nebulae . (1936. ). ‘. Tuning Fork’ classification scheme of galaxies. Laura . Magrini. INAF- . Osservatorio. . Astrofisico. di . Arcetri. In Our Galaxy. Open clusters (disc population): . Many (~2200 known clusters). . even more new candidates in the inner disc from infrared surveys . X-ray sources in galaxies. Marat . Gilfanov. MPA, . GArching. Marat Gilfanov. XMM Workshop 2010. Hans-. Jakob. . Grimm. Pavel. . Shtykovskiy. (IKI/MPA). Rashid . Sunyaev. (MPA/IKI). Rasmus. Voss (MPA, MPE).