PPT-CO imaging surveys of nearby galaxies
Author : conchita-marotz | Published Date : 2016-06-05
Nario Kuno Nobeyama Radio Observatory CO imaging survey of nearby galaxies Gas distribution amp dynamics ltgt structures of galaxies Molecular gas ltgt Star formation
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CO imaging surveys of nearby galaxies: Transcript
Nario Kuno Nobeyama Radio Observatory CO imaging survey of nearby galaxies Gas distribution amp dynamics ltgt structures of galaxies Molecular gas ltgt Star formation. 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,. D.J. Pisano. (West Virginia University). Why study galaxy environment?. Nature vs. Nurture. Can they be distinguished?. What does the environment do to a galaxy?. What would a galaxy look like without any environmental influence?. The Milky Way Galaxy. When you look into the hazy band of light across the sky, you are actually looking at our galaxy from the inside. While an awesome sight, you can only truly begin to see it if you get away from city lights on a moonless night. . With a wide-field multi-IFU spectrograph. Cluster studies. Clusters provide large samples of galaxies in a moderate field. Unique perspective on the interaction of galaxies with their environment. As they operate much as a closed box, they are useful as tracers of galaxy evolution and of cosmology. 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. Paul . Nulsen. (. CfA. ), Christine Jones (. CfA. ), . William Forman (. CfA. ), Eugene . Churazov. (MPA),. Laurence David (. CfA. ), Brian McNamara (Waterloo),. Steven Murray (. CfA. ) . AGN Outbursts in Giant . 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. D. Calzetti (Univ. of Massachusetts). a. nd the LEGUS . Team. https://. legus.stsci.edu. /. HUBBLE2020: Hubble’s 25. th. Anniversary Symposium. STScI. , Baltimore, April 20-24, 2015. NGC3344. NGC1566. Most of the power of galaxies come from the stars. Almost all nearby galaxies. Some galaxies have very bright sources right at the center. Can be as bright as a galaxy!. Or even much brighter. Called . The Hubble Tuning-Fork Diagram. This is the traditional scheme for classifying galaxies:. Elliptical Galaxies. Elliptical galaxies. have smooth, round distributions of stars. They resemble globular clusters, except they are much larger. They . These are called . active. . galaxies. .. . Active Galaxies and Quasars. By looking far away and back in time, astronomers have discovered:. The origin of active galaxy energy sources and outbursts were closely related to the formation and history of galaxies.. around Abell 370, . a galaxy cluster at z = 0.37. International SKA . Forum 2010 . Philip Lah. A New Golden Age for Radio Astronomy. Collaborators:. . Frank Briggs (ANU). . Michael Pracy . Division des lev
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