PPT-Understanding Local Luminous Infrared Galaxies in the

Herschel Era Jason K Chu jasonchu ifahawaiiedu Institute for Astronomy University of Hawaii Collaborators David Sanders IfA Kirsten Larson CaltechIPAC Joe Mazzarella. Nurul Abedin and Martin G Mlynczak NASA Langley Research Center Hampton VA 23681 Tamer F Refaat Old Dominion University Norfolk VA 23524 ABSTRACT There exists a considerable interest in the broadband detectors for CLARREO Mission which can be used t JWST Workshop. – . STScI. Baltimore. June 8, 2011. Mid-Infrared Observation of High . Redshift. Galaxy Evolution. Most star formation activity occurs behind dust . Chary & Pope . 2011. Bouwens. 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?. 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. 101 Slide Set: Finding . the Most Luminous Galaxy. Developed by the . WISE team. 0. Topic: . Galaxies . Concepts: . Galaxies, black holes, early universe, infrared studies. Mission: . WISE. Coordinated by: . Rayet. Stars & the Luminous Blue Variables. 2014/11/12 Wednesday. Luqian Wang. Outline. . Definition/General. . properties. . History. . . Classification. : . Optical/UV-FUV/Infrared. . . FS Figure 2.To find the luminous exitance of a source, first find thefirst find the total flux emitted by the area. Do this by constructing athe flux through the hemisphere, which is all the flux lea Joseph Jensen, Utah Valley University. John Blakeslee, Herzberg Astrophysics. July 4, 2016. . Understanding the systematic limitations of distance measurement techniques is key to solving many problems in cosmology and astrophysics.. Elliptical Galaxies. Spiral Galaxies. Barred Spiral. Lenticular. Irregular (. L. arge . M. agellanic . C. loud). Dwarf Spheroidal Galaxy. Isochrone - 2.5x10. 8. yrs. Isochrone - 4x10. 9. yrs. IMF in the ρ Oph Association. super-massive black hole . occupation fraction. Elena Gallo | University of Michigan. Brendan Miller. , Jenny Greene, Brandon Kelly, . Tommaso. . Treu. , Jong-. Hak. Woo & Vivienne . Baldassare. Harvard-Smithsonian . CfA. July 2012. X-Ray Binaries in Galaxies. XRB populations – the beginning. Detection – needs high resolution & sensitivity. Einstein Observatory . (review . Fabbiano. 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 . Amy Kimball. NRAO Charlottesville (. NAASC. ). Why is quasar “feedback” important for galaxy formation. . (and what are the two feedback modes)?. How to identify candidate “most extreme feedback” objects.