PPT-Virtually all galaxies show a flat rotation curve.

Lets look back at the rotational velocity equation v M interior Gr 05 The rotational velocity is constant at big r values What must we conclude The mass interior to the orbit is still increasing Even after the radius r has gone beyond the last of the stars It must be increasing in order to hold v constant. 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,. Anja. von . der. Linden et al., 2007, MNRAS, 379, 867. On the prevalence of radio-loud active galactic nuclei in brightest cluster galaxies: implications for AGN heating of cooling flows. P. N. Best et al., 2007, MNRAS, 379, 894. Adam Leroy. National Radio Astronomy Observatory. HERITAGE (. Meixner. et al.). Dust in Dwarf Galaxies. Adam Leroy. National Radio Astronomy Observatory. HERITAGE (. Meixner. et al.). SAGE (. Meixner. 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. . 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. David Roberts, Jake Cohen, & Jing Lu. Brandeis University. Lakshmi . Saripalli. & Ravi . Subrahmanyan. Raman Research Institute. 1. Radio Galaxies. X-Shaped Radio Galaxies. Cheung’s Sample. H.-W. 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?. 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 . Ms. Cordaro . SMHS . Earth Science. Review/Warm up – Write this in your journal. (Do not fill in the blanks yet!!). A light year = How far _ _ _ _ _ travels in _ _ _ year.. The electromagnetic spectrum is made up of different size _ _ _ _ _ that produce _ _ _ _ _ _ in the form of radiation.. 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.. Discover the truth and the facts about Flat Belly Fix™ PDF, eBook by Todd Lamb. Click \"SHARE\" and \"DOWNLOAD\" to read the document offline.