PPT-Unbarred Spirals

NGC 1566 SABrsbcSy1 NGC 7331 NGC 628 NGC 1512 SBra NGC 1097 SBsb Barred Spirals Ellipticals NGC 584 E4 NGC 4552M89 E0 NGC 1404 E1 NGC 3265 S0 NGC1291 R SB0 NGC 1377 S0. (Resolved by Galileo). Milky Way:. Galactic Structure and Dynamics. Milky Way has spiral structure. . Galactic Bulge surrounds the Center. . Powerful radio source Sagittarius A at Center. C. ontains Super-Massive Black Hole . Except for nearby, we can only see bright galaxies. I will ignore dwarf . spheroidal. (. dSph. ) and dwarf elliptical (. dE. ) classifications. Galaxies . come in four broad categories, based on their appearance. 23. vs. .. 1. First spiral nebula found in 1845 by the Earl of . Rosse. . Speculated it was beyond our Galaxy.. 1920 - "Great Debate" between Shapley and Curtis on whether spiral nebulae were galaxies beyond our own. Settled in 1924 when Edwin . Toru Kojo . (. Bielefeld U.. ). . . with:. K. Fukushima, Y. Hidaka, L. . McLerran. , R.D. . Pisarski. 1. /11. . (Confined). (. arXiv. : . 1107.2124). (Confined). Interweaving Chiral Spirals. Toru Kojo . Spiral Structure. . The Astronomical Context. By the 1920’s, we knew that the once-mysterious spiral nebulae were flattened galaxies. . Our Milky . Way is . also. flattened. . Two obvious . questions arose:. . A thin liquid crystal film on a surface of photoactive dye turns into a wonderland of exotic moving patterns if just illuminated by a simple lamp. Spirals move and oscillate across the surface in the form of advancing . Lecture 2; . April 9 2013. Previously.. On Astro-2. The goal of cosmology is to understand how the universe formed and evolved.. How can we build a theory of the universe valid at all times in every place? . .. 1. First spiral nebula found in 1845 by the Earl of . Rosse. . Speculated it was beyond our Galaxy.. 1920 - "Great Debate" between Shapley and Curtis on whether spiral nebulae were galaxies beyond our own. Settled in 1924 when Edwin . Jet Propulsion Laboratory. Planet signatures. in transition disks. Heidelberg, Jul . 27. th. , . 2018 . Collaborators. Aaron . Boley. . (. Vancouver). , Axel Brandenburg . (Stockholm). , . Kees. . Dullemond. Galaxies are . not. . alike. For every general rule I give, one can find exceptions. Classifying galaxies is difficult. They look different in different wavelengths. If the galaxy is moving, you have to correct for red-shift. Here’s the Story We’ll Unfold for You…. Hubble’s galaxy classifications: Spirals, . ellipticals. , irregulars. . Structural parts of galaxies: disk, halo, nucleus, bulge. Spiral arms – tracers of star formation. Here’s the Story We’ll Unfold for You…. Hubble’s galaxy classifications: Spirals, . ellipticals. , irregulars. . Structural parts of galaxies: disk, halo, nucleus, bulge. Spiral arms – tracers of star formation. 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. of . Local Galaxies. Michael . Brown. ARC Future Fellow. Monash. University. Where are we now?. NVSS / FIRST / SUMMS. 0.5 . mJy. RMS per beam. 15”-1’ beam. ~30 . uJy. RMS per beam in 12 hours .