7. Dwarf Galaxies

Total Page:16

File Type:pdf, Size:1020Kb

7. Dwarf Galaxies 22.05.2019 Satellite Galaxies SS2019 1 1. DGs around the Milky Way The Magellanic Clouds: LMC SS2019and SMC 2 1 22.05.2019 1.1. The Magellanic System On the southern sky 2 large diffuse and faint patches are optically visible: SS2019 3 The Magellanic Clouds Small Magellanic Cloud (SMC);SS2019 dIrr; dist.: ~ 58 kpc 4 2 22.05.2019 Large Magellanic Cloud (LMC), dIrr; dist.: ~ 58 kpc SS2019 5 optical : stars + lumin. gas 1.2. The many faces of the LMC Star-forming Regions: H SS2019 6 HI withl21cm 3 22.05.2019 (J. van Loon) SS2019 8 (J. van Loon) SS2019 9 4 22.05.2019 (J. van Loon) SS2019 10 1.3. The LMC, a gas-rich Dwarf Irregular Galaxy (dIrr) SS2019 11 5 22.05.2019 (J. van Loon) SS2019 12 Panchromatic picture (J. van Loon) SS2019 13 6 22.05.2019 Further evidence for ram pressure: at its front-side LMC gas is compressed leading to molecular cloud formation triggered star formation Star-forming regions: H SS2019 14 Hot Supernova Gas: X-ray (J. van Loon) SS2019 15 7 22.05.2019 SS2019 16 8.8. The Magellanic Stream Gas bridges between the Magellanic Clouds are formed (Magellanic Stream), showing that this complex is tidally disrupted by the Milky Way. Stripped-off gas drops down to the Galactic disk and feeds the MWG. [Dwarf satellite galaxies are swallowed by larger parent galaxies (see next SS2019 17 Chapt.)] 8 22.05.2019 SS2019 18 1.4. The Magellanic System SS2019 19 9 22.05.2019 Besla et al. (2016) ApJ, 825 SS2019 20 The Magellanic Stream SS2019 21 10 22.05.2019 1.5. Modeling the Magellanic System (2012) ApJ, 421 SS2019 23 Besla et al. (2012) ApJ, 421 SS2019 24 11 22.05.2019 Ram-pressure stripping by the ram-pressure stripping 2 motion through hot halo gas if Pram = IGM·v rel > P0(r) SS2019 25 Computer model of a small satellite galaxy orbiting a larger (edge-on) disk galaxy. As the satellite orbits, stars are stripped from the satellite and orbit in the halo of the larger galaxy. (Kathryn Johnston, Wesleyan): see the bending and tumbling of the satellite‘s figure axis! SS2019 26 12 22.05.2019 1.6. Gas-free Dwarf Galaxies: dSphs Fornax dSph D= 138 kpc Mv = -13.5 SS2019 27 Faint dSphs pure stellar systems, no gas, metal-poor: Z< Z, faint end of dwarf Es, m extremely faint: Mv>-8 , very small: ~ few kpc, close to the MWG Leo I with Regulus = Leo SS2019 28 13 22.05.2019 dE‘s in the vicinity of the Milky Way populate the low-mass end and are named Dwarf Spheroidals: Their surface brightness is only slightly larger than the background; almost no gas LeoI SS2019 29 Ursa Minor dSph SS2019 30 14 22.05.2019 Leo I: D = 250 kpc SS2019 32 1.7. Intrinsic properties of dSphs van den Bergh (2008) dSphs are less Mv = 16.2 – 14.26 log Rh concentrated and flatter than dSphs SS2019 33 15 22.05.2019 Correlations of different galaxy types Tolstoy et al. (2010) ARAA, 47 SS2019 34 SS2019 35 16 22.05.2019 SS2019 36 2. The MWG Satellites SS2019 37 17 22.05.2019 SS2019 38 Grebel, 1998 2.1. The 12 major MWG satellites SS2019 40 18 22.05.2019 2.2. Their Location Marla Geha SS2019 42 Spatial Distribution of MW satellites SS2019 43 19 22.05.2019 SS2019 44 Holtzman et al. (2006) ApJS, 166 SS2019 46 20 22.05.2019 2.3. The Population Box SS2019 47 with courtesy by SS2019 48 Eva Grebel SF continues also through the re-ion.epoch 21 22.05.2019 Grebel & Gallagher (2004) ApJ, 610 Most of the star formation in dSphs continued through the era of re- ionization: evidence for ionizationSS2019 inhomogeneity in the Universe!49 2.4. More distant satellites SS2019 50 22 22.05.2019 Gas-poor Dwarf Galaxies in the Local Group SS2019 Antlia51 DG 2.5. Satellites with gas Sculptur (Carignan 1996) Leo A Dwarf Galaxies (low masses) can easily expel all(?) their gas into their intergalactic environment. Gas is stripped off by tidal and dynamical drag, by this, transforming dIrrs into dEs SS2019 and dSphs(?). 52 23 22.05.2019 Carina II dIrr SS2019 53 SS2019 54 24 22.05.2019 IC 10, dIrr, Dist.: 1400 SS2019kpc, V = 10.3m 55 Leo A in the solar vicinity SS2019 56 25 22.05.2019 2.6. Gas in dSph‘s: almost gas free, but gas infall! Carignan et al. (1988) HI gas outside Sculptor dSph, Welsh et al. (1998) flocculent HVCs gas infall in NGC 205 enhances SF SS2019 57 (see also Bouchard et al. 2003, 2006) Gas displacement by tidal and ram-pressure effects Carignan 1999 HI gas displaced of Phoenix Welsh et al. (1998) SSGas2019 infall in NGC 205 enhances58 SF 26 22.05.2019 HI Environment? Carignan et al. (1998) Bouchard et al. (2003) AJ, 126 Gas clouds around Sculptor dSphs from expulsion? SS2019 59 The Satellites’ gas content Grcevich & Putman, 09, ApJ, 696 SS2019 60 27 22.05.2019 dIrrs of the MW show stronger and more continuous star formation with an increase of Z. Phoenix is in a stage of morphological transition. SS2019 61 SS2019 62 28 22.05.2019 NGC 147 2MASS 3. The M31 system NGC 205 NGC 185 BVR NGC 221 Star-formation regions in NGC 185 and NGC 205 of similar size as in dIrrs M32 NGC 205 SS2019 64 29 22.05.2019 And VII And VI 4. Detection of the Sagittarius Satellite Galaxy If no bright star-forming regions exist, the stellar component of satellite The Sagittarius Dwarf Galaxy SS2019 galaxies is hardly detectible66 at D 24 kpc due to their low brightness. 30 22.05.2019 4.1. Southwards of the MWG center a sample of stars was detected at a distance of 24 kpc due to their collective kinematics: Sgr I Dwarf Galaxy SS2019 67 SS2019 68 31 22.05.2019 SS2019 69 4.2. Satellite Accretion SS2019 70 32 22.05.2019 Computer model of a small satellite galaxy orbiting a larger (edge-on) disk galaxy. As the satellite orbits, stars are stripped from the satellite and orbit in the halo of the larger galaxy. (Kathryn Johnston): see the bending and tumbling of the satellite‘s figure axis! SS2019 71 The tidal stream of Sgr I is detected from enhanced star density. SS2019 72 33 22.05.2019 The tidal stream of Sgr DG is detected from enhanced star density. SS2019 73 SS2019 75 34 22.05.2019 4.3. The Canis Major Satellite Galaxy Canis Major DG discovered recently: 17/11/03, close to the galactic plane at 7.5 kpc distance SS2019 76 The Canis Major tidal Stream SS2019 77 35 22.05.2019 4.4. Tidal Streams Recent sensitive observations of galaxy halos have revealed tidal streamers of satellite galaxies under disruption in a few of them. In M31 HVCs accumulate along the tidal path. SS2019 78 Tidal streams around NGC 5907 SS2019 79 36 22.05.2019 4.5. Search for MW tidal streamers SS2019 80 Belokurov et al. (2007) ApJ, 658 SS2019 81 37 22.05.2019 Belokurov et al. (2007) ApJ, 658 SS2019 82 The Aquarius stellar stream SS2019 83 38 22.05.2019 SS2019 84 Satellites on elliptical orbits experience 1) stretching along the trajectory on their approach to perigalacticum and crushing along the orbit towards apogalacticum because of velocity differences between leading anf trailing part, 2) radial stretching due to the tidal force of the mature galaxy, 3) by this a revolving gravitational potential along the orbit (due to tidal torque), 4) an oscillating equipotential (:=SS 2019tidal radius) 85 that facilitates tidal stripping. 39 22.05.2019 Tidal Force Bodies that are extended over d and located at distance D in the central gravitational field of any mass M experience a Tidal Force d Ftide GM 3 D This results in a mode-2 deformation in radial direction towards and away from the center of mass. The detection of the leading arm confirms the tidal stripping effect. The stripped gas approachsSS2019 the MW disk. 86 Metz et al. (2008) ApJ, 680 SS2019 89 40 22.05.2019 5.2. Cosmological implications Satellite galaxies move in the tidal field and the halo gas of mature galaxies. Cosmological models predict numerous satellite galaxies around Hubble types. SS2019 90 SS2019 91 41 22.05.2019 The evolution for 2 Gyrs SS2019 92 Petrov & Hensler (2011) in prep. Interactions of Sat.s important; e.g. Satellites merge; Gas is removed from the Satellites And contributes to the Galactic halo gas: Small subhalos survive, but without gas! Large Satellites are tidally stretched and partly disrupted dSphs merge: Mass spectrum?SS2019 93 42 22.05.2019 5.3. Gas stripping SS2019 95 43 22.05.2019 SS2019 96 CDM models of Galaxy Stellar Halos Cosmological models based on CDM predict many accretion events through lifetime of a big galaxy. Infalling satellites are torn apart by tidal forces. SS2019 97 44 22.05.2019 4 major questions: 1. Is the Milky Way built-up of dSphs? 2. How did the dSphs evolve? 3. How did the dSphs gained their gas? 4. What does the dSphs distribution tell us? 98 6. Halo Stars by Satellite Accretion The chart above demonstrates the previous conclusions by showing the abundances of alpha elements in dSphs versus solar metallicity. The symbols are as follows: blue triangles, Carina blue triangles plus circles, Leo I red triangles, Sculptor red triangles plus circles, Fornax green triangles, Draco, Ursa Minor, and Sextans from SCS01 black crosses, Glactic disk stars open squares, halo data from McWilliam et al.
Recommended publications
  • A Revised View of the Canis Major Stellar Overdensity with Decam And
    MNRAS 501, 1690–1700 (2021) doi:10.1093/mnras/staa2655 Advance Access publication 2020 October 14 A revised view of the Canis Major stellar overdensity with DECam and Gaia: new evidence of a stellar warp of blue stars Downloaded from https://academic.oup.com/mnras/article/501/2/1690/5923573 by Consejo Superior de Investigaciones Cientificas (CSIC) user on 15 March 2021 Julio A. Carballo-Bello ,1‹ David Mart´ınez-Delgado,2 Jesus´ M. Corral-Santana ,3 Emilio J. Alfaro,2 Camila Navarrete,3,4 A. Katherina Vivas 5 and Marcio´ Catelan 4,6 1Instituto de Alta Investigacion,´ Universidad de Tarapaca,´ Casilla 7D, Arica, Chile 2Instituto de Astrof´ısica de Andaluc´ıa, CSIC, E-18080 Granada, Spain 3European Southern Observatory, Alonso de Cordova´ 3107, Casilla 19001, Santiago, Chile 4Millennium Institute of Astrophysics, Santiago, Chile 5Cerro Tololo Inter-American Observatory, NSF’s National Optical-Infrared Astronomy Research Laboratory, Casilla 603, La Serena, Chile 6Instituto de Astrof´ısica, Facultad de F´ısica, Pontificia Universidad Catolica´ de Chile, Av. Vicuna˜ Mackenna 4860, 782-0436 Macul, Santiago, Chile Accepted 2020 August 27. Received 2020 July 16; in original form 2020 February 24 ABSTRACT We present the Dark Energy Camera (DECam) imaging combined with Gaia Data Release 2 (DR2) data to study the Canis Major overdensity. The presence of the so-called Blue Plume stars in a low-pollution area of the colour–magnitude diagram allows us to derive the distance and proper motions of this stellar feature along the line of sight of its hypothetical core. The stellar overdensity extends on a large area of the sky at low Galactic latitudes, below the plane, and in the range 230◦ <<255◦.
    [Show full text]
  • The Milky Way's Disk of Classical Satellite Galaxies in Light of Gaia
    MNRAS 000,1{20 (2019) Preprint 14 November 2019 Compiled using MNRAS LATEX style file v3.0 The Milky Way's Disk of Classical Satellite Galaxies in Light of Gaia DR2 Marcel S. Pawlowski,1? and Pavel Kroupa2;3 1Leibniz-Institut fur¨ Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany 2Helmholtz-Institut fur¨ Strahlen- und Kernphysik, University of Bonn, Nussallee 14-16, D- 53115 Bonn, Germany 3Charles University in Prague, Faculty of Mathematics and Physics, Astronomical Institute, V Holeˇsoviˇck´ach 2, CZ-180 00 Praha 8, Czech Republic Accepted 2019 November 7. Received 2019 November 7; in original form 2019 August 26 ABSTRACT We study the correlation of orbital poles of the 11 classical satellite galaxies of the Milky Way, comparing results from previous proper motions with the independent data by Gaia DR2. Previous results on the degree of correlation and its significance are confirmed by the new data. A majority of the satellites co-orbit along the Vast Polar Structure, the plane (or disk) of satellite galaxies defined by their positions. The orbital planes of eight satellites align to < 20◦ with a common direction, seven even orbit in the same sense. Most also share similar specific angular momenta, though their wide distribution on the sky does not support a recent group infall or satellites- of-satellites origin. The orbital pole concentration has continuously increased as more precise proper motions were measured, as expected if the underlying distribution shows true correlation that is washed out by observational uncertainties. The orbital poles of the up to seven most correlated satellites are in fact almost as concentrated as expected for the best-possible orbital alignment achievable given the satellite posi- tions.
    [Show full text]
  • VI. Star-Forming Companions of Nearby Field Galaxies
    A&A 486, 131–142 (2008) Astronomy DOI: 10.1051/0004-6361:20079297 & c ESO 2008 Astrophysics The Hα Galaxy Survey VI. Star-forming companions of nearby field galaxies P. A. James1, J. O’Neill2, and N. S. Shane1,3 1 Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK e-mail: [email protected] 2 Wirral Grammar School for Girls, Heath Road, Bebington, Wirral CH63 3AF, UK 3 Planetary Science Group, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK Received 20 December 2007 / Accepted 5 May 2008 ABSTRACT Aims. We searched for star-forming satellite galaxies that are close enough to their parent galaxies to be considered analogues of the Magellanic Clouds. Methods. Our search technique relied on the detection of the satellites in continuum-subtracted narrow-band Hα imaging of the central galaxies, which removes most of the background and foreground line-of-sight companions, thus giving a high probability that we are detecting true satellites. The search was performed for 119 central galaxies at distances between 20 and 40 Mpc, although spatial incompleteness means that we have effectively searched 53 full satellite-containing volumes. Results. We find only 9 “probable” star-forming satellites, around 9 different central galaxies, and 2 more “possible” satellites. After incompleteness correction, this is equivalent to 0.17/0.21 satellites per central galaxy. This frequency is unchanged whether we consider all central galaxy types or just those of Hubble types S0a–Sc, i.e. only the more luminous and massive spiral types.
    [Show full text]
  • The Large Scale Universe As a Quasi Quantum White Hole
    International Astronomy and Astrophysics Research Journal 3(1): 22-42, 2021; Article no.IAARJ.66092 The Large Scale Universe as a Quasi Quantum White Hole U. V. S. Seshavatharam1*, Eugene Terry Tatum2 and S. Lakshminarayana3 1Honorary Faculty, I-SERVE, Survey no-42, Hitech city, Hyderabad-84,Telangana, India. 2760 Campbell Ln. Ste 106 #161, Bowling Green, KY, USA. 3Department of Nuclear Physics, Andhra University, Visakhapatnam-03, AP, India. Authors’ contributions This work was carried out in collaboration among all authors. Author UVSS designed the study, performed the statistical analysis, wrote the protocol, and wrote the first draft of the manuscript. Authors ETT and SL managed the analyses of the study. All authors read and approved the final manuscript. Article Information Editor(s): (1) Dr. David Garrison, University of Houston-Clear Lake, USA. (2) Professor. Hadia Hassan Selim, National Research Institute of Astronomy and Geophysics, Egypt. Reviewers: (1) Abhishek Kumar Singh, Magadh University, India. (2) Mohsen Lutephy, Azad Islamic university (IAU), Iran. (3) Sie Long Kek, Universiti Tun Hussein Onn Malaysia, Malaysia. (4) N.V.Krishna Prasad, GITAM University, India. (5) Maryam Roushan, University of Mazandaran, Iran. Complete Peer review History: http://www.sdiarticle4.com/review-history/66092 Received 17 January 2021 Original Research Article Accepted 23 March 2021 Published 01 April 2021 ABSTRACT We emphasize the point that, standard model of cosmology is basically a model of classical general relativity and it seems inevitable to have a revision with reference to quantum model of cosmology. Utmost important point to be noted is that, ‘Spin’ is a basic property of quantum mechanics and ‘rotation’ is a very common experience.
    [Show full text]
  • Afterschool Universe Session 9 Slide Notes: Galaxies
    This presentation supports the “Background” material in Session 9 of the Afterschool Universe program. This session is about galaxies. The picture shows the Whirlpool galaxy, a large, iconic, spiral galaxy. 1 Let us summarize the main concepts in this Session. We will discuss these in the rest of this presentation. 2 A galaxy is a huge collection of stars, gas and dust. A typical galaxy has about 100 billion stars (that’s 100,000,000,000 stars!), and light takes about 100,000 years to cross a galaxy (in other words, they are typically 100,000 light years ago). But some galaxies are much bigger and some are much smaller. 3 If you look at the sky from a DARK location, you can see a band of light stretching across the sky which is known as the Milky Way. This is our view of our Galaxy - more precisely, this is our view of the disk of our galaxy as seen from the INSIDE. 4 This picture shows another view of our galaxy taken in the infra-red part of the spectrum. The advantage of the infra-red is that it can penetrate the dust that pervades our galaxy’s disk and let us view the central parts of our galaxy. This picture also shows the full sky. The flat disk and central bulge of our galaxy can be seen in this picture. 5 We live in the suburbs of our galaxy. The Sun and its planetary system are about 25,000 light years from the center of the galaxy. This is about half way out to the edge of the disk.
    [Show full text]
  • Groups of Galaxies in the Nearby Universe Held in Santiago De Chile, 5–9 December 2006
    Report on the Conference on Groups of Galaxies in the Nearby Universe held in Santiago de Chile, 5–9 December 2006 Ivo Saviane, Valentin D. Ivanov, Jura Borissova (ESO) n Bi r 10 For every galaxy in the field or in clusters, pe p there are about three galaxies in groups. ou Therefore, the evolution of most galax- Gr r ies actually happens in groups. The Milky pe Way resides in a group, and groups can be found at high redshift. The current xies 1 generation of 10-m-class telescopes and Gala space facilities allows us to study mem- of bers of nearby groups with exquisite de- tail, and their properties can be corre- –1 Number L < 41.7 Log (erg s ) lated with the global properties of their x L > 41.7 Log (erg s–1) host group. Finally, groups are relevant x for cosmology, since they trace large- scale structures better than clusters, and –22 –20 –18 –16 –14 Absolute Magnitude (M ) the evolution of groups and clusters may B be related. Figure 1: Cumulative B-band luminosity function of Strangely, there are three times fewer pa- 25 GEMS groups of galaxies grouped into X-ray- bright and X-ray-faint categories, fitted with one or pers on groups of galaxies than on clus- two Schechter functions, respectively (Miles et ters of galaxies, as revealed by an ADS al. 2004, MNRAS 355, 785; presented by Raychaud- search. Organising this conference was a hury). Mergers could explain the bimodality of the way to focus the attention of the com- luminosity function of X-ray-faint groups.
    [Show full text]
  • Neutral Hydrogen in Local Group Dwarf Galaxies
    Neutral Hydrogen in Local Group Dwarf Galaxies Jana Grcevich Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2013 c 2013 Jana Grcevich All rights reserved ABSTRACT Neutral Hydrogen in Local Group Dwarfs Jana Grcevich The gas content of the faintest and lowest mass dwarf galaxies provide means to study the evolution of these unique objects. The evolutionary histories of low mass dwarf galaxies are interesting in their own right, but may also provide insight into fundamental cosmological problems. These include the nature of dark matter, the disagreement be- tween the number of observed Local Group dwarf galaxies and that predicted by ΛCDM, and the discrepancy between the observed census of baryonic matter in the Milky Way’s environment and theoretical predictions. This thesis explores these questions by studying the neutral hydrogen (HI) component of dwarf galaxies. First, limits on the HI mass of the ultra-faint dwarfs are presented, and the HI content of all Local Group dwarf galaxies is examined from an environmental standpoint. We find that those Local Group dwarfs within 270 kpc of a massive host galaxy are deficient in HI as compared to those at larger galactocentric distances. Ram- 4 3 pressure arguments are invoked, which suggest halo densities greater than 2-3 10− cm− × out to distances of at least 70 kpc, values which are consistent with theoretical models and suggest the halo may harbor a large fraction of the host galaxy’s baryons. We also find that accounting for the incompleteness of the dwarf galaxy count, known dwarf galaxies whose gas has been removed could have provided at most 2.1 108 M of HI gas to the Milky Way.
    [Show full text]
  • Print This Press Release
    PRESS RELEASE Released on March 16th, 2006 Deriving the shape of the Galactic stellar disc Based on the article “Outer structure of the Galactic warp and flare: explaining the Canis Major over- density”, by Momany et al. To be published in Astronomy & Astrophysics. This press release is issued as a collaboration with the Italian Institute for Astrophysics (INAF) and Astronomy & Astrophysics. While analysing the complex structure of the Milky Way, an international team of astronomers from Italy and the United Kingdom has recently derived the shape of the Galactic outer stellar disc, and provided the strongest evidence that, besides being warped, it is at least 70% more extended than previously thought. Their findings will be reported in an upcoming issue of Astronomy & Astrophysics, and is a new step in understanding the large-scale structure of our Galaxy. Using the 2MASS all-sky near infrared catalogue, Yazan Momany and his collaborators reconstructed the outer structure of the Galactic stellar disc, in particular, its warp. Their work will soon be published in Astronomy & Astrophysics. Observationally, the warp is a bending of the Galactic plane upwards in the first and second Galactic longitude quadrants (0<l<180 degrees) and downwards in the third and fourth quadrants (180<l<360 degrees). Although the origin of the warp remains unknown, this feature is seen to be a ubiquitous property of all spiral galaxies. As we are located inside the Galactic disc, it is difficult to unveil specific details of its shape. To appreciate a warped stellar disc one should, therefore, look at other galaxies. Figure 1 shows a good example of what a warped galaxy looks like.
    [Show full text]
  • How Do Central and Satellite Galaxies Quench? - Insights from Spatially Resolved Spectroscopy in the Manga Survey
    Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 11 September 2020 (MN LATEX style file v2.2) How do central and satellite galaxies quench? - Insights from spatially resolved spectroscopy in the MaNGA survey Asa F. L. Bluck1;2;∗, Roberto Maiolino1;2, Joanna M. Piotrowska1;2, James Trussler1;2, Sara L. Ellison3, Sebastian F. Sanchez´ 4, Mallory D. Thorp3, Hossen Teimoorinia5, Jorge Moreno6 & Christopher J. Conselice7 1 Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK 2 Cavendish Laboratory - Astrophysics Group, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UK 3 Department of Physics & Astronomy, University of Victoria, Finnerty Road, Victoria, British Columbia, V8P 1A1, Canada 4 Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, A. P. 70-264, C.P. 04510, Mexico, D.F., Mexico 5 NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada 6 Department of Physics and Astronomy, Pomona College, Claremont, CA 91711, USA 7 Centre for Astronomy and Particle Theory, University of Nottingham, University Park, Nottingham, NG7 2RD, UK ∗ Email: [email protected] 11 September 2020 ABSTRACT We investigate how star formation quenching proceeds within central and satellite galaxies using spatially resolved spectroscopy from the SDSS-IV MaNGA DR15. We adopt a com- plete sample of star formation rate surface densities (ΣSFR), derived in Bluck et al. (2020), to compute the distance at which each spaxel resides from the resolved star forming main sequence (ΣSFR − Σ∗ relation): ∆ΣSFR. We study galaxy radial profiles in ∆ΣSFR, and luminosity weighted stellar age (AgeL), split by a variety of intrinsic and environmental pa- rameters.
    [Show full text]
  • AAS Members Save on Annual Reviews Journals
    AAS Members Save on Annual Reviews Journals Annual Review of Astronomy and Astrophysics #1 JCR® Volume 50 • September 2012 • ISSN: 0066-4146 • ISBN: 978-0-8243-0950-2 • http://astro.annualreviews.org IMPACT FACTOR AAS Member Discounted Price: $62.30 (WORLDWIDE) Regular price: $89.00 (WORLDWIDE) RANKING Co-Editors: Sandra M. Faber, University of California, Santa Cruz and Ewine F. van Dishoeck, Sterrewacht Leiden Associate Editor: John Kormendy, University of Texas, Austin PLANNED TABLE OF CONTENTS AND AUTHORS (SUBJECT TO CHANGE): • Planet-Disk Interactions and Orbital Migration, W. Kley, R.P. Nelson • Adaptive Optics for Astronomy, Richard Davies, Markus Kasper • Pre-Supernova Evolution of Massive Single and Binary Stars, Norbert Langer • Advances in Submillimeter and Far-Infrared Detectors, Jonas Zmuidzinas • Ram-Pressure Stripping of Galaxy Gas, J.H. Van Gorkom • Collisionless Dissipation Processes in Astrophysical Plasma Turbulence, Stuart D. Bale • Relativistic Shocks, Anatoly Spitkovsky • Concensus Cosmology, John E. Carlstrom • Seeing Cosmology Grow, P.J.E. Peebles • Connecting Galactic Star Formation on Global and Local Scales, Robert C. Kennicutt • Solar Magnetic Field, Alan Title • Dynamical Evolution and Resonances of Planetary Systems, Gregory P. Laughlin • Solar Neutrinos, Wick C. Haxton • Formation of Galaxy Clusters, Andrey Kravtsov • Subpopulations in Globular Clusters, Giampaolo Piotto • Galactic Stellar Populations in the Era of Large Surveys, Željko Ivezic • Supermassive Black Holes in the HST Era, John Kormendy • High Redshift Galaxy Evolution, Garth Illingworth • The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs, • Large-Scale Heliosphere, Ed Stone Kevin L. Luhman • Magnetic Fields in Molecular Clouds, Richard M. Crutcher • The Gaseous Galactic Halo, M. Putman, Joshua E.G.
    [Show full text]
  • Commission H1 Annual Report (2019)
    COMMISSION H1 THE LOCAL UNIVERSE (L’UNIVERS LOCAL) PRESIDENT Dante Minniti VICE-PRESIDENT Grazina Tautvaisiene PAST PRESIDENT Eva K. Grebel SECRETARY Aoki Wako ORGANIZING COMMITTEE Evangelie Athanassoula, John Beckman, Maria-Rosa Cioni, Yasuo Fukui, Eva K. Grebel, Margaret Meixner, Dante Minniti, Grazina Tautvaisiene, Aoki Wako, Gang Zhao ANNUAL SUMMARY REPORT 2019 1. Introduction The IAU Commission H1 on “The Local Universe (L'Univers Local)” is one of the three commissions of Division H, “Interstellar Matter and Local Universe”. This Commission H1 was established in mid-2015, and it was presided by Eva Grebel (Germany) during its first triennial period. IAU Commission H1 presently counts with 331 members. Our Commission focuses on studies of the Milky Way and nearby galaxies, where we can resolve galaxies into stars. A range of observational and theoretical research on the stellar populations, interstellar medium, dark matter of local galaxies, etc. are covered in order to understand galaxy formation, history and evolution. Recent and future photometric, spectroscopic, and astrometric surveys (both ground-based and space- based) contribute to the knowledge revolution that this field is experiencing. Current and forthcoming facilities will yield an even deeper understanding of our local Universe. 2. Activities 2019 This past year 2019 organizing committee members attended several international meetings and workshops worldwide, representing the IAU and giving invited/contributed talks and posters. Among the major developments on the area of Milky Way and Nearby galaxies that occurred during the year 2019, we can mention as examples the data releases and important publications from the following large surveys (in random order, incomplete list): * Astrometry - Continuing research on the Gaia DR2 released on April 2018 yielding a number of publications.
    [Show full text]
  • Discovery of a Dwarf Spheroidal Galaxy Behind the Andromeda Galaxy
    Mirach’s Goblin: Discovery of a dwarf spheroidal galaxy behind the Andromeda galaxy David Martínez-Delgado, Eva Grebel, Behnam Javanmardi, Walter Boschin, Nicolas Longeard, Julio Carballo-Bello, Dmitry Makarov, Michael Beasley, Giuseppe Donatiello, Martha Haynes, et al. To cite this version: David Martínez-Delgado, Eva Grebel, Behnam Javanmardi, Walter Boschin, Nicolas Longeard, et al.. Mirach’s Goblin: Discovery of a dwarf spheroidal galaxy behind the Andromeda galaxy. Astronomy and Astrophysics - A&A, EDP Sciences, 2018, 620, pp.A126. 10.1051/0004-6361/201833302. hal- 03152563 HAL Id: hal-03152563 https://hal.archives-ouvertes.fr/hal-03152563 Submitted on 27 Feb 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. A&A 620, A126 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833302 & c ESO 2018 Astrophysics Mirach’s Goblin: Discovery of a dwarf spheroidal galaxy behind the Andromeda galaxy David Martínez-Delgado1, Eva K. Grebel1, Behnam Javanmardi2, Walter Boschin3,4,5 , Nicolas Longeard6, Julio A. Carballo-Bello7, Dmitry Makarov8, Michael A. Beasley4,5, Giuseppe Donatiello9, Martha P. Haynes10, Duncan A. Forbes11, and Aaron J. Romanowsky12,13 1 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr.
    [Show full text]