STELLAR VELOCITY DISPERSION of the LEO a DWARF GALAXY Warren R
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Distances to Local Group Galaxies
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Distances to Local Group Galaxies Alistair R. Walker Cerro Tololo Inter-American Observatory, NOAO, Casilla 603, la Serena, Chile Abstract. Distances to galaxies in the Local Group are reviewed. In particular, the distance to the Large Magellanic Cloud is found to be (m M)0 =18:52 0:10, cor- − ± responding to 50; 600 2; 400 pc. The importance of M31 as an analog of the galaxies observed at greater distances± is stressed, while the variety of star formation and chem- ical enrichment histories displayed by Local Group galaxies allows critical evaluation of the calibrations of the various distance indicators in a variety of environments. 1 Introduction The Local Group (hereafter LG) of galaxies has been comprehensively described in the monograph by Sidney van den Berg [1], with update in [2]. The zero- velocity surface has radius of a little more than 1 Mpc, therefore the small sub-group of galaxies consisting of NGC 3109, Antlia, Sextans A and Sextans B lie outside the the LG by this definition, as do galaxies in the direction of the nearby Sculptor and IC342/Maffei groups. Thus the LG consists of two large spirals (the Galaxy and M31) each with their entourage of 11 and 10 smaller galaxies respectively, the dwarf spiral M33, and 13 other galaxies classified as either irregular or spherical. We have here included NGC 147 and NGC 185 as members of the M31 sub-group [60], whether they are actually bound to M31 is not proven. -
Distribution of Phantom Dark Matter in Dwarf Spheroidals Alistair O
A&A 640, A26 (2020) Astronomy https://doi.org/10.1051/0004-6361/202037634 & c ESO 2020 Astrophysics Distribution of phantom dark matter in dwarf spheroidals Alistair O. Hodson1,2, Antonaldo Diaferio1,2, and Luisa Ostorero1,2 1 Dipartimento di Fisica, Università di Torino, Via P. Giuria 1, 10125 Torino, Italy 2 Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy e-mail: [email protected],[email protected] Received 31 January 2020 / Accepted 25 May 2020 ABSTRACT We derive the distribution of the phantom dark matter in the eight classical dwarf galaxies surrounding the Milky Way, under the assumption that modified Newtonian dynamics (MOND) is the correct theory of gravity. According to their observed shape, we model the dwarfs as axisymmetric systems, rather than spherical systems, as usually assumed. In addition, as required by the assumption of the MOND framework, we realistically include the external gravitational field of the Milky Way and of the large-scale structure beyond the Local Group. For the dwarfs where the external field dominates over the internal gravitational field, the phantom dark matter has, from the star distribution, an offset of ∼0:1−0:2 kpc, depending on the mass-to-light ratio adopted. This offset is a substantial fraction of the dwarf half-mass radius. For Sculptor and Fornax, where the internal and external gravitational fields are comparable, the phantom dark matter distribution appears disturbed with spikes at the locations where the two fields cancel each other; these features have little connection with the distribution of the stars within the dwarfs. -
The Feeble Giant. Discovery of a Large and Diffuse Milky Way Dwarf Galaxy in the Constellation of Crater
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Apollo MNRAS 459, 2370–2378 (2016) doi:10.1093/mnras/stw733 Advance Access publication 2016 April 13 The feeble giant. Discovery of a large and diffuse Milky Way dwarf galaxy in the constellation of Crater G. Torrealba,‹ S. E. Koposov, V. Belokurov and M. Irwin Institute of Astronomy, Madingley Rd, Cambridge CB3 0HA, UK Downloaded from https://academic.oup.com/mnras/article-abstract/459/3/2370/2595158 by University of Cambridge user on 24 July 2019 Accepted 2016 March 24. Received 2016 March 24; in original form 2016 January 26 ABSTRACT We announce the discovery of the Crater 2 dwarf galaxy, identified in imaging data of the VLT Survey Telescope ATLAS survey. Given its half-light radius of ∼1100 pc, Crater 2 is the fourth largest satellite of the Milky Way, surpassed only by the Large Magellanic Cloud, Small Magellanic Cloud and the Sgr dwarf. With a total luminosity of MV ≈−8, this galaxy is also one of the lowest surface brightness dwarfs. Falling under the nominal detection boundary of 30 mag arcsec−2, it compares in nebulosity to the recently discovered Tuc 2 and Tuc IV and UMa II. Crater 2 is located ∼120 kpc from the Sun and appears to be aligned in 3D with the enigmatic globular cluster Crater, the pair of ultrafaint dwarfs Leo IV and Leo V and the classical dwarf Leo II. We argue that such arrangement is probably not accidental and, in fact, can be viewed as the evidence for the accretion of the Crater-Leo group. -
The Extragalactic Distance Scale
The Extragalactic Distance Scale Published in "Stellar astrophysics for the local group" : VIII Canary Islands Winter School of Astrophysics. Edited by A. Aparicio, A. Herrero, and F. Sanchez. Cambridge ; New York : Cambridge University Press, 1998 Calibration of the Extragalactic Distance Scale By BARRY F. MADORE1, WENDY L. FREEDMAN2 1NASA/IPAC Extragalactic Database, Infrared Processing & Analysis Center, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA 2Observatories, Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena CA 91101, USA The calibration and use of Cepheids as primary distance indicators is reviewed in the context of the extragalactic distance scale. Comparison is made with the independently calibrated Population II distance scale and found to be consistent at the 10% level. The combined use of ground-based facilities and the Hubble Space Telescope now allow for the application of the Cepheid Period-Luminosity relation out to distances in excess of 20 Mpc. Calibration of secondary distance indicators and the direct determination of distances to galaxies in the field as well as in the Virgo and Fornax clusters allows for multiple paths to the determination of the absolute rate of the expansion of the Universe parameterized by the Hubble constant. At this point in the reduction and analysis of Key Project galaxies H0 = 72km/ sec/Mpc ± 2 (random) ± 12 [systematic]. Table of Contents INTRODUCTION TO THE LECTURES CEPHEIDS BRIEF SUMMARY OF THE OBSERVED PROPERTIES OF CEPHEID -
What Is an Ultra-Faint Galaxy?
What is an ultra-faint Galaxy? UCSB KITP Feb 16 2012 Beth Willman (Haverford College) ~ 1/10 Milky Way luminosity Large Magellanic Cloud, MV = -18 image credit: Yuri Beletsky (ESO) and APOD NGC 205, MV = -16.4 ~ 1/40 Milky Way luminosity image credit: www.noao.edu Image credit: David W. Hogg, Michael R. Blanton, and the Sloan Digital Sky Survey Collaboration ~ 1/300 Milky Way luminosity MV = -14.2 Image credit: David W. Hogg, Michael R. Blanton, and the Sloan Digital Sky Survey Collaboration ~ 1/2700 Milky Way luminosity MV = -11.9 Image credit: David W. Hogg, Michael R. Blanton, and the Sloan Digital Sky Survey Collaboration ~ 1/14,000 Milky Way luminosity MV = -10.1 ~ 1/40,000 Milky Way luminosity ~ 1/1,000,000 Milky Way luminosity Ursa Major 1 Finding Invisible Galaxies bright faint blue red Willman et al 2002, Walsh, Willman & Jerjen 2009; see also e.g. Koposov et al 2008, Belokurov et al. Finding Invisible Galaxies Red, bright, cool bright Blue, hot, bright V-band apparent brightness V-band faint Red, faint, cool blue red From ARAA, V26, 1988 Willman et al 2002, Walsh, Willman & Jerjen 2009; see also e.g. Koposov et al 2008, Belokurov et al. Finding Invisible Galaxies Ursa Major I dwarf 1/1,000,000 MW luminosity Willman et al 2005 ~ 1/1,000,000 Milky Way luminosity Ursa Major 1 CMD of Ursa Major I Okamoto et al 2008 Distribution of the Milky Wayʼs dwarfs -14 Milky Way dwarfs 107 -12 -10 classical dwarfs V -8 5 10 Sun M L -6 ultra-faint dwarfs Canes Venatici II -4 Leo V Pisces II Willman I 1000 -2 Segue I 0 50 100 150 200 250 300 -
Is There Tension Between Observed Small Scale Structure and Cold Dark Matter?
Is there tension between observed small scale structure and cold dark matter? Louis Strigari Stanford University Cosmic Frontier 2013 March 8, 2013 Predictions of the standard Cold Dark Matter model 26 3 1 1. Density profiles rise towards the centersσannv 3of 10galaxies− cm s− (1) h i' ⇥ ⇢ Universal for all halo masses ⇢(r)= s (2) (r/r )(1 + r/r )2 Navarro-Frenk-White (NFW) model s s 2. Abundance of ‘sub-structure’ (sub-halos) in galaxies Sub-halos comprise few percent of total halo mass Most of mass contained in highest- mass sub-halos Subhalo Mass Function Mass[Solar mass] 1 Problems with the standard Cold Dark Matter model 1. Density of dark matter halos: Faint, dark matter-dominated galaxies appear less dense that predicted in simulations General arguments: Kleyna et al. MNRAS 2003, 2004;Goerdt et al. APJ2006; de Blok et al. AJ 2008 Dwarf spheroidals: Gilmore et al. APJ 2007; Walker & Penarrubia et al. APJ 2011; Angello & Evans APJ 2012 2. ‘Missing satellites problem’: Simulations have more dark matter subhalos than there are observed dwarf satellite galaxies Earilest papers: Kauffmann et al. 1993; Klypin et al. 1999; Moore et al. 1999 Solutions to the issues in Cold Dark Matter 1. The theory is wrong i) Not enough physics in theory/simulations (Talks yesterday by M. Boylan-Kolchin, M. Kuhlen) [Wadepuhl & Springel MNRAS 2011; Parry et al. MRNAS 2011; Pontzen & Governato MRNAS 2012; Brooks et al. ApJ 2012] ii) Cosmology/dark matter is wrong (Talk yesterday by A. Peter) 2. The data is wrong i) Kinematics of dwarf spheroidals (dSphs) are more difficult than assumed ii) Counting satellites a) Many more faint satellites around the Milky Way b) Milky Way is an oddball [Liu et al. -
Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Andrew Lipnicky [email protected]
Rochester Institute of Technology RIT Scholar Works Theses Thesis/Dissertation Collections 7-2017 Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Andrew Lipnicky [email protected] Follow this and additional works at: http://scholarworks.rit.edu/theses Recommended Citation Lipnicky, Andrew, "Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far" (2017). Thesis. Rochester Institute of Technology. Accessed from This Dissertation is brought to you for free and open access by the Thesis/Dissertation Collections at RIT Scholar Works. It has been accepted for inclusion in Theses by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. R I T · · Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Andrew Lipnicky A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology in the College of Science, School of Physics and Astronomy Rochester Institute of Technology © A. Lipnicky July, 2017 Rochester Institute of Technology Ph.D. Dissertation Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Author: Advisor: Andrew Lipnicky Dr. Sukanya Chakrabarti A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology in the College of Science, School of Physics and Astronomy Approved by Dr.AndrewRobinson Date Director, Astrophysical Sciences and Technology Certificate of Approval Astrophysical Sciences and Technology R I T College of Science · · Rochester, NY, USA The Ph.D. Dissertation of Andrew Lipnicky has been approved by the undersigned members of the dissertation committee as satisfactory for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology. -
HST-ACS Photometry of the Isolated Dwarf Galaxy VV124=UGC 4879
A&A 533, A37 (2011) Astronomy DOI: 10.1051/0004-6361/201117275 & c ESO 2011 Astrophysics HST-ACS photometry of the isolated dwarf galaxy VV124=UGC 4879 Detection of the blue horizontal branch and identification of two young star clusters, M. Bellazzini1,S.Perina1, S. Galleti1, and T. Oosterloo2 1 INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: [email protected] 2 Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands Received 17 May 2011 / Accepted 9 July 2011 ABSTRACT We present deep V and I photometry of the isolated dwarf galaxy VV124=UGC 4879, obtained from archival images taken with the Hubble Space Telescope – Advanced Camera for Surveys. In the color-magnitude diagrams of stars at distances greater than 40 from the center of the galaxy, we clearly identify a well-populated, old horizontal branch (HB) for the first time. We show that the distribution of these stars is more extended than that of red clump stars. This implies that very old and metal-poor populations 4 dominate in the outskirts of VV124. We also identify a massive (M = 1.2 ± 0.2 × 10 M) young (age = 250 ± 50 Myr) star cluster 3 (C1), as well as another of younger age (C2, ∼<30 ± 10 Myr) with a mass similar to classical open clusters (M ≤ 3.3 ± 0.5 × 10 M). Both clusters lie at projected distances less than 100 pc from the center of the galaxy. -
The Evening Sky
I N E D R I A C A S T N E O D I T A C L E O R N I G D S T S H A E P H M O O R C I . Z N O e d b l A a r , a l n e O , g N i C R a , Z p s e u I l i C l r a i , R I S C f R a O o s C t p H o L u r E e E & d H P a ( o T F m l O l s u i D R NORTH x ” , N M n E a A o n O X g d A H a x C P M T e r . I o P Polaris H N c S L r y E E e o P Z t n “ n E . EQUATORIAL EDITION i A N H O W T M “ R e T Y N H h E T ” K E ) W S . T T E U W B R N The Evening Sky Map W D E T T . FEBRUARY 2011 WH r A e E C t M82 FREE* EACH MONTH FOR YOU TO EXPLORE, LEARN & ENJOY THE NIGHT SKY O s S L u K l T Y c E CASSIOPEIA h R e r M a A S t A SKY MAP SHOWS HOW i s η M81 Get Sky Calendar on Twitter S P c T s k C A l e e E CAMELOPARDALIS R d J Sky Calendar – February 2011 a O http://twitter.com/skymaps i THE NIGHT SKY LOOKS s B y U O a H N L s D e t A h NE a I t I EARLY FEB 9 PM r T T f S p 1 Moon near Mercury (16° from Sun, morning sky) at 17h UT. -
METALLICITY DISTRIBUTION FUNCTIONS of FOUR LOCAL GROUP DWARF GALAXIES* Teresa L
The Astronomical Journal, 149:198 (14pp), 2015 June doi:10.1088/0004-6256/149/6/198 © 2015. The American Astronomical Society. All rights reserved. METALLICITY DISTRIBUTION FUNCTIONS OF FOUR LOCAL GROUP DWARF GALAXIES* Teresa L. Ross1, Jon Holtzman1, Abhijit Saha2, and Barbara J. Anthony-Twarog3 1 Department of Astronomy, New Mexico State University, P.O. Box 30001, MSC 4500, Las Cruces, NM 88003-8001, USA; [email protected], [email protected] 2 NOAO, 950 Cherry Avenue, Tucson, AZ 85726-6732, USA 3 Department of Physics and Astronomy, University of Kansas, Lawrence, KS 66045-7582, USA; [email protected] Received 2015 January 26; accepted 2015 April 16; published 2015 May 27 ABSTRACT We present stellar metallicities in Leo I, Leo II, IC 1613, and Phoenix dwarf galaxies derived from medium (F390M) and broad (F555W, F814W) band photometry using the Wide Field Camera 3 instrument on board the Hubble Space Telescope. We measured metallicity distribution functions (MDFs) in two ways, (1) matching stars to isochrones in color–color diagrams and (2) solving for the best linear combination of synthetic populations to match the observed color–color diagram. The synthetic technique reduces the effect of photometric scatter and produces MDFs 30%–50% narrower than the MDFs produced from individually matched stars. We fit the synthetic and individual MDFs to analytical chemical evolution models (CEMs) to quantify the enrichment and the effect of gas flows within the galaxies. Additionally, we measure stellar metallicity gradients in Leo I and II. For IC 1613 and Phoenix our data do not have the radial extent to confirm a metallicity gradient for either galaxy. -
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. -
First Stellar Spectroscopy in Leo P
LJMU Research Online Evans, CJ, Castro, N, Gonzalez, OA, Garcia, M, Bastian, N, Cioni, M-RL, Clark, JS, Davies, B, Ferguson, AMN, Kamann, S, Lennon, DJ, Patrick, LR, Vink, JS and Weisz, DR First stellar spectroscopy in Leo P http://researchonline.ljmu.ac.uk/id/eprint/10138/ Article Citation (please note it is advisable to refer to the publisher’s version if you intend to cite from this work) Evans, CJ, Castro, N, Gonzalez, OA, Garcia, M, Bastian, N, Cioni, M-RL, Clark, JS, Davies, B, Ferguson, AMN, Kamann, S, Lennon, DJ, Patrick, LR, Vink, JS and Weisz, DR (2019) First stellar spectroscopy in Leo P. Astronomy and Astrophysics, 622. ISSN 0004-6361 LJMU has developed LJMU Research Online for users to access the research output of the University more effectively. Copyright © and Moral Rights for the papers on this site are retained by the individual authors and/or other copyright owners. Users may download and/or print one copy of any article(s) in LJMU Research Online to facilitate their private study or for non-commercial research. You may not engage in further distribution of the material or use it for any profit-making activities or any commercial gain. The version presented here may differ from the published version or from the version of the record. Please see the repository URL above for details on accessing the published version and note that access may require a subscription. For more information please contact [email protected] http://researchonline.ljmu.ac.uk/ A&A 622, A129 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834145 & c ESO 2019 Astrophysics First stellar spectroscopy in Leo P C.