HST-ACS Photometry of the Isolated Dwarf Galaxy VV124=UGC 4879
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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. -
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 -
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. -
An Observer's Guide to the (Local Group) Dwarf Galaxies: Predictions for Their Own Dwarf Satellite Populations
An observer's guide to the (Local Group) dwarf galaxies: predictions for their own dwarf satellite populations The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Dooley, Gregory A. et al. “An Observer’s Guide to the (Local Group) Dwarf Galaxies: Predictions for Their Own Dwarf Satellite Populations.” Monthly Notices of the Royal Astronomical Society 471, 4 (August 2017): 4894–4909 © 2018 The Author(s) As Published http://dx.doi.org/10.1093/MNRAS/STX1900 Publisher Oxford University Press (OUP) Version Author's final manuscript Citable link https://hdl.handle.net/1721.1/121369 Terms of Use Creative Commons Attribution-Noncommercial-Share Alike Detailed Terms http://creativecommons.org/licenses/by-nc-sa/4.0/ MNRAS 000,1{21 (2017) Preprint 6 September 2017 Compiled using MNRAS LATEX style file v3.0 An observer's guide to the (Local Group) dwarf galaxies: predictions for their own dwarf satellite populations Gregory A. Dooley1?, Annika H. G. Peter2;3, Tianyi Yang4, Beth Willman5, Brendan F. Griffen1 and Anna Frebel1, 1Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 2CCAPP and Department of Physics, The Ohio State University, Columbus, OH 43210, USA 3Department of Astronomy, The Ohio State University, Columbus OH 43210, USA 4Institute of Optics, University of Rochester, Rochester, New York, 14627, USA 5Steward Observatory and LSST, 933 North Cherry Avenue, Tucson, AZ 85721, USA Accepted by MNRAS 2017 July 22. Received 2017 July 22; in original 2016 September 27 ABSTRACT A recent surge in the discovery of new ultrafaint dwarf satellites of the Milky Way has 3 6 inspired the idea of searching for faint satellites, 10 M < M∗ < 10 M , around less massive field galaxies in the Local Group. -
Draft181 182Chapter 10
Chapter 10 Formation and evolution of the Local Group 480 Myr <t< 13.7 Gyr; 10 >z> 0; 30 K > T > 2.725 K The fact that the [G]alactic system is a member of a group is a very fortunate accident. Edwin Hubble, The Realm of the Nebulae Summary: The Local Group (LG) is the group of galaxies gravitationally associ- ated with the Galaxy and M 31. Galaxies within the LG have overcome the general expansion of the universe. There are approximately 75 galaxies in the LG within a 12 diameter of ∼3 Mpc having a total mass of 2-5 × 10 M⊙. A strong morphology- density relation exists in which gas-poor dwarf spheroidals (dSphs) are preferentially found closer to the Galaxy/M 31 than gas-rich dwarf irregulars (dIrrs). This is often promoted as evidence of environmental processes due to the massive Galaxy and M 31 driving the evolutionary change between dwarf galaxy types. High Veloc- ity Clouds (HVCs) are likely to be either remnant gas left over from the formation of the Galaxy, or associated with other galaxies that have been tidally disturbed by the Galaxy. Our Galaxy halo is about 12 Gyr old. A thin disk with ongoing star formation and older thick disk built by z ≥ 2 minor mergers exist. The Galaxy and M 31 will merge in 5.9 Gyr and ultimately resemble an elliptical galaxy. The LG has −1 vLG = 627 ± 22 km s with respect to the CMB. About 44% of the LG motion is due to the infall into the region of the Great Attractor, and the remaining amount of motion is due to more distant overdensities between 130 and 180 h−1 Mpc, primarily the Shapley supercluster. -
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. -
The Rotation of the Halo of NGC6822 Determined from the Radial Velocities of Carbon Stars
The rotation of the halo of NGC6822 determined from the radial velocities of carbon stars { Graham Peter Thompson { Centre for Astrophysics Research School of Physics, Astronomy and Mathematics University of Hertfordshire Submitted to the University of Hertfordshire in part fulfilment of the requirements of the degree of Master of Philosophy in Astrophysics Supervisor: Professor Sean G. Ryan { April 2016 { Declaration I hereby certify that this dissertation has been written by me in the School of Physics, Astronomy and Mathematics, University of Hertfordshire, Hatfield, Hertfordshire, and that it has not been submitted in any previous application for a higher degree. The core of the dissertation is based on original work conducted at the University of Hertfordshire, and some of the ideas for further work are drawn from topics studied during an earlier Master of Science. All material in this dissertation which is not my own work has been properly acknowledged. { Graham Peter Thompson { ii Acknowledgements I thank Professor Ryan for his invaluable support and patient guidance as my super- visor, throughout this study. His incisive questioning, thoughtful comments, helpful suggestions and, at times, hands-on assistance throughout the study, preparation of a paper to MNRAS and the writing of this dissertation have been invaluable. I thank also Dr Lisette Sibbons, whose work on the spectral classification of carbon stars in NGC 6822 was the genesis of my study. Dr Sibbons was responsible for the acquisition and reduction of the spectra I used in the study. She also provided me with background information related to the stars in the sample, and general advice. -
Perseus I and the NGC 3109 Association in the Context of the Local Group Dwarf Galaxy Structures
MNRAS 440, 908–919 (2014) doi:10.1093/mnras/stu321 Advance Access publication 2014 March 15 Perseus I and the NGC 3109 association in the context of the Local Group dwarf galaxy structures Marcel S. Pawlowski‹ and Stacy S. McGaugh Department of Astronomy, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, OH 44106, USA Accepted 2014 February 13. Received 2014 February 13; in original form 2014 January 8 ABSTRACT The recently discovered dwarf galaxy Perseus I appears to be associated with the dominant Downloaded from plane of non-satellite galaxies in the Local Group (LG). We predict its velocity dispersion and those of the other isolated dwarf spheroidals Cetus and Tucana to be 6.5, 8.2 and 5.5 km s−1, respectively. The NGC 3109 association, including the recently discovered dwarf galaxy Leo P, aligns with the dwarf galaxy structures in the LG such that all known nearby non-satellite http://mnras.oxfordjournals.org/ galaxies in the northern Galactic hemisphere lie in a common thin plane (rms height 53 kpc; diameter 1.2 Mpc). This plane has an orientation similar to the preferred orbital plane of the Milky Way (MW) satellites in the vast polar structure. Five of seven of these northern galaxies were identified as possible backsplash objects, even though only about one is expected from cosmological simulations. This may pose a problem, or instead the search for local backsplash galaxies might be identifying ancient tidal dwarf galaxies expelled in a past major galaxy encounter. The NGC 3109 association supports the notion that material preferentially falls towards the MW from the Galactic south and recedes towards the north, as if the MW were moving through a stream of dwarf galaxies. -
The Local Group As a Time Machine: Studying the High-Redshift Universe with Nearby Galaxies
Mon. Not. R. Astron. Soc. 000,1{11 (2015) Printed 1 October 2018 (MN LATEX style file v2.2) The Local Group as a time machine: studying the high-redshift Universe with nearby galaxies Michael Boylan-Kolchin1?, Daniel R. Weisz2y, Benjamin D. Johnson3, James S. Bullock4, Charlie Conroy3, Alex Fitts1 1Department of Astronomy and Joint Space-Science Institute, University of Maryland, College Park, MD 20742-2421, USA 2Astronomy Department, Box 351580, University of Washington, Seattle, WA, USA 3Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge MA 02138, USA 4Department of Physics and Astronomy, University of California at Irvine, Irvine, CA 92697, USA 1 October 2018 ABSTRACT We infer the UV luminosities of Local Group galaxies at early cosmic times (z ∼ 2 and z ∼ 7) by combining stellar population synthesis modeling with star formation histories derived from deep color-magnitude diagrams constructed from Hubble Space Telescope (HST ) observations. Our analysis provides a basis for understanding high-z galaxies { including those that may be unobservable even with the James Webb Space Telescope (JWST ) { in the context of familiar, well-studied objects in the very low-z Universe. We find that, at the epoch of reionization, all Local Group dwarfs were less luminous than the faintest galaxies detectable in deep HST observations of blank fields. We predict that JWST will observe z ∼ 7 progenitors of galaxies similar to the Large Magellanic Cloud today; however, the HST Frontier Fields initiative may already be observing such galaxies, highlighting the power of gravitational lensing. Consensus reionization models require an extrapolation of the observed blank-field luminosity function at z ≈ 7 by at least two orders of magnitude in order to maintain reionization. -
The Milky Way the Milky Way's Neighbourhood
The Milky Way What Is The Milky Way Galaxy? The.Milky.Way.is.the.galaxy.we.live.in..It.contains.the.Sun.and.at.least.one.hundred.billion.other.stars..Some.modern. measurements.suggest.there.may.be.up.to.500.billion.stars.in.the.galaxy..The.Milky.Way.also.contains.more.than.a.billion. solar.masses’.worth.of.free-floating.clouds.of.interstellar.gas.sprinkled.with.dust,.and.several.hundred.star.clusters.that. contain.anywhere.from.a.few.hundred.to.a.few.million.stars.each. What Kind Of Galaxy Is The Milky Way? Figuring.out.the.shape.of.the.Milky.Way.is,.for.us,.somewhat.like.a.fish.trying.to.figure.out.the.shape.of.the.ocean.. Based.on.careful.observations.and.calculations,.though,.it.appears.that.the.Milky.Way.is.a.barred.spiral.galaxy,.probably. classified.as.a.SBb.or.SBc.on.the.Hubble.tuning.fork.diagram. Where Is The Milky Way In Our Universe’! The.Milky.Way.sits.on.the.outskirts.of.the.Virgo.supercluster..(The.centre.of.the.Virgo.cluster,.the.largest.concentrated. collection.of.matter.in.the.supercluster,.is.about.50.million.light-years.away.).In.a.larger.sense,.the.Milky.Way.is.at.the. centre.of.the.observable.universe..This.is.of.course.nothing.special,.since,.on.the.largest.size.scales,.every.point.in.space. is.expanding.away.from.every.other.point;.every.object.in.the.cosmos.is.at.the.centre.of.its.own.observable.universe.. Within The Milky Way Galaxy, Where Is Earth Located’? Earth.orbits.the.Sun,.which.is.situated.in.the.Orion.Arm,.one.of.the.Milky.Way’s.66.spiral.arms..(Even.though.the.spiral. -
Abundance Determinations in the Dirr Galaxy Leo A
Dwarf Galaxies: From the Deep Universe to the Present Proceedings IAU Symposium No. 344, 2019 c International Astronomical Union 2019 K. B. W. McQuinn & S. Stierwalt, eds. doi:10.1017/S1743921318005252 Abundance determinations in the dIrr galaxy Leo A Francisco Ruiz-Escobedo1, Miriam Pe˜na1, Liliana Hern´andez-Mart´ınez2 and Jorge Garc´ıa-Rojas3 1Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico Apdo. Postal 70264, Ciudad de M´exico, 04510, M´exico email: fdruiz,[email protected] 2Instituto de Ciencias Nucleares, Universidad Nacional Aut´onoma de M´exico, Apdo. Postal 70543, Ciudad de M´exico, 04510, M´exico email: [email protected] 3Instituto de Astrof´ısica de Canarias (IAC), E-38200; Universidad de La Laguna, Dept. Astrof´ısica. E-38206, La Laguna, Tenerife, Spain email: [email protected] Abstract. Physical conditions and chemical abundances of two H II regions and a planetary nebula in the dIrr galaxy Leo A are presented. These determinations were performed using the direct method (Te measured) and the ONS method. We also constructed photoionization models for the three nebulae to determine the abundances and to analyse the ionizing stars. The O abundance was determined to be 12+log(O/H) = 7.4 ± 0.2 in all cases. Keywords. galaxies: irregulars, galaxies : individual (Leo A), galaxies: ISM, ISM: abundances, planetary nebulae: general 1. Introduction Dwarf Irregular galaxies (dIrr) are low-mass, gas-rich, low-metallicity systems and seem to be dominated by dark matter. These galaxies are considered the building blocks of large-scale galaxies. The study of the ISM abundances of these galaxies, derived from H II regions and planetary nebulae, allow us to infer their chemical evolution (Hern´andez- Mart´ınez et al. -
An Arecibo 327 Mhz Search for Radio Pulsars and Bursts in the Dwarf Irregular Galaxies Leo a and T Fronefield Crawford 1 and Kohei Hayashi 2, 3
Draft version June 18, 2021 Typeset using LATEX RNAAS style in AASTeX63 An Arecibo 327 MHz Search for Radio Pulsars and Bursts in the Dwarf Irregular Galaxies Leo A and T Fronefield Crawford 1 and Kohei Hayashi 2, 3 1Department of Physics and Astronomy, Franklin and Marshall College, P.O. Box 3003, Lancaster, PA 17604, USA 2Astronomical Institute, Tohoku University, Sendai, Miyagi, 980-8578, Japan 3National Institute of Technology, Ichinoseki College, Takanashi, Hagisho, Ichinoseki, Iwate, 021-8511, Japan ABSTRACT We have conducted an Arecibo 327 MHz search of two dwarf irregular galaxies in the Local Group, Leo A and T, for radio pulsars and single pulses from fast radio bursts and other giant pulse emitters. We detected no astrophysical signals in this search, and we estimate flux density limits on both periodic and burst emission. Our derived luminosity limits indicate that only the most luminous radio pulsars known in our Galaxy and in the Magellanic Clouds (MCs) would have been detectable in our search if they were at the distances of Leo A and T. Given the much smaller stellar mass content and star formation rates of Leo A and T compared to the Milky Way and the MCs, there are likely to be few (if any) extremely luminous pulsars in these galaxies. It is therefore not surprising that we detected no pulsars in our search. Keywords: pulsars; radio transient sources; dwarf irregular galaxies INTRODUCTION The detection and study of extragalactic pulsars offers the rare opportunity to probe the high end of the pulsar luminosity function in another galaxy. Pulsar searches are also sensitive to bursting sources, such as fast radio bursts (FRBs; Lorimer et al.