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Arxiv:1702.04727V1 [Astro-Ph.GA] 15 Feb 2017 Galaxies at Higher Mass and Luminosity
Draft version February 17, 2017 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE DRAGONFLY NEARBY GALAXIES SURVEY. III. THE LUMINOSITY FUNCTION OF THE M101 GROUP Shany Danieli1,2,3, Pieter van Dokkum3, Allison Merritt3, Roberto Abraham4,5, Jielai Zhang4,5,6, I. D. Karachentsev7, and L. N. Makarova7 Draft version February 17, 2017 ABSTRACT We obtained follow-up HST observations of the seven low surface brightness galaxies discovered with the Dragonfly Telephoto Array in the field of the massive spiral galaxy M101. Out of the seven galaxies, only three were resolved into stars and are potentially associated with the M101 group at D = 7 Mpc. Based on HST ACS photometry in the broad F606W and F814W filters, we use a maximum likelihood algorithm to locate the Tip of the Red Giant Branch (TRGB) in galaxy color-magnitude diagrams. +0:35 +0:21 +0:25 Distances are 6:38−0:35; 6:87−0:30 and 6:52−0:27 Mpc and we confirm that they are members of the M101 group. Combining the three confirmed low luminosity satellites with previous results for brighter group members, we find the M101 galaxy group to be a sparsely populated galaxy group consisting of seven group members, down to MV = −9:2 mag. We compare the M101 cumulative luminosity function to that of the Milky Way and M31. We find that they are remarkably similar; In fact, the cumulative luminosity function of the M101 group gets even flatter for fainter magnitudes, and we show that the M101 group might exhibit the two known small-scale flaws in the ΛCDM model, namely `the missing satellite' problem and the `too big to fail' problem. -
The Saga of M81: Global View of a Massive Stellar Halo in Formation
Draft version October 27, 2020 Typeset using LATEX twocolumn style in AASTeX63 The Saga of M81: Global View of a Massive Stellar Halo in Formation Adam Smercina ,1, 2 Eric F. Bell ,1 Paul A. Price,3 Colin T. Slater ,2 Richard D'Souza,1, 4 Jeremy Bailin ,5 Roelof S. de Jong ,6 In Sung Jang ,6 Antonela Monachesi ,7, 8 and David Nidever 9, 10 1Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA 2Astronomy Department, University of Washington, Box 351580, Seattle, WA 98195-1580, USA 3Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 4Vatican Observatory, Specola Vaticana, V-00120, Vatican City State 5Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487-0324, USA 6Leibniz-Institut f¨urAstrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 7Instituto de Investigaci´onMultidisciplinar en Ciencia y Tecnolog´ıa,Universidad de La Serena, Ra´ulBitr´an1305, La Serena, Chile 8Departamento de F´ısica y Astronom´ıa,Universidad de La Serena, Av. Juan Cisternas 1200 N, La Serena, Chile 9Department of Physics, Montana State University, P.O. Box 173840, Bozeman, MT 59717-3840 10National Optical Astronomy Observatory, 950 North Cherry Ave, Tucson, AZ 85719 (Received 31 October, 2019; Revised 31 August, 2020; Accepted 23 October, 2020) Submitted to The Astrophysical Journal ABSTRACT Recent work has shown that Milky Way-mass galaxies display an incredible range of stellar halo properties, yet the origin of this diversity is unclear. The nearby galaxy M81 | currently interacting with M82 and NGC 3077 | sheds unique light on this problem. -
NEUTRAL HYDROGEN CLOUDS in the M81/M82 GROUP KM Chynoweth
University of Massachusetts Amherst ScholarWorks@UMass Amherst Astronomy Department Faculty Publication Series Astronomy 2008 NEUTRAL HYDROGEN CLOUDS IN THE M81/M82 GROUP KM Chynoweth GI Langston Min Yun University of Massachusetts - Amherst FJ Lockman KHR Rubin See next page for additional authors Follow this and additional works at: https://scholarworks.umass.edu/astro_faculty_pubs Part of the Astrophysics and Astronomy Commons Recommended Citation Chynoweth, KM; Langston, GI; Yun, Min; Lockman, FJ; Rubin, KHR; and Scoles, SA, "NEUTRAL HYDROGEN CLOUDS IN THE M81/M82 GROUP" (2008). The Astrophysical Journal. 1129. 10.1088/0004-6256/135/6/1983 This Article is brought to you for free and open access by the Astronomy at ScholarWorks@UMass Amherst. It has been accepted for inclusion in Astronomy Department Faculty Publication Series by an authorized administrator of ScholarWorks@UMass Amherst. For more information, please contact [email protected]. Authors KM Chynoweth, GI Langston, Min Yun, FJ Lockman, KHR Rubin, and SA Scoles This article is available at ScholarWorks@UMass Amherst: https://scholarworks.umass.edu/astro_faculty_pubs/1129 Neutral Hydrogen Clouds in the M81/M82 Group Katie M. Chynoweth1 Vanderbilt University, Physics and Astronomy Department, 1807 Station B, Nashville, TN 37235 Glen I. Langston National Radio Astronomy Observatory, Green Bank, WV 24944 Min S. Yun University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01002 Felix J. Lockman, K.H.R. Rubin2 and Sarah A. Scoles3 National Radio Astronomy Observatory, Green Bank, WV 24944 ABSTRACT We have observed a 3◦ ×3◦ area centered on the M81/M82 group of galaxies using the Robert C. Byrd Green Bank Telescope (GBT) in a search for analogs to the High Velocity Clouds (HVCs) of neutral hydrogen found around our galaxy. -
Astronomy Magazine Special Issue
γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006. -
DUST and ATOMIC GAS in DWARF IRREGULAR GALAXIES of the M81 GROUP: the SINGS and THINGS VIEW Fabian Walter,1 John M
The Astrophysical Journal, 661:102Y114, 2007 May 20 # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. DUST AND ATOMIC GAS IN DWARF IRREGULAR GALAXIES OF THE M81 GROUP: THE SINGS AND THINGS VIEW Fabian Walter,1 John M. Cannon,1, 2 He´le`ne Roussel,1 George J. Bendo,3 Daniela Calzetti,4 Daniel A. Dale,5 Bruce T. Draine,6 George Helou,7 Robert C. Kennicutt, Jr.,8,9 John Moustakas,9,10 George H. Rieke,9 Lee Armus,7 Charles W. Engelbracht,9 Karl Gordon,9 David J. Hollenbach,11 Janice Lee,9 Aigen Li,12 Martin J. Meyer,4 Eric J. Murphy,13 Michael W. Regan,4 John-David T. Smith,9 Elias Brinks,14 W. J. G. de Blok,15 Frank Bigiel,1 and Michele D. Thornley16 Received 2006 September 26; accepted 2007 February 12 ABSTRACT We present observations of the dust and atomic gas phase in seven dwarf irregular galaxies of the M81 group from the Spitzer SINGS and VLA THINGS surveys. The Spitzer observations provide a first glimpse of the nature of the Y À1 nonatomic ISM in these metal-poor (Z 0:1 Z ), quiescent (SFR 0:001 0:1 M yr ) dwarf galaxies. Most detected dust emission is restricted to H i column densities >1 ; 1021 cmÀ2, and almost all regions of high H i column density (>2:5 ; 1021 cmÀ2) have associated dust emission. Spitzer spectroscopy of two regions in the brightest galaxies (IC 2574 and Holmberg II) show distinctly different spectral shapes and aromatic features, although the galaxies have comparable gas-phase metallicities. -
The Extended Virgo Cluster Catalog (EVCC) Covers an Area of 725 Deg2 Or 60.1Mpc2
The Extended Virgo Cluster Catalog Suk Kim1, Soo-Chang Rey1,5, Helmut Jerjen2,Thorsten Lisker3, Eon-Chang Sung4, Youngdae Lee1, Jiwon Chung1, Mina Pak1, Wonhyeong Yi1, and Woong Lee1 Received ; accepted 1Department of Astronomy and Space Science, Chungnam National University, 99 Daehak-ro, arXiv:1409.3283v1 [astro-ph.GA] 11 Sep 2014 Daejeon 305-764, Korea 2Research School of Astronomy and Astrophysics, The Australian National University, Cotter Road, Weston, ACT, 2611, Australia 3Astronomisches Rechen-Institut, Zentrum f¨ur Astronomie der Universit¨at Heidelberg (ZAH), M¨onchhofstraße 12-14, D-69120 Heidelberg, Germany 4Korea Astronomy & Space Science institute, 776 Daedeokdae-ro, Daejeon 305-348, Korea 5Author to whom any correspondence should be addressed –2– ABSTRACT We present a new catalog of galaxies in the wider region of the Virgo cluster, based on the Sloan Digital Sky Survey (SDSS) Data Release 7. The Extended Virgo Cluster Catalog (EVCC) covers an area of 725 deg2 or 60.1Mpc2. It is 5.2 times larger than the footprint of the classical Virgo Cluster Catalog (VCC) and reaches out to 3.5 times the virial radius of the Virgo cluster. We selected 1324 spectroscopically targeted galaxies with radial velocities less than 3000kms−1. In addition, 265 galaxies that have been missed in the SDSS spectroscopic survey but have available redshifts in the NASA Extragalactic Database are also included. Our selection process secured a total of 1589 galaxies of which 676 galaxies are not included in the VCC. The certain and possible cluster members are defined by means of redshift comparison with a cluster infall model. -
1. Introduction 2. the Accordant Group Members
THE ASTROPHYSICAL JOURNAL, 474:74È83, 1997 January 1 ( 1997. The American Astronomical Society. All rights reserved. Printed in U.S.A. DISCORDANT ARGUMENTS ON COMPACT GROUPS HALTON ARP Max-Planck-Institut fu r Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching, Germany Received 1995 December 8; accepted 1996 July 17 ABSTRACT Much print has been dedicated to explaining discordant redshifts in compact groups as unrelated background galaxies. But no one has analyzed the accordant galaxies. It is shown here that when there is a brightest galaxy in the group, the remainder with di†erences of less than 1000 km s~1 are systemati- cally redshifted. This is the same result as obtained in all other well-deÐned groups and demonstrates again an increasing intrinsic redshift with fainter luminosity. DeÐning discordant redshifts as 1000 km s~1 or greater than the brightest galaxy, it is shown that 76 out of 345, or 22% are discordant, reaching excesses of up to 23,000 km s~1. This large percentage cannot be explained by background contamination because the number of discordances would be expected to increase rapidly with larger excesses, exactly opposite to what is observed in compact groups. HicksonÏs logarithmic intensity image of the NGC 1199 group conÐrms earlier direct evidence from Arp that a peculiar, compact object of 13,300 km s~1 redshift is silhouetted in front of the 2705 km s~1 central galaxy. Subject headings: galaxies: clusters: general È galaxies: distances and redshifts 1. INTRODUCTION 2. THE ACCORDANT GROUP MEMBERS Accordant members are here deÐned as galaxies with When redshifts began to be measured in the nearest, *cz \ 1000 km s~1 di†erence from the redshift of the densest groups of galaxies, it quickly became evident that brightest galaxy in the group. -
Winter Sp Target Information
WINTER SP TARGET INFORMATION MESSIER 15 BASIC INFORMATION OBJECT TYPE: Globular Cluster CONSTELLATION: Pegasus BEST VIEW: Late October DISCOVERY: Jean-Dominique Maraldi, 1746 DISTANCE: 33,600 ly DIAMETER: 175 ly APPARENT MAGNITUDE: +6.2 APPARENT DIMENSIONS: 18’ DISTANCE DETERMINATION Globular clusters contain many RR Lyrae stars, which are a type of standard candle. These stars vary in brightness, and the period of variation relates to the star’s luminosity. Comparison of luminosity to apparent magnitude yields the distance. AGE DETERMINATION Astronomers plot the colors and magnitudes of cluster stars on an H-R diagram to get an overall picture of the evolutionary states of the cluster stars. This, in turn, allows astronomers to constrain the age of the cluster. NOTABLE FEATURES/FACTS • M15 contains several hundred thousand stars. • The cluster is estimated to be approximately 13 billion years old, making it one of the oldest structures in our Galaxy. • The total energy output of M15’s stars is 360,000 times the energy of the Sun. • M15 is the most dense globular cluster. Half of its mass is contained within 10 ly of its center. This is probably due to core collapse: stars have settled near the center due to their gravitational influence on one another. • Some astronomers suspect there may be an intermediate-mass black hole at the center of M15. Recent studies, however, have found no evidence of one. • M15 contains Pease 1, the first planetary nebula ever detected in a globular cluster. To date, only a handful of planetaries have been discovered in globulars. • In 2016, astronomers using the Fermi Large Area Telescope reported significant gamma ray emission from M15. -
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. -
Arxiv:1210.8333V2 [Astro-Ph.CO] 27 Nov 2012
Draft version November 2, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 THE HI ENVIRONMENT OF THE M101 GROUP J. Christopher Mihos,1 Katie M. Keating,2 Kelly Holley-Bockelmann,3,4 D.J. Pisano,5,6 and Namir E. Kassim7 Draft version November 2, 2018 ABSTRACT ◦ ◦ 16:8−17:5 −2 We present a wide (8.5 × 6.7 , 1050 × 825 kpc), deep (σNHI = 10 cm ) neutral hydrogen (HI) map of the M101 galaxy group. We identify two new HI sources in the group environment, one an extremely low surface brightness (and hitherto unknown) dwarf galaxy, and the other a starless HI cloud, possibly primordial in origin. Our data show that M101's extended HI envelope takes the form of a ∼ 100 kpc long tidal loop or plume of HI extending to the southwest of the galaxy. The plume 8 17 −2 has an HI mass ∼ 10 M and a peak column density of NHI= 5 × 10 cm , and while it rotates with the main body of M101, it shows kinematic peculiarities suggestive of a warp or flaring out of the rotation plane of the galaxy. We also find two new HI clouds near the plume with masses ∼ 107 M , similar to HI clouds seen in the M81/M82 group, and likely also tidal in nature. Comparing to deep optical imaging of the M101 group, neither the plume nor the clouds have any extended optical counterparts down to a limiting surface brightness of µB= 29.5. We also trace HI at intermediate velocities between M101 and NGC 5474, strengthening the case for a recent interaction between the two galaxies. -
Constraints on the Dynamical Evolution of the Galaxy Group M81 3
Mon. Not. R. Astron. Soc. 000, 000–000 (0000, accepted) Printed 9 January 2017 (MN LATEX style file v2.2) Constraints on the dynamical evolution of the galaxy group M81 W. Oehm1⋆, I. Thies2† and P. Kroupa2,3‡ 1 scdsoft AG, Albert-Nestler-Str. 10, D-76131 Karlsruhe, Germany 2 Helmholtz-Institut f¨ur Strahlen und Kernphysik (HISKP), Nussallee 14-16, D-53115 Bonn, Germany 3 Charles University in Prague, Faculty of Mathematics and Physics, Astronomical Institute, V Holeˇsoviˇck´ach 2, CZ-180 00 Praha 8, Czech Republic 9 January 2017 ABSTRACT According to the standard model of cosmology, galaxies are embedded in dark matter halos which are made of particles beyond the standard model of particle physics, thus extending the mass and the size of the visible baryonic matter by typically two orders of magnitude. The observed gas distribution throughout the nearby M81 group of galaxies shows evidence for past significant galaxy–galaxy interactions but without a merger having occurred. This group is here studied for possible dynamical solutions within the dark-matter standard model. In order to cover a comprehensive set of initial conditions, the inner three core members M81, M82 and NGC 3077 are treated as a three-body model based on Navarro-Frenk-White profiles. The possible orbits of these galaxies are examined statistically taking into account dynamical friction. Long living, non-merging initial constellations which allow multiple galaxy–galaxy encounters comprise unbound galaxies only, which are arriving from a far distance and happen to simultaneously encounter each other within the recent 500 Myr. Our results are derived by the employment of two separate and independent statistical methods, namely a Markov chain Monte Carlo method and the genetic algorithm using the SAP system environment. -
P,'I,Cipal.R, Vestigato,'."/$R .'.,,.;¢". ,"4
FINAL TECHNICAL REPORT NASA ResearchGrant NAG5-6821 UV, Visible, and Gravitational AstrophysicsResearchand Analysis Program Awarded under NASA ResearchAnnouncement97-OSS-01 Period covered:January 1, 1998- December31, 2001 POST-AGB STARS IN NEARBY GALAXIES AS CALIBRATORS FOR lIST P,'i,cipal.r,_vestigato,'."/$r_.'.,,.;¢"._,"4 Howard E. Bond Space Telescope Science Institute 3700 San Martin Drive Baltimore, MD 21218 Post-AGB Stars in Nearby Galaxies as Calibrators for HST Final Report This report summarizes activities carried out with support from the NASA Ultravio- let. Visible, and Gravitational Astrophysics Research and Analysis Program under Grant NAG 5-6821. The Principal Investigator is Howard E. Bond (Space Telescope Science Institute). STScI Postdoctoral Associates Laura K. Fullton (1998), David Alves (1998-2001), and Michael Siegel (2001) were partially supported by this grant. The aim of the program is to calibrate the absolute magnitudes of post-asymptotic- giant-branch (post-AGB or PAGB) stars, which we believe will be an excellent new "standard candle" for measuring extragalactic distances. The argument is that, in old populations, tile stars that are evolving through the PAGB region of the HR diagram arise from only a single main-sequence turnoff mass. In addition, theoretical PAGB evolutionary tracks show that they evolve through this region at constant luminosity; hence the PAGB stars should have an extremely narrow luminosity function. Moreover, as the PAGB stars evolve through spectral types F and A (en route from the AGB to hot stellar remnants and white dwarfs), they have the highest luminosities attained by old stars (both bolometrically and in the visual band).