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Councillor Biographies
BIOGRAPHIES OF COUNCIL MEMBERS The following biographies were complied from the vast information found at the City of Edmonton Archives. Please feel free to contact the Office of the City Clerk or the City of Edmonton Archives if you have more information regarding any of the people mentioned in the following pages. The sources used for each of the biographies are found at the end of each individual summary. Please note that photos and additional biographies of these Mayors, Aldermen and Councillors are available on the Edmonton Public Library website at: http://www.epl.ca/edmonton-history/edmonton-elections/biographies-mayors-and- councillors?id=K A B C D E F G H I, J, K L M N, O P Q, R S T U, V, W, X, Y, Z Please select the first letter of the last name to look up a member of Council. ABBOTT, PERCY W. Alderman, 1920-1921 Born on April 29, 1882 in Lucan, Ontario where he was educated. Left Lucan at 17 and relocated to Stony Plain, Alberta where he taught school from 1901 to 1902. He then joined the law firm of Taylor and Boyle and in 1909 was admitted to the bar. He was on the Board of Trade and was a member of the Library Board for two years. He married Margaret McIntyre in 1908. They had three daughters. He died at the age of 60. Source: Edmonton Bulletin, Nov. 9, 1942 - City of Edmonton Archives ADAIR, JOSEPH W. Alderman, 1921-1924 Born in 1877 in Glasgow. Came to Canada in 1899 and worked on newspapers in Toronto and Winnipeg. -
Statistics and Properties of Emission-Line Regions in the Local
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 27 April 2020 (MN LATEX style file v2.2) Statistics and Properties of Emission-Line Regions in the Local Volume Dwarf Galaxies I. D. Karachentsev1⋆, S.S.Kaisin1† 1Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhnij Arkhyz, KChR, 369167, Russia 27 April 2020 ABSTRACT We used the Hα images from a large sample of nearby late-type dwarf galaxies to investigate properties of their emission structure. The sample consists of three hundred galaxies of the irregular (Irr), Magellanic irregular (Im), blue compact dwarf (BCD), and transition (Tr) types situated within a distance of 11 Mpc. In each galaxy, we indicated: the number of compact HII-regions, the presence of bubble-like or filament-like structures, the presence of a faint diffuse emission, and a sign of the global burst. The larger luminosity of a galaxy, the greater number of compact HII-sources in it. The integral and specific star-formation rates of the dwarf increase steeply with the increase of the number of HII-regions showing the evidence of the epidemic character of star-formation process. The dwarf galaxies with emission-line bubbles, or filaments, or signs of the global star-formation burst have approximately the same hydrogen-mass-to-luminosity ratio as that of the whole sample objects. arXiv:2004.11550v1 [astro-ph.GA] 24 Apr 2020 However, their mean star-formation rate is significantly higher than that of other galaxies in the sample. Emission bubble-like structures are found in the nearby dwarfs with a frequency of 1 case per 4-5 galaxies. -
Una Aproximación Física Al Universo Local De Nebadon
4 1 0 2 local Nebadon de Santiago RodríguezSantiago Hernández Una aproximación física al universo (160.1) 14:5.11 La curiosidad — el espíritu de investigación, el estímulo del descubrimiento, el impulso a la exploración — forma parte de la dotación innata y divina de las criaturas evolutivas del espacio. Tabla de contenido 1.-Descripción científica de nuestro entorno cósmico. ............................................................................. 3 1.1 Lo que nuestros ojos ven. ................................................................................................................ 3 1.2 Lo que la ciencia establece ............................................................................................................... 4 2.-Descripción del LU de nuestro entorno cósmico. ................................................................................ 10 2.1 Universo Maestro ........................................................................................................................... 10 2.2 Gran Universo. Nivel Espacial Superunivesal ................................................................................. 13 2.3 Orvonton. El Séptimo Superuniverso. ............................................................................................ 14 2.4 En el interior de Orvonton. En la Vía Láctea. ................................................................................. 18 2.5 En el interior de Orvonton. Splandon el 5º Sector Mayor ............................................................ 19 -
Surface Brightness Fluctuation Distances for Nearby Dwarf Elliptical
A&A 380, 90–101 (2001) Astronomy DOI: 10.1051/0004-6361:20011408 & c ESO 2001 Astrophysics Surface brightness fluctuation distances for nearby dwarf elliptical galaxies? H. Jerjen1,R.Rekola2, L. Takalo2, M. Coleman1, and M. Valtonen2 1 Research School of Astronomy and Astrophysics, The Australian National University, Mt Stromlo Observatory, Cotter Road, Weston ACT 2611, Australia 2 Tuorla Observatory, University of Turku, V¨ais¨al¨antie 20, 21500 Piikki¨o, Finland Received 12 July 2001 / Accepted 2 October 2001 Abstract. We obtained deep B and R-band CCD images for the dwarf elliptical (dE) galaxies DDO 44, UGC 4998, KK98 77, DDO 71, DDO 113, and UGC 7356 at the Nordic Optical Telescope. Employing Fourier analysis technique we measure stellar R-band surface brightness fluctuations (SBFs) and magnitudes in 29 different fields of the galaxies. Independent tip of the red giant branch distances for DDO 44, KK98 77, DDO 71 are used to convert their set of apparent into absolute SBF magnitudes. The results are combined with the corresponding local (B −R) colours and compared with the (B −R)−M R relation for mainly old, metal-poor stellar populations as predicted by Worthey’s population synthesis models using Padova isochrones. While the colour dependency of the theoretical relation is confirmed by the empirical data, we find a systematic zero point offset between observations and theory in the sense that models are too faint by 0.13 (0.02) mag. Based on these findings we establish a new semiempirical calibration of the SBF method as distance indicator for dE galaxies with an estimated uncertainty of ≈10%. -
An Observational Limit on the Dwarf Galaxy Population of the Local Group
An Observational Limit on the Dwarf Galaxy Population of the Local Group Alan B. Whiting1 Cerro Tololo Inter-American Observatory Casilla 603, La Serena, Chile [email protected] George K. T. Hau University of Durham Mike Irwin University of Cambridge Miguel Verdugo Institut f¨ur Astrophysik G¨ottingen, Germany ABSTRACT We present the results of an all-sky, deep optical survey for faint Local Group dwarf galaxies. Candidate objects were selected from the second Palomar survey (POSS-II) and ESO/SRC survey plates and follow-up observations performed to determine whether they were indeed overlooked members of the Local Group. arXiv:astro-ph/0610551v1 18 Oct 2006 Only two galaxies (Antlia and Cetus) were discovered this way out of 206 candi- dates. Based on internal and external comparisons, we estimate that our visual survey is more than 77% complete for objects larger than one arc minute in size and with a surface brightness greater than an extremely faint limit over the 72% of the sky not obstructed by the Milky Way. Our limit of sensitivity cannot be calculated exactly, but is certainly fainter than 25 magnitudes per square arc second in R, probably 25.5 and possibly approaching 26. We conclude that there are at most one or two Local Group dwarf galaxies fitting our observational cri- teria still undiscovered in the clear part of the sky, and roughly a dozen hidden behind the Milky Way. Our work places the “missing satellite problem” on a firm quantitative observational basis. We present detailed data on all our candidates, including surface brightness measurements. -
Aaron J. Romanowsky Curriculum Vitae (Rev. 1 Septembert 2021) Contact Information: Department of Physics & Astronomy San
Aaron J. Romanowsky Curriculum Vitae (Rev. 1 Septembert 2021) Contact information: Department of Physics & Astronomy +1-408-924-5225 (office) San Jose´ State University +1-409-924-2917 (FAX) One Washington Square [email protected] San Jose, CA 95192 U.S.A. http://www.sjsu.edu/people/aaron.romanowsky/ University of California Observatories +1-831-459-3840 (office) 1156 High Street +1-831-426-3115 (FAX) Santa Cruz, CA 95064 [email protected] U.S.A. http://www.ucolick.org/%7Eromanow/ Main research interests: galaxy formation and dynamics – dark matter – star clusters Education: Ph.D. Astronomy, Harvard University Nov. 1999 supervisor: Christopher Kochanek, “The Structure and Dynamics of Galaxies” M.A. Astronomy, Harvard University June 1996 B.S. Physics with High Honors, June 1994 College of Creative Studies, University of California, Santa Barbara Employment: Professor, Department of Physics & Astronomy, Aug. 2020 – present San Jose´ State University Associate Professor, Department of Physics & Astronomy, Aug. 2016 – Aug. 2020 San Jose´ State University Assistant Professor, Department of Physics & Astronomy, Aug. 2012 – Aug. 2016 San Jose´ State University Research Associate, University of California Observatories, Santa Cruz Oct. 2012 – present Associate Specialist, University of California Observatories, Santa Cruz July 2007 – Sep. 2012 Researcher in Astronomy, Department of Physics, Oct. 2004 – June 2007 University of Concepcion´ Visiting Adjunct Professor, Faculty of Astronomical and May 2005 Geophysical Sciences, National University of La Plata Postdoctoral Research Fellow, School of Physics and Astronomy, June 2002 – Oct. 2004 University of Nottingham Postdoctoral Fellow, Kapteyn Astronomical Institute, Oct. 1999 – May 2002 Rijksuniversiteit Groningen Research Fellow, Harvard-Smithsonian Center for Astrophysics June 1994 – Oct. -
Gas Accretion from Minor Mergers in Local Spiral Galaxies⋆
A&A 567, A68 (2014) Astronomy DOI: 10.1051/0004-6361/201423596 & c ESO 2014 Astrophysics Gas accretion from minor mergers in local spiral galaxies? E. M. Di Teodoro1 and F. Fraternali1;2 1 Department of Physics and Astronomy, University of Bologna, 6/2, Viale Berti Pichat, 40127 Bologna, Italy e-mail: [email protected] 2 Kapteyn Astronomical Institute, Postbus 800, 9700 AV Groningen, The Netherlands Received 7 February 2014 / Accepted 28 May 2014 ABSTRACT We quantify the gas accretion rate from minor mergers onto star-forming galaxies in the local Universe using Hi observations of 148 nearby spiral galaxies (WHISP sample). We developed a dedicated code that iteratively analyses Hi data-cubes, finds dwarf gas-rich satellites around larger galaxies, and estimates an upper limit to the gas accretion rate. We found that 22% of the galaxies have at least one detected dwarf companion. We made the very stringent assumption that all satellites are going to merge in the shortest possible time, transferring all their gas to the main galaxies. This leads to an estimate of the maximum gas accretion rate of −1 0.28 M yr , about five times lower than the average star formation rate of the sample. Given the assumptions, our accretion rate is clearly an overestimate. Our result strongly suggests that minor mergers do not play a significant role in the total gas accretion budget in local galaxies. Key words. galaxies: interactions – galaxies: evolution – galaxies: kinematics and dynamics – galaxies: star formation – galaxies: dwarf 1. Introduction structures in the Universe grow by several inflowing events and have increased their mass content through a small number of The evolution of galaxies is strongly affected by their capabil- major mergers, more common at high redshifts, and through an ity of retaining their gas and accreting fresh material from the almost continuous infall of dwarf galaxies (Bond et al. -
First Results from the MADCASH Survey: a Faint Dwarf Galaxy
Draft version August 10, 2016 Preprint typeset using LATEX style AASTeX6 v. 1.0 FIRST RESULTS FROM THE MADCASH SURVEY: A FAINT DWARF GALAXY COMPANION TO THE LOW MASS SPIRAL GALAXY NGC 2403 AT 3.2 MPC 1 Jeffrey L. Carlin2, David J. Sand3, Paul Price4, Beth Willman2, Ananthan Karunakaran5, Kristine Spekkens5,6, Eric F. Bell7, Jean P. Brodie8, Denija Crnojevic´3, Duncan A. Forbes9, Jonathan Hargis10, Evan Kirby11, Robert Lupton4, Annika H. G. Peter12, Aaron J. Romanowsky8, 13, and Jay Strader14 1Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. 2LSST and Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA; Haverford College, Department of Astronomy, 370 Lancaster Avenue, Haverford, PA 19041, USA; jeff[email protected] 3Texas Tech University, Physics Department, Box 41051, Lubbock, TX 79409-1051, USA 4Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 5Department of Physics, Engineering Physics and Astronomy, Queen’s University, Kingston, Ontario, Canada, K7L 3N6 6Department of Physics, Royal Military College of Canada, P.O. Box 17000, Station Forces, Kingston, ON K7L 7B4, Canada 7Department of Astronomy, University of Michigan, 1085 South University Ave, Ann Arbor, MI 48109, USA 8University of California Observatories, 1156 High Street, Santa Cruz, CA 95064, USA 9Centre for Astrophysics and Supercomputing, Swinburne University, Hawthorn VIC 3122, Australia 10Space Telescope Science Institute, 3700 San Martin Drive, -
World War I Canadian Generals
WORLD WAR I CANADIAN GENERALS 1 CANADIAN GENERAL OFFICERS WW1 General Sir Arthur William CURRIE, GCMG, KCB GOC – 1st Canadian Corps Lieutenant-General Sir Richard Ernest William TURNER, VC, KCB, KCMG, DSO Chief of General Staff in the United Kingdom Major-General Sir Edward Whipple Bancroft MORRISON, KCMG, CB, DSO GOC - Royal Artillery – Canadian Corps Lieutenant-General Sir Archibald Cameron MACDONELL, KCB, CMG, DSO, VD GOC – 1st Canadian Division Major-General Sir Samuel Benfield STEELE, KCMG, CB, MVO GOC – 2nd Canadian Division Lieutenant-General Sir Henry Edward BURSTALL, KCB, KCMG, ADC GOC – 2nd Canadian Division Major-General Malcolm Smith MERCER, CB (KIA) GOC – 3rd Canadian Division Major-General Sir Frederick Oscar Warren LOOMIS, KCB, CMG, DSO and Bar, VD GOC – 3rd Canadian Division Major-General Sir David WATSON, KCB, CMG GOC – 4th Canadian Division Major-General Garnet Burk HUGHES, CB, CMG, DSO GOC – 5th Canadian Division Brigadier-General William St. Pierre HUGHES, DSO, VD CDR - 10th Canadian Infantry Brigade Major-General William Antrobus GRIESBACH, CB, CMG, DSO & Bar GOC – 1st Canadian Infantry Brigade Major-General George Eric McCUAIG, CMG, DSO and Bar GOC – 1st Canadian Infantry Brigade Brigadier-General John Fletcher Leopold EMBURY, CB, CMG, VD, KC GOC – 2nd Canadian Infantry Brigade Brigadier-General Robert Percy CLARK, CMG, DSO, MC GOC – 2nd Canadian Infantry Brigade Brigadier-General Robert Gilmour Edwards LECKIE, CMG GOC – 3rd Canadian Infantry Brigade Brigadier-General Robert R. RENNIE, CB, CMG, DSO, MVO GOC – 4th -
Tracing the Local Volume Galaxy Halo-To-Stellar Mass Ratio with Satellite Kinematics
Received 10 July 2020; Revised 23 August 2020; Accepted 23 August 2020 DOI: xxx/xxxx 10.1002/asna.20210018 ORIGINAL ARTICLE Tracing the Local Volume galaxy halo-to-stellar mass ratio with satellite kinematics Igor Karachentsev | Olga Kashibadze Special Astrophysical Observatory, Russian Academy of Sciences, Russia Rapid advance has been made recently in accurate distance measurements for nearby Correspondence (D < 11 Mpc) galaxies based on the magnitude of the tip of red giant branch stars I. D. Karachentsev, SAO RAS, Nizhny Arkhyz, Karachay-Cherkessia, resolved with the Hubble Space Telescope. We use observational properties of galax- 369167 Russia. Email: [email protected] ies presented in the last version of Updated Nearby Galaxy Catalog to derive a halo mass of luminous galaxies via orbital motion of their companions. Our sample con- Funding Information tains 298 assumed satellites with known radial velocities around 25 Milky Way-like Russian Scientific Foundation, 19– massive galaxies and 65 assumed satellites around 47 fainter dominant galaxies. 02–00145. The average total mass-to-K-band luminosity ratio is 31 , 6M⊙_L⊙ for the lumi- nous galaxies, increasing up to ∼ 200M⊙_L⊙ toward dwarfs. The bulge-dominated luminous galaxies are characterized with êMT _LK ë = 73 , 15M⊙_L⊙, while the disc-dominated spirals have êMT _LK ë = 17:4 , 2:8M⊙_L⊙. We draw attention to a particular subsample of luminous spiral galaxies with signs of declining rotation curve, which have a radial velocity dispersion of satellites less than 55 km/s and a poor dark matter halo with êMT _LK ë = 5:5 , 1:1M⊙_L⊙. -
List of Publications (06/2021)
Prof. Dr. Eva K. Grebel, Astronomisches Rechen-Institut, Zentrum f¨urAstronomie der Universit¨at Heidelberg, M¨onchhofstr. 12{14, D-69120 Heidelberg, Germany List of Publications (06/2021) A. Refereed publications (443) . 1 B. Reviews (34) . 47 C. Conference proceedings etc. (175) 50 D. Abstracts (141) . 66 E. Books (2) . 77 In publications with my students or postdocs their names are underlined when this work was completed (or partially carried out) while they held their position with me. A. Refereed Publications 1. Menon, S.H., Grasha, K., Elmegreen, B.G., Federrath, C., Krumholz, M.R., Calzetti, D., S´anchez, N., Linden, S.T., Adamo, A., Messa, M., Cook, D.O., Dale, D.A., Grebel, E.K., Fumagalli, M., Sabbi, E., Johnson, K.E., Smith, L.J., & Kennicutt, R.C. The Dependence of the Hierarchical Distribution of Star Clusters on Galactic En- vironment 2021, MNRAS, submitted 2. D´ek´any, I., Grebel, E.K., & Pojmanski, G. Metallicity estimation of RR Lyrae stars from their I-band light curves 2021, ApJ, submitted 3. Gatto, M., Ripepi, V., Bellazzini, M., Tosi, M., Cignoni, M., Tortora, C., Leccia, S., Clementini, G., Grebel, E.K., Longo, G., Marconi, M., & Musella, I. STEP Survey II: Structural Analysis of 170 star clusters in the SMC 2021, MNRAS, submitted 4. Orozco-Duarte, R., Wofford, A., Vidal-Garc´ıa, A., Bruzual, G., Charlot, S., Krumholz, M., Hannon, S., Lee, J., Wofford, T., Fumagalli, M., Dale, D., Messa, M., Grebel, E.K., Smith, L., Grasha, K., & Cook, D. Synthetic photometry of OB star clusters with stochastically sampled IMFs: anal- ysis of models and HST observations 2021, MNRAS, submitted 5. -
Jürgen Lamprecht, Ronald C.Stoyan, Klaus Veit
Dieses Dokument ist urheberrechtlich geschützt. Nutzung nur zu privaten Zwecken. Die Weiterverbreitung ist untersagt. Liebe Beobachterinnen, liebe Beobachter, die Waage zu halten zwischen Beiträgen für Gelegenheitsbeobachter und Artikeln für Hardcore-Beob- achter ist erklärtes Ziel von interstellarum. Einerseits also möglichst viele zur Deep-Sky Beobachtung zu motivieren sei es mit dem Auge, Film oder Chip und andererseits geballte Informationen und Erfahrungsaustausch auch für alte Hasen zu bieten. Jene Balance zu halten ist kein leichtes Unterfangen und oft sind Stimmen zu hören, die eine stärkere Berücksichtigung von Themen für den Einsteiger oder Spazierseher fordern oder die große Zahl an semi-professionellen Aufnahmen und detaillierten Zeichnungen beklagen. Um es nochmals zu betonen: Dieses Mißverhältnis liegt nicht an einer Bevorzugung unsererseits von besseren Bildern oder abgehobeneren Beiträgen, sondern ist ein möglichst gutes Spiegelbild des an uns gesandten Materials. Es liegt also zum großen Teil an Ihnen, liebe Leser, das Gleichgewicht zu hal- ten bzw. wiederherzustellen. Niemand möge sich also scheuen seine Ergebnisse zu senden. In diesem Magazin soll kein Wettlauf um das beste Bild stattfinden. Dies würde vollkommen am Amateurge- danken vorbeigehen: Es geht ja nicht darum, mit tollen Ergebnissen zu glänzen, sondern andere teilha- ben zu lassen am Spaß, den man bei einer bestimmten Beobachtung hatte ... Um die Möglichkeiten zur aktiven Teilnahme zu vergrößern wird am Ende des Starhopper künftig eine Liste einfacher Objekte zu finden sein, die in den nächsten Heften besprochen werden. Senden Sie uns Ihre Beobachtungen; wir werden Ergebnisse kleinerer Geräte bevorzugt veröffentlichen! Vielleicht wird interstellarum auch noch zu wenig von Spaziersehern und Gelegenheitsbeobachtern gelesen? In jedem Fall liegt hier ein großes noch unerschlossenes Leserpotential vor, das wir mit Ihrer Hilfe für interstellarum erschließen könnten.