The Galaxies of the Local Group Sidney Van Den Bergh Frontmatter More Information
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II Publications, Presentations
II Publications, Presentations 1. Refereed Publications Izumi, K., Kotake, K., Nakamura, K., Nishida, E., Obuchi, Y., Ohishi, N., Okada, N., Suzuki, R., Takahashi, R., Torii, Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, Y., Ueda, A., Yamazaki, T.: 2010, DECIGO and DECIGO Search for Gravitational-wave Inspiral Signals Associated with pathfinder, Class. Quantum Grav., 27, 084010. Short Gamma-ray Bursts During LIGO's Fifth and Virgo's First Aoki, K.: 2010, Broad Balmer-Line Absorption in SDSS Science Run, ApJ, 715, 1453-1461. J172341.10+555340.5, PASJ, 62, 1333. Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, All- Aoki, K., Oyabu, S., Dunn, J. P., Arav, N., Edmonds, D., Korista sky search for gravitational-wave bursts in the first joint LIGO- K. T., Matsuhara, H., Toba, Y.: 2011, Outflow in Overlooked GEO-Virgo run, Phys. Rev. D, 81, 102001. Luminous Quasar: Subaru Observations of AKARI J1757+5907, Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, PASJ, 63, S457. Search for gravitational waves from compact binary coalescence Aoki, W., Beers, T. C., Honda, S., Carollo, D.: 2010, Extreme in LIGO and Virgo data from S5 and VSR1, Phys. Rev. D, 82, Enhancements of r-process Elements in the Cool Metal-poor 102001. Main-sequence Star SDSS J2357-0052, ApJ, 723, L201-L206. Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, Arai, A., et al. including Yamashita, T., Okita, K., Yanagisawa, TOPICAL REVIEW: Predictions for the rates of compact K.: 2010, Optical and Near-Infrared Photometry of Nova V2362 binary coalescences observable by ground-based gravitational- Cyg: Rebrightening Event and Dust Formation, PASJ, 62, wave detectors, Class. -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
Arxiv:2103.07476V1 [Astro-Ph.GA] 12 Mar 2021
FERMILAB-PUB-21-075-AE-LDRD Draft version September 3, 2021 Typeset using LATEX twocolumn style in AASTeX63 The DECam Local Volume Exploration Survey: Overview and First Data Release A. Drlica-Wagner ,1, 2, 3 J. L. Carlin ,4 D. L. Nidever ,5, 6 P. S. Ferguson ,7, 8 N. Kuropatkin ,1 M. Adamow´ ,9, 10 W. Cerny ,2, 3 Y. Choi ,11 J. H. Esteves,12 C. E. Mart´ınez-Vazquez´ ,13 S. Mau ,14, 15 A. E. Miller,16, 17 B. Mutlu-Pakdil ,2, 3 E. H. Neilsen ,1 K. A. G. Olsen ,6 A. B. Pace ,18 A. H. Riley ,7, 8 J. D. Sakowska ,19 D. J. Sand ,20 L. Santana-Silva ,21 E. J. Tollerud ,11 D. L. Tucker ,1 A. K. Vivas ,13 E. Zaborowski,2 A. Zenteno ,13 T. M. C. Abbott ,13 S. Allam ,1 K. Bechtol ,22, 23 C. P. M. Bell ,16 E. F. Bell ,24 P. Bilaji,2, 3 C. R. Bom ,25 J. A. Carballo-Bello ,26 D. Crnojevic´ ,27 M.-R. L. Cioni ,16 A. Diaz-Ocampo,28 T. J. L. de Boer ,29 D. Erkal ,19 R. A. Gruendl ,30, 31 D. Hernandez-Lang,32, 13, 33 A. K. Hughes,20 D. J. James ,34 L. C. Johnson ,35 T. S. Li ,36, 37, 38 Y.-Y. Mao ,39, 38 D. Mart´ınez-Delgado ,40 P. Massana,19, 41 M. McNanna ,22 R. Morgan ,22 E. O. Nadler ,14, 15 N. E. D. Noel¨ ,19 A. Palmese ,1, 2 A. H. G. Peter ,42 E. S. -
Structural Analysis of the Sextans Dwarf Spheroidal Galaxy
MNRAS 000,1{16 (2015) Preprint 9 October 2018 Compiled using MNRAS LATEX style file v3.0 Structural analysis of the Sextans dwarf spheroidal galaxy T. A. Roderick,1? H. Jerjen,1 G. S. Da Costa,1 A. D. Mackey1 1Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We present wide-field g and i band stellar photometry of the Sextans dwarf spheroidal galaxy and its surrounding area out to four times its half-light radius (rh = 695 pc), based on images obtained with the Dark Energy Camera at the 4-m Blanco tele- scope at CTIO. We find clear evidence of stellar substructure associated with the galaxy, extending to a distance of 820 (2 kpc) from its centre. We perform a sta- tistical analysis of the over-densities and find three distinct features, as well as an extended halo-like structure, to be significant at the 99:7% confidence level or higher. Unlike the extremely elongated and extended substructures surrounding the Hercules dwarf spheroidal galaxy, the over-densities seen around Sextans are distributed evenly about its centre, and do not appear to form noticeable tidal tails. Fitting a King 0 0 model to the radial distribution of Sextans stars yields a tidal radius rt = 83:2 ± 7:1 (2.08±0.18 kpc), which implies the majority of detected substructure is gravitationally bound to the galaxy. This finding suggests that Sextans is not undergoing significant tidal disruption from the Milky Way, supporting the scenario in which the orbit of Sextans has a low eccentricity. -
Dark Matter Searches Targeting Dwarf Spheroidal Galaxies with the Fermi Large Area Telescope
Doctoral Thesis in Physics Dark Matter searches targeting Dwarf Spheroidal Galaxies with the Fermi Large Area Telescope Maja Garde Lindholm Oskar Klein Centre for Cosmoparticle Physics and Cosmology, Particle Astrophysics and String Theory Department of Physics Stockholm University SE-106 91 Stockholm Stockholm, Sweden 2015 Cover image: Top left: Optical image of the Carina dwarf galaxy. Credit: ESO/G. Bono & CTIO. Top center: Optical image of the Fornax dwarf galaxy. Credit: ESO/Digitized Sky Survey 2. Top right: Optical image of the Sculptor dwarf galaxy. Credit:ESO/Digitized Sky Survey 2. Bottom images are corresponding count maps from the Fermi Large Area Tele- scope. Figures 1.1a, 1.2, 1.3, and 4.2 used with permission. ISBN 978-91-7649-224-6 (pp. i{xxii, 1{120) pp. i{xxii, 1{120 c Maja Garde Lindholm, 2015 Printed by Publit, Stockholm, Sweden, 2015. Typeset in pdfLATEX Abstract In this thesis I present our recent work on gamma-ray searches for dark matter with the Fermi Large Area Telescope (Fermi-LAT). We have tar- geted dwarf spheroidal galaxies since they are very dark matter dominated systems, and we have developed a novel joint likelihood method to com- bine the observations of a set of targets. In the first iteration of the joint likelihood analysis, 10 dwarf spheroidal galaxies are targeted and 2 years of Fermi-LAT data is analyzed. The re- sulting upper limits on the dark matter annihilation cross-section range 26 3 1 from about 10− cm s− for dark matter masses of 5 GeV to about 5 10 23 cm3 s 1 for dark matter masses of 1 TeV, depending on the × − − annihilation channel. -
Model Comparison of the Dark Matter Profiles
A&A 558, A35 (2013) Astronomy DOI: 10.1051/0004-6361/201321606 & c ESO 2013 Astrophysics Model comparison of the dark matter profiles of Fornax, Sculptor, Carina and Sextans Maarten A. Breddels and Amina Helmi Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands e-mail: [email protected] Received 28 March 2013 / Accepted 16 August 2013 ABSTRACT Aims. We compare dark matter profile models of four dwarf spheroidal galaxies satellites of the Milky Way using Bayesian evidence. Methods. We use orbit based dynamical models to fit the 2nd and 4th moments of the line of sight velocity distributions of the Fornax, Sculptor, Carina and Sextans dwarf spheroidal galaxies. We compare NFW, Einasto and several cored profiles for their dark halos and present the probability distribution functions of the model parameters. Results. For each galaxy separately we compare the evidence for the various dark matter profiles, and find that it is not possible to distinguish between these specific parametric dark matter density profiles using the current data. Nonetheless, from the combined 2 β/2 evidence, we find that is unlikely that all galaxies are embedded in the same type of cored profiles of the form ρDM ∝ 1/(1 + r ) , where β = 3, 4. For each galaxy, we also obtain an almost model independent, and therefore accurate, constraint on the logarithmic slope of the dark matter density distribution at a radius ∼r−3, i.e. where the logarithmic slope of the stellar density profile is −3. Conclusions. For each galaxy, we find that all best fit models essentially have the same mass distribution over a large range in radius (from just below r−3 to the last measured data point). -
History of Telescopes
1 OUR PLACE IN SPACE Earth: Earth is the third planet from the Sun, and the densest and fifth- largest of the eight planets in the Solar System. It is also the largest of the Solar System’s four terrestrial planets. The Solar System : The Solar System consists of the Sun and those celestial objects bound to it by gravity, all of which were formed from the collapse of a giant molecular cloud approximately 4.6 billion years ago. Of the many objects that orbit the Sun, most of the mass is contained within eight relatively solitary planets whose orbits are almost circular and lie within a nearly flat disc called the ecliptic plane. The four smaller inner planets, Mercury, Venus, Earth and Mars, also called the terrestrial planets, are primarily composed of rock and metal. The four outer planets, the gas giants, are substantially more massive than the terrestrials. They are Jupiter, Saturn, Uranus and Neptune. The Sun: The Sun is the star at the center of the Solar System. It has a diameter of about 1,392,000 kilometers about 109 times that of Earth, and its mass (about 2 × 1030 kilograms, 330,000 times that of Earth) accounts for about 99.86% of the total mass of the Solar System. The Milky way Galaxy: The Milky Way Galaxy is the galaxy in which the Solar System is located. The Milky Way is a barred spiral galaxy that is part of the Local Group of galaxies. It is one of billions of galaxies in the observable universe. The Local Group: The Local Group is the group of galaxies that includes our galaxy, the Milky Way. -
The Variable Star Population in the Sextans Dwarf Spheroidal Galaxy
TheThe variablevariable starstar populationpopulation inin thethe SextansSextans dwarfdwarf spheroidalspheroidal galaxygalaxy Kathy Vivas Cerro Tololo Interamerican Observatory La Serena, Chile In collaboration with Javier Alonso-García (U. of Antofagasta, Chile) Mario Mateo (U. of Michigan, USA) Alistair Walker (CTIO, Chile) David Nidever (NOAO, USA) DECam Community Science Workshop 2018 1 The Role of Variable Stars ● Tracers of different stellar populations ● Standard candles → Distance Scale Variable stars in the Carina dwarf spheroidal galaxy (Vivas & Mateo 2013) DECam Community Science Workshop 2018 2 Properties of the Satellites of the Milky Way Drlica-Wagner et al., 2015 The new discoveries are likely to be ultra-faint dwarf galaxies. Gallart et al. 2015 Classical dwarfs display a variety of SFRs DECam Community Science Workshop 2018 3 CMDs of Satellite Dwarfs Brown et al 2014 On the other hand, ultra-faint dwarfs seem Monelli et al 2003 to be consistent with only and old Galaxies like Carina show obvious population signs of multiple bursts of star formation DECam Community Science Workshop 2018 4 Leo T: a UFD with extended star formation Clementini et al (2012) DECam Community Science Workshop 2018 5 Helium-Burning Pulsating Stars 3.0 Anomalous Cepheids 2.0 0.7 RR Lyrae Stars Variable stars and theoretical isochrones in Leo I (Fiorentino et al 2012) DECam Community Science Workshop 2018 6 Dwarf Cepheid Stars (collective name for δ Scuti or SX Phe) Intermediate age population TO Old Population TO Coppola et al 2015, Vivas & Mateo 2013 DECam Community Science Workshop 2018 7 Dwarf Cepheids as distance indicators Need to study more systems! Cohen et al (2012) P-L relationship (independent of metallicity) → standard candles DECam Community Science Workshop 2018 8 Dwarf Cepheids in other galaxies 85 dwarf cepheids in Fornax A few thousand in (Poretti et al. -
Mirando El Cielo
1 Mirando el cielo Guillermo Sánchez (http://diarium.usal.es/guillermo) Última actualización: 2013-05-11 1.0. Sobre la elaboración es este artículo. Todos los cálculos realizados para elaborar este artículo están realizados con el programa Mathematica , sin embargo Ud no los verá. A veces observará que algún texto aparece en inglés esto es debido a que se muestra directamente el resultado de la salida del programa. Si está interesado en el uso de este programa en cálculos astrónomicos y otros muchos campos puede visitar: http://diarium.usal.es/guillermo/mathematica/ . 1.1. La época dorada de la astronomía y cosmología La contemplación del cielo una noche estrellada, lejos de la contaminación lumínica, es uno de los espectáculos más sobrecogedores del que se puede disfrutar. No es extraño que durante milenios los seres humanos observasen el cielo y se diesen cuenta de que el Sol y la Luna siguen ciclos regulares. La mayoría de las culturas hicieron interpretaciones mitológicas o religiosas de los astros pero también los utilizaron con un sentido práctico, para el establecimiento de calendarios que sirvieron, entre otras cosas, para planificar las cosechas. Por ejemplo, los egipcios asociaban la aparición de Sirio, la estrella más brillante del hemisferio norte (ahora sabemos es un sistema binario), como preludio de la crecida del Nilo. El advenimiento del telescopio hace poco más de 400 años (1609): el número de astros observables paso de tres o cuatro mil astros, que se observan a simple vista, a miles de millones; la luna lejos de ser una esfera perfecta pues estaba cubierta de montañas y cráteres; las estrellas errantes (los planetas) no eran simples puntos de luz, tenían satélites y alguno hasta estaba rodeado de un anillo. -
Stellar Populations at the Center of Ic 16131 Andrew A
THE ASTRONOMICAL JOURNAL, 118:1657È1670, 1999 October ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. STELLAR POPULATIONS AT THE CENTER OF IC 16131 ANDREW A. COLE,2 ELINE TOLSTOY,3 JOHN S. GALLAGHER III,2 JOHN G. HOESSEL,2 JEREMY R. MOULD,4 JON A. HOLTZMAN,5 ABHIJIT SAHA,6 GILDA E. BALLESTER,7 CHRISTOPHER J. BURROWS,8,9 JOHN T. CLARKE,7 DAVID CRISP,10 RICHARD E. GRIFFITHS,11 CARL J. GRILLMAIR,12 JEFF J. HESTER,13 JOHN E. KRIST,8 VIKKI MEADOWS,10 PAUL A. SCOWEN,13 KARL R. STAPELFELDT,10 JOHN T. TRAUGER,10 ALAN M. WATSON,14 AND JAMES R. WESTPHAL15 Received 1999 March 29; accepted 1999 May 26 ABSTRACT We have observed the center of the Local Group dwarf irregular galaxy IC 1613 with the WFPC2 aboard the Hubble Space Telescope in the F439W, F555W, and F814W Ðlters. We analyze the resulting color-magnitude diagrams (CMDs) using the main-sequence and giant-branch luminosity functions and comparisons with theoretical stellar models to derive a preliminary star formation history for this galaxy. We Ðnd a dominant old stellar population (age B7 Gyr), identiÐable by the strong red giant branch (RGB) and red clump populations. From the (V [I) color of the RGB, we estimate a mean metallicity of the intermediate-age stellar population [Fe/H] \[1.38 ^ 0.31. We conÐrm a distance of 715 ^ 40 kpc using the I magnitude of the RGB tip. The main-sequence luminosity function down to I B 25 provides ] ~4 ~1 evidence for a roughly constant star formation rate (SFR) of approximately 3.5 10 M_ yr across the WFPC2 Ðeld of view (0.22 kpc2) during the past 250È350 Myr. -
November 2020 BRAS Newsletter
A Mars efter Lowell's Glober ca. 1905-1909”, from Percival Lowell’s maps; National Maritime Museum, Greenwich, London (see Page 6) Monthly Meeting November 9th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: Chuck Allen from the Astronomical League will speak about The Cosmic Distance Ladder, which explores the historical advancement of distance determinations in astronomy. What's In This Issue? President’s Message Member Meeting Minutes Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner – John Nagle ALPO 2020 Conference Astro-Photos by BRAS Members - MARS Messages from the HRPO REMOTE DISCUSSION Solar Viewing Edge of Night Natural Sky Conference Recent Entries in the BRAS Forum Observing Notes: Pisces – The Fishes Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society BRAS YouTube Channel Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 24 November 2020 President’s Message Welcome to the home stretch for 2020. The nights are starting earlier and earlier as the weather becomes more and more comfortable and all of our old favorites of the fall and winter skies really start finding their places right where they belong. October was a busy month for us, with several big functions at the Observatory, including two oppositions and two more all night celebrations. By comparison, November is looking fairly calm, the big focus there is going to be our third annual Natural Sky Conference on the 13th, which I’m encouraging people who care about the state of light pollution in our city and the surrounding area to get involved in. -
Biennial Report 2004 2005 Published in Spain by the ISAAC NEWTON GROUP of TELESCOPES (ING) ISSN 1575–8966 Legal License: TF–1142 /99
I SAAC N EWTON G ROUP OF T ELESCOPES Biennial Report 2004 2005 Published in Spain by the ISAAC NEWTON GROUP OF TELESCOPES (ING) ISSN 1575–8966 Legal license: TF–1142 /99 Apartado de correos, 321 E-38700 Santa Cruz de La Palma; Canary Islands; Spain Tel: +34 922 425 400 Fax: +34 922 425 401 URL: http://www.ing.iac.es/; http://www.ast.cam.ac.uk/ING/ (UK mirror) Editor and designer: Javier Méndez ([email protected]) Preprinting: Gráficas El Time. Tel: +34 922 416 651 Printing: Gráficas Sabater. Tel: +34 922 623 555 Front cover: IC1396 or the Elephant Trunk Nebula. Image obtained as part of the Isaac Newton Telescope Photometric Hα Survey of the Northen Galactic Plane, and it was prepared by Nick Wright, University College London. Inset: Photograph of laser test on the William Herschel Telescope as part of GLAS preparatory study. Credit: Javier Méndez. Other picture credits: Nik Szymanek (WHT, p. 4); Nik Szymanek (INT, p. 4); Nik Szymanek (JKT, p. 4); Nik Szymanek (ING, p. 5); Jens Moser (WHT, back); Jens Moser (INT, back); Nik Szymanek (JKT, back). The ING Biennial Report is available online at http://www.ing.iac.es/PR/AR/ or at http://www.ast.cam.ac.uk/ING/PR/AR/. ISAAC NEWTON GROUP OF TELESCOPES Biennial Report of the PPARC-NWO-IAC ING Board 2004 – 2005 ISAAC NEWTON GROUP William Herschel Telescope Isaac Newton Telescope Jacobus Kapteyn Telescope 4 • ING BIENNIAL R EPORT 2004–2005 OF TELESCOPES The Isaac Newton Group of Telescopes (ING) consists of the 4.2- metre William Herschel Telescope (WHT), the 2.5-metre Isaac Newton Telescope (INT) and the 1.0-metre Jacobus Kapteyn Telescope (JKT).