The Southern Hemisphere

Total Page:16

File Type:pdf, Size:1020Kb

The Southern Hemisphere R O T H N MAJOR URSA T THE SOUTHERN HEMISPHERE S AURIGA E N W O LYNX H With Glenn Dawes R T T R H β O E A Spot the peak of the Alpha Centaurid meteor N M36 GEMINI S T α shower and enjoy a view of the stars in Orion’s Belt LEO MINOR LEO Almach Castor α M37 CANCER Pollux γ β When to use this chart M35 ANDROMEDA 22nd β M44 Beehive M44 Sickle The chart accurately matches the sky on the 1 Feb at 00:00 AEDT (13:00 UT) LEO δ dates and times shown for Sydney, Australia. γ γ 25th 15 Feb at 23:00 AEDT (12:00 UT) δ The sky is different at other times as the stars δ 31 Feb at 22:00 AEDT (11:00 UT) crossing it set four minutes earlier each night. X γ BERENICES Ecliptic Rosette Nebula Rosette M64 Betelgeuse COMA CANIS MINOR CANIS α Regulus α δ M66 M86 β α β FEBRUARY HIGHLIGHTS STARS AND CONSTELLATIONS “V” 28th M87 Aldebaran α β δ ORION The Alpha Centaurids is one of the The three distinctive Belt stars of α γ Winter Triangle Winter Procyon Alpheratz few meteor showers that’s exclusive Orion are possibly the most easily Hyades to the Southern Hemisphere. Active from recognised asterism visible from anywhere M60 α M49 HYDRA γ δ 31 January to 20 February, its peak is in the world. From left to right (west β M78 st 1 VIRGO δ TAURUS MONOCEROS expected on the 8th. With a new Moon on to east) Mintaka (Delta (d) Orionis), W α M48 ζ the 12th, the evenings through to the early Alnilam (Epsilon ( ) Orionis) and Alnitak δ e ε γ β M50 α M43 Alphard morning at peak offer dark skies. Although (Zeta (z) Orionis) are all hot stars Venus of Mirror Sirius γ β peak rates can be low (five per hour), it (O or B spectral classes). Alnilam and CRATER M47 γ δ compensates by producing bright yellow Alnitak are blue supergiants and are α M42 β β α or blue coloured fireballs that leave trains. only dimmed to second magnitude Rigel ξ Ghost of Jupiter of Ghost ρ ANTLIA PYXIS α γ The Alpha Centaurids radiant is close to by distance, about 2,000 and 1,200 γ M41 M104 γ PUPPIS E T Celestial Equator Celestial β Alpha ( ) Centauri and Beta ( ) Centauri. lightyears away, respectively. δ a b A S Spica δ δ E S β CORVUS γ α α δ T W α β α LEPUS Cr 135 Cr ζ THE PLANETS γ CANIS MAJOR π β Ahadi NGC 2298 NGC The evening skies are sparse with start of twilight midmonth. Mercury β γ R only Mars and Uranus on offer, both follows these outer planets into the γ Canopus 4th setting close to 23:00 midmonth. Likewise, morning and catches up. Low in the early ο the morning offers little until dawn. After eastern dawn sky, these planets are seen VELA δ ERIDANUS COLUMBA Eta Carina Nebula last month, Saturn then Jupiter appears passing Venus; Saturn is closest on the M83 False Cross β CAELUM out of the solar glow, rising around the 6th with Jupiter and Mercury on the 14th. EQUULEUS δ α α CENTAURUS CARINA α R PICTOR γ LIBRA γ β α DEEP-SKY OBJECTS CRUX γ δ α ε δ β α FORNAX w Cen β γ The naked-eye star Pi (p) Puppis, or Move 6° west of Collinder 135 NGC 2397 β β γ δ Ahadi (RA 7h 17.1m dec. –37° 06’) is a to discover the globular cluster DORADO Coal Acrux α VOLANS double, offering colour contrast with mag. NGC 2298 (RA 6h 49.0m, dec. -36° 00’). Sack Tarantula Nebulaα Jewel Box β α α α LMC +2.9 and +7.9 components, yellow and blue It is fainter (at mag. +9.3) and smaller Alpha Centaurids HOROLOGIUM β γ γ δ α Peak 08 Feb γ R respectively, separated by 1 arcminute. than many globulars with a halo only β β δ δ Pi Puppis is also the brightest member around 3 arcminutes across and a β Hadar MENSA RETICULUM MUSCA β γ of a large open cluster, Collinder 135. Its few scattered faint stars around the δ Rigel Kent LUPUS α CHAMAELEON most distinctive feature is three mag. +5.0 edge. The brightness rises quickly α δ δ blue stars (two close together) in a line to a 2-arcminute core which plateaus, β α γ South Celestial Pole forming an isosceles triangle with Pi showing little further brightening near γ γ Achernar α γ Puppis, fitting in a 0.5° diameter circle. the centre. CIRCINUS S γ OCTANS HYDRUS δ O α T δ β S U NORMA β E T TRIANGULUMδ APUS β SMC H W E γ 47 Tucanae H A AUSTRALE α β T Chart key S β U T PHOENIX O S STAR ASTEROID BRIGHTNESS: GALAXY DIFFUSE α TRACK γ NEBULOSITY MAG. 0 δ OPEN CLUSTER & BRIGHTER ARA β METEOR α DOUBLE STAR MAG. +1 GLOBULAR RADIANT δ γ β MAG. +2 CLUSTER VARIABLE STAR QUASAR MAG. +3 δ γ PLANETARY PAVO α COMET TRACK MAG. +4 TUCANA CORONAAUSTRALIS NEBULA PLANET & FAINTER CHART: PETECHART: LAWRENCE BBC Sky at Night Magazine February 2021 SOUTH BBC Sky at Night Magazine February 2021.
Recommended publications
  • Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects
    Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Porto Alegre 2017 Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Dissertação elaborada sob orientação do Prof. Dr. Eduardo Luis Damiani Bica, co- orientação do Prof. Dr. Charles José Bon- ato e apresentada ao Instituto de Física da Universidade Federal do Rio Grande do Sul em preenchimento do requisito par- cial para obtenção do título de Mestre em Física. Porto Alegre 2017 Acknowledgements To my parents, who supported me and made this possible, in a time and place where being in a university was just a distant dream. To my dearest friends Elisabeth, Robert, Augusto, and Natália - who so many times helped me go from "I give up" to "I’ll try once more". To my cats Kira, Fen, and Demi - who lazily join me in bed at the end of the day, and make everything worthwhile. "But, first of all, it will be necessary to explain what is our idea of a cluster of stars, and by what means we have obtained it. For an instance, I shall take the phenomenon which presents itself in many clusters: It is that of a number of lucid spots, of equal lustre, scattered over a circular space, in such a manner as to appear gradually more compressed towards the middle; and which compression, in the clusters to which I allude, is generally carried so far, as, by imperceptible degrees, to end in a luminous center, of a resolvable blaze of light." William Herschel, 1789 Abstract We provide a sample of 170 Galactic Globular Clusters (GCs) and analyse its spatial distribution properties.
    [Show full text]
  • A Basic Requirement for Studying the Heavens Is Determining Where In
    Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun­ damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short).
    [Show full text]
  • Exploding Star in NGC 2397 31 March 2008
    Exploding star in NGC 2397 31 March 2008 Camera for Surveys (ACS). One atypical feature of this Hubble image is the view of supernova SN 2006bc taken when it was still fairly faint and its brightness on the increase. Astronomers from Queen's University Belfast in Northern Ireland, led by Professor of Astronomy Stephen J. Smartt, requested the image as part of a long project studying the massive exploding stars — supernovae. Exactly which types of star will explode and the lowest mass of star that can produce a supernova are not known. When a supernova is discovered in a nearby galaxy the group begins a painstaking search of earlier Hubble images of the same galaxy to locate the NGC 2397, pictured in this image from Hubble, is a star that later exploded; often one of hundreds of classic spiral galaxy with long prominent dust lanes millions of stars in the galaxy. This is a little like along the edges of its arms, seen as dark patches and sifting through days of CCTV footage to find one streaks silhouetted against the starlight. Hubble's frame showing a suspect. If the astronomers find a exquisite resolution allows the study of individual stars in star at the location of the later explosion, they may nearby galaxies. Located nearly 60 million light-years work out the mass and type of star from its away from Earth, the galaxy NGC 2397 is typical of most spirals, with mostly older, yellow and red stars in its brightness and colour. Only six such stars have central portion, while star formation continues in the been identified before they exploded and the outer, bluer spiral arms.
    [Show full text]
  • Abundances for Globular Cluster Giants
    A&A manuscript no. (will be inserted by hand later) ASTRONOMY AND Your thesaurus codes are: ASTROPHYSICS (08.01.1; 08.01.03; 08.16.3; 10.07.3) 24.8.2017 Abundances for Globular Cluster Giants: I. Homogeneous Metallicities for 24 Clusters E. Carretta1,3, R. G. Gratton2 1 Osservatorio Astronomico di Bologna, Via Zamboni 33, I-40126 Bologna, ITALY 2 Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, ITALY 3 Dipartimento d’Astronomia, Universit`adi Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, ITALY Received 28 February 1996/Accepted 21 May 1996 Abstract. We have obtained high resolution, high signal- calibration of the ∆S index) and our new cluster metallici- to-noise ratio CCD echelle spectra of 10 bright red giants ties. It could be tentatively ascribed to non-linearity in the in 3 globular clusters (47 Tuc, NGC 6752 and NGC 6397) [Fe/H]−∆S relationship. The impact of new metallicities roughly spanning the whole range of metallicities of the on major astrophysical problems is exemplified through galactic globular cluster system. The analysis of this newly a simple exercise on the Oosterhoff effect in the classical acquired material reveals no significant evidence of star- pair M 3 and M 15. to-star variation of the [Fe/H] ratio in these three clusters. Moreover, a large set of high quality literature data (equiv- Key words: Stars: abundances - Stars: Atmospheres - alent widths from high dispersion CCD spectra) was re- Stars: Population II - globular clusters: general analyzed in an homogeneous and self-consistent way to in- tegrate our observations and derive new metal abundances for more than 160 bright red giants in 24 globular clusters (i.e.
    [Show full text]
  • Characterizing the V-Band Light-Curves of Hydrogen-Rich Type Ii Supernovae∗
    The Astrophysical Journal, 786:67 (35pp), 2014 May 1 doi:10.1088/0004-637X/786/1/67 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. CHARACTERIZING THE V-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE∗ Joseph P. Anderson1,2, Santiago Gonzalez-Gait´ an´ 1, Mario Hamuy1,3, Claudia P. Gutierrez´ 1,3, Maximilian D. Stritzinger4, Felipe Olivares E.5, Mark M. Phillips6, Steve Schulze7, Roberto Antezana1, Luis Bolt8, Abdo Campillay6, Sergio Castellon´ 6, Carlos Contreras4, Thomas de Jaeger1,3,Gaston´ Folatelli9, Francisco Forster¨ 1, Wendy L. Freedman10, Luis Gonzalez´ 1, Eric Hsiao6, Wojtek Krzeminski´ 11, Kevin Krisciunas12, Jose´ Maza1, Patrick McCarthy10, Nidia I. Morrell6, Sven E. Persson10, Miguel Roth6, Francisco Salgado13, Nicholas B. Suntzeff12, and Joanna Thomas-Osip6 1 Departamento de Astronom´ıa, Universidad de Chile, Casilla 36-D, Santiago, Chile; [email protected] 2 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile 3 Millennium Institute of Astrophysics, Casilla 36-D, Santiago, Chile 4 Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 5 Departamento de Ciencias Fisicas, Universidad Andres Bello, Avda. Republica 252, Santiago, Chile 6 Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile 7 Instituto de Astrof´ısica, Facultad de F´ısica, Pontif´ıcia Universidad Catolica´ de Chile, Casilla 306, Santiago 22, Chile 8 Argelander Institut fur¨ Astronomie, Universitat¨ Bonn, Auf dem Hugel¨ 71, D-53111 Bonn, Germany 9 Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan 10 Observatories of the Carnegie Institution for Science, Pasadena, CA 91101, USA 11 N.
    [Show full text]
  • Type II Supernovae As Probes of Environment Metallicity: Observations of Host H II Regions J
    A&A 589, A110 (2016) Astronomy DOI: 10.1051/0004-6361/201527691 & c ESO 2016 Astrophysics Type II supernovae as probes of environment metallicity: observations of host H II regions J. P. Anderson1, C. P. Gutiérrez1; 2; 3, L. Dessart4, M. Hamuy3; 2, L. Galbany2; 3, N. I. Morrell5, M. D. Stritzinger6, M. M. Phillips5, G. Folatelli7, H. M. J. Boffin1, T. de Jaeger2; 3, H. Kuncarayakti2; 3, and J. L. Prieto8; 2 1 European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile e-mail: [email protected] 2 Millennium Institute of Astrophysics, Casilla 36-D, Santiago, Chile 3 Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile 4 Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Boulevard de l’Observatoire, CS 34229, 06304 Nice Cedex 4, France 5 Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile 6 Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark 7 Instituto de Astrofísica de La Plata, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, CONICET, Paseo del Bosque S/N, B1900FWA, La Plata, Argentina 8 Núcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile Received 3 November 2015 / Accepted 28 January 2016 ABSTRACT Context. Spectral modelling of type II supernova atmospheres indicates a clear dependence of metal line strengths on progenitor metallicity. This dependence motivates further work to evaluate the accuracy with which these supernovae can be used as environment metallicity indicators. Aims.
    [Show full text]
  • Ngc Catalogue Ngc Catalogue
    NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39
    [Show full text]
  • Arxiv:1911.02835V1 [Astro-Ph.SR] 7 Nov 2019 Astronomy, Monash University, Melbourne, Clayton 3800, Australia
    The Astronomy and Astrophysics Review manuscript No. (will be inserted by the editor) What is a Globular Cluster? An observational perspective Raffaele Gratton1 · Angela Bragaglia2 · Eugenio Carretta2 · Valentina D’Orazi1;3 · Sara Lucatello1 · Antonio Sollima2 Received: date / Accepted: date Abstract Globular clusters are large and dense agglomerate of stars. At variance with smaller clusters of stars, they exhibit signs of some chemical evolution. At least for this reason, they are intermediate between open clusters and massive objects such as nuclear clusters or compact galaxies. While some facts are well established, the increasing amount of observational data is revealing a complexity that has so far de- fied the attempts to interpret the whole data set in a simple scenario. We review this topic focusing on the main observational features of clusters in the Milky Way and its satellites. We find that most of the observational facts related to the chemical evo- lution in globular clusters are described as being primarily a function of the initial mass of the clusters, tuned by further dependence on the metallicity – that mainly affects specific aspects of the nucleosynthesis processes involved – and on the envi- ronment, that likely determines the possibility of independent chemical evolution of the fragments or satellites where the clusters form. We review the impact of multiple populations on different regions of the colour-magnitude diagram and underline the constraints related to the observed abundances of lithium, to the cluster dynamics, and to the frequency of binaries in stars of different chemical composition. We then re-consider the issues related to the mass budget and the relation between globular cluster and field stars.
    [Show full text]
  • Atlante Grafico Delle Galassie
    ASTRONOMIA Il mondo delle galassie, da Kant a skylive.it. LA RIVISTA DELL’UNIONE ASTROFILI ITALIANI Questo è un numero speciale. Viene qui presentato, in edizione ampliata, quan- [email protected] to fu pubblicato per opera degli Autori nove anni fa, ma in modo frammentario n. 1 gennaio - febbraio 2007 e comunque oggigiorno di assai difficile reperimento. Praticamente tutte le galassie fino alla 13ª magnitudine trovano posto in questo atlante di più di Proprietà ed editore Unione Astrofili Italiani 1400 oggetti. La lettura dell’Atlante delle Galassie deve essere fatto nella sua Direttore responsabile prospettiva storica. Nella lunga introduzione del Prof. Vincenzo Croce il testo Franco Foresta Martin Comitato di redazione e le fotografie rimandano a 200 anni di studio e di osservazione del mondo Consiglio Direttivo UAI delle galassie. In queste pagine si ripercorre il lungo e paziente cammino ini- Coordinatore Editoriale ziato con i modelli di Herschel fino ad arrivare a quelli di Shapley della Via Giorgio Bianciardi Lattea, con l’apertura al mondo multiforme delle altre galassie, iconografate Impaginazione e stampa dai disegni di Lassell fino ad arrivare alle fotografie ottenute dai colossi della Impaginazione Grafica SMAA srl - Stampa Tipolitografia Editoria DBS s.n.c., 32030 metà del ‘900, Mount Wilson e Palomar. Vecchie fotografie in bianco e nero Rasai di Seren del Grappa (BL) che permettono al lettore di ripercorrere l’alba della conoscenza di questo Servizio arretrati primo abbozzo di un Universo sempre più sconfinato e composito. Al mondo Una copia Euro 5.00 professionale si associò quanto prima il mondo amatoriale. Chi non è troppo Almanacco Euro 8.00 giovane ricorderà le immagini ottenute dal cielo sopra Bologna da Sassi, Vac- Versare l’importo come spiegato qui sotto specificando la causale.
    [Show full text]
  • The Messier Objects
    Warren H. Finlay Concise Catalog of Deep-Sky Objects Astrophysical Information for 550 Galaxies, Clusters and Nebulae Second Edition The Patrick Moore The Patrick Moore Practical Astronomy Series For further volumes: http://www.springer.com/series/3192 Concise Catalog of Deep-Sky Objects Astrophysical Information for 550 Galaxies, Clusters and Nebulae Warren H. Finlay Second Edition Warren H. Finlay Edmonton , AB , Canada ISSN 1431-9756 ISSN 2197-6562 (electronic) ISBN 978-3-319-03169-9 ISBN 978-3-319-03170-5 (eBook) DOI 10.1007/978-3-319-03170-5 Springer Cham Heidelberg New York Dordrecht London Library of Congress Control Number: 2014938104 © Springer International Publishing Switzerland 2003, 2014 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifi cally the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfi lms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. Exempted from this legal reservation are brief excerpts in connection with reviews or scholarly analysis or material supplied specifi cally for the purpose of being entered and executed on a computer system, for exclusive use by the purchaser of the work. Duplication of this publication or parts thereof is permitted only under the provisions of the Copyright Law of the Publisher’s location, in its current version, and permission for use must always be obtained from Springer. Permissions for use may be obtained through RightsLink at the Copyright Clearance Center.
    [Show full text]
  • The Black Hole Mass Function Derived from Local Spiral Galaxies
    PUBLISHED IN THE ASTROPHYSICAL JOURNAL, 789:124 (16PP),2014 JULY 10 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE BLACK HOLE MASS FUNCTION DERIVED FROM LOCAL SPIRAL GALAXIES BENJAMIN L. DAVIS1 , JOEL C. BERRIER1,2,5,LUCAS JOHNS3,6 ,DOUGLAS W. SHIELDS1,2, MATTHEW T. HARTLEY2,DANIEL KENNEFICK1,2, JULIA KENNEFICK1,2, MARC S. SEIGAR1,4 , AND CLAUD H.S. LACY1,2 Published in The Astrophysical Journal, 789:124 (16pp), 2014 July 10 ABSTRACT We present our determination of the nuclear supermassive black hole mass (SMBH) function for spiral galax- ies in the local universe, established from a volume-limited sample consisting of a statistically complete col- lection of the brightest spiral galaxies in the southern (δ< 0◦) hemisphere. Our SMBH mass function agrees well at the high-mass end with previous values given in the literature. At the low-mass end, inconsistencies exist in previous works that still need to be resolved, but our work is more in line with expectations based on modeling of black hole evolution. This low-mass end of the spectrum is critical to our understanding of the mass function and evolution of black holes since the epoch of maximum quasar activity. A limiting luminos- ity (redshift-independent) distance, DL = 25.4 Mpc (z =0.00572) and a limiting absolute B-band magnitude, MB = −19.12 define the sample. These limits define a sample of 140 spiral galaxies, with 128 measurable pitch angles to establish the pitch angle distribution for this sample. This pitch angle distribution function may be useful in the study of the morphology of late-type galaxies.
    [Show full text]
  • The Origin of Globular Cluster FSR 1758 Fu-Chi Yeh1, Giovanni Carraro1, Vladimir I
    A&A 635, A125 (2020) Astronomy https://doi.org/10.1051/0004-6361/201937093 & c ESO 2020 Astrophysics The origin of globular cluster FSR 1758 Fu-Chi Yeh1, Giovanni Carraro1, Vladimir I. Korchagin2, Camilla Pianta1, and Sergio Ortolani1 1 Department of Physics and Astronomy Galileo Galilei, Vicolo Osservatorio 3, 35122 Padova, Italy e-mail: [email protected] 2 Southern Federal University, Rostov on Don, Russian Federation Received 10 November 2019 / Accepted 5 February 2020 ABSTRACT Context. Globular clusters in the Milky Way are thought to have either an in situ origin, or to have been deposited in the Galaxy by past accretion events, like the spectacular Sagittarius dwarf galaxy merger. Aims. We probe the origin of the recently discovered globular cluster FSR 1758, often associated with some past merger event and which happens to be projected toward the Galactic bulge. We performed a detailed study of its Galactic orbit, and assign it to the most suitable Galactic component. Methods. We employed three different analytical time-independent potential models to calculate the orbit of the cluster by using the Gauss Radau spacings integration method. In addition, a time-dependent bar potential model is added to account for the influence of the Galactic bar. We ran a large suite of simulations via a Montecarlo method to account for the uncertainties in the initial conditions. Results. We confirm previous indications that the globular cluster FSR 1758 possesses a retrograde orbit with high eccentricity. The comparative analysis of the orbital parameters of star clusters in the Milky Way, in tandem with recent metallicity estimates, allows us to conclude that FSR 1758 is indeed a Galactic bulge intruder.
    [Show full text]