Deconstructing the Antlia Cluster Core⋆
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XMM–Newton Observations of NGC 3268 in the Antlia Galaxy Cluster: Characterization of a Hidden Group of Galaxies at Z ≈ 0.41
MNRAS 00, 1 (2018) doi:10.1093/mnras/sty1401 Advance Access publication 2018 May 28 XMM–Newton observations of NGC 3268 in the Antlia Galaxy Cluster: characterization of a hidden group of galaxies at z ≈ 0.41 I. D. Gargiulo,1,4‹ F. Garc´ıa,2,3,4,5 J. A. Combi,2,3,4 J. P. Caso1,2,4 and L. P. Bassino1,2,4 1Instituto de Astrof´ısica de La Plata (CCT La Plata, CONICET, UNLP), Paseo del Bosque s/n, B1900FWA La Plata, Argentina 2Facultad de Ciencias Astronomicas´ y Geof´ısicas, Universidad Nacional de La Plata, Paseo del Bosque, B1900FWA La Plata, Argentina 3Instituto Argentino de Radioastronom´ıa (CCT-La Plata, CONICET; CICPBA), C.C. No. 5, 1894 Villa Elisa, Argentina 4Consejo Nacional de Investigaciones Cient´ıficas y Tecnicas,´ Rivadavia 1917, Ciudad Autonoma´ de Buenos Aires, C1033AAJ Buenos Aires, Argentina 5Laboratoire AIM (UMR 7158 CEA/DRF-CNRS-Universite´ Paris Diderot), Irfu/Departament´ d’Astrophysique, Centre de Saclay, F-91191 Gif-sur-Yvette, France Accepted 2018 May 25. Received 2018 May 25; in original form 2016 December 1 ABSTRACT We report on a detailed X-ray study of the extended emission of the intracluster medium (ICM) around NGC 3268 in the Antlia Cluster of galaxies, together with a characterization of an extended source in the field, namely a background cluster of galaxies at z ≈ 0.41, which was previously accounted as an X-ray point source. The spectral properties of the extended emission of the gas present in Antlia were studied using data from the XMM–Newton satellite, complemented with optical images of Cerro Tololo Inter-American Observatory (CTIO) Blanco telescope, to attain for associations of the optical sources with the X-ray emission. -
The Puzzling Nature of Dwarf-Sized Gas Poor Disk Galaxies
Dissertation submitted to the Department of Physics Combined Faculties of the Astronomy Division Natural Sciences and Mathematics University of Oulu Ruperto-Carola-University Oulu, Finland Heidelberg, Germany for the degree of Doctor of Natural Sciences Put forward by Joachim Janz born in: Heidelberg, Germany Public defense: January 25, 2013 in Oulu, Finland THE PUZZLING NATURE OF DWARF-SIZED GAS POOR DISK GALAXIES Preliminary examiners: Pekka Heinämäki Helmut Jerjen Opponent: Laura Ferrarese Joachim Janz: The puzzling nature of dwarf-sized gas poor disk galaxies, c 2012 advisors: Dr. Eija Laurikainen Dr. Thorsten Lisker Prof. Heikki Salo Oulu, 2012 ABSTRACT Early-type dwarf galaxies were originally described as elliptical feature-less galax- ies. However, later disk signatures were revealed in some of them. In fact, it is still disputed whether they follow photometric scaling relations similar to giant elliptical galaxies or whether they are rather formed in transformations of late- type galaxies induced by the galaxy cluster environment. The early-type dwarf galaxies are the most abundant galaxy type in clusters, and their low-mass make them susceptible to processes that let galaxies evolve. Therefore, they are well- suited as probes of galaxy evolution. In this thesis we explore possible relationships and evolutionary links of early- type dwarfs to other galaxy types. We observed a sample of 121 galaxies and obtained deep near-infrared images. For analyzing the morphology of these galaxies, we apply two-dimensional multicomponent fitting to the data. This is done for the first time for a large sample of early-type dwarfs. A large fraction of the galaxies is shown to have complex multicomponent structures. -
Naming the Extrasolar Planets
Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named. -
Early-Type Galaxies in the Antlia Cluster: Catalogue and Isophotal Analysis
MNRAS 477, 1760–1771 (2018) doi:10.1093/mnras/sty611 Advance Access publication 2018 March 7 Early-type galaxies in the Antlia cluster: catalogue and isophotal analysis Juan P. Calderon,´ 1,2,3‹ Lilia P. Bassino,1,2,3 Sergio A. Cellone1,3,4 and Mat´ıas Gomez´ 5 1Consejo Nacional de Investigaciones Cient´ıficas y Tecnicas,´ Rivadavia 1917, Buenos Aires, Argentina 2Instituto de Astrof´ısica de La Plata (CCT La Plata - CONICET - UNLP), La Plata, Argentina 3Facultad de Ciencias Astronomicas´ y Geof´ısicas, Universidad Nacional de La Plata, Paseo del Bosque, B1900FWA La Plata, Argentina Downloaded from https://academic.oup.com/mnras/article-abstract/477/2/1760/4924514 by Universidad Andres Bello user on 28 May 2019 4Complejo Astronomico´ El Leoncito (CONICET - UNLP - UNC - UNSJ), San Juan, Argentina 5Departamento de Ciencias F´ısicas, Facultad de Ciencias Exactas, Universidad Andres Bello, Santiago, Chile Accepted 2018 February 26. Received 2018 February 26; in original form 2017 December 14 ABSTRACT We present a statistical isophotal analysis of 138 early-type galaxies in the Antlia cluster, located at a distance of ∼ 35 Mpc. The observational material consists of CCD images of four 36 × 36 arcmin2 fields obtained with the MOSAIC II camera at the Blanco 4-m telescope at Cerro Tololo Interamerican Observatory. Our present work supersedes previous Antlia studies in the sense that the covered area is four times larger, the limiting magnitude is MB ∼−9.6 mag, and the surface photometry parameters of each galaxy are derived from Sersic´ model fits extrapolated to infinity. In a companion previous study we focused on the scaling relations obtained by means of surface photometry, and now we present the data, on which the previous paper is based, the parameters of the isophotal fits as well as an isophotal analysis. -
The Constellation Microscopium, the Microscope Microscopium Is A
The Constellation Microscopium, the Microscope Microscopium is a small constellation in the southern sky, defined in the 18th century by Nicolas Louis de Lacaille in 1751–52 . Its name is Latin for microscope; it was invented by Lacaille to commemorate the compound microscope, i.e. one that uses more than one lens. The first microscope was invented by the two brothers, Hans and Zacharius Jensen, Dutch spectacle makers of Holland in 1590, who were also involved in the invention of the telescope (see below). Lacaille first showed it on his map of 1756 under the name le Microscope but Latinized this to Microscopium on the second edition published in 1763. He described it as consisting of "a tube above a square box". It contains sixty-nine stars, varying in magnitude from 4.8 to 7, the lucida being Gamma Microscopii of apparent magnitude 4.68. Two star systems have been found to have planets, while another has a debris disk. The stars that now comprise Microscopium may formerly have belonged to the hind feet of Sagittarius. However, this is uncertain as, while its stars seem to be referred to by Al-Sufi as having been seen by Ptolemy, Al-Sufi does not specify their exact positions. Microscopium is bordered Capricornus to the north, Piscis Austrinus and Grus to the west, Sagittarius to the east, Indus to the south, and touching on Telescopium to the southeast. The recommended three-letter abbreviation for the constellation, as adopted Seen in the 1824 star chart set Urania's Mirror (lower left) by the International Astronomical Union in 1922, is 'Mic'. -
Educator's Guide: Orion
Legends of the Night Sky Orion Educator’s Guide Grades K - 8 Written By: Dr. Phil Wymer, Ph.D. & Art Klinger Legends of the Night Sky: Orion Educator’s Guide Table of Contents Introduction………………………………………………………………....3 Constellations; General Overview……………………………………..4 Orion…………………………………………………………………………..22 Scorpius……………………………………………………………………….36 Canis Major…………………………………………………………………..45 Canis Minor…………………………………………………………………..52 Lesson Plans………………………………………………………………….56 Coloring Book…………………………………………………………………….….57 Hand Angles……………………………………………………………………….…64 Constellation Research..…………………………………………………….……71 When and Where to View Orion…………………………………….……..…77 Angles For Locating Orion..…………………………………………...……….78 Overhead Projector Punch Out of Orion……………………………………82 Where on Earth is: Thrace, Lemnos, and Crete?.............................83 Appendix………………………………………………………………………86 Copyright©2003, Audio Visual Imagineering, Inc. 2 Legends of the Night Sky: Orion Educator’s Guide Introduction It is our belief that “Legends of the Night sky: Orion” is the best multi-grade (K – 8), multi-disciplinary education package on the market today. It consists of a humorous 24-minute show and educator’s package. The Orion Educator’s Guide is designed for Planetarians, Teachers, and parents. The information is researched, organized, and laid out so that the educator need not spend hours coming up with lesson plans or labs. This has already been accomplished by certified educators. The guide is written to alleviate the fear of space and the night sky (that many elementary and middle school teachers have) when it comes to that section of the science lesson plan. It is an excellent tool that allows the parents to be a part of the learning experience. The guide is devised in such a way that there are plenty of visuals to assist the educator and student in finding the Winter constellations. -
Searching for Star-Forming Dwarf Galaxies in the Antlia Cluster?
A&A 563, A118 (2014) Astronomy DOI: 10.1051/0004-6361/201322615 & c ESO 2014 Astrophysics Searching for star-forming dwarf galaxies in the Antlia cluster? O. Vaduvescu1,C.Kehrig2, L. P. Bassino3,4,5, A. V. Smith Castelli3,4,5, and J. P. Calderón3,4,5 1 Isaac Newton Group of Telescopes, Apto. 321, 38700 Santa Cruz de la Palma, Canary Islands, Spain e-mail: [email protected] 2 Instituto de Astrofísica de Andalucía (CSIC), Apto. 3004, 18080 Granada, Spain 3 Grupo de Investigación CGGE, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque, B1900FWA La Plata, Argentina 4 Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), C1033AAJ Ciudad Autónoma de Buenos Aires, Argentina 5 Instituto de Astrofísica de La Plata (CCT-La Plata, CONICET-UNLP), Paseo del Bosque, B1900FWA La Plata, Argentina Received 5 September 2013 / Accepted 31 January 2014 ABSTRACT Context. The formation and evolution of dwarf galaxies in clusters need to be understood, and this requires large aperture telescopes. Aims. In this sense, we selected the Antlia cluster to continue our previous work in the Virgo, Fornax, and Hydra clusters and in the Local Volume (LV). Because of the scarce available literature data, we selected a small sample of five blue compact dwarf (BCD) candidates in Antlia for observation. Methods. Using the Gemini South and GMOS camera, we acquired the Hα imaging needed to detect star-forming regions in this sample. With the long-slit spectroscopic data of the brightest seven knots detected in three BCD candidates, we derived their basic chemical properties. -
Galaxy Populations in the Antlia Cluster – I
Mon. Not. R. Astron. Soc. 386, 2311–2322 (2008) doi:10.1111/j.1365-2966.2008.13211.x Galaxy populations in the Antlia cluster – I. Photometric properties of early-type galaxies Anal´ıa V. Smith Castelli,1,2† Lilia P. Bassino,1,2† Tom Richtler,3† Sergio A. Cellone,1,2† Cristian Aruta‡ and Leopoldo Infante4† 1Facultad de Ciencias Astronomicas´ y Geof´ısicas, Universidad Nacional de La Plata, Paseo del Bosque, B1900FWA La Plata, Argentina 2 Instituto de Astrof´ısica de la Plata (CONICET-UNLP) Downloaded from https://academic.oup.com/mnras/article-abstract/386/4/2311/1467775 by guest on 18 December 2018 3Departamento de F´ısica, Universidad de Concepcion,´ Casilla 160-C, Concepcion,´ Chile 4Departamento de Astronom´ıa y Astrof´ısica, Pontificia Universidad Catolica´ de Chile, Casilla 306, Santiago 22, Chile Accepted 2008 March 7. Received 2008 March 6; in original form 2007 November 16 ABSTRACT We present the first colour–magnitude relation (CMR) of early-type galaxies in the central region of the Antlia cluster, obtained from CCD wide-field photometry in the Washington photometric system. Integrated (C − T1) colours, T1 magnitudes, and effective radii have been measured for 93 galaxies (i.e. the largest galaxies sample in the Washington system till now) from the FS90 Antlia Group catalogue. Membership of 37 objects can be confirmed through new radial velocities and data collected from the literature. The resulting colour– magnitude diagram shows that early-type FS90 galaxies that are spectroscopically confirmed Antlia members or that were considered as definite members by FS90, follow a well-defined σ ∼ . -
Early-Type Galaxies in the Antlia Cluster: Global Properties
MNRAS 000,1–16 (2020) Preprint 14 July 2020 Compiled using MNRAS LATEX style file v3.0 Early-type galaxies in the Antlia Cluster: global properties Juan P. Calderón1;2;3?, Lilia P. Bassino1;2;3, Sergio A. Cellone1;3;4, Matías Gómez5 and Juan P. Caso1;2;3 1Consejo Nacional de Investigaciones Científicas y Técnicas, Godoy Cruz 2290, C1425FQB, Ciudad Autónoma de Buenos Aires, Argentina 2Instituto de Astrofísica de La Plata (CCT La Plata – CONICET - UNLP), Paseo del Bosque S/N, B1900FWA La Plata, Argentina 3Facultad de Ciencias Astronómicas y Geofísicas de la Universidad Nacional de La Plata, Paseo del Bosque S/N, B1900FWA La Plata, Argentina 4Complejo Astronómico El Leoncito (CONICET - UNLP - UNC - UNSJ), San Juan, Argentina 5Departamento de Ciencias Físicas, Facultad de Ciencias Exactas, Universidad Andres Bello, Santiago, Chile ... ABSTRACT We present an extension of our previous research on the early-type galaxy population of the Antlia cluster (d ∼ 35 Mpc), achieving a total coverage of ∼ 2.6 deg2 and performing surface photometry for ∼ 300 galaxies, 130 of which are new uncatalogued ones. Such new galaxies mainly fall in the low surface brightness (LSB) regime, but there are also some lenticulars (S0) which support the existence of unique functions that connect bright and dwarf galaxies in the scaling relations. We analyse the projected spatial distribution of galaxies up to a distance of ∼ 800 kpc from NGC 3268, the adopted centre, as well as the radial velocity distribution and the correlation between galaxy colour and effective radius with the projected spatial distribution. We also obtain the luminosity function of the early-type galaxies and the distribution of stellar masses using the T1-band magnitudes and adopted mass-luminosity ratios. -
Cold Gas, Star Formation, and Substructure in the Nearby Antlia Cluster
University of Groningen KAT-7 science verification Hess, Kelley M.; Jarrett, T. H.; Carignan, Claude; Passmoor, Sean S.; Goedhart, Sharmila Published in: Monthly Notices of the Royal Astronomical Society DOI: 10.1093/mnras/stv1372 IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2015 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Hess, K. M., Jarrett, T. H., Carignan, C., Passmoor, S. S., & Goedhart, S. (2015). KAT-7 science verification: Cold gas, star formation, and substructure in the nearby Antlia Cluster. Monthly Notices of the Royal Astronomical Society, 452(2), 1617-1636. https://doi.org/10.1093/mnras/stv1372 Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. -
Oriontelescopes.Com Oct
THE EVENING SKY FOR OCTOBER, 2014 NORTH Early October — 10 p.m. Mid October — 9 p.m. URSA MAJOR Late October — 8 p.m. Pointers Big Dipper M51 ζ M81 Winter Hexagon2281 M82 κ M101 LYNX BOÖTES URSA μ M37 AURIGA MINOR M I L K Y W A Y DRACO CAMELOPARDALIS M36 Polaris Little Dipper M38 Capella α CORONA 16,17 BOREALIS ε M1 6543 ν M13 SERPENS CAPUT Double M92 Cluster CEPHEUS Keystone M103 ρ 457 Algol β PERSEUS η M52 Aldebaran μ E M34 δ Vega C 7789 ε Double-Double L γ Hyades I M45 CASSIOPEIA ζ HERCULES P Pleiades M39 Deneb LYRA T TRIANGULUM ORION I M31 α C 7243 M57 752 M110 CYGNUS EAST 7000 M29 χ M32 61 M56 (P a M33 6871 th β o ANDROMEDA Albireo f ARIES OPHIUCHUS WEST S LACERTA Summer Triangle u n TAURUS & VULPECULA I.4665 p γ M27 la n 6633 et s) SAGITTA E 70 Q Great Square DELPHINUS U γ A T γ PISCES of Pegasus O ϑ M14 R PEGASUS M15 Altair Uranus α γ ζ SERPENS EQUULEUS CAUDA Mira ο TX AQUILA M I L KM11 Y W A Y SCUTUM M26 ζ M2 M16 ERIDANUS M17 Neptune M18 AQUARIUS α M24 M25 CETUS M28 M22 7293 FORNAX 253 M30 SAGITTARIUS CAPRICORNUS Teapot Fomalhaut M55 SCULPTOR PISCIS AUSTRINUS 0 55 MICROSCOPIUM 0 20 Star magnitudes N IO R TI Moon IL PHOENIX W Phases GRUS –1 012345 FIRST Oct. 1 SOUTH Double star FULL How To Use This Chart Variable star Oct. -
The Properties of Galaxies in the Virgo and Fornax Clusters: What We've
The Properties of Galaxies in the Virgo and Fornax Clusters: What We’ve Learned Patrick Côté (HIA) HST Observations (11/07) Virgo Fornax solar system star clusters galaxies/AGN other stars ISM/nebulae galaxy clusters 30 March - 3 April, 2009, “Galaxy Evolution and Environment”, Kuala Lumpur, Malaysia Talk Outline • The Virgo and Fornax Clusters in Context • Properties at a Glance stellar nuclei globular AGNs/SBHs & SBHs cluster systems Virgo luminosity red sequence & functions galaxy scaling Fornax relations diffuse light cluster & the ICM structure & UCDS, cEs morphology • A Look Ahead: The Next Generation Virgo Cluster Survey • Summary and Conclusions Virgo and Fornax at a Glance Virgo Fornax Richness Class 1 0 Ω ≈ 100 deg2 ≈ 10 deg2 Distance 16.5 ± 0.1 ± 1.1 Mpc 20.0 ± 0.3 ± 1.4 Mpc σ(vr) ≈ 750 km/s (A), 400 km/s (B) 374 ± 26 km/s R200 1.55 ± 0.06 Mpc (5.4 ± 0.2 deg) ≈ 0.67 Mpc (1.9 deg): Rs 0.56 ± 0.18 Mpc (1.9 ± 0.6 deg) ≈ 50 kpc (0.14 deg): c 2.8 ± 0.7 13.4: 14 13 M200 (4.2 ± 0.5)×10 M⦿ ~ 1.3×10 M⦿ Mgas/Mtot 8-14% (A), ≈ 0.5% (B) ~ 8% Mgal/Mtot 3-4% (A), ≈ 4% (B) ~ 6% ‹kT›x 2.58 ± 0.03 keV 1.20 ± 0.04 keV ‹Fe›x 0.34 ± 0.02 solar 0.23 ± 0.03 solar Virgo and Fornax at a Glance Virgo Fornax Richness Class 1 0 Ω ≈ 100 deg2 ≈ 10 deg2 Distance 16.5 ± 0.1 ± 1.1 Mpc 20.0 ± 0.3 ± 1.4 Mpc σ(vr) ≈ 750 km/s (A), 400 km/s (B) 374 ± 26 km/s R200 1.55 ± 0.06 Mpc (5.4 ± 0.2 deg) ≈ 0.67 Mpc (1.9 deg): Rs 0.56 ± 0.18 Mpc (1.9 ± 0.6 deg) ≈ 50 kpc (0.14 deg): c 2.8 ± 0.7 13.4: 14 13 M200 (4.2 ± 0.5)×10 M⦿ ~ 1.3×10 M⦿ Mgas/Mtot 8-14% (A), ≈ 0.5% (B) ~ 8% Mgal/Mtot 3-4% (A), ≈ 4% (B) ~ 6% ‹kT›x 2.58 ± 0.03 keV 1.20 ± 0.04 keV ‹Fe›x 0.34 ± 0.02 solar 0.23 ± 0.03 solar Cluster Morphology: Virgo • Smith and Shapley (1930s), Reaves (1950s-1980s), de Vaucouleurs et al.