Hubble Steals a Look at NGC 1222 11 November 2016

Image: Hubble steals a look at NGC 1222 11 November 2016 galaxy. Although its peculiarities were first seen in photographic images, these were not able to reveal the level of fine detail that can be recovered by Hubble. The image taken by Hubble allows us to see an astonishing amount of structure in this galaxy, emphasizing its colorful history. Against the smooth background of old stars that was the original lenticular galaxy, we can clearly see dark filaments of dust and bright filaments of gas, both associated with the powerful star formation process. Provided by NASA Credit: ESA/NASA NGC 1222, seen in this image taken with the Wide Field Camera 3 on board the NASA/ESA Hubble Space Telescope is a galaxy with a rather eventful story to tell. NGC 1222 has been described as a peculiar example of a type of galaxy known as a lenticular galaxy. Astronomers think that NGC 1222 is in the process of swallowing up two much smaller dwarf galaxies that strayed too close to it. It is likely that the encounter was the trigger for the starburst in NGC 1222, bringing in fresh supplies of gas that are now fueling the burst of star formation. Typically, this kind of galaxy would present a rather smooth appearance on the sky and would consist mostly of old, reddish stars. A bit dull, perhaps. But NGC 1222 is certainly not a typical member of its class—and it's anything but dull. Observations show the characteristic features of very recent star formation on a huge scale—an event known as a starburst. The reason for all this violent activity is caused by the fact that NGC 1222 is not alone. It actually contains three compact regions, each of which appears to be the central nucleus of a 1 / 2 APA citation: Image: Hubble steals a look at NGC 1222 (2016, November 11) retrieved 1 October 2021 from https://phys.org/news/2016-11-image-hubble-ngc.html This document is subject to copyright. Apart from any fair dealing for the purpose of private study or research, no part may be reproduced without the written permission. The content is provided for information purposes only. 2 / 2 Powered by TCPDF (www.tcpdf.org).

Copy Link

Recommended publications

IRAC Near-Infrared Features in the Outer Parts of S4G Galaxies
Mon. Not. R. Astron. Soc. 000, 1{26 (2014) Printed 15 June 2018 (MN LATEX style file v2.2) Spitzer/IRAC Near-Infrared Features in the Outer Parts of S4G Galaxies Seppo Laine,1? Johan H. Knapen,2;3 Juan{Carlos Mu~noz{Mateos,4:5 Taehyun Kim,4;5;6;7 SébastienComerón,8;9 Marie Martig,10 Benne W. Holwerda,11 E. Athanassoula,12 Albert Bosma,12 Peter H. Johansson,13 Santiago Erroz{Ferrer,2;3 Dimitri A. Gadotti,5 Armando Gil de Paz,14 Joannah Hinz,15 Jarkko Laine,8;9 Eija Laurikainen,8;9 Kar´ınMenéndez{Delmestre,16 Trisha Mizusawa,4;17 Michael W. Regan,18 Heikki Salo,8 Kartik Sheth,4;1;19 Mark Seibert,7 Ronald J. Buta,20 Mauricio Cisternas,2;3 Bruce G. Elmegreen,21 Debra M. Elmegreen,22 Luis C. Ho,23;7 Barry F. Madore7 and Dennis Zaritsky24 1Spitzer Science Center - Caltech, MS 314-6, Pasadena, CA 91125, USA 2Instituto de Astrof´ısica de Canarias, E-38205 La Laguna, Tenerife, Spain 3Departamento de Astrof´ısica, Universidad de La Laguna, 38206 La Laguna, Spain 4National Radio Astronomy Observatory/NAASC, Charlottesville, 520 Edgemont Road, VA 22903, USA 5European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile 6Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea 7The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA 8Division of Astronomy, Department of Physics, University of Oulu, P.O. Box 3000, 90014 Oulu, Finland 9Finnish Centre of Astronomy with ESO (FINCA), University of Turku, Väisäläntie20, FIN-21500 Piikkiö 10Max-Planck Institut fürAstronomie, Königstuhl17 D-69117 Heidelberg, Germany 11Leiden Observatory, Leiden University, P.O.
[Show full text]
The Applicability of Far-Infrared Fine-Structure Lines As Star Formation
A&A 568, A62 (2014) Astronomy DOI: 10.1051/0004-6361/201322489 & c ESO 2014 Astrophysics The applicability of far-infrared ﬁne-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types? Ilse De Looze1, Diane Cormier2, Vianney Lebouteiller3, Suzanne Madden3, Maarten Baes1, George J. Bendo4, Médéric Boquien5, Alessandro Boselli6, David L. Clements7, Luca Cortese8;9, Asantha Cooray10;11, Maud Galametz8, Frédéric Galliano3, Javier Graciá-Carpio12, Kate Isaak13, Oskar Ł. Karczewski14, Tara J. Parkin15, Eric W. Pellegrini16, Aurélie Rémy-Ruyer3, Luigi Spinoglio17, Matthew W. L. Smith18, and Eckhard Sturm12 1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium e-mail: [email protected] 2 Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle Str. 2, 69120 Heidelberg, Germany 3 Laboratoire AIM, CEA, Université Paris VII, IRFU/Service d0Astrophysique, Bat. 709, 91191 Gif-sur-Yvette, France 4 UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK 5 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 6 Laboratoire d0Astrophysique de Marseille − LAM, Université Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille CEDEX 13, France 7 Astrophysics Group, Imperial College, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK 8 European Southern Observatory, Karl
[Show full text]
0 Luminous Compact Blue Galaxies
Graduate Theses, Dissertations, and Problem Reports 2015 Evolution of z ~ 0 Luminous Compact Blue Galaxies Katherine Rabidoux Follow this and additional works at: https://researchrepository.wvu.edu/etd Recommended Citation Rabidoux, Katherine, "Evolution of z ~ 0 Luminous Compact Blue Galaxies" (2015). Graduate Theses, Dissertations, and Problem Reports. 6464. https://researchrepository.wvu.edu/etd/6464 This Dissertation is protected by copyright and/or related rights. It has been brought to you by the The Research Repository @ WVU with permission from the rights-holder(s). You are free to use this Dissertation in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you must obtain permission from the rights-holder(s) directly, unless additional rights are indicated by a Creative Commons license in the record and/ or on the work itself. This Dissertation has been accepted for inclusion in WVU Graduate Theses, Dissertations, and Problem Reports collection by an authorized administrator of The Research Repository @ WVU. For more information, please contact [email protected]. Evolution of z 0 Luminous Compact Blue Galaxies ∼ Katie Rabidoux Dissertation submitted to the Eberly College of Arts and Sciences at West Virginia University in partial fulﬁllment of the requirements for the degree of Doctor of Philosophy in Physics Dr. D.J. Pisano, Ph.D., Chair Dr. Loren Anderson, Ph.D. Dr. Amy Keesee, Ph.D. Dr. Dave Frayer, Ph.D. Dr. Yu Gu, Ph.D. Department of Physics and
[Show full text]
The Atlas3d Project-V. the CO Tully-Fisher Relation of Early-Type
Mon. Not. R. Astron. Soc. 000, 1–17 (2009) Printed 1 November 2018 (MN LATEX style ﬁle v2.2) The ATLAS3D project – V. The CO Tully-Fisher relation of early-type galaxies Timothy A. Davis1?, Martin Bureau1, Lisa M. Young2y, Katherine Alatalo3, Leo Blitz3, Michele Cappellari1, Nicholas Scott1, Maxime Bois4;5, Fred´ eric´ Bournaud6, Roger L. Davies1, P. Tim de Zeeuw4;7, Eric Emsellem4;5, Sadegh Khochfar8, Davor Krajnovic´4, Harald Kuntschner9, Pierre-Yves Lablanche5, Richard M. McDermid10, Raffaella Morganti11;12, Thorsten Naab13, Tom Oosterloo11;12, Marc Sarzi14, Paolo Serra11, and Anne-Marie Weijmans15z 1Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK 2Physics Department, New Mexico Institute of Mining and Technology, Socorro, NM 87801, USA 3Department of Astronomy, Campbell Hall, University of California, Berkeley, CA 94720, USA 4European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 5Universite´ Lyon 1, Observatoire de Lyon, Centre de Recherche Astrophysique de Lyon and Ecole Nationale Superieure´ de Lyon, 9 avenue Charles Andre,´ F-69230 Saint-Genis Laval, France 6Laboratoire AIM Paris-Saclay, CEA/IRFU/SAp CNRS Universite´ Paris Diderot, 91191 Gif-sur-Yvette Cedex, France 7Sterrewacht Leiden, Leiden University, Postbus 9513, 2300 RA Leiden, the Netherlands 8Max Planck Institut fur¨ extraterrestrische Physik, PO Box 1312, D-85478 Garching, Germany 9Space Telescope European Coordinating Facility, European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 10Gemini Observatory, Northern Operations Centre, 670 N. A‘ohoku Place, Hilo, HI 96720, USA 11Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands 12Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands 13Max-Planck-Institut fur¨ Astrophysik, Karl-Schwarzschild-Str.
[Show full text]
GALEX UV COLOR RELATIONS for NEARBY EARLY-TYPE GALAXIES Jose´ Donas,1 Jean-Michel Deharveng,1 R
The Astrophysical Journal Supplement Series, 173:597Y606, 2007 December # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALEX UV COLOR RELATIONS FOR NEARBY EARLY-TYPE GALAXIES Jose´ Donas,1 Jean-Michel Deharveng,1 R. Michael Rich,2 Sukyoung K. Yi,3 Young-Wook Lee,3 Alessandro Boselli,1 Armando Gil de Paz,4 Samuel Boissier,1 Ste´phane Charlot,5 Samir Salim,2 Luciana Bianchi,6 Tom A. Barlow,7 Karl Forster,7 Peter G. Friedman,7 Timothy M. Heckman,8 Barry F. Madore,9 D. Christopher Martin,7 Bruno Milliard,1 Patrick Morrissey,7 Susan G. Neff,10 David Schiminovich,11 Mark Seibert,7 Todd Small,7 Alex S. Szalay,8 Barry Y. Welsh,12 and Ted K. Wyder7 Received 2006 May 4; accepted 2006 July 20 ABSTRACT We use GALEX/optical photometry to construct color-color relationships for early-type galaxies sorted by mor- phological type. We have matched objects in the GALEX GR1 public release and the ﬁrst IR1.1 internal release, with the RC3 early-type galaxies having a morphological type À5:5 T < À1:5, with mean error on T < 1:5 and mean error on (B À V )T < 0:05. After visual inspection of each match, we are left with 130 galaxies with reliable GALEX pipeline photometry in the far-UVand near-UV bands. This sample is divided into ellipticals (À5:5 T < À3:5) and lenticulars (À3:5 T < À1:5). After correction for Galactic extinction, the color-color diagrams FUV À NUV versus (B À V )Tc are plotted for the two subsamples.
[Show full text]
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it.
[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]
HERSCHEL SPECTROSCOPY of EARLY TYPE GALAXIES Ryen Carl Lapham and Lisa M
Draft version November 7, 2018 Preprint typeset using LATEX style emulateapj v. 12/16/11 HERSCHEL SPECTROSCOPY OF EARLY TYPE GALAXIES Ryen Carl Lapham and Lisa M. Young Physics Department, New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801; [email protected], [email protected] and Alison Crocker Physics Department, Reed College, Portland, OR 97202; [email protected] Draft version November 7, 2018 ABSTRACT We present Herschel spectroscopy of atomic lines arising in photodissociation regions as well as ion- ization regions of nearby early-type galaxies (ETGs), focusing on the volume-limited Atlas3D sample. Our data include the [C II], [O I], and [N II] 122 and 205 µm lines, along with ancillary data includ- ing CO and H I maps. We find ETGs have [C II]/FIR ratios slightly lower than spiral galaxies in the KINGFISH sample, and several ETGs have unusually large [N II] 122/[C II] ratios. The [N II] 122/[C II] ratio is correlated with UV colors and there is a strong anti-correlation of [C II]/FIR with NUV-K seen in both spirals and ETGs, likely due to a softer radiation field with fewer photons avail- able to ionize carbon and heat the gas. The correlation thus makes a [C II] deficit in galaxies with redder stellar populations. The high [N II] 122/[C II] (and low [C II]/FIR) line ratios could also be affected by the removal of much of the diffuse, low density gas, which is consistent with the low H I/H2 ratios.
[Show full text]
A COMPENDIUM of FAR-INFRARED LINE and CONTINUUM EMISSION for 227 GALAXIES OBSERVED by the INFRARED SPACE OBSERVATORY James R
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Caltech Authors The Astrophysical Journal Supplement Series, 178:280Y301, 2008 October A # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. A COMPENDIUM OF FAR-INFRARED LINE AND CONTINUUM EMISSION FOR 227 GALAXIES OBSERVED BY THE INFRARED SPACE OBSERVATORY James R. Brauher,1 Daniel A. Dale,2 and George Helou1 Received 2008 March 25; accepted 2008 May 19 ABSTRACT Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wave- length Spectrometer on the Infrared Space Observatory. The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or H ii regions: [O iii]52m, [N iii]57m, [O i]63m, [O iii]88m, [N ii]122m, [O i] 145 m, and [C ii]158m. Molecular lines such as OH at 53, 79, 84, 119, and 163 m, and H 2O at 58, 66, 75, 101, and 108 m are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detec- tions of Milky Way [C ii]158m and an unidentified line near 74 m in NGC 1068 are also reported. Finally, con- tinuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170 m are derived for a subset of galaxies in which the far-infrared emission is contained within the 7500 ISO LWS beam.
[Show full text]
TABLE 1 Explanation of CVRHS Symbols A
TABLE 1 Explanation of CVRHS Symbols a Symbol Description 1 2 General Terms ETG An early-type galaxy, collectively referring to a galaxy in the range of types E to Sa ITG An intermediate-type galaxy, taken to be in the range Sab to Sbc LTG A late-type galaxy, collectively referring to a galaxy in the range of types Sc to Im ETS An early-type spiral, taken to be in the range S0/a to Sa ITS An intermediate-type spiral, taken to be in the range Sab to Sbc LTS A late-type spiral, taken to be in the range Sc to Scd XLTS An extreme late-type spiral, taken to be in the range Sd to Sm classical bulge A galaxy bulge that likely formed from early mergers of smaller galaxies (Kormendy & Kennicutt 2004; Athanassoula 2005) pseudobulge A galaxy bulge made of disk material that has secularly collected into the central regions of a barred galaxy (Kormendy 2012) PDG A pure disk galaxy, a galaxy lacking a classical bulge and often also lacking a pseudobulge Stage stage The characteristic of galaxy morphology that recognizes development of structure, the widespread distribution of star formation, and the relative importance of a bulge component along a sequence that correlates well with basic characteristics such as integrated color, average surface brightness, and HI mass-to-blue luminosity ratio Elliptical Galaxies E galaxy A galaxy having a smoothly declining brightness distribution with little or no evidence of a disk component and no inﬂections (such as lenses) in the luminosity distribution (examples: NGC 1052, 3193, 4472) En An elliptical galaxy
[Show full text]
Star Formation and Nuclear Activity of Local Luminous Infrared Galaxies
PhD Thesis Star Formation and Nuclear Activity of Local Luminous Infrared Galaxies Memoria de tesis doctoral presentada por D. Miguel Pereira Santaella para optar al grado de Doctor en Ciencias F´ısicas Universidad Autónoma Consejo Superior de Madrid de Investigaciones Cient´ıficas Facultad de Ciencias Instituto de Estructura de la Materia Departamento de F´ısica Teórica Centro de Astrobiolog´ıa Madrid, noviembre de 2011 Directora: Dra. Almudena Alonso Herrero Instituto de F´ısica de Cantabria Tutora: Prof.ª Rosa Dom´ınguez Tenreiro Universidad Autónoma de Madrid Agradecimientos En primer lugar quer´ıadar las gracias a mi directora de tesis, Almudena Alonso Herrero, por haber confiado en mi desde un principio para realizar este trabajo, as´ı como por todo su interés y dedicación durante estos cuatro años. Además me gustar´ıa agradecer la ayuda y consejos de Luis Colina. En este tiempo he tenido la oportunidad de realizar estancias en centros de in- vestigación extranjeros de los que guardo un grato recuerdo personal y cient´ıfico. En particular me gustar´ıaagradecer a George Rieke y a Martin Ward su hospitalidad y amabilidad durante mis visitas al Steward Observatory en la Universidad de Arizona y a la Universidad de Durham. Y volviendo a Madrid, quisiera agradecer a Tanio y a Marce el apoyo y la ayuda que me ofrecieron en los inciertos comienzos de este proyecto. También quiero dar las gra- cias a todos (Arancha, Nuria, Alvaro,´ Alejandro, Julia, Jairo, Javier, Ruymán, Fabián, entre otros) por las interesantes conversaciones, a veces incluso sobre ciencia, en las sobremesas, cafés, etc.
[Show full text]
Early-Type Galaxies with Tidal Debris and Their Scaling Relations in the Spitzer Survey of Stellar Structure in Galaxies (S4g)
The Astrophysical Journal, 753:43 (18pp), 2012 July 1 doi:10.1088/0004-637X/753/1/43 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. EARLY-TYPE GALAXIES WITH TIDAL DEBRIS AND THEIR SCALING RELATIONS IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) Taehyun Kim1,2,3, Kartik Sheth1,4,5,JoannahL.Hinz6, Myung Gyoon Lee3, Dennis Zaritsky6, Dimitri A. Gadotti2, Johan H. Knapen7,8, Eva Schinnerer9, Luis C. Ho10, Eija Laurikainen11,12, Heikki Salo11, E. Athanassoula13, Albert Bosma13, Bonita de Swardt14, Juan-Carlos Munoz-Mateos˜ 1, Barry F. Madore10,Sebastien´ Comeron´ 15, Michael W. Regan16,Kar´ın Menendez-Delmestre´ 17, Armando Gil de Paz18, Mark Seibert10, Jarkko Laine11, Santiago Erroz-Ferrer7,8, and Trisha Mizusawa1,4,5 1 National Radio Astronomy Observatory/NAASC, 520 Edgemont Road, Charlottesville, VA 22903, USA 2 European Southern Observatory, Casilla 19001, Santiago 19, Chile 3 Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Republic of Korea 4 Spitzer Science Center, 1200 East California Boulevard, Pasadena, CA 91125, USA 5 Infrared Processing and Analysis Center, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA 6 Steward Observatory University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA 7 Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain 8 Departamento de Astrof´ısica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain 9 Max-Planck-Institut fur¨ Astronomie,
[Show full text]