Annual Report 2011 Facts and Figures of 2011
Total Page:16
File Type:pdf, Size:1020Kb

Load more
Recommended publications
-
ESO to Build World's Biggest Eye on the Sky 11 June 2012
ESO to build world's biggest eye on the sky 11 June 2012 36/) and Switzerland voted in favour of the start of the E-ELT programme. Four further countries voted in favour ad referendum: Belgium, Finland, Italy, and the United Kingdom. The remaining four Member States are actively working towards joining the programme in the near future. Following the resolution, spending on elements of the project other than the initial civil works will not commence until the contributions pledged by the Member States, as agreed in the funding principles Artist's impression of the European Extremely Large approved by Council in late 2011, exceed 90% of Telescope (E-ELT) in its enclosure on Cerro Armazones, the 1083 million euro cost-to-completion (at 2012 a 3060-metre mountaintop in Chile's Atacama Desert. The 39.3-meter E-ELT will be the largest optical/infrared prices). telescope in the world -- the world's biggest eye on the sky. Operations are planned to start early in the next On the current schedule the first large E-ELT decade, and the E-ELT will tackle some of the biggest industrial contracts would have to be approved and scientific challenges of our time. Credit: ESO/L. Calçada major funding committed within the next year. This is expected to provide sufficient time for the conditions to be satisfied: the confirmations of the votes from Belgium, Finland, Italy, and the United ESO's governing body, the Council, met today, at Kingdom; other Member States to join the project; the ESO Headquarters in Garching, Germany. -
Libro Resumen Sea2016v55 0.Pdf
2 ...................................................................................................................................... 4 .................................................................................................. 4 ........................................................................................................... 4 PATROCINADORES .................................................................................................................... 5 RESUMEN PROGRAMA GENERAL ............................................................................................ 7 PLANO BIZKAIA ARETOA .......................................................................................................... 8 .......................................................................................... 9 CONFERENCIAS PLENARIAS ................................................................................................... 14 ............................................................................................. 19 ................................................................................................ 21 ............... 23 CIENCIAS PLANETARIAS ......................................................................................................... 25 - tarde ....................................................................................................... 25 - ............................................................................................ 28 - tarde ................................................................................................ -
HST-ACS Photometry of the Isolated Dwarf Galaxy VV124=UGC 4879
A&A 533, A37 (2011) Astronomy DOI: 10.1051/0004-6361/201117275 & c ESO 2011 Astrophysics HST-ACS photometry of the isolated dwarf galaxy VV124=UGC 4879 Detection of the blue horizontal branch and identification of two young star clusters, M. Bellazzini1,S.Perina1, S. Galleti1, and T. Oosterloo2 1 INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: [email protected] 2 Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands Received 17 May 2011 / Accepted 9 July 2011 ABSTRACT We present deep V and I photometry of the isolated dwarf galaxy VV124=UGC 4879, obtained from archival images taken with the Hubble Space Telescope – Advanced Camera for Surveys. In the color-magnitude diagrams of stars at distances greater than 40 from the center of the galaxy, we clearly identify a well-populated, old horizontal branch (HB) for the first time. We show that the distribution of these stars is more extended than that of red clump stars. This implies that very old and metal-poor populations 4 dominate in the outskirts of VV124. We also identify a massive (M = 1.2 ± 0.2 × 10 M) young (age = 250 ± 50 Myr) star cluster 3 (C1), as well as another of younger age (C2, ∼<30 ± 10 Myr) with a mass similar to classical open clusters (M ≤ 3.3 ± 0.5 × 10 M). Both clusters lie at projected distances less than 100 pc from the center of the galaxy. -
Recent Results from the SAURON Galaxy Survey Tim De Zeeuw
Recent Results from the SAURON Galaxy Survey Tim de Zeeuw European Southern Observatory Abstract Much world-wide effort is devoted to the study of the formation and evolution of galaxies, ranging from observations of the most distant objects in the early Universe to detailed analysis of the motions of individual stars in the Milky Way, combined with theoretical work and numerical simulations. Integral field spectroscopy makes it possible to measure the motions en physical properties of stellar populations in nearby galaxies, and to determine the properties of the supermassive black holes in their centres. A representative survey of nearby early-type galaxies and spiral bulges with SAURON, a panoramic integral-field spectrograph custom-built for the UK/NL/E 4.2m William Herschel Telescope on La Palma, reveals a fascinating diversity of properties. The stellar and gaseous kinematics and the line-strength distributions provide the intrinsic shape of the galaxies, their orbital structure, the mass-to-light ratio as a function of radius, the frequency and structure of kinematically decoupled cores, the masses of nuclear black holes, and the relation between orbital structure and the age and metallicity of the stellar populations. This 'fossil record' gives key insight into the galaxy formation process. The talk will summarize recent results of the SAURON survey, and briefly discuss the next steps. Resume Tim de Zeeuw received his PhD degree from Leiden University. He worked at the Institute for Advanced Study and Caltech before returning to Leiden as professor of astronomy. His research focuses on the formation, structure and dynamics of galaxies. He directed the Netherlands Research School for Astronomy and Leiden Observatory, and served on oversight committees for AURA, ESA, ESO and NASA. -
An Observer's Guide to the (Local Group) Dwarf Galaxies: Predictions for Their Own Dwarf Satellite Populations
An observer's guide to the (Local Group) dwarf galaxies: predictions for their own dwarf satellite populations The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Dooley, Gregory A. et al. “An Observer’s Guide to the (Local Group) Dwarf Galaxies: Predictions for Their Own Dwarf Satellite Populations.” Monthly Notices of the Royal Astronomical Society 471, 4 (August 2017): 4894–4909 © 2018 The Author(s) As Published http://dx.doi.org/10.1093/MNRAS/STX1900 Publisher Oxford University Press (OUP) Version Author's final manuscript Citable link https://hdl.handle.net/1721.1/121369 Terms of Use Creative Commons Attribution-Noncommercial-Share Alike Detailed Terms http://creativecommons.org/licenses/by-nc-sa/4.0/ MNRAS 000,1{21 (2017) Preprint 6 September 2017 Compiled using MNRAS LATEX style file v3.0 An observer's guide to the (Local Group) dwarf galaxies: predictions for their own dwarf satellite populations Gregory A. Dooley1?, Annika H. G. Peter2;3, Tianyi Yang4, Beth Willman5, Brendan F. Griffen1 and Anna Frebel1, 1Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 2CCAPP and Department of Physics, The Ohio State University, Columbus, OH 43210, USA 3Department of Astronomy, The Ohio State University, Columbus OH 43210, USA 4Institute of Optics, University of Rochester, Rochester, New York, 14627, USA 5Steward Observatory and LSST, 933 North Cherry Avenue, Tucson, AZ 85721, USA Accepted by MNRAS 2017 July 22. Received 2017 July 22; in original 2016 September 27 ABSTRACT A recent surge in the discovery of new ultrafaint dwarf satellites of the Milky Way has 3 6 inspired the idea of searching for faint satellites, 10 M < M∗ < 10 M , around less massive field galaxies in the Local Group. -
Draft181 182Chapter 10
Chapter 10 Formation and evolution of the Local Group 480 Myr <t< 13.7 Gyr; 10 >z> 0; 30 K > T > 2.725 K The fact that the [G]alactic system is a member of a group is a very fortunate accident. Edwin Hubble, The Realm of the Nebulae Summary: The Local Group (LG) is the group of galaxies gravitationally associ- ated with the Galaxy and M 31. Galaxies within the LG have overcome the general expansion of the universe. There are approximately 75 galaxies in the LG within a 12 diameter of ∼3 Mpc having a total mass of 2-5 × 10 M⊙. A strong morphology- density relation exists in which gas-poor dwarf spheroidals (dSphs) are preferentially found closer to the Galaxy/M 31 than gas-rich dwarf irregulars (dIrrs). This is often promoted as evidence of environmental processes due to the massive Galaxy and M 31 driving the evolutionary change between dwarf galaxy types. High Veloc- ity Clouds (HVCs) are likely to be either remnant gas left over from the formation of the Galaxy, or associated with other galaxies that have been tidally disturbed by the Galaxy. Our Galaxy halo is about 12 Gyr old. A thin disk with ongoing star formation and older thick disk built by z ≥ 2 minor mergers exist. The Galaxy and M 31 will merge in 5.9 Gyr and ultimately resemble an elliptical galaxy. The LG has −1 vLG = 627 ± 22 km s with respect to the CMB. About 44% of the LG motion is due to the infall into the region of the Great Attractor, and the remaining amount of motion is due to more distant overdensities between 130 and 180 h−1 Mpc, primarily the Shapley supercluster. -
The Rotation of the Halo of NGC6822 Determined from the Radial Velocities of Carbon Stars
The rotation of the halo of NGC6822 determined from the radial velocities of carbon stars { Graham Peter Thompson { Centre for Astrophysics Research School of Physics, Astronomy and Mathematics University of Hertfordshire Submitted to the University of Hertfordshire in part fulfilment of the requirements of the degree of Master of Philosophy in Astrophysics Supervisor: Professor Sean G. Ryan { April 2016 { Declaration I hereby certify that this dissertation has been written by me in the School of Physics, Astronomy and Mathematics, University of Hertfordshire, Hatfield, Hertfordshire, and that it has not been submitted in any previous application for a higher degree. The core of the dissertation is based on original work conducted at the University of Hertfordshire, and some of the ideas for further work are drawn from topics studied during an earlier Master of Science. All material in this dissertation which is not my own work has been properly acknowledged. { Graham Peter Thompson { ii Acknowledgements I thank Professor Ryan for his invaluable support and patient guidance as my super- visor, throughout this study. His incisive questioning, thoughtful comments, helpful suggestions and, at times, hands-on assistance throughout the study, preparation of a paper to MNRAS and the writing of this dissertation have been invaluable. I thank also Dr Lisette Sibbons, whose work on the spectral classification of carbon stars in NGC 6822 was the genesis of my study. Dr Sibbons was responsible for the acquisition and reduction of the spectra I used in the study. She also provided me with background information related to the stars in the sample, and general advice. -
Perseus I and the NGC 3109 Association in the Context of the Local Group Dwarf Galaxy Structures
MNRAS 440, 908–919 (2014) doi:10.1093/mnras/stu321 Advance Access publication 2014 March 15 Perseus I and the NGC 3109 association in the context of the Local Group dwarf galaxy structures Marcel S. Pawlowski‹ and Stacy S. McGaugh Department of Astronomy, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, OH 44106, USA Accepted 2014 February 13. Received 2014 February 13; in original form 2014 January 8 ABSTRACT The recently discovered dwarf galaxy Perseus I appears to be associated with the dominant Downloaded from plane of non-satellite galaxies in the Local Group (LG). We predict its velocity dispersion and those of the other isolated dwarf spheroidals Cetus and Tucana to be 6.5, 8.2 and 5.5 km s−1, respectively. The NGC 3109 association, including the recently discovered dwarf galaxy Leo P, aligns with the dwarf galaxy structures in the LG such that all known nearby non-satellite http://mnras.oxfordjournals.org/ galaxies in the northern Galactic hemisphere lie in a common thin plane (rms height 53 kpc; diameter 1.2 Mpc). This plane has an orientation similar to the preferred orbital plane of the Milky Way (MW) satellites in the vast polar structure. Five of seven of these northern galaxies were identified as possible backsplash objects, even though only about one is expected from cosmological simulations. This may pose a problem, or instead the search for local backsplash galaxies might be identifying ancient tidal dwarf galaxies expelled in a past major galaxy encounter. The NGC 3109 association supports the notion that material preferentially falls towards the MW from the Galactic south and recedes towards the north, as if the MW were moving through a stream of dwarf galaxies. -
ESO@50 — the First 50 Years of ESO Held at ESO Headquarters, Garching, Germany, 3–7 September 2012
Astronomical News Report on the Workshop ESO@50 — The First 50 Years of ESO held at ESO Headquarters, Garching, Germany, 3–7 September 2012 Jeremy Walsh1 Young stars and planets Transients Eric Emsellem1 Michael West1 ESO’s next major milestone, the Atacama Steven Smartt (Belfast) summarised Large Millimeter/submillimeter Array detection and follow-up surveys for bright (ALMA) featured strongly in the first few transients which have recently begun at 1 ESO talks. Some of the first Cycle 0 results La Silla Observatory. The La Silla–QUEST in young stars and star-forming regions survey (see Baltay et al., p. 34) produces were presented by Leonardo Testi (ESO) transient alerts within days and these In recognition of the 50th anniversary where the high spatial resolution and sen- are followed up spectroscopically by the of the signing of the ESO Convention, a sitivity of ALMA will bring many ad vances. Public ESO Survey of Transient Objects special science workshop was held at The field of astrochemistry was covered (PESSTO) with EFOSC on the New Tech- ESO Headquarters in Garching to focus by Ewine van Dishoeck (Leiden), con- nology Telescope (NTT). on the main scientific topics where centrating on very high spectral resolution, ESO has made important contributions, including some ALMA spectra from pro- The Very Large Telescope (VLT) was very from Solar System astronomy to funda toplanetary discs, demonstrating the well timed for the beginning of the era mental physics, and to provide a per potential for finding new species (up to of observations of gamma-ray burst after- spective for future scientific challenges. -
Solo Dwarf Galaxy Survey: Exploring Dwarfs in the Local Group
Solo Dwarf Galaxy Survey: Exploring dwarfs in the Local Group Clare Higgs PhD Supervisor: Alan McConnachie August 1, 2019 Solo Collaboration: [email protected] M. Irwin, N. Annau, N. Bate, G. Lewis, M. Walker, P. Côté, K. Venn, G. Battaglia @astrohigglet Local Group and a little beyond. ➡ Inside 3 Mpc. Low mass. MV >-18 NEARBY ISOLATED DWARF GALAXIES Not within the virial radius of a large galaxy ➡ More than 300 kpc from M31 and the Milky Way Why … DWARF GALAXIES ‣ Sensitive probes of galaxy formation and evolution Why … NEARBY ‣ Resolved stellar populations Why … ISOLATED ‣ Intrinsic properties of low mass galaxies Solitary Local (Solo) Dwarf Galaxy Survey Solo Observations M Name Alt. Name RA Dec. Distance E(B V ) Tel. Filt. Notes HIObservations M M HI − ? HI M? [kpc] [Mags.] [106M ][106M ] h m s o WLM DDO221 00 01 58.2 15 27039” 933 34 0.030 M gi 2014B LITTLE THINGS 43 61 1.4 − ± C gi 2013B/2016B ” h m s o AndXVIII 00 02 14.5 +45 05020” 1355 81 0.102 C gi 2018B K.S. 2014 0.63 h m s o ± ESO410-G005 KK98 00 15 31.6 32 10048” 1923 35 0.013 M ugi 2012B 3.5 0.73 0.2 h m s − o ± Cetus 00 26 11.0 11 02040” 755 24 0.038 M gi 2014B K.S. 2014 2.6 − ± C g 2016B ” ” h m s o ESO294-G010 00 26 33.4 41 51019” 2032 37 0.013 M g i 2014B 2.7 0.34 0.1 h m s − o ± IC1613 DDO8 01 04 47.8 +02 07004” 755 42 0.030 M ugi 2012B LITTLE THINGS 100 65 0.7 ± C gi 2016B ” ” h m s o KKs3 02 24 44.4 73 30051” 2120 70 0.045 M gi 2017A h m s − o ± Perseus 03 01 22.8 +40 59017” 785 65 0.062 C gi 2016B h m s o ± Eridanus II 03 44 21.1 43 32000” 785 65 M gi 2017A h m s − -
ESO and the International Year of Astronomy 2009 Opening Ceremony
Astronomical News that LPs make use of an expensive The workshop overall was very success- complement the current arsenal of pro- resource and that they have to provide ful and clarified the need for, and the gramme types undertaken with ESO additional benefits for the community. competitive edge of, Large Programmes facilities at the upper end. It is planned to This has led to the requirement that at ESO facilities. The increased demand monitor their success in another work- reduced data from LPs, once published, for the 3.6-metre telescope after the shop in a few years time. should be returned to the ESO Archive time limit for LPs was raised to four years so that they can be used by other astron- speaks for itself. There are some very omers, possibly for different purposes. substantial programmes in progress, References The large investment by the community which will keep this telescope busy for Wagner, S. & Leibundgut, B. 2004, The Messenger, into LPs should justify this modest return. years to come. 115, 41 There was a lively discussion on how this return should be achieved and Beyond the Large Programmes, the Pub- whether it would put astronomers using lic Surveys with VISTA and VST will Notes ESO facilities at a disadvantage com- start during this year and next year. These 1 http://www.eso.org/sci/meetings/LP2008/program. pared to users of private observatories. will be truly massive projects, which html ESO and the International Year of Astronomy 2009 Opening Ceremony Pedro Russo1 2 Figure 1. Catherine Cesarky, IAU President, Lars Lindberg Christensen1 addressing the audience during the IYA2009 Opening Ceremony Douglas Pierce-Price1 Yours to Discover”. -
Spiral Galaxies of the Virgo Cluster: Eleven More Intermediate-Mass Black Hole Candidates with an Associated X-Ray Point-Source
Spiral galaxies of the Virgo cluster: Eleven more intermediate-mass black hole candidates with an associated X-ray point-source Journal: Monthly Notices of the Royal Astronomical Society Manuscript ID MN-20-5071-MJ Manuscript type: Main Journal Date Submitted by the 16-Dec-2020 Author: Complete List of Authors: Graham, Alister; Swinburne University of Technology, Centre for Astrophysics & Supercomputing Soria, Roberto; University of the Chinese Academy of Sciences, College of Astronomy and Space Sciences; Curtin University, International Centre for Radio Astronomy Research; The University of Sydney, Sydney Institute for Astronomy, School of Physics Davis, Benjamin; Swinburne University of Technology, Centre for Astrophysics and Supercomputing; New York University - Abu Dhabi Campus, Center for Astro, Particle, and Planetary Physics Kolehmainen, Mari; Universite de Strasbourg, Observatoire Astronomique Maccarone, Tom; Texas Tech University, Department of Physics Miller-Jones, James; Curtin University of Technology, Curtin Institute of Radio Astronomy Motch, Christian; University of Strasbourg, Observatoire Astronomique Swartz, Doug; Universities Space Research Association, NASA Marshall Space Flight Center galaxies: spiral < Galaxies, galaxies: active < Galaxies, galaxies: nuclei < Galaxies, galaxies: star clusters: general < Galaxies, (galaxies:) Keywords: quasars: supermassive black holes < Galaxies, X-rays: galaxies < Resolved and unresolved sources as a function of wavelength Page 1 of 22 1 2 3 A 4 MNRAS 000,1{22 (0000) Preprint 16 December 2020 Compiled using MNRAS L TEX style file v3.0 5 6 7 8 Spiral galaxies of the Virgo cluster: Eleven more 9 intermediate-mass black hole candidates with an associated 10 11 X-ray point-source 12 13 14 Alister W. Graham1?, Roberto Soria2;3;4, Benjamin L.