8 results on '"Bodo Ziegler"'
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2. The ELT-MOS (MOSAIC): towards the construction phase
- Author
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Francois Hammer, Simon Morris, Pascal Jagourel, Richard Myers, Olivier Le Fèvre, Alexis Finogenov, Jari Kotilainen, Bruno Castilho, Göran Östlin, Jose Afonso, Marc Dubbledam, Madeline Close, Phil Parr-Burman, Timothy Morris, Fanny Chemla, Fatima de Frondat, Andreas Kelz, Isabelle Guinouard, Ian Lewis, Kevin Middleton, Ramon Navarro, Marie Larrieu, Johan Pragt, Annemieke Janssen, Kjetil Dohlen, Kacem El Hadi, Eric Gendron, Yanbin Yang, Martyn Wells, Marc Conan, Thierry Fusco, Sylvestre Taburet, Mickael Frotin, Nadia Berkourn, Edwin Bergin, Mathieu Puech, Gavin Dalton, Myriam Rodrigues, Ruben Janssen, Ewan Fitzsimons, Beatriz Barbuy, Jean-Gabriel Cuby, Lex Kaper, Martin Roth, Gérard Rousset, Sofia Feltzing, Andreas Korn, Jesús Gallego, África Castillo Morales, Jorge Iglesias-Paramo, Laura Pentericci, Bodo Ziegler, Daniel Schaerer, Hideki Takami, Christopher Evans, Luc Simard, Beaussier, Catherine, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Oskar Klein Centre [Stockholm], Stockholm University, DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], and ONERA-Université Paris Saclay (COmUE)
- Subjects
[SDU] Sciences of the Universe [physics] ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,[SDU]Sciences of the Universe [physics] ,[SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph] ,ComputingMilieux_MISCELLANEOUS - Abstract
International audience
- Published
- 2018
3. Galaxy Evolution
- Author
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Bodo Ziegler
- Subjects
Space and Planetary Science ,Astronomy and Astrophysics - Published
- 2004
- Full Text
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4. The science case for multi-object spectroscopy on the European ELT
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Chris Evans, Mathieu Puech, Jose Afonso, Omar Almaini, Philippe Amram, Hervé Aussel, Beatriz Barbuy, Alistair Basden, Nate Bastian, Giuseppina Battaglia, Beth Biller, Piercarlo Bonifacio, Nicholas Bouché, Andy Bunker, Elisabetta Caffau, Stephane Charlot, Michele Cirasuolo, Yann Clenet, Francoise Combes, Chris Conselice, Thierry Contini, Jean-Gabriel Cuby, Gavin Dalton, Alex de Koter, Karen Disseau, Jim Dunlop, Benoît Epinat, Fabrizio Fiore, Sofia Feltzing, Annette Ferguson, Hector Flores, Adriano Fontana, Thierry Fusco, Dimitri Gadotti, Anna Gallazzi, Jesus Gallego, Emanuele Giallongo, Thiago Gonçalves, Damien Gratadour, Eike Guenther, Francois Hammer, Vanessa Hill, Marc Huertas-Company, Roridgo Ibata, Lex Kaper, Andreas Korn, Søren Larsen, Olivier Le Fèvre, Bertrand Lemasle, Claudia Maraston, Simona Mei, Yannick Mellier, Simon Morris, Göran Östlin, Thibaut Paumard, Roser Pello, Laura Pentericci, Celine Peroux, Patrick Petitjean, Myriam Rodrigues, Lucía Rodríguez-Muñoz, Daniel Rouan, Hugues Sana, Daniel Schaerer, Eduardo Telles, Scott Trager, Laurence Tresse, Niraj Welikala, Stefano Zibetti, and Bodo Ziegler
- Subjects
astro-ph.SR ,astro-ph.GA ,astro-ph.IM - Abstract
This White Paper presents the scientific motivations for a multi-object spectrograph (MOS) on the European Extremely Large Telescope (E-ELT). The MOS case draws on all fields of contemporary astronomy, from extra-solar planets, to the study of the halo of the Milky Way and its satellites, and from resolved stellar populations in nearby galaxies out to observations of the earliest 'first-light' structures in the partially-reionised Universe. The material presented here results from thorough discussions within the community over the past four years, building on the past competitive studies to agree a common strategy toward realising a MOS capability on the E-ELT. The cases have been distilled to a set of common requirements which will be used to define the MOSAIC instrument, entailing two observational modes ('high multiplex' and 'high definition'). When combined with the unprecedented sensitivity of the E-ELT, MOSAIC will be the world's leading MOS facility. In analysing the requirements we also identify a high-multiplex MOS for the longer-term plans for the E-ELT, with an even greater multiplex (>1000 targets) to enable studies of large-scale structures in the high-redshift Universe. Following the green light for the construction of the E-ELT the MOS community, structured through the MOSAIC consortium, is eager to realise a MOS on the E-ELT as soon as possible. We argue that several of the most compelling cases for ELT science, in highly competitive areas of modern astronomy, demand such a capability. For example, MOS observations in the early stages of E-ELT operations will be essential for follow-up of sources identified by the James Webb Space Telescope (JWST). In particular, multi-object adaptive optics and accurate sky subtraction with fibres have both recently been demonstrated on sky, making fast-track development of MOSAIC feasible.
- Published
- 2015
5. The Age of Elliptical Galaxies in Clusters
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Bodo Ziegler and Ralf Bender
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- 1996
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6. Galaxy Evolution.
- Author
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Bodo Ziegler
- Published
- 2003
- Full Text
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7. The Dust and Molecular Gas in the Brightest Cluster Galaxy in MACS 1931.8-2635.
- Author
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Kevin Fogarty, Marc Postman, Yuan Li, Helmut Dannerbauer, Hauyu Baobab Liu, Megan Donahue, Bodo Ziegler, Anton Koekemoer, and Brenda Frye
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GALAXY clusters ,DUST ,SPECTRAL energy distribution ,ACTIVE galactic nuclei ,COLD gases ,PLANETARY nebulae - Abstract
We present new Atacama Large Millimeter Array observations of the molecular gas and far-infrared continuum around the brightest cluster galaxy (BCG) in the cool-core cluster MACS 1931.8-2635. Our observations reveal (1.9 ± 0.3) × 10
10 M⊙ of molecular gas, on par with the largest known reservoirs of cold gas in a cluster core. We detect CO(1−0), CO(3−2), and CO(4−3) emission from both diffuse and compact molecular gas components that extend from the BCG center out to ∼30 kpc to the northwest, tracing the UV knots and Hα filaments observed by the Hubble Space Telescope. Due to the lack of morphological symmetry, we hypothesize that the ∼300 km s−1 velocity of the CO in the tail is not due to concurrent uplift by active galactic nucleus (AGN) jets; rather, we may be observing the aftermath of a recent AGN outburst. The CO spectral line energy distribution suggests that molecular gas excitation is influenced by processes related to both star formation and recent AGN feedback. Continuum emission in Bands 6 and 7 arises from dust and is spatially coincident with young stars and nebular emission observed in the UV and optical. We constrain the temperature of several dust clumps to be ≲10 K, which is too cold to be directly interacting with the surrounding ∼4.8 keV intracluster medium (ICM). The cold dust population extends beyond the observed CO emission and must either be protected from interacting with the ICM or be surrounded by local volumes of ICM that are several keV colder than observed by Chandra. [ABSTRACT FROM AUTHOR]- Published
- 2019
- Full Text
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8. CLASH-VLT: Constraints on the Dark Matter Equation of State from Accurate Measurements of Galaxy Cluster Mass Profiles
- Author
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D. D. Kelson, Marc Postman, E. Munari, Keiichi Umetsu, Leonidas A. Mou, Narciso Benítez, Andrea Biviano, Tom Broadhurst, Wei Zheng, Elinor Medezinski, Julian Merten, Barbara Sartoris, Marco Lombardi, Marisa Girardi, Paolo Tozzi, Nicole G. Czakon, Larry Bradley, Holland C. Ford, Megan Donahue, Stella Seitz, Christian Maier, Anton M. Koekemoer, Matthias Bartelmann, Mario Nonino, Italo Balestra, U. Kuchner, Stefano Ettori, Claudio Grillo, Dan Coe, Alexander Fritz, Oliver Czoske, Peter Melchior, Adi Zitrin, Stefano Borgani, Doron Lemze, V. Presotto, Marco Scodeggio, M. Annunziatella, Massimo Meneghetti, Bodo L. Ziegler, Piero Rosati, Amata Mercurio, Sartoris, Barbara, Andrea, Biviano, Piero, Rosati, Borgani, Stefano, Keiichi, Umetsu, Matthias, Bartelmann, Girardi, Marisa, Claudio, Grillo, Doron, Lemze, Adi, Zitrin, Italo, Balestra, Amata, Mercurio, Mario, Nonino, Marc, Postman, Nicole, Czakon, Larry, Bradley, Tom, Broadhurst, Dan, Coe, Elinor, Medezinski, Peter, Melchior, Massimo, Meneghetti, Julian, Merten, Annunziatella, Marianna, Narciso, Benitez, Oliver, Czoske, Megan, Donahue, Stefano, Ettori, Holland, Ford, Alexander, Fritz, Dan, Kelson, Anton, Koekemoer, Ulrike, Kuchner, Marco, Lombardi, Christian, Maier, Leonidas A., Moustaka, Munari, Emiliano, Presotto, Valentina, Marco, Scodeggio, Stella, Seitz, Paolo, Tozzi, Wei, Zheng, and Bodo, Ziegler
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cosmology: theory – dark matter – equation of state ,Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Equation of state (cosmology) ,General relativity ,Dark matter ,FOS: Physical sciences ,theory – dark matter – equation of state [cosmology] ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Galaxy ,galaxies: clusters: individual (1206.2−0847) ,Baryon ,clusters: individual (1206.2−0847) [galaxies] ,Gravitational potential ,galaxies: clusters: general ,Space and Planetary Science ,Content (measure theory) ,clusters: general [galaxies] ,Galaxy cluster ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
A pressureless scenario for the Dark Matter (DM) fluid is a widely adopted hypothesis, despite the absence of a direct observational evidence. According to general relativity, the total mass-energy content of a system shapes the gravitational potential well, but different test particles perceive this potential in different ways depending on their properties. Cluster galaxy velocities, being $\ll$c, depend solely on the gravitational potential, whereas photon trajectories reflect the contributions from the gravitational potential plus a relativistic-pressure term that depends on the cluster mass. We exploit this phenomenon to constrain the Equation of State (EoS) parameter of the fluid, primarily DM, contained in galaxy clusters. We use the complementary information provided by the kinematic and lensing mass profiles of the galaxy cluster MACS 1206.2-0847 at $z=0.44$, as obtained in an extensive imaging and spectroscopic campaign within the CLASH survey. The unprecedented high quality of our data-set and the properties of this cluster are well suited to determine the EoS parameter of the cluster fluid. Since baryons contribute at most $15\%$ to the total mass in clusters and their pressure is negligible, the EoS parameter we derive describes the behavior of the DM fluid. We obtain the most stringent constraint on the DM EoS parameter to date, $w=(p_r+2\,p_t)/(3\,c^2\rho)=0.00\pm0.15\mathrm{(stat)}\pm0.08\mathrm{(syst)}$, averaged over the radial range $0.5\,\mathrm{Mpc}\leq$$r$$\leq$$r_{200}$, where $p_r$ and $p_t$ are the radial and tangential pressure, and $\rho$ is the density. We plan to further improve our constraint by applying the same procedure to all clusters from the ongoing CLASH-VLT program., Comment: 5 pages, 1 figures, accepted for publication in the Astrophysical Journal Letters
- Published
- 2014
- Full Text
- View/download PDF
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