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44 results on '"C., Balkowski"'

1. Kinematics and dynamics of the luminous infrared galaxy pair NGC 5257/58 (Arp 240)

Author: C. Balkowski, E. Laurikainen, H. Salo, Abel Bernal, J. A. Gomez-Lopez, Isaura Fuentes-Carrera, Margarita Rosado, Héctor O. Castañeda, P. Amram, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, star formationgalaxies, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, NGC 5257 -galaxies, 01 natural sciences, Gravitation, individual: NGC 5258 [galaxies], kinematics and dynamics -galaxies, 0103 physical sciences, galaxies, kinematics and dynamics [galaxies], individual, 010303 astronomy & astrophysics, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Luminous infrared galaxy, Physics, [PHYS]Physics [physics], Spiral galaxy, individual: NGC 5257 [galaxies], Mass distribution, Star formation, interactions [galaxies], NGC 5258, Astronomy and Astrophysics, spiral -galaxies, Astrophysics - Astrophysics of Galaxies, Galaxy, spiral [galaxies], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, interactions -galaxies, star formation [galaxies], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Encounters between galaxies modify their morphology, kinematics, and star formation (SF) history. The relation between these changes and external perturbations is not straightforward. The great number of parameters involved requires both the study of large samples and individual encounters where particular features, motions, and perturbations can be traced and analysed in detail. We analysed the morphology, kinematics, and dynamics of two luminous infrared spiral galaxies, NGC 5257 and NGC 5258, in which SF is mostly confined to the spiral arms, in order to understand interactions between galaxies of equivalent masses and SF processes during the encounter. Using scanning Fabry-Perot interferometry, we studied the contribution of circular and non-circular motions and the response of the ionized gas to external perturbations. We compared the kinematics with direct images of the pair and traced the SF processes and gravitational effects due to the presence of the other galaxy. The SED of each member of the pair was fitted. A mass model was fitted to the rotation curve of each galaxy. Large, non-circular motions detected in both galaxies are associated with a bar, spiral arms, and HII regions for the inner parts of the galaxies, and with the tidal interaction for the outer parts of the discs. Bifurcations in the rotation curves indicate that the galaxies have recently undergone their pericentric passage. The pattern speed of a perturbation of one of the galaxies is computed. Location of a possible corotation seems to indicate that the gravitational response of the ionized gas in the outer parts of the disc is related to the regions where ongoing SF is confined. The SED fit indicates a slightly different star formation history for each member of the pair. For both galaxies, a pseudo-isothermal halo better fits the global mass distribution., Comment: 34 pages, 13 figures, 8 tables. Accepted for publication in A&A
Published: 2018
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2. IMAGES IV: strong evolution of the oxygen abundance in gaseous phases of intermediate mass galaxies fromz ~ 0.8

Author: B. Guiderdoni, Göran Östlin, Ajit K. Kembhavi, Nicole P. H. Nesvadba, Isaura Fuentes-Carrera, F. Hammer, C. J. Cesarsky, Herve Wozniak, C. Balkowski, Lucia Pozzetti, Benoit Neichel, Hector Flores, Joel Vernet, Miguel Rodrigues, P. Amram, Daniela Vergani, S. di Serego Alighieri, R. Delgado, C. D. Ravikumar, Yun-Feng Liang, Helmut Dannerbauer, M. D. Lehnert, Mathieu Puech, A. Rawat, Y. Yang, 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: spiral, Stellar mass, Metallicity, Extinction (astronomy), Population, FOS: Physical sciences, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Tully–Fisher relation, 01 natural sciences, infrared: galaxies, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectral resolution, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Space and Planetary Science, galaxies: evolution, galaxies: ISM
Abstract: Intermediate mass galaxies (logM(Msun)>10) at z~0.6 are the likeliest progenitors of the present-day numerous population of spirals. There is growing evidence that they have evolved rapidly since the last 6 to 8 Gyr ago, and likely have formed a significant fraction of their stellar mass, often showing perturbed morphologies and kinematics. We have gathered a representative sample of 88 such galaxies and have provided robust estimates of their gas phase metallicity. For doing so, we have used moderate spectral resolution spectroscopy at VLT/FORS2 with unprecedented high S/N allowing to remove biases coming from interstellar absorption lines and extinction to establish robust values of R23=([OII]3727 + [OIII]4959,5007)/Hbeta. We definitively confirm that the predominant population of z~0.6 starbursts and luminous IR galaxies (LIRGs) are on average, two times less metal rich than the local galaxies at a given stellar mass. We do find that the metal abundance of the gaseous phase of galaxies is evolving linearly with time, from z=1 to z=0 and after comparing with other studies, from z=3 to z=0. Combining our results with the reported evolution of the Tully Fisher relation, we do find that such an evolution requires that ~30% of the stellar mass of local galaxies have been formed through an external supply of gas, thus excluding the close box model. Distant starbursts & LIRGs have properties (metal abundance, star formation efficiency & morphologies) similar to those of local LIRGs. Their underlying physics is likely dominated by gas infall probably through merging or interactions. Our study further supports the rapid evolution of z~0.4-1 galaxies. Gas exchanges between galaxies is likely the main cause of this evolution., 21 pages, 12 figures, A&A, In press
Published: 2008

3. Based on the observations with the 100-m telescope at Effelsberg operated by the Max-Planck-Institut für Radioastronomie (MPIfR) on behalf of the Max-Planck-Gesellschaft

Author: Rainer Beck, C. Balkowski, Krzysztof T. Chyzy, B. Vollmer, Marek Wezgowiec, Marian Soida, and Marek Urbanik
Subjects: Physics, Spiral galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), Virgo Cluster, Galaxy, Magnetic field, Ram pressure, Radio telescope, symbols.namesake, Space and Planetary Science, Faraday effect, symbols, Astrophysics::Galaxy Astrophysics
Abstract: Because of its proximity the Virgo Cluster is an excellent target for studying interactions of galaxies with the cluster environment. Both the high-velocity tidal interactions and effects of ram pressure stripping by the intracluster gas can be investigated. Optical and/or \ion{H}{i} observations do not always show effects of weak interactions between galaxies and their encounters with the cluster medium. For this reason we searched for possible anomalies in the magnetic field structure in Virgo Cluster spirals which could be attributed to perturbations in their gas distribution and kinematics. Five angularly large Virgo Cluster spiral galaxies (NGC 4501, NGC 4438, NGC 4535, NGC 4548 and NGC 4654) were the targets for a sensitive total power and polarization study using the 100-m radio telescope in Effelsberg at 4.85 GHz. For two objects polarization data at higher frequencies have been obtained allowing Faraday rotation analysis. Distorted magnetic field structures were identified in all galaxies. Interaction-induced magnetized outflows were found in NGC 4438 (due to nuclear activity) and NGC 4654 (a combination of tidal tails and ram pressure effects). Almost all objects (except the anaemic NGC 4548) exhibit distortions in polarized radio continuum attributable to influence of the ambient gas. For some galaxies they agree with observations of other species, but sometimes (NGC 4535) the magnetic field is the only tracer of the interaction with the cluster environment. The cluster environment clearly affects the evolution of the galaxies due to ram pressure and tidal effects. Magnetic fields provide a very long-lasting memory of past interactions. Therefore, they are a good tracer of weak interactions which are difficult to detect by other observations., Comment: 13 pages, 12 figures
Published: 2007

4. Introducing the CTA concept

Author: A. Mathieu, R. G. Wagner, K. Panagiotidis, S Rosier Lees, Julien Rousselle, M. Gómez Berisso, Michela Uslenghi, Stephen Maxfield, R. C. Shellard, Ivica Puljak, T. Le Flour, Thomas Schanz, Tobias C. Walther, Juanan Aguilar, Pierre Colin, M. Chikawa, N. Fouque, Mosè Mariotti, G. Fontaine, Merja Tornikoski, V. Diez-Blanco, Enrico Giro, A. Krepps, G. Koss, J. M. Martin, Sergio Billotta, E. de Oña Wilhelmi, Keitaro Takahashi, S. Buson, P. Brook, S. Steiner, M. Dyrda, Joseph Silk, Sera Markoff, P. Lubinski, U. Schwanke, Sauvik Bhattacharyya, J. Ripken, T. Haubold, C. Zurbach, H. Wetteskind, R. Hermel, J. Darling, J. Nicolau-Kukliński, Konstancja Satalecka, M. Videla, Stefan Funk, P. Conconi, S. Bajtlik, Lukasz Stawarz, J. M. Paredes, K. Reitberger, Stefan Wagner, Teresa Mineo, David Kieda, G. Pareschi, Shigeto Kabuki, Makoto Sawada, Antonio Stamerra, Rodolfo Canestrari, N. Baby, G. Crimi, P. Kostka, J. Grube, R. Zanin, I. K. Kominis, L. Mc Comb, R. Sternberger, M. Fesquet, M. Tokarz, David Fink, Daniela Dorner, N. Hamer Heras, A. Moralejo Olaizola, M. de Naurois, Diego F. Torres, Claes Fransson, K. Nishijima, Yutaka Fujita, L. Fresnillo, B. García, R. Kossakowski, A. Masserot, H. von Gunten, Alkiviadis F. Bais, Ciro Bigongiari, A. Saggion, G. Papyan, I. Mrusek, K. Farakos, J. Michałowski, A. Franckowiak, Fernando Martinez, M. Doert, R. Wawrzaszek, Michele Doro, L. Sapozhnikov, Claudia Lavalley, D. Thuermann, A.A. Zdziarski, Cristina Knapic, Karen Byrum, N. Neyroud, Petr Schovanek, W. Domainko, D. Kastana, E. Birsin, Adrian Biland, F. Sánchez, Alexandre Marcowith, M. Errando, R. L. C. Starling, J. Schultze, A. Weinstein, B. B. Singh, Yassir Moudden, Jelena Aleksić, C. L. Naumann, V. Waegebaert, M. Shayduk, U. F. Katz, Gianpiero Tagliaferri, M. Schroedter, A. Vollhardt, O. Reimann, Hideyuki Ohoka, Vincenzo Testa, C. Jablonski, Tsuguya Naito, J. Schäfer, Stavros Maltezos, A. Wierzcholska, P. Wawer, L. Nellen, F. Mirabel, Tatsuo Yoshida, P. H. Carton, Nina Nowak, L. Platos, Riccardo Rando, P. P. Krueger, R. Wischnewski, W. Romaszkan, E. Fede, Martino Marisaldi, Markus Gaug, Richard Willingale, J. H. Buckley, U. De AlmeidaBarres, J. Knapp, Saverio Lombardi, D. della Volpe, A. Herrero, A. Bottani, E. Delagnes, Martin J. Hardcastle, C. Morello, Anna Lipniacka, T. Greenshaw, M. Renaud, Giancarlo Cusumano, Jonathan Biteau, M. Sowiński, J. R. T. de Mello Neto, T. B. Humensky, Michael G. Richer, G. Parks, G. Grasseau, H. Baba, Gino Tosti, Damir Lelas, H. Krawzcynski, David Paneque, M. Barcelo, R. Dickherber, P. Ferrando, Shinji Hara, D. Florin, Hideaki Katagiri, T. Shibata, Fuyuki Tokanai, N. A. McCubbin, J. Gomez-Ortega, D. Nakajima, A. Liolios, P. Laporte, Orjan Dale, A. Sillanpää, Dainis Dravins, Timothée Grégoire, Nu. Komin, A. Mihailidis, L. Sidoli, Shiu-Hang Lee, A. W. Chen, J. M. Illa, A. Kuznetsov, P. Munar-Adrover, D. Dominis Prester, Marcos Daniel Actis, Abraham D. Falcone, L. Journet, D. Hadasch, N. Galante, A. Murphy, C. J. Todero Peixoto, S. Wiesand, A. Aravantinos, A. C. Rovero, J. L. Dournaux, P. Romano, M. Hrabovsky, R. de los Reyes Lopez, M. Ostrowski, J. Pallota, Geza Gyuk, Petar Temnikov, R. Dubois, Jan Ebr, R. Koul, David J. Smith, S. Schwarzburg, P. Manigot, Chad Finley, Tarek M. Hassan, Giuseppe Sottile, Evgeni Ovcharov, P. J. Rajda, F. Krennrich, Peter L. Moore, W. B. Focke, W. Bednarek, Elena Amato, Kazunori Kohri, J. Gamez-Garcia, I. Oya, A. Shibuya, German Hermann, William H. Lee, Dorota Sobczyńska, X. Zhou, C. Balkowski, G. Vallejo, M. Hayashida, M. Bitossi, Loukas Vlahos, H. Lockart, N. Geffroy, L. Tibaldo, Marek Jamrozy, Luke O'c. Drury, Pratik Majumdar, P. Sutcliffe, S. Schlenstedt, M. Palatka, Christophe Champion, H. Ueno, M. Rupiński, P. Giommi, J. Schwarz, G. Pühlhofer, Takashi Saito, W. van Driel, C. van Eldik, Q. Xiong, Yasuo Fukui, A. Donat, A. Ibarra, R. S. Warwick, Michiko Ohishi, A. W. Smith, J.-P. Lenain, Aion Viana, Terry Ashton, Guillaume Dubus, Jacek Niemiec, K. Kodani, Luis Ángel Tejedor, A. Wörnlein, Takanori Yoshikoshi, Masahiro Teshima, W. Gäbele, Ll. Font, Olaf Reimer, J. F. Valdés-Galicia, Lucy Fortson, J. P. Osborne, Mattia Fornasa, Keith Bechtol, Masayuki Tanaka, Shigehiro Nagataki, M. Rataj, M. Ribordy, Emmanuel Moulin, I. de la Calle, K. Winiarski, C. Jeanney, I. Mognet, I. Vegas, C. Juffroy, Yutaka Ohira, A. Jacholkowska, Matthew Wood, A. E. Suárez, J. Bähr, K. M. Schure, J. Maya, M. Dafonseca, J. Tasan, R. Sugawara, M. Bourgeat, A. Mancilla, D. Pelat, Olga Botner, D. Nedbal, G. Depaola, Robert Wagner, T. Okuda, H. Arnaldi, Josep Martí, P. Corona, T. Bonev, D. Yelos, J. Sieiro, V. Scalzotto, Jacco Vink, D. Languignon, Marco Ajello, J. Vandenbrouke, Philipp Mertsch, M. Mordalska, P. Wegner, P. Ziółkowski, P. T. O'Brien, A. Nozato, Robert D. Preece, B. Huber, Matteo Balbo, J.R. Bogart, R. Kankanyan, K. Mori, T. Jogler, Seth Digel, Claudio Vuerli, Hiromitsu Takahashi, Thomas Lohse, K. Saito, A. W. Borgland, Elisa Prandini, Helene Sol, Ryan Heller, M. Bogdan, D. Dumas, M. Stodulski, Y. Awane, Piercarlo Bonifacio, Pedro L. Luque-Escamilla, Judith H. Croston, Fabio Pizzolato, P. M. Chadwick, M. K. Daniel, Riccardo Paoletti, Reiko Orito, Katsuaki Asano, R. Frei, G. Disset, Valerie Connaughton, Juhani Huovelin, Hiroyasu Tajima, S. Vercellone, F. Feinstein, G. Decerprit, Riccardo Smareglia, S. Spyrou, Gustavo E. Romero, J. Shi, J. Carr, N. Girard, Dirk L. Hoffmann, Andreas Zech, Markus Boettcher, Osvaldo Catalano, Akira Okumura, M. Dohmke, C. Föhr, Sabrina Casanova, R. A. Cameron, Jan Conrad, K. Umehara, K. K. Yadav, A. Paizis, John L. Quinn, L. Pogosyan, C. Farnier, William J. Potter, Domenico Impiombato, Tadashi Kifune, Jonathan Granot, Gernot Maier, M. Cieślar, S. Palanque, G.W. Fraser, J. Prast, R. Bose, Heidi Sandaker, G. Lamanna, Dusan Mandat, J.F. Glicenstein, J. Harris, D. Naumann, J. Ziolkowski, Michał Szanecki, C. Delgado, J. Kocot, W. Lustermann, Sabine Elles, J. Schmoll, L. Gérard, M. López, Norita Kawanaka, V. Gika, B. Lieunard, A. Pichel, Martin Pohl, Mariusz Sterzel, S. Vincent, Paolo De Coppi, J. Lande, O. Blanch Bigas, Gianluca Giavitto, Yusuke Konno, Julian Sitarek, M. Panter, P.-O. Petrucci, F. Henault, M. Prouza, Philip Kaaret, Josep Colomé, Luciano Nicastro, German Martinez, L. Gebremedhin, J. M. Yebras, Apostolos Mastichiadis, A. S. Madhavan, Thomas J. Maccarone, K. Berger, R. Buehler, P. Jean, N. Sartore, F. Toussenel, Aris Karastergiou, W. Kluźniak, A. Djannati-Ataï, S. J. Fegan, Louis Antonelli, A. González Muñoz, J. Berdugo, S. S. Upadhya, M. Sidz, F. Mottez, Patrick Vogler, F. Di Pierro, Wystan Benbow, B. Sacco, L. Chiappetti, J. Dumm, R. Firpo Curcoll, David Gascon, V. Boccone, J. Krause, J. P. Avernet, B. Peyaud, B. De Lotto, Ana Babić, T. O. B. Schmidt, I. M. McHardy, T. Schweizer, S. P. Wakely, Daniel Gall, Frank M. Rieger, E. Sant'Ambrogio, M. Kagaya, P. Vincent, R. C. Rannot, Sandro Mereghetti, A. De Angelis, M. Scarcioffolo, R. White, G. H. Sembroski, Takeshi Nakamori, C. Medina, M. A. De Oliveira Leigui, Subir Sarkar, A. Marszałek, Reshmi Mukherjee, K. Nakayama, A. Fiasson, S. Giarrusso, T. Bernardino, J. P. Finley, D. Neise, L. O. Takalo, F. Grañena, Nikola Godinovic, H. Sasaki, P. Zychowski, Francesco Dazzi, B. Courty, A. Basili, Vitaly Neustroev, B. Khélifi, T. Glanzman, M. Trifoglio, Regis Terrier, R. A. Ong, E. M. Santos, M. Minuti, Thomas Bretz, R. Moderski, J. Kushida, S. Royer, Emilio Molinari, Etienne Lyard, J. Houles, Juan Abel Barrio, T. Lerch, S. Rivoire, T. Kishimoto, M. Cailles, M. Casiraghi, Nikolaos Stergioulas, J. Gaweda, S. Koyama, Ingomar Allekotte, E. Ismailova, Elina Giannakaki, S. Schwemmer, Ryo Yamazaki, G. Fasola, Christoph Deil, Jose Luis Contreras, T. Bird, Miguel A. Sánchez-Conde, J. Dick, E. Edy, D. Parsons, R. Pyzioł, R. Mirzoyan, Manjuli R. Sharma, J. Borkowski, Jonathan S. Lapington, Cameron B Rulten, Rino Bandiera, Volker Beckmann, Jun Kakuwa, Dimitris Balis, Kenji Toma, Anna Barnacka, Andrea Santangelo, L. Padilla, Peter Eger, G. Decock, Karol Seweryn, N. Sakaki, Darko Veberič, Andrea Bulgarelli, B. Rudak, M. Pérez, H. Koppel, Felix Spanier, M. I. Martínez, D. Horville, Marco Molinaro, R. Walter, P. Ramon, S. Brau-Nogue, J. Camprecios, K. Kärcher, John H. Seiradakis, S. Criswell, D. J. Leopold, V. J. Guarino, R. Gredig, S. Vorobiov, Viktor Gruev, Gareth Hughes, Daniele Spiga, Quirin Weitzel, N. Håkansson, Susumu Inoue, U. Straumann, Juan Cortina, B. Behera, Jürgen Knödlseder, Daniel Nieto, Tomasz Szepieniec, H. Prokoph, Jerzy Grygorczuk, G. De La Vega, Jim Hinton, E. Chabanne, M. Mahabir, R. Krobot, M. Capalbi, Miroslav Pech, C. Díaz, J. Ludwin, F. Gianotti, Garret Cotter, Claudio Melioli, Hiroaki Yamamoto, C. Veyssiere, Kunihito Ioka, S. Sun, J. M. Parraud, L. Rob, Felix Aharonian, G. Maneva, D. Melkumyan, T. Schwab, J. Kasperek, J. M. Huet, E. Lorenz, S. Tanaka, Y. A. Gallant, S. Couturier, B.W. Favill, J. Boix Gargallo, Andrea Tiengo, Leszek Bogacz, Andreu Sanuy, Christian Fruck, J. Sykes, C. Martens, A. Yoshida, Marek Sikora, E. Racero, G. Rouaix, N. Bhat, A. Salini, A. S. Barber, Mauro Ghigo, Jan Ridky, K. Kosack, Konrad Bernlöhr, C. Tenzer, Alice Allafort, M. Torres, Catherine Boisson, Grzegorz Kowal, M. Karczewski, G. Agnetta, Victor Stamatescu, Anthony H. Gonzalez, S. Rousselle, Giovanni Bonanno, A. Zajczyk, A. Gadola, P. Martin, V. Zitelli, I. Manthos, N. Maragos, A. Dettlaff, F. Profeti, S. Colonges, S. Gunji, S. Cazaux, S. Colafrancesco, M. Paz Arribas, Rika Hagiwara, Darell Engelhaupt, Nestor Mirabal, Johann Cohen-Tanugi, S. Grunewald, Abby M. Green, I. D. Davids, D. Nosek, T. Yamamoto, Gagik Tovmassian, R. Sakonaka, Miguel Alcubierre, C. Baixeras, T. L. Usher, Kazufumi Torii, H. Lüdecke, L. Wiśniewski, B. Kellner-Leidel, P. Demange, F. Gonzalez, B. Moal, V. De Caprio, V. Golev, K. Katarzyński, V. Bugaev, A. Reimer, J. Koziol, G. Pojmanski, Alessandro Carosi, J. Bolmont, A. Nikolaidis, R. J. García López, V. A. Kudryavtsev, C. Stegmann, J.-P. Ernenwein, M. Fiorini, Ivone F. M. Albuquerque, Marco Tavani, P. Korohoda, A. Giuliani, E. Carmona, C. Bauer, Kostas D. Kokkotas, O. Tibolla, G. Deleglise, Pierre Brun, Dinko Dimitrov, I. Jung, R. Steenkamp, Marc Ribó, Kathrin Egberts, P. Reardon, Adriano Ghedina, Stefan Rosén, N. Hidaka, Trygve Buanes, A. Segreto, H. Huan, Juri Poutanen, Ruben Lopez-Coto, S. Cavazzani, Massimiliano Belluso, A. Kretzschmann, F. De Frondat, A. Riviere, J. F. Olive, Tsunefumi Mizuno, Serena Mattiazzo, M. González, D. Fantinel, Matteo Cerruti, S. Vergani, Sabrina Einecke, N. La Palombara, Reinhard Schlickeiser, P. Antoranz, Pol Bordas, D. Paillot, V. de Souza, Yasushi Fukazawa, Phil Evans, Werner Hofmann, Hugh Dickinson, F. Roy, Yvonne Becherini, E. O. Angüner, D. Corti, T. C. Arlen, Francesco Russo, V. R. Chitnis, D. Ross, R. Gabriele, Massimo Persic, E. Fokitis, A. Bonardi, D. Garrido, A. Niedźwiecki, L. Cossio, Hidetoshi Kubo, Y. de Oliveira, F. Mattana, Anna Szostek, M. Compin, S. Blake, F. Lucarelli, Petter Hofverberg, Felix Ryde, M. Gougerot, C. Boutonnet, Dimitrios Emmanoulopoulos, A. Mangano, P. Vallania, Jose Miguel Miranda, A. Manalaysay, M. Raue, A. Bouvier, Shohei Yanagita, Nektarios Vlahakis, Joni Tammi, M. Naumann-Godo, Kohta Murase, E. Fillin-Martino, Jiri Chudoba, K. Hatanaka, A. Lopatin, N. Otte, G. Rojas, Tomonori Totani, K. S. Gothe, J. P. Vialle, D. Kolitzus, K. Warda, Hironori Matsumoto, J. Rico, P. Ringegni, James Chiang, R. McKay, A. Bobkov, Aya Bamba, H. Takami, B. Giebels, O. Grimm, S. Basso, F. Dubois, Victor Zabalza, A. Förster, Pasquale Blasi, Alexandros Papayannis, A. G. Akhperjanian, Eckhard Kendziorra, James A. Anderson, Giuseppe Malaguti, R. Welsing, S. Pita, A. Ozieblo, Heide Costantini, D. Tezier, J.-H. Köhne, M. Tluczykont, Ll. Garrido, Alexander Varón Sandoval, Matthew R. Orr, Dominique Durand, F. Chollet, O. Luz, E. O. Saemann, Jun Kataoka, M. Proyetti, C. Barbier, Jürgen Barnstedt, L. Bouchet, Hiroshi Muraishi, Anton N. Baushev, L. A. Otero, Denis Bastieri, S. Incorvaia, Tihomir Surić, V. La Parola, Nathan Smith, Karl-Heinz Sulanke, F. Bernard, Luca Stringhetti, S. Paiano, S. Federici, Hector Flores, Karl Mannheim, Michael S. Briggs, Giovanna Pedaletti, E. M. de Gouveia Dal Pino, J. D. Smith, G. La Rosa, Alicia López-Oramas, M. Janiak, Gary Drake, G. Talbot, Petr Travnicek, Elisabetta Bissaldi, Mario Meucci, R. Northrop, V. Scapin, Vito Conforti, J. D. Ponz, T. Aghajani, J. J. Jimenez, A. D. Supanitsky, Hernán Asorey, M. Werner, Brian Reville, A. Haupt, C. Skole, Gilles Henri, Daniele Gardiol, V. Vassiliev, R. Platzer, Y. Saito, A. La Barbera, Allan Hallgren, C. Eleftheriadis, S. Cantu, G. Maurin, K. Lacombe, A. Le Padellec, F. Stinzing, T. Hayakawa, A. Cillis, M. Suchenek, I. Monteiro, V. Sahakian, A. Di Paola, Grzegorz Madejski, A. De Luca, Andreas Quirrenbach, P. A. Caraveo, N. A. 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F., Torre, M., Torre, G., Tosti, T., Totani, C., Toussenel, G., Tovmassian, P., Travnicek, M., Trifoglio, I., Troyano, K., Tsingano, H., Ueno, K., Umehara, S. S., Upadhya, T., Usher, M., Uslenghi, J. F., Valdes Galicia, P., Vallania, G., Vallejo, W. v., Driel, C. v., Eldik, J., Vandenbrouke, J., Vanderwalt, H., Vankov, G., Vasileiadi, V., Vassiliev, D., Veberic, I., Vega, S., Vercellone, S., Vergani, C., Veyssiere, J. P., Vialle, A., Viana, M., Videla, P., Vincent, S., Vincent, J., Vink, N., Vlahaki, L., Vlaho, P., Vogler, A., Vollhardt, H. . ., P., S., Vorobiov, C., Vuerli, V., Waegebaert, R., Wagner, R. G., Wagner, S., Wagner, S. P., Wakely, R., Walter, T., Walther, K., Warda, R., Warwick, P., Wawer, R., Wawrzaszek, N., Webb, P., Wegner, A., Weinstein, Q., Weitzel, R., Welsing, M., Werner, H., Wetteskind, R., White, A., Wierzcholska, S., Wiesand, M., Wilkinson, D. A., William, R., Willingale, K., Winiarski, R., Wischnewski, L., Wisniewski, M., Wood, A., Woernlein, Q., Xiong, K. K., Yadav, H., Yamamoto, T., Yamamoto, R., Yamazaki, S., Yanagita, J. M., Yebra, D., Yelo, A., Yoshida, T., Yoshida, T., Yoshikoshi, V., Zabalza, M., Zacharia, A., Zajczyk, R., Zanin, A., Zdziarski, A., Zech, A., Zhao, X., Zhou, K., Zietara, J., Ziolkowski, P., Ziolkowski, V., Zitelli, C., Zurbach, P., Zychowski, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), APC - Astrophysique des Hautes Energies (APC - AHE), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, CTA, Laboratoire Univers et Théories (LUTH (UMR_8102)), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Laboratoire d'Annecy de Physique des Particules (LAPP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Next generation Cherenkov telescopes, Ciencias Físicas, 01 natural sciences, 7. Clean energy, TeV GAMMA-RAY ASTRONOMY, Observatory, Air showers, HESS, Cherenkov Telescopes, 010303 astronomy & astrophysics, MISSION, SUPERNOVA REMNANT W44, TELESCOPE, ASTRONOMY, EMISSION, Physics, ta213, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, TeV gamma-ray astronomy, ddc:540, CIENCIAS NATURALES Y EXACTAS, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Air shower, AIR SHOWERS, Astrophysics::High Energy Astrophysical Phenomena, 0103 physical sciences, Preparatory phase, ta115, TeV gamma-ray astronomy Air showers Cherenkov Telescopes, 010308 nuclear & particles physics, business.industry, CHERENKOV TELESCOPES, Física, Astronomy, Institut für Physik und Astronomie, Astronomy and Astrophysics, ASTROFÍSICA, Cherenkov Telescope Array, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astronomía, Design study, Telecommunications, business
Abstract: The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project., La lista completa de autores puede consultarse en el documento o en la página web de la revista., Facultad de Ingeniería
Published: 2013

5. Large-scale magnetized outflows from the Virgo Cluster spiral NGC 4569

Author: Rainer Beck, Dominik J. Bomans, Marian Soida, Marek Urbanik, C. Balkowski, Krzysztof T. Chyzy, and B. Vollmer
Subjects: Physics, Spiral galaxy, Astrophysics::High Energy Astrophysical Phenomena, individual: NGC 4569 IC 3583 [galaxies], Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Virgo Cluster, galaxies [radio continuum], Galaxy, Ram pressure, Radio telescope, magnetic fields [galaxies], X-shaped radio galaxy, Space and Planetary Science, Intracluster medium, Astrophysics::Solar and Stellar Astrophysics, Disc, Astrophysics::Galaxy Astrophysics
Abstract: Using the Effelsberg radio telescope at 4.85 GHz and 8.35 GHz we discovered large symmetric lobes of polarized radio emission around the strongly Hi deficient Virgo cluster spiral galaxy NGC 4569. These lobes extend up to 24 kpc from the galactic disk. Our observations were complemented by 1.4 GHz continuum emission from existing Hi observations. This is the first time that such huge radio continuum lobes are observed in a cluster spiral galaxy. The eastern lobe seems detached and has a flat spectrum typical of in-situ cosmic ray electron acceleration. The western lobe is diffuse and possesses vertical magnetic fields over its whole volume. The lobes are not powered by an AGN, but probably by a nuclear starburst that occurred ∼30 Myr ago, producing ≥10 5 supernovae. Since the radio lobes are symmetric, they resist ram pressure due to the galaxy's rapid motion within the intracluster medium.
Published: 2006

6. The GALEX Ultraviolet Virgo Cluster Survey (GUViCS). I: The UV luminosity function of the central 12 sq.deg

Author: Laura Ferrarese, Emmanuel Momjian, Leslie K. Hunt, Eric Emsellem, J. I. Davies, Catherine Vlahakis, José M. Solanes, Noah Brosch, Matthew Smith, Jacopo Fritz, Andrés Jordán, Kelley M. Hess, James E. Taylor, W. van Driel, I. De Looze, Marco Grossi, Samuel Boissier, Patrick R. Durrell, Maarten Baes, Alessandro Boselli, S. di Serego Alighieri, Thomas Erben, Simona Mei, Sebastien Heinis, Pierre-Alain Duc, Thomas M. Hughes, Emmanuel M. Xilouris, O. Spector, Brian R. Kent, D. A. Garcia-Appadoo, Emmanouil Papastergis, Giuseppe Gavazzi, C. Balkowski, Bernd Vollmer, Kristine Spekkens, O. Ilbert, Laura Magrini, Lauren A. MacArthur, Riccardo Giovanelli, O. Cucciati, Suzanne C. Madden, Ariane Lançon, Marcel Clemens, C. Valotto, Vassilis Charmandaris, Luca Cortese, Marc Huertas-Company, Martha P. Haynes, Joris Verstappen, Scott Chapman, Aliakbar Dariush, Diego G. Lambas, Ronald P. Olowin, Astronomy, 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), A. Boselli, S. Boissier, S. Heini, L. Cortese, O. Ilbert, T. Hughe, O. Cucciati, J. Davie, L. Ferrarese, R. Giovanelli, M. P. Hayne, M. Bae, C. Balkowski, N. Brosch, S. C. Chapman, V. Charmandari, M. S. Clemen, A. Dariush, I. De Looze, S. di Serego Alighieri, P.-A. Duc, P. R. Durrell, E. Emsellem, T. Erben, J. Fritz, D. A. Garcia-Appadoo, G. Gavazzi, M. Grossi, A. Jordán, K. M. He, M. Huertas-Company, L. K. Hunt, B. R. Kent, D. G. Lamba, A. Lançon, L. A. MacArthur, S. C. Madden, L. magrini, S. Mei, E. Momjian, R. P. Olowin, E. Papastergi, M. W. L. Smith, J. M. Solane, O. Spector, K. Spekken, J. E. Taylor, C. Valotto, W. van Driel, J. Verstappen, C. Vlahaki, B. Vollmer, and E. M. Xilouris
Subjects: HI SOURCE CATALOG, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COMA CLUSTER, FAST ALPHA SURVEY, DATA RELEASE, NEARBY CLUSTERS, FOS: Physical sciences, DWARF ELLIPTIC GALAXIES, Astrophysics, medicine.disease_cause, 01 natural sciences, Luminosity, STAR-FORMATION, 0103 physical sciences, Galaxy formation and evolution, medicine, Cluster (physics), fundamental parameters [galaxies], EARLY-TYPE GALAXIES, 010303 astronomy & astrophysics, galaxies: fundamental parameter, evolution [galaxies], Luminosity function (astronomy), luminosity function [galaxies], Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, galaxies: fundamental parameters, clusters: individual: Virgo [galaxies], BAND SURFACE PHOTOMETRY, Virgo Cluster, Galaxy, galaxies: luminosity function, Physics and Astronomy, Space and Planetary Science, mass function, galaxies: luminosity function, mass function, galaxies: clusters: individual: Virgo, ultraviolet: galaxies, astro-ph.CO, ultraviolet: galaxie, DIGITAL SKY SURVEY, galaxies [ultraviolet], galaxies: evolution, Ultraviolet, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) is a complete blind survey of the Virgo cluster covering about 40 sq. deg. in the far UV (FUV, lambda_eff=1539A, Delta-lambda=442A) and about 120 sq. deg. in the near UV (NUV, lambda_eff=2316A, Delta-lambda=1060A). The goal of the survey is to study the ultraviolet (UV) properties of galaxies in a rich cluster environment, spanning a wide luminosity range from giants to dwarfs, and regardless of prior knowledge of their star formation activity. The UV data will be combined with those in other bands (optical: NGVS; far-infrared - submm: HeViCS; HI: ALFALFA) and with our multizone chemo-spectrophotometric models of galaxy evolution to make a complete and exhaustive study of the effects of the environment on the evolution of galaxies in high density regions. We present here the scientific objectives of the survey, describing the observing strategy and briefly discussing different data reduction techniques. Using UV data already in-hand for the central 12 sq. deg. we determine the FUV and NUV luminosity functions of the Virgo cluster core for all cluster members and separately for early- and late-type galaxies and compare it to the one obtained in the field and other nearby clusters (Coma, A1367). This analysis shows that the FUV and NUV luminosity functions of the core of the Virgo clusters are flatter (alpha about -1.1) than those determined in Coma and A1367. We discuss the possible origin of this difference, 18 pages, 14 figures, accepted in A&A, high resolution version of figure 1 and 2 and other information available at http://galex.oamp.fr/guvics/observations.html
Published: 2011

7. Chemical and spectrophotometric evolution of low surface brightness galaxies

Author: D. Monnier Ragaigne, C. Balkowski, Nikos Prantzos, Karen O'Neil, Samuel Boissier, and W. van Driel
Subjects: Physics, Brightness, Angular momentum, Star formation, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, High surface, Space and Planetary Science, Homogeneous, Computer Science::Multimedia, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, Astrophysics::Galaxy Astrophysics
Abstract: Based on the results of recent surveys, we have constructed a relatively homogeneous set of observational data concerning the chemical and photometric properties of Low Surface Brightness galaxies (LSBs). We have compared the properties of this data set with the predictions of models of the chemical and spectrophotometric evolution of LSBs. The basic idea behind the models, i.e. that LSBs are similar to 'classical' High Surface Brightness spirals except for a larger angular momentum, is found to be consistent with the results of their comparison with these data. However, some observed properties of the LSBs (e.g. their colours, and specifically the existence of red LSBs) as well as the large scatter in these properties, cannot be reproduced by the simplest models with smoothly evolving star formation rates over time. We argue that the addition of bursts and/or truncations in the star formation rate histories can alleviate that discrepancy., Comment: Accepted in MNRAS. 14 pages. 13 figures
Published: 2003

8. Non-confirmation of reported $\ion{H}{I}$ clouds without optical counterparts in the Hercules cluster

Author: P. Papaderos, C. Balkowski, José M. Vílchez, V. Cayatte, Trinh X. Thuan, John M. Dickey, W. van Driel, H. Hernández, Karen O'Neil, Pierre-Alain Duc, Jorge Iglesias-Páramo, 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), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Arecibo Observatory, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Astronomy, University of Minnesota, 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), Sternwarte Weinheim, Instituto de Astrofisica de Andalucia, CSIC (IAA), and Astronomy Department, University of Virginia, Charlottesville
Subjects: Physics, Gregorian telescope, Galactic astronomy, Continuum (measurement), 010308 nuclear & particles physics, media_common.quotation_subject, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, general, clusters, individual, Hercules cluster, galaxies, ISM, radio lines, 01 natural sciences, law.invention, Space and Planetary Science, law, Sky, 0103 physical sciences, Surface brightness, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, media_common
Abstract: 21 cm HI line observations were made with the Arecibo Gregorian telescope of 9 HI clouds in the Hercules Cluster which were reported as tenative detections in a VLA HI study of the cluster (Dickey 1997) and for which our deep CCD imaging failed to find any optical counterparts. No sensitive observations could be made of one of these (sw-174) due to the presence of a close-by strong continuum source. The other 8 tentative HI detections were not reconfirmed by the Arecibo HI measurements. The CCD images did reveal faint, low surface brightness counterparts near the centres of two other VLA HI sources invisible on the Palomar Sky Survey, sw-103 and sw-194., Comment: 7 pages, accepted for Astronomy and Astrophysics on 8 Nov. 2002; new references added on 23 Dec. 2002
Published: 2003

9. Commission 28: Galaxies: (Galaxies)

Author: S. Okamura, E. Sadler, C. Balkowski, F. Bertola, J. Binney, D. Burstein, P. de Zeeuw, A. Fairall, T. Heckman, S. Lilly, and Z.-L. Zou
Published: 2002

10. $\mathsf{^{12}}$CO(1-0) observations of NGC 4848: A Coma galaxy after stripping

Author: V. Cayatte, B. Vollmer, C. Balkowski, Jonathan Braine, and Wolfgang J. Duschl
Subjects: Physics, Spiral galaxy, Star formation, media_common.quotation_subject, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Ram pressure, Space and Planetary Science, Coincident, Sky, Coma Cluster, Astrophysics::Galaxy Astrophysics, media_common
Abstract: We study the molecular gas content and distribution in the Coma cluster spiral galaxy NGC 4848. Plateau de Bure interferometric CO(1-0) observations reveal a lopsided H_2 distribution with an off-center secondary maximum coincident with the inner part of the HI. NGC 4848 is not at all deficient in molecular gas as it contains M_H_2~4x10^9 M_solar. At the interface between the CO and HI emission regions, about 8 kpc NW of the center, however, strong star formation is present as witnessed by Halpha and radio continuum emission. This is the region in which earlier Fabry-Perot observations revealed a double-peaked Halpha line, indicating gas at two different velocities at the same sky position. In order to understand these observations, we present the results of numerical simulations of the ISM-ICM interaction. We suggest that NGC 4848 already passed through the center of the cluster about 4x10^8 years ago. At the observed stage ram pressure has no more direct dynamical influence on the galaxy's ISM. We observe the galaxy when a fraction of the stripped gas is falling back onto the galaxy. Ram pressure is thus a short-lived event with longer-lasting consequences. The combination of ram-pressure and rotation results in gas at different velocities colliding where the double-peaked Halpha line is observed. Ram-pressure can thus result, after re-accretion, in displaced molecular gas without the H_2 itself being pushed efficiently by the ICM. A scenario where two interactions take place simultaneously is also consistent with the available data but less probable on the basis of our numerical simulations., 15 pages with 20 figures. A&A, in press
Published: 2001

11. HI deficiency in the galaxy cluster ACO 3627

Author: Renee C. Kraan-Korteweg, Patricia A. Henning, C. Balkowski, V. Cayatte, Patrick A. Woudt, W. van Driel, B. Vollmer, and Wolfgang J. Duschl
Subjects: Physics, Spiral galaxy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, Astrophysics, Galaxy, Ram pressure, Great Attractor, Space and Planetary Science, Coma Cluster, Astrophysics::Galaxy Astrophysics, Spiral, Galaxy cluster
Abstract: ATCA 21 cm HI observations of the rich galaxy cluster ACO 3627 in the Great Attractor region are presented. Three fields of 30' diameter located within one Abell radius of ACO 3627 were observed with a resolution of 15'' and an rms noise of \sim 1 mJy/beam. Only two galaxies were detected in these fields. We compare their HI distribution to new optical R-band images and discuss their velocity fields. The first galaxy is a gas-rich unperturbed spiral whereas the second shows a peculiar HI distribution. The estimated 3-sigma HI mass limit of our observations is \sim 7 x 10^8 M_{\odot} for a line width of 150 km s^{-1}. The non-detection of a considerable number of luminous spiral galaxies indicates that the spiral galaxies are HI deficient. The low detection rate is comparable to the HI deficient Coma cluster (Bravo-Alfaro et al. 2000). ACO 3627 is a bright X-ray cluster. We therefore suspect that ram pressure stripping is responsible for the HI deficiency of the bright cluster spirals.
Published: 2001

12. Commission 28: Galaxies: (Galaxies)

Author: Michael Feast, F. Bertola, P. de Zeeuw, S. Chakrabarti, C. Balkowski, D. Burstein, Z.-L. Zou, Virginia Trimble, J. Huchra, R. Wielebinsky, Sadanori Okamura, and A. Zasov
Subjects: Luminous infrared galaxy, Radio galaxy, Law, Galaxy group, Political science, Elliptical galaxy, Astronomy, Commission, Disc, Galaxy, Luminosity function (astronomy)
Abstract: This report covers the period July 1996 to June 1999. It has been prepared by the President of the Commission with contributions from the members of the Organizing Committee and Dr. E.M. Corsini. As discussed in Kyoto and decided by the Organizing Committee, the report is meant to be in the “short” version.
Published: 2000

13. Detection and Velocities of Hα Emission Regions in Stephan's Quintet

Author: C. Balkowski, Henri Plana, J. Boulesteix, C. Mendes de Oliveira, P. Amram, and Michael Bolte
Subjects: Physics, symbols.namesake, Space and Planetary Science, symbols, Astronomy, Astronomy and Astrophysics, Astrophysics, Hubble sequence
Abstract: We present observations of Hα emission of Stephan's Quintet obtained with a scanning Fabry-Perot interferometer and samplings of ~11 km s-1 and ~1''. Our observations show an intragroup arclike feature formed of bright Hα knots and diffuse gas distributed along tidal tails associated with NGC 7318B and possibly also NGC 7318A. New velocities for 23 emitting regions detected along the Hα structure are presented. South of NGC 7318B, along a path covering ~12 h−175 kpc, H II regions with velocities ranging from 5540 to 6700 km s-1 are detected, suggesting that two or more overlapping tidal tails and/or a bow-shock region may have been formed through several interaction events within the group.
Published: 1999

14. Environmental Effects on the Kinematics of Virgo Cluster Galaxies

Author: Claude Carignan, Philippe Amram, C. Adami, J. Boulesteix, Alessandro Boselli, L. Chemin, M. Marcelin, Olivier Hernandez, O. Garrido, V. Cayatte, C. Balkowski, B. Vollmer, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), P.-A. Duc, J. Braine, and E. Brinks, 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), and Beaussier, Catherine
Subjects: Physics, 010504 meteorology & atmospheric sciences, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Velocity dispersion, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Virgo Cluster, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 13. Climate action, 0103 physical sciences, Elliptical galaxy, Interacting galaxy, Brightest cluster galaxy, 010303 astronomy & astrophysics, Lenticular galaxy, Astrophysics::Galaxy Astrophysics, Galaxy cluster, 0105 earth and related environmental sciences, Dwarf galaxy
Abstract: We present results from an ongoing survey dedicated to the ionized gas kinematics of Virgo cluster spiral galaxies using Fabry-Perot interferometry. Our goal is to study the environmental effects on galaxy evolution in the Virgo cluster. We report here on the Halpha distribution map and velocity field of NGC 4438, the prototype of an interacting galaxy near the centre of the cluster., Comment: 2 pages, 1 figure, to be published in "IAU Symposium 217, Recycling intergalactic and interstellar matter", ASP Conf Series
Published: 2004

15. Science with GYES: A multifibre high-resolution spectrograph for the prime focus of the Canada-France-Hawaii Telescope

Author: Piercarlo Bonifacio, R. Kudritzky, C. Turon, Y. Viala, Denis Mourard, Raymond G. Carlberg, Annie C. Robin, Caroline Soubiran, Rosine Lallement, Misha Haywood, R. Monier, D. Briot, Frédéric Arenou, Yves Fremat, Olivier Bienaymé, Christophe Martayan, Elisabetta Caffau, P. Francois, P. de Laverny, K. A. Venn, A. E. Gomez, Benoit Famaey, Vanessa Hill, C. Balkowski, B. Lemasle, Fr. Royer, Nicolas Nardetto, D. Katz, Myriam Rodrigues, N. Robichon, Carine Babusiaux, A. Recio Blanco, Astronomy, 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), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), University of Toronto, Royal Observatory of Belgium [Brussels] (ROB), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Ian S. McLean, Suzanne K. Ramsay, Hideki Takami, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Royal Observatory of Belgium [Brussels], Centre National de la Recherche Scientifique (CNRS), and HEPPI - LATMOS
Subjects: Physics, Proper motion, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010308 nuclear & particles physics, Astronomy, Astrophysics, 01 natural sciences, Prime (order theory), law.invention, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Telescope, Radial velocity, Stars, law, 0103 physical sciences, Magnitude (astronomy), Satellite, 010303 astronomy & astrophysics, Spectrograph
Abstract: International audience; We present the scientific motivations for GYES: a high multiplex (of the order of several hundred), high resolution (about 20 000), spectrograph to be placed at the prime focus of the CFHT. The main purpose of such an instrument is to conduct a spectroscopic survey complementary to the Gaia mission. The final Gaia catalogue (expected around 2020) will provide accurate distances, proper motions and spectrophotometry for all the stars down to a magnitude of 20. The spectroscopic instrument on board the Gaia satellite will provide intermediate resolution (R=11 500) spectra for stars down to the 17th magnitude. For the fainter stars there will be no radial velocity information. For all the stars the chemical information will be limited to a few species. A multifibre spectrograph at the prime focus of the CFHT will be able to provide the high resolution spectra for stars fainter than 13th magnitude, needed to obtain both accurate radial velocities and detailed chemical abundances. The possible use of GYES will not be limited to Gaia complementary surveys and we here describe the potentialities of such an instrument. We describe here how the scientific drivers are translated into technical requirements. The results of our on-going feasibility study are described in an accompanying poster.
Published: 2010

16. Kinematics of galaxies in Compact Groups. Studying the B-band Tully-Fisher relation

Author: C. Mendes de Oliveira, Benoit Epinat, S. Torres-Flores, P. Amram, Claude Carignan, C. Balkowski, Henri Plana, Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Velocity dispersion, Sigma, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Tully–Fisher relation, 01 natural sciences, Galaxy, Redshift, Luminosity, Compact group, Space and Planetary Science, 0103 physical sciences, 10. No inequality, 010303 astronomy & astrophysics, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We obtained new Fabry-Perot data cubes and derived velocity fields, monochromatic and velocity dispersion maps for 28 galaxies in the Hickson compact groups 37, 40, 47, 49, 54, 56, 68, 79 and 93. We find that one third of the non-barred compact group galaxies have position angle misalignments between the stellar and gaseous components. This and the asymmetric rotation curves are clear signatures of kinematic perturbations, probably due to interactions among compact group galaxies. A comparison between the B-band Tully-Fisher relation for compact group galaxies and that for the GHASP field-galaxy sample shows that, despite the high fraction of compact group galaxies with asymmetric rotation curves, these lie on the Tully-Fisher relation defined by galaxies in less dense environments, although with more scatter. This is in agreement with previous results, but now confirmed for a larger sample of 41 galaxies. We confirm the tendency for compact group galaxies at the low-mass end of the Tully-Fisher relation (HCG 49b, 89d, 96c, 96d and 100c) to have either a magnitude that is too bright for its mass (suggesting brightening by star formation) and/or a low maximum rotational velocity for its luminosity (suggesting tidal stripping). These galaxies are outside the Tully Fisher relation, at the 1 sigma level, even when the minimum acceptable values of inclinations are used to compute their maximum velocities. The inclusion of such galaxies with v, 17 figures. Accepted for publication in Astronomy and Astrophysics. Hickson compact groups Fabry-Perot data are available at http://fabryperot.oamp.fr/PerotFabry/
Published: 2010

17. IMAGES-III: The evolution of the Near-Infrared Tully-Fisher relation over the last 6 Gyr

Author: Joel Vernet, Nicole P. H. Nesvadba, L. Chemin, B. Guiderdoni, P. Amram, F. Hammer, S. di Serego Alighieri, Benoit Epinat, C. J. Cesarsky, Lucia Pozzetti, C. D. Ravikumar, Isaura Fuentes-Carrera, Yun-Feng Liang, C. Balkowski, M. D. Lehnert, A. Rawat, Helmut Dannerbauer, Goeran Oestlin, Ajit K. Kembhavi, Mathieu Puech, Herve Wozniak, Y. Yang, Hector Flores, Benoit Neichel, D. Vergani, 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: spiral, Field (physics), FOS: Physical sciences, Angular velocity, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Tully–Fisher relation, Rotation, 01 natural sciences, Luminosity, galaxies: high-redshift, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, Physics, galaxies, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, interactions, galaxies: general, Galaxy, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract: Using the multi-integral field spectrograph GIRAFFE at VLT, we have derived the K-band Tully-Fisher relation (TFR) at z~0.6 for a representative sample of 65 galaxies with emission lines. We confirm that the scatter in the z~0.6 TFR is caused by galaxies with anomalous kinematics, and find a positive and strong correlation between the complexity of the kinematics and the scatter that they contribute to the TFR. Considering only relaxed-rotating disks, the scatter, and possibly also the slope of the TFR, do not appear to evolve with z. We detect an evolution of the K-band TFR zero point between z~0.6 and z=0, which, if interpreted as an evolution of the K-band luminosity of rotating disks, would imply that a brightening of 0.66+/-0.14 mag occurs between z~0.6 and z=0. Any disagreement with the results of Flores et al. (2006) are attributed to both an improvement of the local TFR and the more detailed accurate measurement of the rotation velocities in the distant sample. Most of the uncertainty can be explained by the relatively coarse spatial-resolution of the kinematical data. Because most rotating disks at z~0.6 are unlikely to experience further merging events, one may assume that their rotational velocity does not evolve dramatically. If true, our result implies that rotating disks observed at z~0.6 are rapidly transforming their gas into stars, to be able to double their stellar masses and be observed on the TFR at z=0. The rotating disks observed are indeed emission-line galaxies that are either starbursts or LIRGs, which implies that they are forming stars at a high rate. Thus, a significant fraction of the rotating disks are forming the bulk of their stars within 6 to 8 Gyr, in good agreement with former studies of the evolution of the M-Z relation., 17 pages, 11 figures, accepted for publication in A&A. v2 taking into account comments from language editor
Published: 2008

18. IMAGES II. A surprisingly low fraction of undisturbed rotating spiral disks at z~0.6: The morpho-kinematical relation 6 Gyrs ago

Author: Herve Wozniak, A. Rawat, Hector Flores, M. Lehnert, Yanchun Liang, I. Fuentes-Carrera, Nicole P. H. Nesvadba, Joel Vernet, Benoit Neichel, C. D. Ravikumar, Catherine Cesarsky, M. Puech, D. Vergani, B. Guiderdoni, Lucia Pozzetti, Göran Östlin, C. Balkowski, Helmut Dannerbauer, Francois Hammer, Yanbin Yang, S. di Serego Alighieri, R. Delgado, P. Amram, Ajit Kembhavi, 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), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), Observatoire de Paris - Site de Paris (OP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Inter-University Centre for Astronomy and Astrophysics [Pune] (IUCAA), National Astronomical Observatories, Chinese Academy of Sciences, Chinese Academy of Sciences [Beijing] (CAS), Stockholm Observatory Department of Astronomy, Stockholm University, INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), Space Telescope European Coordinating Facility (STECF), Space Telescope European Coordinating Facility, INAF - Osservatorio Astrofisico di Arcetri (OAA), Beaussier, Catherine, Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, European Southern Observatory (ESO), Inter-University Centre for Astronomy and Astrophysics (IUCAA), IFARHU-SENACYT, Technological University of Panama, National Astronomical Observatoires-CAS, Stockholm Observatory, AlbaNova University Center, INAF-Osservatorio Astronomico di Bologna (OABO), Department of Physics, University of Calicut, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: FOS: Physical sciences, Kinematics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Peculiar galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, biology, 010308 nuclear & particles physics, Gas supply, Astrophysics (astro-ph), Astronomy and Astrophysics, Morpho, biology.organism_classification, Galaxy, Accretion (astrophysics), Stars, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a first combined analysis of the morphological and dynamical properties for the Intermediate MAss Galaxy Evolution Sequence (IMAGES) sample. It is a representative sample of 52 z~0.6 galaxies with Mstell from 1.5 to 15 10^10Msun and possessing 3D resolved kinematics and HST deep imaging in at least two broad band filters. We aim at evaluate robustly the evolution of rotating spirals since z~0.6, as well as to test the different schemes for classifying galaxies morphologically. We used all the information provided by multi-band images, color maps and 2 dimensional light fitting to assign to each object a morphological class. We divided our sample between spiral disks, peculiar objects, compact objects and mergers. Using our morphological classification scheme, 4/5 of identified spirals are rotating disks and more than 4/5 of identified peculiar galaxies show complex kinematics, while automatic classification methods such as Concentration-Asymmetry and GINI-M20 severely overestimate the fraction of relaxed disk galaxies. Using this methodology, we find that the fraction of rotating spirals has increased by a factor ~ 2 during the last 6 Gyrs, a much higher fraction that found previously based on morphologies alone. These rotating spiral disks are forming stars very rapidly, doubling their stellar masses over the last 6 Gyrs, while most of their stars have been formed few Gyrs earlier, which reveals the presence of a large gas supply. Because they are likely the progenitors of local spirals, we can conjecture how their properties are evolving. Their disks show some evidence for an inside-out growth and the gas supply/accretion is not made randomly as the disk need to be stable in order to match the local disk properties., Typos corrected, reference added
Published: 2008

19. A Virgo high-resolution Halpha kinematical survey : II. The Atlas

Author: C. Adami, J. Boulesteix, M. Marcelin, P. Amram, L. Chemin, O. Garrido, A. Boselli, Oscar F. Hernández, V. Cayatte, Claude Carignan, C. Balkowski, 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), Département de Physique [Montréal], Université de Montréal (UdeM), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), 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), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université de Montréal [Montréal], PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Département de Physique et Observatoire du Mont-Mégantic, Université de Montréal, Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de Marseille Provence (OAMP), and Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: clusters: individual: NGC 4438, FOS: Physical sciences, Astrophysics, Kinematics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, galaxies: interactions, 010303 astronomy & astrophysics, Spiral, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Line (formation), Physics, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Virgo Cluster, Galaxy, Interferometry, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Irregular galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: A catalog of ionized gas velocity fields for a sample of 30 spiral and irregular galaxies of the Virgo cluster has been obtained by using three-dimensional optical data. The aim of this survey is to study the influence of high density environments on the gaseous kinematics of local cluster galaxies. Observations of the Halpha line by means of Fabry-Perot interferometry have been performed at the Canada-France-Hawaii, ESO 3.6m, Observatoire de Haute-Provence 1.93m and Observatoire du mont Megantic telescopes at angular and spectral samplings from 0.4" to 1.6" and 7 to 16 km/s. A recently developed, automatic and adaptive spatial binning technique is used to reach a nearly constant signal-to-noise ratio (S/N) over the whole field-of-view, allowing to keep a high spatial resolution in high S/N regions and extend the detection of signal in low S/N regions. This paper is part of a series and presents the integrated emission-line and velocity maps of the galaxies. Both Halpha morphologies and kinematics exhibit signs of perturbations in the form of e.g. external filaments, inner and nuclear spiral- and ring-like structures, inner kinematical twists, kinematical decoupling of a nuclear spiral, streaming motions along spiral arms and misalignment between kinematical and photometric orientation axes., 17 pages, 9 figures, accepted for publication in MNRAS. All high-res. figures are available on http://www.astro.umontreal.ca/fantomm/virgo . High res. versions of the article are available on ftp://ftp.astro.umontreal.ca/outgoing/chemin
Published: 2006

20. 3D spectroscopy with VLT/GIRAFFE. I. The true Tully Fisher relationship at z ˜ 0.6

Author: C. Balkowski, M. Puech, Philippe Amram, H. Flores, Francois Hammer, 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), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Physics, Stellar mass, 010308 nuclear & particles physics, Star formation, Dark matter, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Baryon, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Spectroscopy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; A precise derivation of the evolution of the Tully Fisher is crucial to understand the interplay between dark matter and baryonic matter in cosmological models, using 15 deployable integral field units of FLAMES/GIRAFFE at VLT, we have recovered the velocity fields of 35 galaxies at intermediate redshift (0.4 < z < 0.75). This facility is able to recover the velocity fields of almost all the emission line galaxies with IAB=15 Å. In our sample, we find only 35% rotating disks. These rotating disks produce a Tully-Fisher relationship (stellar mass or MK versus Vmax) which has apparently not evolved in slope, zero point and scatter since z=0.6. The only evolution found is a brightening of the B band luminosity of a third of the disks, possibly due to an enhancement of the star formation. The very large scatters found in previously reported Tully-Fisher relationships at moderate redshifts are caused by the numerous (65%) galaxies with perturbed or complex kinematics. Those galaxies include minor or major mergers, merger remnants and/or inflow/outflows and their kinematics can be easily misidentified by slit spectroscopy. Their presence suggests a strong evolution in the dynamical properties of galaxies during the last 7 Gyr.
Published: 2006

21. A Virgo high-resolution Halpha kinematical survey: I. NGC 4438

Author: C. Adami, M. Marcelin, A. Boselli, V. Cayatte, L. Chemin, Oscar F. Hernández, Claude Carignan, C. Balkowski, J. Boulesteix, P. Amram, O. Garrido, Département de Physique [Montréal], Université de Montréal [Montréal], Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université de Montréal (UdeM), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), and 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)
Subjects: galaxies: clusters: individual: NGC 4438, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, Surface brightness, Disc, Dwarf elliptical galaxy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Virgo Cluster, Galaxy, Interferometry, Space and Planetary Science, Vector field
Abstract: New Halpha emission-line observations of the Virgo cluster galaxy NGC 4438 are presented. Fabry-Perot interferometry data at an effective angular resolution of ~2" are used to map the kinematics of the ionized gas in the galaxy. For the first time we obtain a velocity field covering a large area in NGC 4438, much larger than that deduced from previous HI and CO maps. The kinematics of the extended, low surface brightness Halpha filaments to the West of the galactic disk is discussed. We report on the discovery of a northern Halpha structure which is clumpier than the other filaments. Evidence for multiple spectral components through the data-cube are presented in a nuclear shell and in the approaching half of the disk. The role of VCC 1040, a dwarf elliptical galaxy located to the South of NGC 4438, is presented to investigate the origin of a small-scale stellar tail of NGC 4438. It could be due to a minor tidal interaction between the two galaxies., 11 pages, 11 figures, accepted for publication in A&A. To obtain a higher resolution version, go to ftp://ftp.astro.umontreal.ca/outgoing/chemin/file1664.ps.gz
Published: 2005

22. A nearby massive galaxy cluster behind the Milky Way

Author: C. Balkowski, P. A. Henning, V. Cayatte, Patrick A. Woudt, Renee C. Kraan-Korteweg, and A. P. Fairall
Subjects: Physics, Multidisciplinary, Norma Cluster, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Abell 2744, Galaxy group, Brightest cluster galaxy, Interacting galaxy, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Dwarf galaxy
Abstract: THE recession velocities of relatively nearby galaxies show systematic deviations from a uniform expansion field. These deviations indicate the presence of the 'Great Attractor'—a large concentration of mass (∼5 x 1016 solar masses) that lies in the direction of the southern Milky Way1,2. Attempts to quantify both the nature and extent of the Great Attractor3–11 have been hampered by the fact that it is largely hidden by the disk of the Milky Way. Although there is an excess of galaxies in this region12, no dominant galaxy cluster or other concentration of mass has hitherto been identified. Here we present results from a survey of galaxies obscured (or partially obscured) by the southern Milky Way. Our results show that a previously identified galaxy cluster, Abell 3627, which lies only 9 ° from the predicted centre of the Great Attractor13, is very massive (∼5 x 1015 solar masses). The cluster's redshift is also near that predicted for the core of the Great Attractor2,3,12–14, suggesting that it lies at or near the bottom of the Attractor's gravitational potential well.
Published: 1996

23. The Compact Group of Galaxies HCG 31 is in an early phase of merging

Author: Henri Plana, P. Amram, Jean-Luc Gach, Claude Carignan, C. Balkowski, Olivier Hernandez, J. Boulesteix, C. Mendes de Oliveira, Laerte Sodré, Eduardo S. Cypriano, Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Velocity dispersion, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, 01 natural sciences, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Compact group, Space and Planetary Science, Galaxy group, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Dwarf galaxy
Abstract: We have obtained high spectral resolution (R = 45900) Fabry-Perot velocity maps of the Hickson Compact Group HCG 31 in order to revisit the important problem of the merger nature of the central object A+C and to derive the internal kinematics of the candidate tidal dwarf galaxies in this group. Our main findings are: (1) double kinematic components are present throughout the main body of A+C, which strongly suggests that this complex is an ongoing merger (2) regions $A2$ and E, to the east and south of complex A+C, present rotation patterns with velocity amplitudes of $\sim 25 km s^{-1}$ and they counterrotate with respect to A+C, (3) region F, which was previously thought to be the best example of a tidal dwarf galaxy in HCG 31, presents no rotation and negligible internal velocity dispersion, as is also the case for region $A1$. HCG 31 presents an undergoing merger in its center (A+C) and it is likely that it has suffered additional perturbations due to interactions with the nearby galaxies B, G and Q., Comment: 5 pages + figures - Accepted to ApJ Letter
Published: 2004
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24. Extragalactic Large-Scale Structures behind the Southern Milky Way. IV. Redshifts Obtained with MEFOS

Author: P. Felenbok, C. Balkowski, Renee C. Kraan-Korteweg, Patrick A. Woudt, V. Cayatte, Department of Astronomy, and Faculty of Science
Subjects: Milky Way, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Large-scale structure, Great Attractor, surveys, Catalogue astronomique, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Distance, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Zone of Avoidance, Astronomy and Astrophysics, Astronomical catalogues, Galaxies, Redshift survey, clusters: individual: ACO 3627, Galaxy, Redshift, Red shift, Distances, Structure grande échelle, Stars, Space and Planetary Science, Déplacement vers le rouge, large-scale structure of Universe, Astrophysics::Earth and Planetary Astrophysics, galaxies: distances and redshifts, catalogs, ISM: dust, extinction
Abstract: Abbreviated: As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266deg < l < 338deg, |b| < 10deg), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way. A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v, Comment: 11 pages, 7 figures; accepted for publication in A&A. Tables 1 and 2 will be available in electronic format at the CDS. Figure 1 at full resolution, and both tables are available at http://mensa.ast.uct.ac.za/~pwoudt/data/H4462/)
Published: 2003
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25. A search for Low Surface Brightness galaxies in the near-infrared III. Nancay HI line observation

Author: Thomas H. Jarrett, D. Monnier Ragaigne, C. Balkowski, W. van Driel, and Stephen E. Schneider
Subjects: Physics, Near-infrared spectroscopy, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Galaxy, law.invention, Telescope, Space and Planetary Science, law, Surface brightness, Line (formation)
Abstract: A total of 334 Low Surface Brightness galaxies detected in the 2MASS all-sky near-infrared survey have been observed in the 21 cm HI line using the Nancay telescope. All have a K_s-band mean central surface brightness, measured within a 5 arcsec radius, fainter than 18 mag/arcsec^2 and a K_s-band isophotal radius at the 20 mag/arcsec^2 level larger than 20 arcsec. We present global HI line parameters for the 171 clearly detected objects and the 23 marginal detections, as well as upper limits for the undetected objects. The 171 clear detections comprise 50 previously uncatalogued objects and 41 objects with a PGC entry only., Accepted for publication by Astronomy and Astrophysics on 15 May 2003, 41 pages
Published: 2003

26. A search for Low Surface Brightness galaxies in the near-infrared I. Selection of the sample

Author: C. Balkowski, Thomas H. Jarrett, D. Monnier Ragaigne, W. van Driel, and Stephen E. Schneider
Subjects: Physics, Brightness, education.field_of_study, Near-infrared spectroscopy, Population, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Sample (graphics), Galaxy, High surface, Space and Planetary Science, Surface brightness, education
Abstract: A sample of about 3,800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and K_s-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5 arcsec radius around their centre fainter than 18 mag/sq.arcsec in the K_s band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and `classical' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a (B_T_c)-(K_T) colour which is on average 0.9 mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects., Comment: accepted for publication in Astronomy and Astrophysics on 24/2/2003; 62 pages
Published: 2003
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27. The Properties of Low Surface Brightness Galaxies

Author: D. Monnier Ragaigne, W. Van Driel, C. Balkowski, S. Boissier, and N. Prantzos
Published: 2003

28. From Spirals to Low Surface Brightness Galaxies

Author: Nikos Prantzos, C. Balkowski, W. van Driel, S. Boissier, and D. Monnier Ragaigne
Subjects: Physics, Luminous infrared galaxy, Radio galaxy, Surface brightness fluctuation, Galaxy group, Elliptical galaxy, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Disc, Lenticular galaxy, Astrophysics::Galaxy Astrophysics, Peculiar galaxy
Abstract: We show that simple models of the chemical and spectrophotometric evolution of galaxies can be used to explore the properties of present-day galaxies and especially the causes of the observed variety among disc galaxies. We focus on the link between ‘classical’ spirals and Low Surface Brightness galaxies.
Published: 2003

29. Structure, mass and distance of the Virgo cluster from a Tolman-Bondi model

Author: José M. Solanes, T. Sanchis, C. Balkowski, Pascal Fouqué, Fouqué, Pascal, Departement de recherche SPAtiale (DESPA), Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Cepheid variable, Structure (category theory), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], General Relativity and Quantum Cosmology, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Virial mass, Radius, Virgo Cluster, Galaxy, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
Abstract: We have applied a relativistic Tolman-Bondi model of the Virgo cluster to a sample of 183 galaxies with measured distances within a radius of 8 degrees from M87. We find that the sample is significantly contaminated by background galaxies which lead to too large a cluster mean distance if not excluded. The Tolman-Bondi model predictions, together with the HI deficiency of spiral galaxies, allows one to identify these background galaxies. One such galaxy is clearly identified among the 6 calibrating galaxies with Cepheid distances. As the Tolman-Bondi model predicts the expected distance ratio to the Virgo distance, this galaxy can still be used to estimate the Virgo distance, and the average value over the 6 galaxies is 15.4 +- 0.5 Mpc. Well-known background groups of galaxies are clearly recovered, together with filaments of galaxies which link these groups to the main cluster, and are falling into it. No foreground galaxy is clearly detected in our sample. Applying the B-band Tully-Fisher method to a sample of 51 true members of the Virgo cluster according to our classification gives a cluster distance of 18.0 +- 1.2 Mpc, larger than the mean Cepheid distance. Finally, the same model is used to estimate the Virgo cluster mass, which is M = 1.2 10^{15} Msun within 8 degrees from the cluster center (2.2 Mpc radius), and amounts to 1.7 virial mass., Comment: 12 pages, 7 figures. Astronomy and Astrophysics, in press (accepted May 31, 2001)
Published: 2001

30. Unusual magnetic fields in the interacting spiral NGC 3627

Author: Rainer Beck, Marian Soida, Richard Wielebinski, C. Balkowski, and Marek Urbanik
Subjects: Physics, Turbulent diffusion, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), Dust lane, Galaxy, Magnetic field, Radio telescope, symbols.namesake, Space and Planetary Science, Faraday effect, symbols, Halo, Astrophysics::Galaxy Astrophysics
Abstract: By observing the interacting galaxy NGC 3627 in radio polarization we try to answer the question to which degree the magnetic field follows the galactic gas flows. We obtained total power and polarized intensity maps at 8.46 GHz and 4.85 GHz using the VLA in its compact D-configuration. In order to overcome the zero-spacing problems, the interferometric data were combined with single-dish measurements obtained with the Effelsberg 100-m radio telescope. The observed magnetic field structure in NGC 3627 suggests that two field components are superposed. One component smoothly fills the interarm space and shows up also in the outermost disk regions, the other component follows a symmetric S-shaped structure. In the western disk the latter component is well aligned with an optical dust lane, following a bend which is possibly caused by external interactions. However, in the SE disk the magnetic field crosses a heavy dust lane segment, apparently being insensitive to strong density-wave effects. We suggest that the magnetic field is decoupled from the gas by high turbulent diffusion, in agreement with the large \ion{H}{i} line width in this region. We discuss in detail the possible influence of compression effects and non-axisymmetric gas flows on the general magnetic field asymmetries in NGC 3627. On the basis of the Faraday rotation distribution we also suggest the existence of a large ionized halo around this galaxy., Comment: 11 pages, 11 figures
Published: 2001
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31. Kinematics and morphology of ionized gas in Hickson Compact Group 18

Author: P. Amram, C. Mendes de Oliveira, Henri Plana, and C. Balkowski
Subjects: Physics, Distribution (number theory), Group (mathematics), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Kinematics, Plasma, Astrophysics::Cosmology and Extragalactic Astrophysics, Interferometry, Compact group, Space and Planetary Science, Vector field, Irregular galaxy, Astrophysics::Galaxy Astrophysics
Abstract: We present new observations of $H\alpha $ emission in the Hickson Compact Group 18 (HCG 18) obtained with a scanning Fabry-Perot interferometer. The velocity field does not show motions of individual group members but, instead, a complex common velocity field for the whole group. The gas distribution is very asymmetric with clumps of maximum intensity coinciding with the optically brightest knots. Comparing $H\alpha $ and HI data we conclude that HCG 18 is not a compact group but instead a large irregular galaxy with several clumps of star formation., Comment: Accepted for publication in Astronomical Journal (13p 6 figures)
Published: 2000

32. The ESO Slice Project (ESP) Redshift Survey

Author: G. Vettolani, E. Zucca, A. Cappi, R. Merighi, M. Mignoli, G. Stirpe, G. Zamorani, H. MacGillivray, C. Collins, C. Balkowski, V. Cayatte, S. Maurogordato, D. Proust, G. Chincarini, L. Guzzo, D. Maccagni, R. Scaramella, A. Blanchard, and M. Ramella
Subjects: Physics, Scale structure, Galaxy formation and evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectroscopy, Wide field, Cosmology, Field (geography), Redshift
Abstract: In this short survey of the applications of wide-field, multi-object spectroscopy to galaxy evolution, large-scale structure and cosmology, I interleave summaries of the general goals and state of play in these fields with specific examples based on my own recent work. I first briefly review the goals and figures of merit for current and future redshift surveys, before examining some recent results from deep surveys in the field, cluster redshift surveys and surveys of large scale structure. I take a look beyond redshift surveys to other probes of galaxy evolution before concluding with a discussion of the future prospects for such studies using the next generation of wide-field, multi-object spectrographs on large telescopes.
Published: 1997

33. A Tidal Dwarf Galaxy in the Hercules Cluster?

Author: W. van Driel, John M. Dickey, Pierre-Alain Duc, C. Balkowski, Jorge Iglesias-Páramo, P. Amram, P. Papaderos, H. Hernández, V. Cayatte, José M. Vílchez, Karen O'Neil, and F. Bournaud
Subjects: Physics, Computer Science::Hardware Architecture, Galactic astronomy, Milky Way, Cluster (physics), Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf spheroidal galaxy, Dwarf galaxy
Abstract: A candidate Tidal Dwarf Galaxy, ce-61, was identified in the merger system IC 1182 in the Hercules supercluster. The multi-wavelength data we obtained so far do not prove, however, that it is kinematically detached from the IC 1182 system and gravitationally bound.
Published: 2004

34. Determining the morpho-kinematic properties of a face-on merger atz~ 0.7

Author: C. Balkowski, S. Peirani, Myriam Rodrigues, Hector Flores, I. Fuentes-Carrera, Y. B. Yang, and Francois Hammer
Subjects: Physics, 010308 nuclear & particles physics, Star formation, Perturbation (astronomy), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Kinematics, Astrophysics, Mass ratio, 01 natural sciences, Galaxy, Redshift, Integral field spectrograph, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Context. At intermediate redshifts, many galaxies seem to have experienced an interaction. It is not always straightforward to determine what type of encounter or perturbation is observed, nor the outcome of this event. In some cases, only the use of both morphological and kinematical information can determine the true configuration of an encounter at intermediate redshift. Aims. We present the morphological and kinematical analysis of a system at z = 0.74 to understand its configuration, interacting stage, and evolution. Methods. Using the integral field spectrograph GIRAFFE, long-slit spectroscopy by FORS2, direct optical images from the HST-ACS, and ISAAC near-infrared images, we determine the morphology of this system, its star-formation history, and its extended kinematics to propose a possible configuration for the system. Numerical simulations are used to test different interacting scenarii. Results. We identify this system to be a face-on disk galaxy with a very bright bar that is interacting with a smaller companion such that the galaxy and the companion have a mass ratio of 3:1. The relevance of kinematical information and the constraints that it imposes on the interpretation of the observations of distant galaxies are particularly greater in this case. Conclusions. This object represents one of the clearest examples of how one can misinterpret morphology in the absence of kinematical information.
Published: 2010

35. What Can We Learn From Dynamics Of Nearby Galaxies To Study Distant Galaxies?

Author: P. Amram, C. Balkowski, and B. Epinat
Subjects: Physics, Space and Planetary Science, Extremely Large Telescope, Astronomy, Astronomy and Astrophysics, Astrophysics, Galaxy, Redshift, 3d kinematics
Abstract: This is an ongoing project.During last few years, new instruments like GIRAFFE (Flores, H., Hammer, F., Puech, M., et al., 2006, A&A 455,107) or SINFONI (Förster Schreiber, N.M., Genzel, R., Lehnert, M.D., et al., 2006, ApJ 645,1062) have began investigations on 3D kinematics of high redshift galaxies. This is just the head of the iceberg as Extremely Large Telescope will allow this kind of study on a larger sample. By now, it is important to be able to recover the actual kinematic parameters, and overall to disentangle evolutionnary effects from distance effects.
Published: 2006

36. Do rotation curves of spiral galaxies in clusters decline?

Author: W. T. Sullivan, M. Marcelin, P. Amram, V. Cayatte, and C. Balkowski
Subjects: Physics, Spiral galaxy, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy groups and clusters, Space and Planetary Science, Elliptical galaxy, Brightest cluster galaxy, Interacting galaxy, Lenticular galaxy, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Galaxy rotation curve
Abstract: Rotation curves for 21 spiral galaxies in five clusters have been obtained in a search for possible effects of the cluster environment on individual galaxy dynamics. We find no significant evidence for anything more than a small influence of the cluster environment. In particular, using 12 selected galaxies we do not confirm the strong correlation between slope of rotation curve and location within a cluster reported by Whitmore, Fobes, & Rubin
Published: 1993

37. Extragalactic large-scale structures behind the southern Milky Way

Author: A. Woudt, P., C. Kraan-Korteweg, R., Cayatte, V., C. Balkowski, and Felenbok, P.
Abstract: As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region ($266^\circ \le \ell \le 338^\circ$, $|\,b\,| \la 10^\circ$), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg [CITE]; Woudt & Kraan-Korteweg [CITE]). A total of 947 galaxies have been observed, a small percentage of the spectra ($N = 109$, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances ($v \la 30\,000$ km s$^{-1}$) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al. [CITE]; Fairall et al. [CITE]; Woudt et al. [CITE]) and the 64-m Parkes radio telescope (Kraan-Korteweg et al. [CITE]). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.
Published: 2004

38. The Galaxian Surface Density in the Nearby Universe

Author: P. Fontanelli, C. Balkowski, and P. Chamaraux
Subjects: Physics, Surface (mathematics), Simple (abstract algebra), media_common.quotation_subject, Astrophysics, Universe, Galaxy, Redshift, media_common
Abstract: A simple study of the galaxian surface density maps of the nearby Universe, obtained from CGCG, MCG and ESO catalogues, has allowed to evidence 3 new large-scale structures. Analysis of the redshifts of the galaxies in the corresponding zones shows that two of them are probably real three-dimensional entities.
Published: 1987

39. Observational Evidence for Non-Velocity Redshift in Stephan's Quintet

Author: C. Balkowski, L. Bottinelli, P. Chamaraux, L. Gouguenheim, and J. Heidmann
Abstract: Distance determinations of the high-redshift galaxy NGC 7319 in Stephan's Quintet, based on 21-cm line observations, yield a value much smaller than the cosmological distance. At the 98.7 % level, a part of the redshift of this galaxy which could amount to 5000 km s−1 is anomalous.
Published: 1974

40. A study of H I-selected galaxies in the Hercules cluster

Author: John M. Dickey, V. Cayatte, José M. Vílchez, P. Papaderos, Jorge Iglesias-Páramo, C. Balkowski, Trinh X. Thuan, Pierre-Alain Duc, W. van Driel, H. Hernández, Karen O'Neil, 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), 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), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Sternwarte Weinheim, Instituto de Astrofisica de Andalucia, CSIC (IAA), Arecibo Observatory, Department of Astronomy, University of Minnesota, and Astronomy Department, University of Virginia, Charlottesville
Subjects: 010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Disc galaxy, 01 natural sciences, Spectral line, 0103 physical sciences, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dwarf galaxy, media_common, Physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Redshift, Galaxy, Photometry (astronomy), Space and Planetary Science, Sky, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], abundances, dwarf, general, galaxies, clusters, individual, Hercules cluster
Abstract: The present study is aimed at a sample of 22 galaxies detected in the blind VLA HI survey of the Hercules cluster by Dickey (1997), 18 of which were selected on an HI line width smaller than 270 km/s and 4 others with only tentative optical counterparts on the Palomar Sky Survey. Sensitive single-dish HI line spectra were obtained for 20 of them, and for one (47-154) the VLA detection was not confirmed. Optical surface photometry was obtained of 10 objects, for 8 of which optical spectroscopy was obtained as well. Based on various selection criteria, two (ce-143 and ne-204) can be classified as dwarfs. The objects of which optical observations were made show star formation properties similar to those of published samples of actively star forming galaxies, and approximately half of them have properties intermediate between those of dwarf galaxies and low-luminosity disc galaxies. No optical redshifts could be obtained for two of the galaxies (sw-103 and sw-194) and their physical association with the HI clouds detected at their positions therefore remains uncertain. Unique among the objects is the Tidal Dwarf Galaxy ce-061 in a tail of the IC 1182 merger system., Comment: 20 pages, 19 figures, accepted for publication in A&A

41. an overview of the MHONGOOSE survey: Observing nearby galaxies with MeerKAT

Author: Gyula I. G. Józsa, Frank Bigiel, J. A. Sellwood, D. M. Lucero, B. S. Koribalski, Ioannis Bagetakos, Adam K. Leroy, B. S. Frank, Francoise Combes, Snezana Stanimirovic, Matthew Smith, John Conway, J. S. Gallagher, A. Bosma, Hans-Rainer Klöckner, Claude Carignan, O. I. Wong, R. C. Kraan-Korteweg, Filippo Fraternali, L. Chemin, W. J. G. de Blok, C. Balkowski, Elizabeth A. K. Adams, Stephane Leon, Tobias Westmeier, M. Kapala, Manuel Meyer, M. Bershady, S. L. Blyth, Gerhardt R. Meurer, P. Amram, D. J. Pisano, Attila Popping, S. Ratcliffe, George Heald, Stacy S. McGaugh, Fabian Walter, Benne W. Holwerda, Tom Oosterloo, Eric M. Wilcots, Lourdes Verdes-Montenegro, Roy Booth, Edward C. Elson, K. J. van der Heyden, Benoit Epinat, E. Athanassoula, Thomas H. Jarrett, S. H. Oh, Patrick Woudt, K. Sheth, B. Namumba, J. Fiege, Elias Brinks, Brad K. Gibson, W. van Driel, M. Mogotsi, Terry Williams, Helmut Jerjen, A. Sorgho, S. I. Loubser, A. A. Zijlstra, Anke Schröder, Robert Beswick, P. A. Henning, A. Bouchard, Eva Schinnerer, Jayanne English, and Kristine Spekkens
Subjects: Physics, Star formation, Molecular cloud, media_common.quotation_subject, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Universe, Accretion (astrophysics), Supernova, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics, media_common, Dwarf galaxy, QB
Abstract: MHONGOOSE is a deep survey of the neutral hydrogen distribution in a representative sample of 30 nearby disk and dwarf galaxies with HI masses from 10^6 to ~10^{11} M_sun, and luminosities from M_R ~ -12 to M_R ~ -22. The sample is selected to uniformly cover the available range in log(M_HI). Our extremely deep observations, down to HI column density limits of well below 10^{18} cm^{-2} - or a few hundred times fainter than the typical HI disks in galaxies - will directly detect the effects of cold accretion from the intergalactic medium and the links with the cosmic web. These observations will be the first ever to probe the very low-column density neutral gas in galaxies at these high resolutions. Combination with data at other wavelengths, most of it already available, will enable accurate modelling of the properties and evolution of the mass components in these galaxies and link these with the effects of environment, dark matter distribution, and other fundamental properties such as halo mass and angular momentum. MHONGOOSE can already start addressing some of the SKA-1 science goals and will provide a comprehensive inventory of the processes driving the transformation and evolution of galaxies in the nearby universe at high resolution and over 5 orders of magnitude in column density. It will be a Nearby Galaxies Legacy Survey that will be unsurpassed until the advent of the SKA, and can serve as a highly visible, lasting statement of MeerKAT's capabilities., To be published in "MeerKAT Science: On the Pathway to the SKA". Proceedings of Science. Workshop held 25-27 May, 2016 Stellenbosch, South Africa

42. The ESO slice project (ESP) galaxy redshift survey III. The sample

Author: E. Zucca, C. Balkowski, D. Proust, Chris A. Collins, S. Maurogordato, V. Cayatte, Luigi Guzzo, G. M. Stirpe, Giampaolo Vettolani, Roberto Scaramella, A. Cappi, R. Merighi, Guido Chincarini, G. Zamorani, H. MacGillivray, M. Ramella, M. Mignoli, Alain Blanchard, D. Maccagni, and P. Felenbok
Subjects: Physics, Astrophysics (astro-ph), General Physics and Astronomy, Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spanned volume, Redshift survey, Galaxy, Redshift, Pencil (optics), Limiting magnitude, Astrophysics::Galaxy Astrophysics, Data reduction
Abstract: The ESO Slice Project (ESP) is a galaxy redshift survey extending over about 23 square degrees, in a region near the South Galactic Pole. The survey is ~85% complete to the limiting magnitude b_J=19.4 and consists of 3342 galaxies with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one-dimensional pencil beams; the spanned volume is ~ 5 x 10^4 Mpc^3 at the sensitivity peak (z ~ 0.1). In this paper we present the description of the observations and of the data reduction, the ESP redshift catalogue and the analysis of the quality of the velocity determinations., Comment: 10 pages, 4 encapsulated figures, uses A&A LATEX; A&A Supplements in press (June 1998 issue)

43. A redshift survey in the South Galactic Pole region

Author: Alain Blanchard, E. Zucca, C. Balkowski, D. Maccagni, Giampaolo Vettolani, M. Ramella, H. MacGillivray, M. Mignoli, Luigi Guzzo, P. Felenbok, Roberto Scaramella, G. Zamorani, R. Merighi, Chris A. Collins, A. Cappi, D. Proust, G. M. Stirpe, J. M. Alimi, Sophie Maurogordato, V. Cayatte, and Guido Chincarini
Subjects: Physics, Limiting magnitude, Astrophysics, Redshift survey, Galaxy, Redshift, Square (algebra)
Abstract: We present preliminary results of a galaxy redshift survey we are accomplishing as an ESO Key Project over about 40 square degrees in a region near the South Galactic Pole, to a limiting magnitude bJ = 19.4. Up to now ∼ 50% of the survey has been completed, providing about 2000 galaxy redshifts.

44. Reconstructing cluster peculiar velocities within 20000 km/sR

Author: BRANCHINI, ENZO FRANCO, Plionis M., S. Maurogordato, C. Balkowski, C. Tao, and J. Tran Thanh Van, Branchini, ENZO FRANCO, and Plionis, M.
Subjects: large scale structures, cosmology
Published: 1995

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