Results 71 to 80 of about 87,149 (376)
Star cluster formation and star formation: the role of environment and star-formation efficiencies [PDF]
, 2008 “The original publication is available at www.springerlink.com”. Copyright Springer. DOI: 10.1007/s10509-009-0088-5By analyzing global starburst properties in various kinds of starburst and post-starburst galaxies and relating them to the properties of ...A. Pasquali, A. Schulz, B.C. Whitmore, B.C. Whitmore, B.C. Whitmore, B.G. Elmegreen, B.W. Miller, C. Maraston, C.D. Wilson, C.D. Wilson, C.J. Jog, C.J. Jog, D. Calzetti, E. Hummel, F. Schweizer, F. Schweizer, F. Schweizer, F. Schweizer, G. Parmentier, G. Parmentier, G. Trancho, G. Worthey, G.R. Meurer, H. Krueger, J. Gorgas, J. Schulz, J.H. Brown, K.A. Knierman, M. Haas, M.D. Mora, O.M. Kurth, P. Anders, P. Anders, P. Anders, P. Anders, P. Goudfrooij, P. Goudfrooij, P. Goudfrooij, P. Goudfrooij, P.M. Solomon, R. Grijs de, R. Grijs de, S. Bergh van der, S.C. Gallagher, S.E. Zepf, S.G. Boutloukos, S.S. Larsen, S.S. Larsen, T. Lilly, T. Lilly, U. Fritze-v. Alvensleben, U. Fritze-v. Alvensleben, U. Fritze-v. Alvensleben, U. Fritze-v. Alvensleben, Uta Fritze, Y. Gao, Y. Gao, Y. Li, Y. Shioya +58 morecore +2 more sourcesTHE SEQUENTIAL STAR FORMATION IN GLOBULAR CLUSTERS
Odessa Astronomical Publications, 2008 The results of [O/Na] abundance modelling in globular clusters NGC 2808 and NGC 6752 are presented. The evolutionary scenario allowing to reproduce characteristic observed features of [O/Na] distribution function has been suggested.M. V. Ryabova, Yu. A. Shchekinovdoaj +1 more sourceMultiple populations in globular clusters. Lessons learned from the
Milky Way globular clusters
, 2012 Recent progress in studies of globular clusters has shown that they are not
simple stellar populations, being rather made of multiple generations. Evidence
stems both from photometry and spectroscopy.A Bellini, A Bragaglia, A Bragaglia, A Buzzoni, A Dotter, A Duquennoy, A D’Ercole, A D’Ercole, A Helmi, A Helmi, A Kayser, A Klypin, A Koch, A Korn, A Krabbe, A Maeder, A Marino, A McWilliam, A Moretti, A Mucciarelli, A Mucciarelli, A Recio-Blanco, A Renzini, A Sandage, A Sarajedini, A Siebert, A Sollima, A Sollima, AA Kepley, AAR Valcarce, AC Boley, AD Mackey, AF Marino, AF Marino, AF Marino, AF Marino, AGW Cameron, AI Karakas, AK Dupree, Angela Bragaglia, AP Milone, AP Milone, AP Milone, AP Milone, AR Walker, AV Kravtsov, AV Macciò, AV Sweigart, AV Sweigart, B Davies, B Davies, B Gao, B Letarte, B Moore, B Yanny, BB Behr, BB Behr, BG Elmegreen, BJ Anthony-Twarog, BJ Armosky, BW Carney, C Chiappini, C Conroy, C Lardo, C Sneden, C Sneden, C Sneden, C Sosin, CA Pilachowski, CB Stephenson, CF McKee, CI Johnson, CI Johnson, CJ Grillmair, CJ Lada, CJ Walcher, D Butler, D Carollo, D Fabbian, D Harbeck, D Heggie, D Schaerer, D Yong, D Yong, D Yong, D Yong, D Yong, D Yong, D Yong, D Yong, D-G Roh, DA Crocker, DC Heggie, DE McLaughlin, DE McLaughlin, DK Lai, E Bica, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Carretta, E Hennekemper, E Pancino, E Pancino, E Pancino, E Tolstoy, E Vesperini, E Vesperini, E Vesperini, EA Mallia, EN Kirby, Eugenio Carretta, EW Olszewski, F Caputo, F D’Antona, F D’Antona, F D’Antona, F D’Antona, F D’Antona, F D’Antona, F D’Antona, F D’Antona, F D’Antona, F Fusi Pecci, F Grundahl, FR Ferraro, FR Ferraro, FR Ferraro, FR Ferraro, G Bertelli, G James, G Marchi De, G Marchi De, G Michaud, G Pace, G Parmentier, G Parmentier, G Piotto, G Piotto, G Piotto, G Piotto, G Schaller, G Tenorio-Tagle, G Zhao, GE Langer, GH Smith, GH Smith, GH Smith, GH Smith, GM Silva de, GS Costa Da, H Baumgardt, HB Richer, HJGLM Lamers, HL Morrison, I Negueruela, I-J Sackmann, II Ivans, II Ivans, IU Roederer, IU Roederer, J Anderson, J Dabringhausen, J Goodman, J Greissl, J Norris, J Pflamm-Altenburg, J Rossa, J Vinkó, J-W Lee, JA Johnson, JE Hesser, JE Norris, JE Norris, JG Cohen, JG Cohen, JG Cohen, JG Cohen, JG Cohen, JG Cohen, JG Cohen, JG Cohen, JL Greenstein, JM Scalo, JMD Kruijssen, JP Brodie, JR Hurley, JS Bullock, JW Truran, K Bekki, K Bekki, K Bekki, K Bekki, K Bekki, K Bekki, K Bekki, K Freeman, K Freeman, K Glatt, K Jordi, K Lind, K Lind, KC Freeman, L Aguilar, L Girardi, L Greggio, L Origlia, L Pasquini, L Pasquini, L Sbordone, L Siess, LM Stanford, LM Stanford, LR Bedin, M Arnould, M Bellazzini, M Catelan, M Catelan, M Criscienzo di, M Criscienzo di, M Gieles, M Henon, M Hilker, M Jurić, M Odenkirchen, M Odenkirchen, M Ricotti, M Salaris, M Shetrone, M Steinmetz, M Steinmetz, M Trenti, M Wadepuhl, M Zoccali, MAC Perryman, MF Nieva, MH Siegel, MM Briley, MM Briley, MM Briley, MM Briley, N Bastian, N Ivanova, N Ivanova, N Prantzos, N Prantzos, OY Gnedin, P Bonifacio, P Goudfrooij, P Ventura, P Ventura, P Ventura, P Ventura, P Ventura, P Ventura, P Ventura, P Ventura, PA Denisenkov, PL Cottrell, R Gilmozzi, R Gratton, R Gratton, R Gratton, Raffaele G. Gratton, RC Brüns, RC Peterson, RD Cannon, RG Gratton, RG Gratton, RG Gratton, RG Gratton, RG Gratton, RG Gratton, RG Gratton, RG Gratton, RI Thompson, RK Bhatia, RM Cavallo, RM Rich, RP Kraft, RP Kraft, RP Kraft, RP Kraft, RW Romani, S Bergh van den, S Bergh van den, S Cassisi, S Moehler, S Moehler, S Rubele, S Villanova, S Villanova, S Villanova, S-H Chun, S-I Han, SA Becker, SC Keller, SDM White, SE Mink de, SF Portegies Zwart, SG Ryan, SL Martell, SL Martell, SL Martell, SM Fall, SM Fall, SP Goodwin, SV Ramírez, SV Ramírez, SW Campbell, SW Campbell, T Bloecker, T Böker, T Böker, T Decressin, T Decressin, T Decressin, T Decressin, T Decressin, TC Beers, TD Kinman, V Belokurov, V Caloi, V Caloi, V Caloi, V Caloi, V D’Orazi, V D’Orazi, V D’Orazi, V D’Orazi, V D’Orazi, V Kravtsov, V Kravtsov, VV Smith, W Osborn, WE Harris, WE Harris, WE Harris, WR Brown, Y-W Lee, Y-W Lee, Y-W Lee, Z-X Shen, Z-X Shen, Ž Ivezić +359 morecore +1 more sourceModeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog [PDF]
Astrophysical Journal Supplement Series, 2019 We present a set of 148 independent N-body simulations of globular clusters (GCs) computed using the code CMC (Cluster Monte Carlo). At an age of ∼10–13 Gyr, the resulting models cover nearly the full range of cluster properties exhibited by the Milky ...K. Kremer, Claire S. Ye, N. Z. Rui, Newlin C. Weatherford, S. Chatterjee, G. Fragione, C. Rodriguez, M. Spera, F. Rasio +8 moresemanticscholar +1 more sourceStar-Forming Galaxies at z~2 and the Formation of the Metal-Rich
Globular Cluster Population
, 2010 We examine whether the super star-forming clumps (R~1-3 kpc; M~10^8-10^9.5
Msun) now known to be a key component of star-forming galaxies at z~2 could be
the formation sites of the locally observed old globular cluster population.Armandroff, Ashman, Barmby, Bournaud, Bournaud, Bridges, Brodie, Conroy, Cowie, Cresci, Côté, Côté, Daddi, De Angeli, de Grijs, Dekel, Elmegreen, Elmegreen, Elmegreen, Elmegreen, Elmegreen, Elmegreen, Elson, English, Erb, Erb, Escala, Fall, Forbes, Förster Schreiber, Förster Schreiber, Genel, Genzel, Genzel, Halliday, Harris, Huchra, Immeli, Jordán, Kristen L. Shapiro, Kuntschner, Mannucci, McLaughlin, McLaughlin, McLaughlin, Mendel, Minniti, Murray, Natascha M. Förster Schreiber, Noguchi, Peng, Peng, Peng, Pettini, Puzia, Quider, Reddy, Reinhard Genzel, Rhode, Rhode, Rudnick, Scannapieco, Schroder, Searle, Strader, Tacconi, Thomas, Trujillo, van den Bergh, Wilson, Zepf, Zinn +71 morecore +1 more sourceBlack holes: The next generation—repeated mergers in dense star clusters and their gravitational-wave properties [PDF]
Physical Review D, 2019 When two black holes merge in a dense star cluster, they form a new black hole with a well-defined mass and spin. If that "second-generation" black hole remains in the cluster, it will continue to participate in dynamical encounters, form binaries, and ...C. Rodriguez, M. Zevin, P. Amaro-Seoane, S. Chatterjee, K. Kremer, F. Rasio, Claire S. Ye +6 moresemanticscholar +1 more sourcer-process Abundance Patterns in the Globular Cluster M92
The Astrophysical Journal, 2023 Whereas light-element abundance variations are a hallmark of globular clusters, there is little evidence for variations in neutron-capture elements. A significant exception is M15, which shows a star-to-star dispersion in neutron-capture abundances of at Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev +2 moredoaj +1 more sourceJWST/NIRCam Probes Young Star Clusters in the Reionization Era Sunrise Arc
The Astrophysical Journal, 2023 Star cluster formation in the early universe and its contribution to reionization
remains largely unconstrained to date. Here we present JWST/NIRCam imaging of
the most highly magnified galaxy known at z ∼ 6,
the Sunrise arc.Eros Vanzella, Adélaïde Claeyssens, Brian Welch, Angela Adamo, Dan Coe, Jose M. Diego, Guillaume Mahler, Gourav Khullar, Vasily Kokorev, Masamune Oguri, Swara Ravindranath, Lukas J. Furtak, Tiger Yu-Yang Hsiao, Abdurro’uf, Nir Mandelker, Gabriel Brammer, Larry D. Bradley, Maruša Bradač, Christopher J. Conselice, Pratika Dayal, Mario Nonino, Felipe Andrade-Santos, Rogier A. Windhorst, Nor Pirzkal, Keren Sharon, S. E. de Mink, Seiji Fujimoto, Adi Zitrin, Jan J. Eldridge, Colin Norman +29 moredoaj +1 more source
