Browsing by Author "D'Ago, Giuseppe"
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- ItemAstroinformatics-based search for globular clusters in the Fornax Deep Survey(2019) Angora, Giuseppe; Brescia, Massimo; Cavuoti, Stefano; Paolillo, M.; Longo, Giuseppe; Cantiello, M.; Capaccioli, M.; D'Abrusco, Raffaele; D'Ago, Giuseppe; Puzia, Thomas H.; Hilker, Michael; Iodice, Enrichetta; Mieske, Steffen; Napolitano, Nicola R.; Peletier, R.; Pota, Vincenzo; Riccio, Giuseppe; Spavone, Marilena
- ItemBuilding the Largest Spectroscopic Sample of Ultracompact Massive Galaxies with the Kilo Degree Survey(IOP PUBLISHING LTD, 2020) Scognamiglio, Diana; Tortora, Crescenzo; Spavone, Marilena; Spiniello, Chiara; Napolitano, Nicola R.; D'Ago, Giuseppe; La Barbera, Francesco; Getman, Fedor; Roy, Nivya; Raj, Maria Angela; Radovich, Mario; Brescia, Massimo; Cavuoti, Stefano; Koopmans, Leon V. E.; Kuijken, Koen H.; Longo, Giuseppe; Petrillo, Carlo EnricoUltracompact massive galaxies (UCMGs), i.e., galaxies with stellar masses M. > 8 ' 1010M. and effective radii Re < 1.5 kpc, are very rare systems, in particular at low and intermediate redshifts. Their origin as well as their number density across cosmic time are still under scrutiny, especially because of the paucity of spectroscopically confirmed samples. We have started a systematic census of UCMG candidates within the ESO Kilo Degree Survey, together with a large spectroscopic follow-up campaign to build the largest possible sample of confirmed UCMGs. This is the third paper of the series and the second based on the spectroscopic follow-up program. Here, we present photometrical and structural parameters of 33 new candidates at redshifts 0.15. z. 0.5 and confirm 19 of them as UCMGs, based on their nominal spectroscopically inferred M. and Re. This corresponds to a success rate of 58%, nicely consistent with our previous findings. The addition of these 19 newly confirmed objects allows us to fully assess the systematics on the system selection-and to finally reduce the number density uncertainties. Moreover, putting together the results from our current and past observational campaigns and some literature data, we build the largest sample of UCMGs ever collected, comprising 92 spectroscopically confirmed objects at 0.1. z. 0.5. This number raises to 116, allowing for a 3s tolerance on the M. and Re thresholds for the UCMG definition. For all these galaxies, we have estimated the velocity dispersion values at the effective radii, which have been used to derive a preliminary mass-velocity dispersion correlation.
- ItemIntrinsic Morphology of Ultra-diffuse Galaxies(IOP PUBLISHING LTD, 2020) Rong, Yu; Dong, Xiao Yu; Puzia, Thomas H.; Galaz, Gaspar; Sanchez Janssen, Ruben; Cao, Tianwen; van der Burg, Remco F. J.; Sifon, Cristobal; Pina, Pavel E. Mancera; Marcelo, Mora; D'Ago, Giuseppe; Zhang, Hong Xin; Johnston, Evelyn J.; Eigenthaler, PaulWith the published data of apparent axis ratios for 1109 ultra-diffuse galaxies (UDGs) located in 17 low-redshift (z similar to 0.020-0.063) galaxy clusters and 84 UDGs in two intermediate-redshift (z similar to 0.308-0.348) clusters, we take advantage of a Markov Chain Monte Carlo approach and assume a triaxial model to investigate the intrinsic morphologies of UDGs. In contrast to the conclusion of Burkert, i.e., the underlying shapes of UDGs are purely prolate (C = B < A), we find that the data favor the oblate-triaxial models (i.e., thick disks with C < B less than or similar to A) over the nearly prolate ones. We also find that the intrinsic morphologies of UDGs are related to their stellar masses/luminosities, environments, and redshifts. First, the more luminous UDGs have puffier morphologies compared with the less luminous counterparts; the UDG morphologic dependence on luminosity is distinct from that of the typical quiescent dwarf ellipticals (dEs) and dwarf spheroidals (dSphs); in this sense, UDGs may not be simply treated as an extension of the dE/dSph class with similar evolutionary histories; they may differ not only in size. Second, the UDGs with smaller clustercentric distances are more puffed up, compared with the counterparts with larger clustercentric distances; in combination with the UDG thickness dependence on luminosity, the puffier morphologies of UDGs with high luminosities or located in the denser environments are very likely to be attributed to tidal interactions with massive galaxies. Third, we find that the intermediate-redshift UDGs are more flattened, compared with the low-redshift counterparts, which plausibly suggests a "disky" origin for the high-redshift, newly born UDGs.
- ItemNature versus nurture : relic nature and environment of the most massive passive galaxies at z < 0.5(2020) Tortora, C.; Napolitano, N. R.; Radovich, M.; Spiniello, C.; Hunt, L.; Roy, N.; Moscardini, L.; Scognamiglio, D.; Spavone, M.; D'Ago, Giuseppe; Cavuoti, S.; Longo, G.; Bellagamba, F.; Maturi, M.; Roncarelli, M.
- ItemOGLE-2013-BLG-0911Lb : A Secondary on the Brown-dwarf Planet Boundary around an M Dwarf(2020) Miyazaki, S; Sumi, T; Bennett, DP; Udalski, A; Shvartzvald, Y; Street, R; Bozza, V; Yee, JC; Rabus, Markus; D'Ago, Giuseppe; Bond, IA; Rattenbury, N; Koshimoto, N; Suzuki, D; Fukui, A; Abe, F; Bhattacharya, A; Barry, R; Donachie, M; Fujii, H; Hirao, Y; Itow, Y; Kamei, Y; Kondo, I; Li, MCA; Ling, CH; Matsubara, Y; Matsuo, T; Muraki, Y; Nagakane, M; Ohnishi, K; Ranc, C; Saito, T; Sharan, A; Shibai, H; Suematsu, H; Sullivan, DJ; Tristram, PJ; Yamakawa, T; Yonehara, A; Skowron, J; Poleski, R; Mroz, P; Szymanski, MK; Soszynski, I; Pietrukowicz, Pawel; KozLowski, S; Ulaczyk, K; Wyrzykowski, L; Friedmann, M; Kaspi, S; Maoz, D; Albrow, M; Christie, G; DePoy, DL; Gal-Yam, A; Gould, A; Lee, CU; Manulis, I; McCormick, J; Natusch, T; Ngan, H; Pogge, RW; Porritt, I; Tsapras, Y; Bachelet, E; Hundertmark, MPG; Dominik, M; Bramich, DM; Cassan, A; Jaimes, RF; Horne, K; Schmidt, R; Snodgrass, C; Wambsganss, J; Steele, IA; Menzies, J; Mao, S; Jorgensen, UG; Burgdorf, MJ; Ciceri, S; Novati, SC; Evans, DF; Hinse, TC; Kains, N; Kerins, E; Korhonen, H; Mancini, L; Popovas, A; Rahvar, S; Scarpetta, G; Skottfelt, J; Southworth, J; Peixinho, N; Verma, P
- ItemThe Next Generation Fornax Survey (NGFS): VII. A MUSE view of the nuclear star clusters in Fornax dwarf galaxies(OUP, 2020) Johnston, E. J.; Puzia, Thomas H.; D'Ago, Giuseppe; Eigenthaler, Paul; Galaz, Gaspar; Häußler, B.; Mora Genskowsky, Marcelo Daniel; Órdenes Briceño, Yasna; Rong, Y.; Spengler, C.; Vogt, F.; Côté, P.; Grebel, E. K.; Hilker, M.; Mieske, S.; Miller, B.; Sánchez-Janssen, R.; Taylor, M. A.; Zhan, Hong-XinClues to the formation and evolution of nuclear star clusters (NSCs) lie in their stellar populations. However, these structures are often very faint compared to their host galaxy, and spectroscopic analysis of NSCs is hampered by contamination of light from the rest of the system. With the introduction of wide-field integral field unit (IFU) spectrographs, new techniques have been developed to model the light from different components within galaxies, making it possible to cleanly extract the spectra of the NSCs and study their properties with minimal contamination from the light of the rest of the galaxy. This work presents the analysis of the NSCs in a sample of 12 dwarf galaxies in the Fornax Cluster observed with the Multi-Unit Spectroscopic Explorer (MUSE). Analysis of the stellar populations and star formation histories reveal that all the NSCs show evidence of multiple episodes of star formation, indicating that they have built up their mass further since their initial formation. The NSCs were found to have systematically lower metallicities than their host galaxies, which is consistent with a scenario for mass assembly through mergers with infalling globular clusters, whilst the presence of younger stellar populations and gas emission in the core of two galaxies is indicative of in-situ star formation. We conclude that the NSCs in these dwarf galaxies likely originated as globular clusters that migrated to the core of the galaxy that have built up their mass mainly through mergers with other infalling clusters, with gas-inflow leading to in-situ star formation playing a secondary role.
- ItemTransit timing variations in the WASP-4 planetary system(2019) Southworth, J.; Dominik, M.; Jorgensen, U. G.; Andersen, M. I.; Bozza, V.; Burgdorf, M. J.; D'Ago, Giuseppe; Dib, S.; Jaimes, R. F.; Fujii, Y. I.; Gill, S.; Haikala, L. K.; Hinse, T. C.; Hundertmark, M.; Khalouei, E.; Korhonen, H.; Longa Pena, P.; Mancini, L.; Peixinho, N.; Rabus, Markus; Rahvar, S.; Sajadian, S.; Skottfelt, J.; Snodgrass, C.; Spyratos, P.; Tregloan Reed, J.; Unda Sanzana, E.; Von Essen, C.