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112 results on '"ARNABOLDI M."'

2. The VISTA Variables in the Vía Láctea eXtended (VVVX) ESO public survey: Completion of the observations and legacy

Author

Saito, R. K., Hempel, M., Alonso-García, J., Lucas, P. W., Minniti, D., Alonso, S., Baravalle, L., Borissova, J., Caceres, C., Chené, A. N., Cross, N. J. G., Duplancic, F., Garro, E. R., Gómez, M., Ivanov, V. D., Kurtev, R., Luna, A., Majaess, D., Navarro, M. G., Pullen, J. B., Rejkuba, M., Sanders, J. L., Smith, L. C., Albino, P. H. C., Alonso, M. V., Amôres, E. B., Angeloni, R., Arias, J. I., Arnaboldi, M., Barbuy, B., Bayo, A., Beamin, J. C., Bedin, L. R., Bellini, A., Benjamin, R. A., Bica, E., Bonatto, C. J., Botan, E., Braga, V. F., Brown, D. A., Cabral, J. B., Camargo, D., Caratti o Garatti, A., Carballo-Bello, J. A., Catelan, M., Chavero, C., Chijani, M. A., Clariá, J. J., Coldwell, G. V., Contreras Peña, C., Contreras Ramos, R., Corral-Santana, J. M., Cortés, C. C., Cortés-Contreras, M., Cruz, P., Daza-Perilla, I. V., Debattista, Victor P, Dias, B., Donoso, L., D'Souza, R., Emerson, J. P., Federle, S., Fermiano, V., Fernandez, J., Fernández-Trincado, J. G., Ferreira, T., Ferreira Lopes, C. E., Firpo, V., Flores-Quintana, C., Fraga, L., Froebrich, D., Galdeano, D., Gavignaud, I., Geisler, D., Gerhard, O. E., Gieren, W., Gonzalez, O. A., Gramajo, L. V., Gran, F., Granitto, P. M., Griggio, M., Guo, Z., Gurovich, S., Hilker, M., Jones, H., Kammers, R., Kuhn, M. A., Kumar, M. S .N., Kundu, R., Lares, M., Libralato, M., Lima, E., Maccarone, T. J., Marchant Cortés, P., Martin, E. L., Masetti, N., Matsunaga, N., Mauro, F., McDonald, I., Mejías, A., Mesa, V., Milla-Castro, F. P., Minniti, J. H., Moni Bidin, C., Montenegro, K., Morris, C., Motta, V., Navarete, F., Navarro Molina, C., Nikzat, F., Nilo Castellón, J. L., Obasi, C., Ortigoza-Urdaneta, M., Palma, T., Parisi, C., Pena Ramírez, K., Pereyra, L., Perez, N., Petralia, I., Pichel, A., Pignata, G., Ramírez Alegría, S., Rojas, A. F., Rojas, D., Roman-Lopes, A., Rovero, A. C., Saroon, S., Schmidt, E. O., Schröder, A. C., Schultheis, M., Sgró, M. A., Solano, E., Soto, M., Stecklum, B., Steeghs, D., Tamura, M., Tissera, P., Valcarce, A. A. R., Valotto, C. A., Vasquez, S., Villalon, C., Villanova, S., Vivanco Cádiz, F., Zelada Bacigalupo, R., Zijlstra, A., Zoccali, M., Saito, R. K., Hempel, M., Alonso-García, J., Lucas, P. W., Minniti, D., Alonso, S., Baravalle, L., Borissova, J., Caceres, C., Chené, A. N., Cross, N. J. G., Duplancic, F., Garro, E. R., Gómez, M., Ivanov, V. D., Kurtev, R., Luna, A., Majaess, D., Navarro, M. G., Pullen, J. B., Rejkuba, M., Sanders, J. L., Smith, L. C., Albino, P. H. C., Alonso, M. V., Amôres, E. B., Angeloni, R., Arias, J. I., Arnaboldi, M., Barbuy, B., Bayo, A., Beamin, J. C., Bedin, L. R., Bellini, A., Benjamin, R. A., Bica, E., Bonatto, C. J., Botan, E., Braga, V. F., Brown, D. A., Cabral, J. B., Camargo, D., Caratti o Garatti, A., Carballo-Bello, J. A., Catelan, M., Chavero, C., Chijani, M. A., Clariá, J. J., Coldwell, G. V., Contreras Peña, C., Contreras Ramos, R., Corral-Santana, J. M., Cortés, C. C., Cortés-Contreras, M., Cruz, P., Daza-Perilla, I. V., Debattista, Victor P, Dias, B., Donoso, L., D'Souza, R., Emerson, J. P., Federle, S., Fermiano, V., Fernandez, J., Fernández-Trincado, J. G., Ferreira, T., Ferreira Lopes, C. E., Firpo, V., Flores-Quintana, C., Fraga, L., Froebrich, D., Galdeano, D., Gavignaud, I., Geisler, D., Gerhard, O. E., Gieren, W., Gonzalez, O. A., Gramajo, L. V., Gran, F., Granitto, P. M., Griggio, M., Guo, Z., Gurovich, S., Hilker, M., Jones, H., Kammers, R., Kuhn, M. A., Kumar, M. S .N., Kundu, R., Lares, M., Libralato, M., Lima, E., Maccarone, T. J., Marchant Cortés, P., Martin, E. L., Masetti, N., Matsunaga, N., Mauro, F., McDonald, I., Mejías, A., Mesa, V., Milla-Castro, F. P., Minniti, J. H., Moni Bidin, C., Montenegro, K., Morris, C., Motta, V., Navarete, F., Navarro Molina, C., Nikzat, F., Nilo Castellón, J. L., Obasi, C., Ortigoza-Urdaneta, M., Palma, T., Parisi, C., Pena Ramírez, K., Pereyra, L., Perez, N., Petralia, I., Pichel, A., Pignata, G., Ramírez Alegría, S., Rojas, A. F., Rojas, D., Roman-Lopes, A., Rovero, A. C., Saroon, S., Schmidt, E. O., Schröder, A. C., Schultheis, M., Sgró, M. A., Solano, E., Soto, M., Stecklum, B., Steeghs, D., Tamura, M., Tissera, P., Valcarce, A. A. R., Valotto, C. A., Vasquez, S., Villalon, C., Villanova, S., Vivanco Cádiz, F., Zelada Bacigalupo, R., Zijlstra, A., and Zoccali, M.

Abstract

Context. The ESO public survey VISTA Variables in the Vía Láctea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from 2009−2015. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from 562 to 1700 sq. deg., as well as providing additional epochs in JHKs filters from 2016−2023. Aims. With the completion of VVVX observations during the first semester of 2023, we present here the observing strategy, a description of data quality and access, and the legacy of VVVX. Methods. VVVX took ∼ 2000 hours, covering about 4% of the sky in the bulge and southern disk. VVVX covered most of the gaps left between the VVV and the VISTA Hemisphere Survey (VHS) areas and extended the VVV time baseline in the obscured regions affected by high extinction and hence hidden from optical observations. Results. VVVX provides a deep JHKs catalogue of & 1.5 × 109 point sources, as well as a Ks band catalogue of ∼ 107 variable sources. Within the existing VVV area, we produced a 5D map of the surveyed region by combining positions, distances, and proper motions of well-understood distance indicators such as red clump stars, RR Lyrae, and Cepheid variables. Conclusions. In March 2023 we successfully finished the VVVX survey observations that started in 2016, an accomplishment for ESO Paranal Observatory upon 4200 hours of observations for VVV+VVVX. The VVV+VVVX catalogues complement those from the Gaia mission at low Galactic latitudes and provide spectroscopic targets for the forthcoming ESO high-multiplex spectrographs MOONS and 4MOST.

Published
2024
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4. INSPIRE: INvestigating Stellar Population In RElics

Author

D’Ago, G., primary, Spiniello, C., additional, Coccato, L., additional, Tortora, C., additional, La Barbera, F., additional, Arnaboldi, M., additional, Bevacqua, D., additional, Ferré-Mateu, A., additional, Gallazzi, A., additional, Hartke, J., additional, Hunt, L. K., additional, Martín-Navarro, I., additional, Napolitano, N. R., additional, Pulsoni, C., additional, Radovich, M., additional, Saracco, P., additional, Scognamiglio, D., additional, and Zibetti, S., additional

Published
2023
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5. The Fornax Cluster VLT Spectroscopic Survey:IV. cold kinematical substructures in the Fornax core from COSTA

Author

Napolitano, N. R., Gatto, M., Spiniello, C., Cantiello, M., Hilker, M., Arnaboldi, M., Tortora, C., Chaturvedi, A., D'Abrusco, R., Li, R., Paolillo, M., Peletier, R., Saifollahi, T., Spavone, M., Venhola, A., Pota, V., Capaccioli, M., Longo, G., Napolitano, N. R., Gatto, M., Spiniello, C., Cantiello, M., Hilker, M., Arnaboldi, M., Tortora, C., Chaturvedi, A., D'Abrusco, R., Li, R., Paolillo, M., Peletier, R., Saifollahi, T., Spavone, M., Venhola, A., Capaccioli, M., Longo, G., and Astronomy

Subjects
Physics, formation [galaxies], interactions [galaxies], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Core (optical fiber), intergalactic medium, galaxies: interactions, galaxies: formation, galaxies: kinematics and dynamics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), kinematics and dynamics [galaxies], galaxies: interactions, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, intergalactic medium, Fornax Cluster, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics
Abstract

The COld STream finder Algorithm (COSTA) is a novel algorithm to find streams in the phase space of planetary nebulae (PNe) and globular cluster (GCs) populations. COSTA isolates groups of particles with small velocity dispersion, using an iterative sigma-clipping over a defined number of neighbor particles. We have applied COSTA to a catalog of about 2000 PNe and GCs from the Fornax Cluster VLT Spectroscopic Survey (FVSS), within 200 kpc from the cluster core, to detect cold substructures and characterize their kinematics. We have found 13 cold substructures, with velocity dispersion ranging from 20 to 100 kms^{-1}, which are likely associated either to large galaxies or to ultra-compact dwarf (UCD) galaxies in the Fornax core. These streams show a clear correlation of their luminosity with the internal velocity dispersion, and their surface brightness with size and distance from the cluster center that are compatible with dissipative processes producing them. However, we cannot exclude that some of these substructures have formed by violent relaxation of massive satellites finally merged into the central galaxy. Among these substructures we have: a stream connecting NGC1387 to the central galaxy, NGC1399, previously reported in literature; a new giant stream produced by the interaction of NGC1382 with NGC1380 and possibly NGC1381; a series of streams kinematically connected to nearby ultra compact dwarf galaxies; clumps of tracers with no clear kinematical association to close cluster members. We show evidence for a variety of cold substructure predicted in simulations. Most of the streams are kinematically connected to UCDs, supporting the scenario that they can be remnants of disrupted dwarf systems. [abridged], 27 Pages, 15 Figures. Accepted for publication in Astronomy and Astrophysics

Published
2022

6. The halo of M 105 and its group environment as traced by planetary nebula populations

Author

Hartke, J., primary, Arnaboldi, M., additional, Gerhard, O., additional, Coccato, L., additional, Merrifield, M., additional, Kuijken, K., additional, Pulsoni, C., additional, Agnello, A., additional, Bhattacharya, S., additional, Spiniello, C., additional, Cortesi, A., additional, Freeman, K. C., additional, Napolitano, N. R., additional, and Romanowsky, A. J., additional

Published
2022
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7. Galaxy populations in the Hydra I cluster from the VEGAS survey:I. optical properties of a large sample of dwarf galaxies

Author

La Marca, A. (Antonio), Peletier, R. (Reynier), Iodice, E. (Enrichetta), Paolillo, M. (Maurizio), Choque Challapa, N. (Nelvy), Venhola, A. (Aku), Forbes, D. A. (Duncan A.), Cantiello, M. (Michele), Hilker, M. (Michael), Rejkuba, M. (Marina), Arnaboldi, M. (Magda), Spavone, M. (Marilena), D’Ago, G. (Giuseppe), Raj, M. A. (Maria Angela), Ragusa, R. (Rossella), Mirabile, M. (Marco), Rampazzo, R. (Roberto), Spiniello, C. (Chiara), Mieske, S. (Steffen), Schipani, P. (Pietro), La Marca, A. (Antonio), Peletier, R. (Reynier), Iodice, E. (Enrichetta), Paolillo, M. (Maurizio), Choque Challapa, N. (Nelvy), Venhola, A. (Aku), Forbes, D. A. (Duncan A.), Cantiello, M. (Michele), Hilker, M. (Michael), Rejkuba, M. (Marina), Arnaboldi, M. (Magda), Spavone, M. (Marilena), D’Ago, G. (Giuseppe), Raj, M. A. (Maria Angela), Ragusa, R. (Rossella), Mirabile, M. (Marco), Rampazzo, R. (Roberto), Spiniello, C. (Chiara), Mieske, S. (Steffen), and Schipani, P. (Pietro)

Abstract

Context: Due to their relatively low stellar mass content and diffuse nature, the evolution of dwarf galaxies can be strongly affected by their environment. Analyzing the properties of the dwarf galaxies over a wide range of luminosities, sizes, morphological types, and environments, we can obtain insights about their evolution. At ∼50 Mpc, the Hydra I cluster of galaxies is among the closest cluster in the z ≃ 0 Universe, and an ideal environment to study dwarf galaxy properties in a cluster environment. Aims: We exploit deep imaging data of the Hydra I cluster to construct a new photometric catalog of dwarf galaxies in the cluster core, which is then used to derive properties of the Hydra I cluster dwarf galaxy population as well as to compare it with other clusters. Moreover, we investigate the dependency of dwarf galaxy properties on their surrounding environment. Methods: The new wide-field g- and r-band images of the Hydra I cluster obtained with the OmegaCAM camera on the VLT Survey Telescope (VST) in the context of the VST Early-type GAlaxy Survey (VEGAS) were used to study the dwarf galaxy population in the Hydra I cluster core down to r-band magnitude Mr = −11.5 mag. We used an automatic detection tool to identify dwarf galaxies from a ∼1 deg² field centered on the Hydra I core, covering almost half of the cluster virial radius. The photometric pipeline was used to estimate the principal photometric parameters for all targets. Scaling relations and visual inspection were used to assess the cluster membership and construct a new dwarf galaxy catalog. Finally, based on the new catalog, we studied the structural (Sérsic index n, effective radius Re, and axis ratio) and photometric (colors and surface brightness) properties of the dwarf galaxies, also investigating how they vary as a function of clustercentric distance. Results: The new Hydra I dwarf catalog contains 317 galaxies with a luminosity between −18.5 < Mr < −11.5 mag, a semi-major axi

Published
2022

8. Galaxy populations in the Hydra I cluster from the VEGAS survey

Author

La Marca, A. (Antonio), Iodice, E. (Enrichetta), Cantiello, M. (Michele), Forbes, D. A. (Duncan A.), Rejkuba, M. (Marina), Hilker, M. (Michael), Arnaboldi, M. (Magda), Greggio, L. (Laura), Spiniello, C. (Chiara), Mieske, S. (Steffen), Venhola, A. (Aku), Spavone, M. (Marilena), D’Ago, G. (Giuseppe), Raj, M. A. (Maria Angela), Ragusa, R. (Rossella), Mirabile, M. (Marco), Rampazzo, R. (Roberto), Peletier, R. (Reynier), Paolillo, M. (Maurizio), Challapa, N. C. (Nelvy Choque), and Schipani, P. (Pietro)

Subjects
dwarf [galaxies], formation [galaxies], photometry [galaxies], clusters: individual: Hydra I [galaxies], evolution [galaxies]
Abstract

In this work, we extend the catalog of low-surface brightness (LSB) galaxies, including ultra-diffuse galaxy (UDG) candidates, within ≈0.4Rvir of the Hydra I cluster of galaxies based on deep images from the VST Early-type GAlaxy Survey (VEGAS). The new galaxies were found by applying an automatic detection tool and carrying out additional visual inspections of g and r band images. This led to the detection of 11 UDGs and 8 more LSB galaxies. For all of them, we assessed the cluster membership using the color–magnitude relation derived for early-type giant and dwarf galaxies in Hydra I. The UDGs and new LSB galaxies found in Hydra I span a wide range of central surface brightness (22.7 ≲ μ0, g ≲ 26.5 mag arcsec⁻²), effective radius (0.6 ≲ Re ≲ 4.0 kpc), and color (0.4 ≤ g − r ≤ 0.9 mag), and have stellar masses in the range ∼5 × 10⁶ − 2 × 10⁸ M⊙. The 2D projected distribution of both galaxy types is similar to the spatial distribution of dwarf galaxies, with over-densities in the cluster core and north of the cluster center. They have similar color distribution and comparable stellar masses to the red dwarf galaxies. Based on photometric selection, we identify a total of nine globular cluster (GC) candidates associated to the UDGs and four to the LSB galaxies, with the highest number of candidates in an individual UDG being three. We find that there are no relevant differences between dwarfs, LSB galaxies, and UDGs: the structural parameters (i.e., surface brightness, size, color, and n-index) and GC content of the three classes have similar properties and trends. This finding is consistent with UDGs being the extreme LSB tail of the size–luminosity distribution of dwarfs in this environment.

Published
2022

9. INSPIRE: INvestigating Stellar Population In RElics

Author

Spiniello, C., primary, Tortora, C., additional, D’Ago, G., additional, Coccato, L., additional, La Barbera, F., additional, Ferré-Mateu, A., additional, Pulsoni, C., additional, Arnaboldi, M., additional, Gallazzi, A., additional, Hunt, L., additional, Napolitano, N. R., additional, Radovich, M., additional, Scognamiglio, D., additional, Spavone, M., additional, and Zibetti, S., additional

Published
2021
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10. INSPIRE: INvestigating Stellar Population in RElics: I. Survey presentation and pilot study

Author

Oxford Hintze Centre for Astrophysical Surveys (UK), La Caixa, Bonn-Cologne Graduate School of Physics and Astronomy, Sun Yat-sen University, International Max Planck Research Schools, Spiniello, C., Tortora, C., D'Ago, G., Coccato, Lodovico, Barbera, F. la, Ferré-Mateu, Anna, Napolitano, N. R., Spavone, M., Scognamiglio, D., Arnaboldi, M., Gallazzi, A., Hunt, L., Moehler, S., Radovich, Milan, Zibetti, Stefano, Oxford Hintze Centre for Astrophysical Surveys (UK), La Caixa, Bonn-Cologne Graduate School of Physics and Astronomy, Sun Yat-sen University, International Max Planck Research Schools, Spiniello, C., Tortora, C., D'Ago, G., Coccato, Lodovico, Barbera, F. la, Ferré-Mateu, Anna, Napolitano, N. R., Spavone, M., Scognamiglio, D., Arnaboldi, M., Gallazzi, A., Hunt, L., Moehler, S., Radovich, Milan, and Zibetti, Stefano

Abstract

[Context] Massive elliptical galaxies are thought to form through a two-phase process. At early times (z > 2), an intense and fast starburst forms blue and disk-dominated galaxies. After quenching, the remaining structures become red, compact, and massive (i.e. red nuggets). Then, a time-extended second phase, which is dominated by mergers, causes structural evolution and size growth. Given the stochastic nature of mergers, a small fraction of red nuggets survive, without any interaction, massive and compact until today: these are relic galaxies. Since this fraction depends on the processes dominating the size growth, counting relics at low-z is a valuable way of disentangling between different galaxy evolution models. [Aims] In this paper, we introduce the INvestigating Stellar Population In RElics (INSPIRE) Project, which aims to spectroscopically confirm and fully characterise a large number of relics at 0:1z0:5. We focus here on the first results based on a pilot study targeting three systems, representative of the whole sample. [Methods] For these three candidates, we extracted 1D optical spectra over an aperture of r = 0:4000, which comprises 30% of the galaxies’ light, and we obtained the line-of-sight integrated stellar velocity and velocity dispersion. We also inferred the stellar [/Fe] abundance from line-index measurements and mass-weighted age and metallicity from full-spectral fitting with single stellar population models. [Results] Two galaxies have large integrated stellar velocity dispersion values (250 km s), confirming their massive nature. They are populated by stars with super-solar metallicity and [/Fe]. Both objects have formed 80% of their stellar mass within a short (0:5:0 Gyr) initial star formation episode occurred only 1 Gyr after the Big Bang. The third galaxy has a more extendedstar formation history and a lower velocity dispersion. Thus we confirm two out of three candidates as relics. [Conclusions] This paper is the first step towards

Published
2021

11. INSPIRE: INvestigating stellar population in RElics: II. First data release (DR1)

Author

Oxford Hintze Centre for Astrophysical Surveys (UK), International Max Planck Research Schools, Bonn-Cologne Graduate School of Physics and Astronomy, Spiniello, C., Tortora, C., D'Ago, G., Coccato, Lodovico, Barbera, F. la, Ferré-Mateu, Anna, Arnaboldi, M., Gallazzi, A., Hunt, L., Napolitano, N. R., Radovich, Milan, Scognamiglio, D., Spavone, M., Zibetti, Stefano, Oxford Hintze Centre for Astrophysical Surveys (UK), International Max Planck Research Schools, Bonn-Cologne Graduate School of Physics and Astronomy, Spiniello, C., Tortora, C., D'Ago, G., Coccato, Lodovico, Barbera, F. la, Ferré-Mateu, Anna, Arnaboldi, M., Gallazzi, A., Hunt, L., Napolitano, N. R., Radovich, Milan, Scognamiglio, D., Spavone, M., and Zibetti, Stefano

Abstract

[Context] The INvestigating Stellar Population In RElics (INSPIRE) is an ongoing project targeting 52 ultra-compact massive galaxies at 0.1 < z < 0.5 with the X-shooter at VLT spectrograph (XSH). These objects are the ideal candidates to be 'relics', massive red nuggets that have formed at high redshift (z > 2) through a short and intense star formation burst, and then have evolved passively and undisturbed until the present day. Relics provide a unique opportunity to study the mechanisms of star formation at high-z. [Aims] INSPIRE is designed to spectroscopically confirm and fully characterise a large sample of relics, computing their number density in the redshift window 0.1 < z < 0.5 for the first time, thus providing a benchmark for cosmological galaxy formation simulations. In this paper, we present the INSPIRE Data Release (DR1), comprising 19 systems with observations completed in 2020. [Methods] We use the methods already presented in the INSPIRE Pilot, but revisiting the 1D spectral extraction. For the 19 systems studied here, we obtain an estimate of the stellar velocity dispersion, fitting the two XSH arms (UVB and VIS) separately at their original spectral resolution to two spectra extracted in different ways. We estimate [Mg/Fe] abundances via line-index strength and mass-weighted integrated stellar ages and metallicities with full spectral fitting on the combined (UVB+VIS) spectrum. [Results] For each system, different estimates of the velocity dispersion always agree within the errors. Spectroscopic ages are very old for 13/19 galaxies, in agreement with the photometric ones, and metallicities are almost always (18/19) super-solar, confirming the mass-metallicity relation. The [Mg/Fe] ratio is also larger than solar for the great majority of the galaxies, as expected. We find that ten objects formed more than 75% of their stellar mass (M∗) within 3 Gyr from the big bang and classify them as relics. Among these, we identify four galaxies that had alrea

Published
2021

16. The first detection of ultra-diffuse galaxies in the Hydra I cluster from the VEGAS survey

Author

Iodice, E., primary, Cantiello, M., additional, Hilker, M., additional, Rejkuba, M., additional, Arnaboldi, M., additional, Spavone, M., additional, Greggio, L., additional, Forbes, D. A., additional, D’Ago, G., additional, Mieske, S., additional, Spiniello, C., additional, La Marca, A., additional, Rampazzo, R., additional, Paolillo, M., additional, Capaccioli, M., additional, and Schipani, P., additional

Published
2020
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21. The Hydra I cluster core

Author

Hilker, M., primary, Richtler, T., additional, Barbosa, C. E., additional, Arnaboldi, M., additional, Coccato, L., additional, and Mendes de Oliveira, C., additional

Published
2018
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22. The extended Planetary Nebula Spectrograph (ePN.S) early-type galaxy survey: The kinematic diversity of stellar halos and the relation between halo transition scale and stellar mass

Author

Pulsoni, C., primary, Gerhard, O., additional, Arnaboldi, M., additional, Coccato, L., additional, Longobardi, A., additional, Napolitano, N. R., additional, Moylan, E., additional, Narayan, C., additional, Gupta, V., additional, Burkert, A., additional, Capaccioli, M., additional, Chies-Santos, A. L., additional, Cortesi, A., additional, Freeman, K. C., additional, Kuijken, K., additional, Merrifield, M. R., additional, Romanowsky, A. J., additional, and Tortora, C., additional

Published
2018
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27. The Hydra I cluster core

Author

Barbosa, C. E., primary, Arnaboldi, M., additional, Coccato, L., additional, Hilker, M., additional, Mendes de Oliveira, C., additional, and Richtler, T., additional

Published
2016
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35. The Planetary Nebula Spectrograph survey of S0 galaxy kinematics

Author

Cortesi, A., primary, Arnaboldi, M., additional, Coccato, L., additional, Merrifield, M. R., additional, Gerhard, O., additional, Bamford, S., additional, Romanowsky, A. J., additional, Napolitano, N. R., additional, Douglas, N. G., additional, Kuijken, K., additional, Capaccioli, M., additional, Freeman, K. C., additional, Chies-Santos, A. L., additional, and Pota, V., additional

Published
2013
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46. Eddington ratios of faint AGN at intermediate redshift: evidence for a population of half-starved black holes

Author

Gavignaud, I., primary, Wisotzki, L., additional, Bongiorno, A., additional, Paltani, S., additional, Zamorani, G., additional, Møller, P., additional, Le Brun, V., additional, Husemann, B., additional, Lamareille, F., additional, Schramm, M., additional, Le Fèvre, O., additional, Bottini, D., additional, Garilli, B., additional, Maccagni, D., additional, Scaramella, R., additional, Scodeggio, M., additional, Tresse, L., additional, Vettolani, G., additional, Zanichelli, A., additional, Adami, C., additional, Arnaboldi, M., additional, Arnouts, S., additional, Bardelli, S., additional, Bolzonella, M., additional, Cappi, A., additional, Charlot, S., additional, Ciliegi, P., additional, Contini, T., additional, Foucaud, S., additional, Franzetti, P., additional, Guzzo, L., additional, Ilbert, O., additional, Iovino, A., additional, McCracken, H. J., additional, Marano, B., additional, Marinoni, C., additional, Mazure, A., additional, Meneux, B., additional, Merighi, R., additional, Pellò, R., additional, Pollo, A., additional, Pozzetti, L., additional, Radovich, M., additional, Zucca, E., additional, Bondi, M., additional, Busarello, G., additional, Cucciati, O., additional, de la Torre, S., additional, Gregorini, L., additional, Mellier, Y., additional, Merluzzi, P., additional, Ripepi, V., additional, Rizzo, D., additional, and Vergani, D., additional

Published
2008
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47. The cosmic star formation rate evolution fromz = 5 toz = 0 from the VIMOS VLT deep survey

Author

Tresse, L., primary, Ilbert, O., additional, Zucca, E., additional, Zamorani, G., additional, Bardelli, S., additional, Arnouts, S., additional, Paltani, S., additional, Pozzetti, L., additional, Bottini, D., additional, Garilli, B., additional, Le Brun, V., additional, Le Fèvre, O., additional, Maccagni, D., additional, Picat, J.-P., additional, Scaramella, R., additional, Scodeggio, M., additional, Vettolani, G., additional, Zanichelli, A., additional, Adami, C., additional, Arnaboldi, M., additional, Bolzonella, M., additional, Cappi, A., additional, Charlot, S., additional, Ciliegi, P., additional, Contini, T., additional, Foucaud, S., additional, Franzetti, P., additional, Gavignaud, I., additional, Guzzo, L., additional, Iovino, A., additional, McCracken, H. J., additional, Marano, B., additional, Marinoni, C., additional, Mazure, A., additional, Meneux, B., additional, Merighi, R., additional, Pellò, R., additional, Pollo, A., additional, Radovich, M., additional, Bondi, M., additional, Bongiorno, A., additional, Busarello, G., additional, Cucciati, O., additional, Lamareille, F., additional, Mathez, G., additional, Mellier, Y., additional, Merluzzi, P., additional, and Ripepi, V., additional

Published
2007
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50. The VIMOS VLT Deep Survey: the build-up of the colour–density relation

Author

Cucciati, O., primary, Iovino, A., additional, Marinoni, C., additional, Ilbert, O., additional, Bardelli, S., additional, Franzetti, P., additional, Le Fèvre, O., additional, Pollo, A., additional, Zamorani, G., additional, Cappi, A., additional, Guzzo, L., additional, McCracken, H. J., additional, Meneux, B., additional, Scaramella, R., additional, Scodeggio, M., additional, Tresse, L., additional, Zucca, E., additional, Bottini, D., additional, Garilli, B., additional, Le Brun, V., additional, Maccagni, D., additional, Picat, J. P., additional, Vettolani, G., additional, Zanichelli, A., additional, Adami, C., additional, Arnaboldi, M., additional, Arnouts, S., additional, Bolzonella, M., additional, Charlot, S., additional, Ciliegi, P., additional, Contini, T., additional, Foucaud, S., additional, Gavignaud, I., additional, Marano, B., additional, Mazure, A., additional, Merighi, R., additional, Paltani, S., additional, Pellò, R., additional, Pozzetti, L., additional, Radovich, M., additional, Bondi, M., additional, Bongiorno, A., additional, Busarello, G., additional, de la Torre, S., additional, Gregorini, L., additional, Lamareille, F., additional, Mathez, G., additional, Mellier, Y., additional, Merluzzi, P., additional, Ripepi, V., additional, Rizzo, D., additional, Temporin, S., additional, and Vergani, D., additional

Published
2006
Full Text
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