Zobrazeno 1 - 10
of 217
pro vyhledávání: '"D'Onghia, E."'
Autor:
Poggio, E., Khanna, S., Drimmel, R., Zari, E., D'Onghia, E., Lattanzi, M. G., Palicio, P. A., Recio-Blanco, A., Thulasidharan, L.
We analyse the three-dimensional structure and kinematics of two samples of young stars in the Galactic disc, containing respectively young giants ($\sim$16000 stars out to heliocentric distances of $\sim$7 kpc) and classical Cepheids ($\sim$3400 sta
Externí odkaz:
http://arxiv.org/abs/2407.18659
Autor:
Devereaux, T., Cassata, P., Ibar, E., Accard, C., Guillaume, C., Béthermin, M., Dessauges-Zavadsky, M., Faisst, A., Jones, G. C., Zanella, A., Bardelli, S., Boquien, M., D'Onghia, E., Giavalisco, M., Ginolfi, M., Gobat, R., Hayward, C. C., Koekemoer, A. M., Lemaux, B., Magdis, G., Mendez-Hernandez, H., Molina, J., Pozzi, F., Romano, M., Tasca, L., Vergani, D., Zamorani, G., Zucca, E.
Publikováno v:
A&A 686, A156 (2024)
Context: From redshift 6 to redshift $\approx$ 4 galaxies grow rapidly from low mass galaxies towards the more mature massive galaxies we see at the cosmic noon. Growth via gas accretion and mergers undoubtedly shape this evolution - however, there c
Externí odkaz:
http://arxiv.org/abs/2311.11493
Publikováno v:
A&A 631, A16 (2019)
We want to study how the velocity segregation and the radial profile of the velocity dispersion depend on the prominence of the brightest cluster galaxies (BCGs). We divide a sample of 102 clusters and groups of galaxies into four bins of magnitude g
Externí odkaz:
http://arxiv.org/abs/1907.09483
Akademický článek
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Autor:
Corsini, E. M., Morelli, L., Zarattini, S., Aguerri, J. A. L., Costantin, L., D'Onghia, E., Girardi, M., Kundert, A., Méndez-Abreu, J., Thomas, J.
Publikováno v:
A&A 618, A172 (2018)
Fossil groups (FGs) are galaxy aggregates with an extended and luminous X-ray halo, which are dominated by a very massive early-type galaxy and lack of L* objects. FGs are indeed characterized by a large magnitude gap between their central and surrou
Externí odkaz:
http://arxiv.org/abs/1809.01251
Autor:
Richter, P., Fox, A. J., Wakker, B. P., Howk, J. C., Lehner, N., Barger, K. A., D'Onghia, E., Lockman, F. J.
We present a new precision measurement of gas-phase abundances of S, O, N, Si, Fe, P, Al, Ca as well as molecular hydrogen (H_2) in the Leading Arm (region II, LAII) of the Magellanic Stream (MS) towards the Seyfert galaxy NGC 3783. The results are b
Externí odkaz:
http://arxiv.org/abs/1808.09455
Autor:
Shabani, F., Grebel, E. K., Pasquali, A., D'Onghia, E., Gallagher III, J. S., Adamo, A., Messa, M., Elmegreen, B. G., Dobbs, C., Gouliermis, D. A., Calzetti, D., Grasha, K., Elmegreen, D. M., Cignoni, M., Dale, D. A., Aloisi, A., Smith, L. J., Tosi, M., Thilker, D. A., Lee, J. C., Sabbi, E., Kim, H., Pellerin, A.
One of the main theories for explaining the formation of spiral arms in galaxies is the stationary density wave theory. This theory predicts the existence of an age gradient across the arms. We use the stellar cluster catalogues of the galaxies NGC 1
Externí odkaz:
http://arxiv.org/abs/1805.05643
Autor:
Aguerri, J. A. L., Longobardi, A., Zarattini, S., Kundert, A., D'Onghia, E., Dominguez-Palmero, L.
It is thought that fossil systems are relics of structure formation in the primitive Universe. They are galaxy aggregations that have assembled their mass at high redshift with few or no subsequent accretion. Observationally these systems are selecte
Externí odkaz:
http://arxiv.org/abs/1710.09229
Using the Illustris cosmological simulation, we investigate the origin of fossil groups in the $M_{200}=10^{13}-10^{13.5}M_{\odot}/h$ mass regime. We examine the formation of the two primary features of fossil groups: the large magnitude gap between
Externí odkaz:
http://arxiv.org/abs/1706.08542
Autor:
Zarattini, S., Girardi, M., Aguerri, J. A. L., Boschin, W., Barrena, R., del Burgo, C., Castro-Rodriguez, N., Corsini, E. M., D'Onghia, E., Kundert, A., Méndez-Abreu, J., Sánchez-Janssen, R.
Publikováno v:
A&A 586, A63 (2016)
Fossil groups are expected to be the final product of galaxy merging within galaxy groups. In simulations, they are predicted to assemble their mass at high redshift. This early formation allows for the innermost $M^\ast$ galaxies to merge into a mas
Externí odkaz:
http://arxiv.org/abs/1511.02854