Institution
Roma Tre University
Education•Rome, Lazio, Italy•
About: Roma Tre University is a education organization based out in Rome, Lazio, Italy. It is known for research contribution in the topics: Large Hadron Collider & Galaxy. The organization has 4434 authors who have published 15352 publications receiving 374888 citations. The organization is also known as: Universita degli Studi Roma Tre & RomaTre.
Papers published on a yearly basis
Papers
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TL;DR: In this article, the population of 47 compact binary mergers detected with a false-alarm rate of 0.614 were dynamically assembled, and the authors found that the BBH rate likely increases with redshift, but not faster than the star formation rate.
Abstract: We report on the population of 47 compact binary mergers detected with a false-alarm rate of 0.01 are dynamically assembled. Third, we estimate merger rates, finding RBBH = 23.9-+8.614.3 Gpc-3 yr-1 for BBHs and RBNS = 320-+240490 Gpc-3 yr-1 for binary neutron stars. We find that the BBH rate likely increases with redshift (85% credibility) but not faster than the star formation rate (86% credibility). Additionally, we examine recent exceptional events in the context of our population models, finding that the asymmetric masses of GW190412 and the high component masses of GW190521 are consistent with our models, but the low secondary mass of GW190814 makes it an outlier.
468 citations
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TL;DR: In this paper, the mass, spin, and redshift distributions of binary black hole (BBH) mergers with LIGO and Advanced Virgo observations were analyzed using phenomenological population models.
Abstract: We present results on the mass, spin, and redshift distributions with phenomenological population models using the 10 binary black hole (BBH) mergers detected in the first and second observing runs completed by Advanced LIGO and Advanced Virgo. We constrain properties of the BBH mass spectrum using models with a range of parameterizations of the BBH mass and spin distributions. We find that the mass distribution of the more massive BH in such binaries is well approximated by models with no more than 1% of BHs more massive than 45 M and a power-law index of (90% credibility). We also show that BBHs are unlikely to be composed of BHs with large spins aligned to the orbital angular momentum. Modeling the evolution of the BBH merger rate with redshift, we show that it is flat or increasing with redshift with 93% probability. Marginalizing over uncertainties in the BBH population, we find robust estimates of the BBH merger rate density of R= (90% credibility). As the BBH catalog grows in future observing runs, we expect that uncertainties in the population model parameters will shrink, potentially providing insights into the formation of BHs via supernovae, binary interactions of massive stars, stellar cluster dynamics, and the formation history of BHs across cosmic time.
464 citations
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TL;DR: In this paper, the cosmological evolution of the density of active galactic nuclei (AGNs) and their NH distribution as a function of the unabsorbed 2-10 keV luminosity up to redshift 4 was determined.
Abstract: We have determined the cosmological evolution of the density of active galactic nuclei (AGNs) and of their NH distribution as a function of the unabsorbed 2–10 keV luminosity up to redshift 4. We used the HELLAS2XMM sample combined with other published catalogs, yielding a total of 508 AGNs. Our best fit is obtained with a luminosity-dependent density evolution (LDDE) model where low-luminosity (LX � 10 43 ergs s � 1 ) AGNs peak at z � 0:7, while high-luminosity AGNs (LX > 10 45 ergs s � 1 )p eak atz � 2:0. A pure luminosity evolution model (PLE) can instead be rejected. There is evidence that the fraction of absorbed (NH > 10 22 cm � 2 ) AGNs decreases with the intrinsic X-ray luminosity and increases with the redshift. Our best-fit solution provides a good fit to the observed counts, the cosmic X-ray background, and to the observed fraction of absorbed AGNs as a function of the flux in the 10 � 15 ergs cm � 2 s � 1 10 44 ergs s � 1 ) AGNs have a density of 267 deg � 2 at fluxesS2� 10 > 10 � 15 ergs cm � 2 s � 1 . Using these results, "# (
454 citations
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TL;DR: In this article, a search for squarks and gluinos in final states containing jets, missing transverse momentum and no electrons or muons is presented, and the data were recorded by the ATLAS experiment in sqrt(s) = 7 TeV proton-proton collisions at the Large Hadron Collider.
452 citations
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TL;DR: In this paper, the authors present a critical review of the global value chain (GVC) literature in light of the "technological capabilities" approach to innovation in less-developed countries (LDCs).
Abstract: This paper presents a critical review of the global value chain (GVC) literature in light of the “technological capabilities” approach to innovation in less-developed countries (LDCs). Participation in GVC is beneficial for firms in LDCs, which are bound to source technology internationally. However, the issues of learning and technological efforts at the firm level remain largely hidden in the GVC literature. We propose a shift in the empirical and theoretical agenda, arguing that research should integrate the analysis of the endogenous process of technological capability development, including specific firm-level efforts, and of the mechanisms allowing knowledge to flow within and between different global value chains into the GVC literature.
451 citations
Authors
Showing all 4598 results
Name | H-index | Papers | Citations |
---|---|---|---|
Andrew White | 149 | 1494 | 113874 |
Sw. Banerjee | 146 | 1906 | 124364 |
Fuqiang Wang | 145 | 1518 | 95014 |
Stefano Giagu | 139 | 1651 | 101569 |
Silvia Masi | 139 | 669 | 97618 |
Filippo Ceradini | 131 | 1016 | 82732 |
Mattias Ellert | 131 | 1022 | 82637 |
Francesco Lacava | 130 | 1042 | 79680 |
Giovanni Organtini | 129 | 1438 | 85866 |
Georg Zobernig | 129 | 1125 | 83321 |
Monica Verducci | 129 | 896 | 76002 |
Marzio Nessi | 129 | 1046 | 78641 |
Cristian Stanescu | 128 | 922 | 76446 |
Domizia Orestano | 128 | 982 | 78297 |
Lashkar Kashif | 128 | 782 | 74072 |