Institution
International School for Advanced Studies
Education•Trieste, Friuli-Venezia Giulia, Italy•
About: International School for Advanced Studies is a education organization based out in Trieste, Friuli-Venezia Giulia, Italy. It is known for research contribution in the topics: Galaxy & Dark matter. The organization has 3751 authors who have published 13433 publications receiving 588454 citations. The organization is also known as: SISSA & Scuola Internazionale Superiore di Studi Avanzati.
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TL;DR: In this paper, the authors derived a component-field expansion of the Green-Schwarz action for the type IIA string, in an arbitrary background of massless NS-NS and R-R bosonic fields, up to quadratic order in the fermionic coordinates θ using the usual derivation of Buscher T-duality rules.
223 citations
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International School for Advanced Studies1, University of Science and Technology of China2, INAF3, Open University4, University of Nottingham5, Cardiff University6, Ghent University7, University of Hertfordshire8, Complutense University of Madrid9, Imperial College London10, University of California, Irvine11, Spanish National Research Council12, UK Astronomy Technology Centre13, University of Edinburgh14, University of the Western Cape15, University of Padua16, Ames Research Center17, Leiden University18
TL;DR: In this paper, the authors used the Herschel Astrophysical Terahertz Large Area Survey Science Demonstration Phase survey data to determine the luminosity functions (LFs) at rest-frame wavelengths of 100 and 250 μm and at several redshifts z gsim 1, for bright submillimeter galaxies with star formation rates (SFRs) gsim 100 M ☉ yr−1.
Abstract: Exploiting the Herschel Astrophysical Terahertz Large Area Survey Science Demonstration Phase survey data, we have determined the luminosity functions (LFs) at rest-frame wavelengths of 100 and 250 μm and at several redshifts z gsim 1, for bright submillimeter galaxies with star formation rates (SFRs) gsim 100 M ☉ yr–1. We find that the evolution of the comoving LF is strong up to z ≈ 2.5, and slows down at higher redshifts. From the LFs and the information on halo masses inferred from clustering analysis, we derived an average relation between SFR and halo mass (and its scatter). We also infer that the timescale of the main episode of dust-enshrouded star formation in massive halos (M H gsim 3 × 1012 M ☉) amounts to ~7 × 108 yr. Given the SFRs, which are in the range of 102-103 M ☉ yr–1, this timescale implies final stellar masses of the order of 1011-1012 M ☉. The corresponding stellar mass function matches the observed mass function of passively evolving galaxies at z gsim 1. The comparison of the statistics for submillimeter and UV-selected galaxies suggests that the dust-free, UV bright phase is gsim 102 times shorter than the submillimeter bright phase, implying that the dust must form soon after the onset of star formation. Using a single reference spectral energy distribution (SED; the one of the z ≈ 2.3 galaxy SMM J2135-0102), our simple physical model is able to reproduce not only the LFs at different redshifts >1 but also the counts at wavelengths ranging from 250 μm to ≈1 mm. Owing to the steepness of the counts and their relatively broad frequency range, this result suggests that the dispersion of submillimeter SEDs of z > 1 galaxies around the reference one is rather small.
223 citations
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TL;DR: The existence of a UV attractive fixed point puts bounds on the type and number of massless minimally coupled matter fields, and the existence of such a fixed point has been shown to be asymptotically safe as mentioned in this paper.
Abstract: Recent studies of the ultraviolet behavior of pure gravity suggest that it admits a non-Gaussian attractive fixed point, and therefore that the theory is asymptotically safe. We consider the effect on this fixed point of massless minimally coupled matter fields. The existence of a UV attractive fixed point puts bounds on the type and number of such fields.
223 citations
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TL;DR: In this paper, an imaginary time path integral approach to the quench dynamics of conformal field theories is presented, which can be applied to the determination of the time dependence of correlation functions and entanglement entropy for both global and local quenches.
Abstract: We review the imaginary time path integral approach to the quench dynamics of conformal field theories. We show how this technique can be applied to the determination of the time dependence of correlation functions and entanglement entropy for both global and local quenches. We also briefly review other quench protocols. We carefully discuss the limits of applicability of these results to realistic models of condensed matter and cold atoms.
223 citations
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Agenzia Spaziale Italiana1, INAF2, Helsinki Institute of Physics3, Aalto University4, Goddard Space Flight Center5, International School for Advanced Studies6, Spanish National Research Council7, Istituto Nazionale di Fisica Nucleare8, Instituto Politécnico Nacional9, University of Perugia10, University of Geneva11, University of Michigan12, Max Planck Society13, University of Padua14, University of Turku15, University of Manchester16, Australia Telescope National Facility17, Pennsylvania State University18, University of Milan19, SLAC National Accelerator Laboratory20, University of Helsinki21, California Institute of Technology22, University of Cambridge23, Russian Academy of Sciences24, University of Ferrara25, Haverford College26, Tufts University27, University of Oviedo28, Chinese Academy of Sciences29
TL;DR: In this paper, simultaneous Planck, Swift, Fermi, and ground-based data for 105 blazars belonging to three samples with flux limits in the soft X-ray, hard Xray, and gamma-ray bands, with additional 5 GHz flux-density limits to ensure a good probability of a Planck detection.
Abstract: We present simultaneous Planck, Swift, Fermi, and ground-based data for 105 blazars belonging to three samples with flux limits in the soft X-ray, hard X-ray, and gamma-ray bands, with additional 5 GHz flux-density limits to ensure a good probability of a Planck detection. We compare our results to those of a companion paper presenting simultaneous Planck and multi-frequency observations of 104 radio-loud northern active galactic nuclei selected at radio frequencies. While we confirm several previous results, our unique data set allows us to demonstrate that the selection method strongly influences the results, producing biases that cannot be ignored. Almost all the BL Lac objects have been detected by the Fermi Large Area Telescope (LAT), whereas 30% to 40% of the flat-spectrum radio quasars (FSRQs) in the radio, soft X-ray, and hard X-ray selected samples are still below the gamma-ray detection limit even after integrating 27 months of Fermi-LAT data. The radio to sub-millimetre spectral slope of blazars is quite flat, with (alpha) approx 0 up to about 70GHz, above which it steepens to (alpha) approx -0.65. The BL Lacs have significantly flatter spectra than FSRQs at higher frequencies. The distribution of the rest-frame synchrotron peak frequency (nu(sup s)(sub peak)) in the spectral energy distribution (SED) of FSRQs is the same in all the blazar samples with (nu(sup s)(sub peak)) = 10(exp 13.1 +/- 0.1) Hz, while the mean inverse Compton peak frequency, (nu(sup IC)(sub peak)), ranges from 10(exp 21) to 10(exp 22) Hz. The distributions of nu(sup s)(sub peak) and nu(sup IC)(sub peak) of BL Lacs are much broader and are shifted to higher energies than those of FSRQs; their shapes strongly depend on the selection method. The Compton dominance of blazars. defined as the ratio of the inverse Compton to synchrotron peak luminosities, ranges from less than 0.2 to nearly 100, with only FSRQs reaching values larger than about 3. Its distribution is broad and depends strongly on the selection method, with gamma-ray selected blazars peaking at approx 7 or more, and radio-selected blazars at values close to 1, thus implying that the common assumption that the blazar power budget is largely dominated by high-energy emission is a selection effect. A comparison of our multi-frequency data with theoretical predictions shows that simple homogeneous SSC models cannot explain the simultaneous SEDs of most of the gamma-ray detected blazars in all samples. The SED of the blazars that were not detected by Fermi~LAT may instead be consistent with SSC emission. Our data challenge the correlation between bolometric luminosity and nu(sup s)(sub peak) predicted by the blazar sequence.
222 citations
Authors
Showing all 3802 results
Name | H-index | Papers | Citations |
---|---|---|---|
Sabino Matarrese | 155 | 775 | 123278 |
G. de Zotti | 154 | 718 | 121249 |
J. González-Nuevo | 144 | 500 | 108318 |
Matt J. Jarvis | 144 | 1064 | 85559 |
Carlo Baccigalupi | 137 | 518 | 104722 |
L. Toffolatti | 136 | 376 | 95529 |
Michele Parrinello | 133 | 637 | 94674 |
Marzio Nessi | 129 | 1046 | 78641 |
Luigi Danese | 128 | 394 | 92073 |
Lidia Smirnova | 127 | 944 | 75865 |
Michele Pinamonti | 126 | 846 | 69328 |
David M. Alexander | 125 | 652 | 60686 |
Davide Maino | 124 | 410 | 88117 |
Dipak Munshi | 124 | 365 | 84322 |
Peter Onyisi | 114 | 694 | 60392 |