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28 results on '"Foffa, S."'

1. Combining chirp mass, luminosity distance and sky localisation from gravitational wave events to detect the cosmic dipole

Author

Grimm, N., Pijnenburg, M., Mastrogiovanni, S., Bonvin, C., Foffa, S., and Cusin, G.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A key test of the isotropy of the Universe on large scales consists in comparing the dipole in the Cosmic Microwave Background (CMB) temperature with the dipole in the distribution of sources at low redshift. Current analyses find a dipole in the number counts of quasars and radio sources that is 2-5 times larger than expected from the CMB, leading to a tension reaching 5$\sigma$. In this paper, we derive a consistent framework to measure the dipole independently from gravitational wave (GW) detections. We exploit the fact that the observer velocity does not only change the distribution of events in the sky, but also the luminosity distance and redshifted chirp mass, that can be extracted from the GW waveform. We show that the estimator with higher signal-to-noise ratio is the dipole in the chirp mass measured from a population of binary neutron stars. Combining all estimators (accounting for their covariance) improves the detectability of the dipole by 30-50 percent compared to number counting of binary black holes alone. We find that a few $10^6$ events are necessary to detect a dipole consistent with the CMB one, whereas if the dipole is as large as predicted by radio sources, it will already be detectable with $10^5$ events, which would correspond to a single year of observation with next generation GW detectors. GW sources provide therefore a robust and independent way of testing the isotropy of the Universe., Comment: 17 pages, 11 figures, accepted for publication in MNRAS; minor revision compared to Version 1

Published
2023
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2. Detection and estimation of the cosmic dipole with the Einstein Telescope and Cosmic Explorer

Author

Mastrogiovanni, S., Bonvin, C., Cusin, G., and Foffa, S.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

One of the open issues of the standard cosmological model is the value of the cosmic dipole measured from the Cosmic Microwave Background (CMB), as well as from the number count of quasars and radio sources. These measurements are currently in tension, with the number count dipole being 2-5 times larger than expected from CMB measurements. This discrepancy has been pointed out as a possible indication that the cosmological principle is not valid. In this paper, we explore the possibility of detecting and estimating the cosmic dipole with gravitational waves (GWs) from compact binary mergers detected by the future next-generation detectors Einstein Telescope and Cosmic Explorer. We model the expected signal and show that for binary black holes, the dipole amplitude in the number count of detections is independent of the characteristics of the population and provides a systematic-free tool to estimate the observer velocity. We introduce techniques to detect the cosmic dipole from number counting of GW detections and estimate its significance. We show that a GW dipole consistent with the amplitude of the dipole in radio galaxies would be detectable with $>3\sigma$ significance with a few years of observation ($10^6$ GW detections) and estimated with a $16\%$ precision, while a GW dipole consistent with the CMB one would require at least $10^7$ GW events for a confident detection. We also demonstrate that a total number $N_{\rm tot}$ of GW detections would be able to detect a dipole with amplitude $v_o/c \simeq1/\sqrt{N_{\rm tot}}$., Comment: 10 pages, 10 figures. Updated to the published version. We also corrected a bug for Fig.1 and Fig.2 concerning the SNR calculation (missing 2.2 factor). Rest of the paper holds same conclusions

Published
2022
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3. Prospects for Fundamental Physics with LISA

Author

Barausse, Enrico, Berti, Emanuele, Hertog, Thomas, Hughes, Scott A., Jetzer, Philippe, Pani, Paolo, Sotiriou, Thomas P., Tamanini, Nicola, Witek, Helvi, Yagi, Kent, Yunes, Nicolas, Abdelsalhin, T., Achucarro, A., Aelst, K. V., Afshordi, N., Akcay, S., Annulli, L., Arun, K. G., Ayuso, I., Baibhav, V., Baker, T., Bantilan, H., Barreiro, T., Barrera-Hinojosa, C., Bartolo, N., Baumann, D., Belgacem, E., Bellini, E., Bellomo, N., Ben-Dayan, I., Bena, I., Benkel, R., Bergshoefs, E., Bernard, L., Bernuzzi, S., Bertacca, D., Besancon, M., Beutler, F., Beyer, F., Bhagwat, S., Bicak, J., Biondini, S., Bize, S., Blas, D., Boehmer, C., Boller, K., Bonga, B., Bonvin, C., Bosso, P., Bozzola, G., Brax, P., Breitbach, M., Brito, R., Bruni, M., Brügmann, B., Bulten, H., Buonanno, A., Burke, A. O., Burko, L. M., Burrage, C., Cabral, F., Calcagni, G., Caprini, C., Cárdenas-Avendaño, A., Celoria, M., Chatziioannou, K., Chernoff, D., Clough, K., Coates, A., Comelli, D., Compère, G., Croon, D., Cruces, D., Cusin, G., Dalang, C., Danielsson, U., Das, S., Datta, S., de Boer, J., De Luca, V., De Rham, C., Desjacques, V., Destounis, K., Di Filippo, F., Dima, A., Dimastrogiovanni, E., Dolan, S., Doneva, D., Duque, F., Durrer, R., East, W., Easther, R., Elley, M., Ellis, J. R., Emparan, R., Ezquiaga, J. M., Fairbairn, M., Fairhurst, S., Farmer, H. F., Fasiello, M. R., Ferrari, V., Ferreira, P. G., Ficarra, G., Figueras, P., Fisenko, S., Foffa, S., Franchini, N., Franciolini, G., Fransen, K., Frauendiener, J., Frusciante, N., Fujita, R., Gair, J., Ganz, A., Garcia, P., Garcia-Bellido, J., Garriga, J., Geiger, R., Geng, C., Gergely, L. Á., Germani, C., Gerosa, D., Giddings, S. B., Gourgoulhon, E., Grandclement, P., Graziani, L., Gualtieri, L., Haggard, D., Haino, S., Halburd, R., Han, W. -B., Hawken, A. J., Hees, A., Heng, I. S., Hennig, J., Herdeiro, C., Hervik, S., Holten, J. v., Hoyle, C. J. D., Hu, Y., Hull, M., Ikeda, T., Isi, M., Jenkins, A., Julié, F., Kajfasz, E., Kalaghatgi, C., Kaloper, N., Kamionkowski, M., Karas, V., Kastha, S., Keresztes, Z., Kidder, L., Kimpson, T., Klein, A., Klioner, S., Kokkotas, K., Kolesova, H., Kolkowitz, S., Kopp, J., Koyama, K., Krishnendu, N. V., Kroon, J. A. V., Kunz, M., Lahav, O., Landragin, A., Lang, R. N., Poncin-Lafitte, C. Le, Lemos, J., Li, B., Liberati, S., Liguori, M., Lin, F., Liu, G., Lobo, F. S. N., Loll, R., Lombriser, L., Lovelace, G., Macedo, R. P., Madge, E., Maggio, E., Maggiore, M., Marassi, S., Marcoccia, P., Markakis, C., Martens, W., Martinovic, K., Martins, C. J. A. P., Maselli, A., Mastrogiovanni, S., Matarrese, S., Matas, A., Mavromatos, N. E., Mazumdar, A., Meerburg, P. D., Megias, E., Miller, J., Mimoso, J. P., Mittnacht, L., Montero, M. M., Moore, B., Martin-Moruno, P., Musco, I., Nakano, H., Nampalliwar, S., Nardini, G., Nielsen, A., Novák, J., Nunes, N. J., Okounkova, M., Oliveri, R., Oppizzi, F., Orlando, G., Oshita, N., Pappas, G., Paschalidis, V., Peiris, H., Peloso, M., Perkins, S., Pettorino, V., Pikovski, I., Pilo, L., Podolsky, J., Pontzen, A., Prabhat, S., Pratten, G., Prokopec, T., Prouza, M., Qi, H., Raccanelli, A., Rajantie, A., Randall, L., Raposo, G., Raymond, V., Renaux-Petel, S., Ricciardone, A., Riotto, A., Robson, T., Roest, D., Rollo, R., Rosofsky, S., Ruan, J. J., Rubiera-García, D., Ruiz, M., Rusu, M., Sabatie, F., Sago, N., Sakellariadou, M., Saltas, I. D., Sberna, L., Sathyaprakash, B., Scheel, M., Schmidt, P., Schutz, B., Schwaller, P., Shao, L., Shapiro, S. L., Shoemaker, D., Silva, A. d., Simpson, C., Sopuerta, C. F., Spallicci, A., Stefanek, B. A., Stein, L., Stergioulas, N., Stott, M., Sutton, P., Svarc, R., Tagoshi, H., Tahamtan, T., Takeda, H., Tanaka, T., Tantilian, G., Tasinato, G., Tattersall, O., Teukolsky, S., Tiec, A. L., Theureau, G., Trodden, M., Tolley, A., Toubiana, A., Traykova, D., Tsokaros, A., Unal, C., Unnikrishnan, C. S., Vagenas, E. C., Valageas, P., Vallisneri, M., Brand, J. Van den, Broeck, C. Van den, van de Meent, M., Vanhove, P., Varma, V., Veitch, J., Vercnocke, B., Verde, L., Vernieri, D., Vernizzi, F., Vicente, R., Vidotto, F., Visser, M., Vlah, Z., Vretinaris, S., Völkel, S., Wang, Q., Wang, Yu-Tong, Werner, M. C., Westernacher, J., Weygaert, R. v. d., Wiltshire, D., Wiseman, T., Wolf, P., Wu, K., Yamada, K., Yang, H., Yi, L., Yue, X., Yvon, D., Zilhão, M., Zimmerman, A., and Zumalacarregui, M.

Subjects
General Relativity and Quantum Cosmology
Abstract

In this paper, which is of programmatic rather than quantitative nature, we aim to further delineate and sharpen the future potential of the LISA mission in the area of fundamental physics. Given the very broad range of topics that might be relevant to LISA, we present here a sample of what we view as particularly promising directions, based in part on the current research interests of the LISA scientific community in the area of fundamental physics. We organize these directions through a "science-first" approach that allows us to classify how LISA data can inform theoretical physics in a variety of areas. For each of these theoretical physics classes, we identify the sources that are currently expected to provide the principal contribution to our knowledge, and the areas that need further development. The classification presented here should not be thought of as cast in stone, but rather as a fluid framework that is amenable to change with the flow of new insights in theoretical physics., Comment: 22 pages, 1 figure, to appear in General Relativity and Gravitation

Published
2020
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4. Testing modified gravity at cosmological distances with LISA standard sirens

Author

Belgacem, E., Calcagni, G., Crisostomi, M., Dalang, C., Dirian, Y., Ezquiaga, J. M., Fasiello, M., Foffa, S., Ganz, A., Garcia-Bellido, J., Lombriser, L., Maggiore, M., Tamanini, N., Tasinato, G., Zumalacarregui, M., Barausse, E., Bartolo, N., Bertacca, D., Klein, A., Matarrese, S., and Sakellariadou, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Theory
Abstract

Modifications of General Relativity leave their imprint both on the cosmic expansion history through a non-trivial dark energy equation of state, and on the evolution of cosmological perturbations in the scalar and in the tensor sectors. In particular, the modification in the tensor sector gives rise to a notion of gravitational-wave (GW) luminosity distance, different from the standard electromagnetic luminosity distance, that can be studied with standard sirens at GW detectors such as LISA or third-generation ground based experiments. We discuss the predictions for modified GW propagation from some of the best studied theories of modified gravity, such as Horndeski or the more general degenerate higher order scalar-tensor (DHOST) theories, non-local infrared modifications of gravity, bigravity theories and the corresponding phenomenon of GW oscillation, as well as theories with extra or varying dimensions. We show that modified GW propagation is a completely generic phenomenon in modified gravity. We then use a simple parametrization of the effect in terms of two parameters $(\Xi_0,n)$, that is shown to fit well the results from a large class of models, to study the prospects of observing modified GW propagation using supermassive black hole binaries as standard sirens with LISA. We construct mock source catalogs and perform detailed Markov Chain Monte Carlo studies of the likelihood obtained from LISA standard sirens alone, as well as by combining them with CMB, BAO and SNe data to reduce the degeneracies between cosmological parameters. We find that the combination of LISA with the other cosmological datasets allows one to measure the parameter $\Xi_0$ that characterizes modified GW propagation to the percent level accuracy, sufficient to test several modified gravity theories. [Abridged], Comment: 69 pages, 18 figures. References and additional explanations added. Matches published version

Published
2019
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5. Testing modified gravity at cosmological distances with LISA standard sirens

Author

Belgacem, E, Calcagni, G, Crisostomi, M, Dalang, C, Dirian, Y, Ezquiaga, JM, Fasiello, M, Foffa, S, Ganz, A, García-Bellido, J, Lombriser, L, Maggiore, M, Tamanini, N, Tasinato, G, Zumalacárregui, M, Barausse, E, Bartolo, N, Bertacca, D, Klein, A, Matarrese, S, and Sakellariadou, M

Subjects
dark energy theory, gravitational wave detectors, gravitational waves / theory, astro-ph.CO, gr-qc, hep-th, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

Modifications of General Relativity leave their imprint both on the cosmic expansion history through a non-trivial dark energy equation of state, and on the evolution of cosmological perturbations in the scalar and in the tensor sectors. In particular, the modification in the tensor sector gives rise to a notion of gravitational-wave (GW) luminosity distance, different from the standard electromagnetic luminosity distance, that can be studied with standard sirens at GW detectors such as LISA or third-generation ground based experiments. We discuss the predictions for modified GW propagation from some of the best studied theories of modified gravity, such as Horndeski or the more general degenerate higher order scalar-tensor (DHOST) theories, non-local infrared modifications of gravity, bigravity theories and the corresponding phenomenon of GW oscillation, as well as theories with extra or varying dimensions. We show that modified GW propagation is a completely generic phenomenon in modified gravity. We then use a simple parametrization of the effect in terms of two parameters (Ξ0,n), that is shown to fit well the results from a large class of models, to study the prospects of observing modified GW propagation using supermassive black hole binaries as standard sirens with LISA. We construct mock source catalogs and perform detailed Markov Chain Monte Carlo studies of the likelihood obtained from LISA standard sirens alone, as well as by combining them with CMB, BAO and SNe data to reduce the degeneracies between cosmological parameters. We find that the combination of LISA with the other cosmological datasets allows one to measure the parameter Ξ0 that characterizes modified GW propagation to the percent level accuracy, sufficient to test several modified gravity theories. LISA standard sirens can also improve constraints on GW oscillations induced by extra field content by about three orders of magnitude relative to the current capability of ground detectors. We also update the forecasts on the accuracy on H0 and on the dark-energy equation of state using more recent estimates for the LISA sensitivity.

Published
2019

7. Tail terms in gravitational radiation reaction via effective field theory

Author

Foffa, S. and Sturani, R.

Subjects
General Relativity and Quantum Cosmology
Abstract

Gravitational radiation reaction affects the dynamics of gravitationally bound binary systems. Here we focus on the leading "tail" term which modifies binary dynamics at fourth post-Newtonian order, as first computed by Blanchet and Damour. We re-produce this result using effective field theory techniques in the framework of the Lagrangian formalism suitably extended to include dissipation effects. We recover the known logarithmic tail term, consistently with the recent interpretation of the logarithmic tail term in the mass parameter as a renormalization group effect of the Bondi mass of the system., Comment: 17 pages, 3 figures. Result interpretation revised in v2, figures and reference added

Published
2011
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8. Effective field theory calculation of conservative binary dynamics at third post-Newtonian order

Author

Foffa, S. and Sturani, R.

Subjects
General Relativity and Quantum Cosmology, High Energy Physics - Theory
Abstract

We reproduce the two-body gravitational conservative dynamics at third post-Newtonian order for spin-less sources by using the effective field theory methods for the gravitationally bound two-body system, proposed by Goldberger and Rothstein. This result has been obtained by automatizing the computation of Feynman amplitudes within a Mathematica algorithm, paving the way for higher-order computations not yet performed by traditional methods., Comment: 24 pages, 6 figures. Typos corrected and references added in v2. Typos corrected in v3

Published
2011
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9. IGEC2: A 17-month search for gravitational wave bursts in 2005-2007

Author

Astone, P., Baggio, L., Bassan, M., Bignotto, M., Bonaldi, M., Bonifazi, P., Cerdonio, M., Coccia, E., Conti, L., D'Antonio, S., Emilio, M. di Paolo, Drago, M., Fafone, V., Falferi, P., Foffa, S., Fortini, P., Frasca, S., Giordano, G., Hamilton, W. O., Hanson, J., Johnson, W. W., Liguori, N., Longo, S., Maggiore, M., Marin, F., Marini, A., McHugh, M. P., Mezzena, R., Miller, P., Minenkov, Y., Mion, A., Modestino, G., Moleti, A., Nettles, D., Ortolan, A., Pallottino, G. V., Pizzella, G., Poggi, S., Prodi, G. A., Re, V., Rocchi, A., Ronga, F., Salemi, F., Sturani, R., Taffarello, L., Terenzi, R., Vedovato, G., Vinante, A., Visco, M., Vitale, S., Weaver, J., Zendri, J. P., and Zhang, P.

Subjects
General Relativity and Quantum Cosmology
Abstract

We present here the results of a 515 days long run of the IGEC2 observatory, consisting of the four resonant mass detectors ALLEGRO, AURIGA, EXPLORER and NAUTILUS. The reported results are related to the fourfold observation time from Nov. 6 2005 until Apr. 14 2007, when Allegro ceased its operation. This period overlapped with the first long term observations performed by the LIGO interferometric detectors. The IGEC observations aim at the identification of gravitational wave candidates with high confidence, keeping the false alarm rate at the level of 1 per century, and high duty cycle, namely 57% with all four sites and 94% with at least three sites in simultaneous observation. The network data analysis is based on time coincidence searches over at least three detectors: the four 3-fold searches and the 4-fold one are combined in a logical OR. We exchanged data with the usual blind procedure, by applying a unique confidential time offset to the events in each set of data. The accidental background was investigated by performing sets of 10^8 coincidence analyses per each detector configuration on off-source data, obtained by shifting the time series of each detector. The thresholds of the five searches were tuned so as to control the overall false alarm rate to 1/century. When the confidential time shifts was disclosed, no gravitational wave candidate was found in the on-source data. As an additional output of this search, we make available to other observatories the list of triple coincidence found below search thresholds, corresponding to a false alarm rate of 1/month., Comment: 10 pages, 8 figures Accepted for publication on Phys. Rev. D

Published
2010
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10. Coherent detection method of gravitational wave bursts for spherical antennas

Author

Foffa, S. and Sturani, R.

Subjects
General Relativity and Quantum Cosmology
Abstract

We provide a comprehensive theoretical framework and a quantitative test of the method we recently proposed for processing data from a spherical detector with five or six transducers. Our algorithm is a trigger event generator performing a coherent analysis of the sphere channels. In order to test our pipeline we first built a detailed numerical model of the detector, including deviations from the ideal case such as quadrupole modes splitting, and non-identical transducer readout chains. This model, coupled with a Gaussian noise generator, has then been used to produce six time series, corresponding to the outputs of the six transducers attached to the sphere. We finally injected gravitational wave burst signals into the data stream, as well as bursts of non-gravitational origin in order to mimic the presence of non-Gaussian noise, and then processed the mock data. We report quantitative results for the detection efficiency versus false alarm rate and for the affordability of the reconstruction of the direction of arrival. In particular, the combination of the two direction reconstruction methods can reduce by a factor of 10 the number false alarms due to the non-Gaussian noise., Comment: 31 pages, 15 figures

Published
2008
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11. All-sky search of NAUTILUS data

Author

Astone, P., Bassan, M., Bonifazi, P., Borkowski, K. M., Budzyński, R. J., Chincarini, A., Coccia, E., D'Antonio, S., Emilio, M. Di Paolo, Fafone, V., Frasca, S., Foffa, S., Giordano, G., Jaranowski, P., Kondracki, W., Królak, A., Maggiore, M., Marini, A., Minenkov, Y., Modena, I., Modestino, G., Moleti, A., Pallottino, G. V., Palomba, C., Parodi, R., Pietka, M., Pizzella, G., Pletsch, H. J., Quintieri, L., Ricci, F., Rocchi, A., Ronga, F., Sturani, R., Terenzi, R., Vaccarone, R., and Visco, M.

Subjects
General Relativity and Quantum Cosmology
Abstract

A search for periodic gravitational-wave signals from isolated neutron stars in the NAUTILUS detector data is presented. We have analyzed half a year of data over the frequency band $<922.2; 923.2>$ Hz, the spindown range $<-1.463\times10^{-8}; 0>$ Hz/s and over the entire sky. We have divided the data into 2 day stretches and we have analyzed each stretch coherently using matched filtering. We have imposed a low threshold for the optimal detection statistic to obtain a set of candidates that are further examined for coincidences among various data stretches. For some candidates we have also investigated the change of the signal-to-noise ratio when we increase the observation time from two to four days. Our analysis has not revealed any gravitational-wave signals. Therefore we have imposed upper limits on the dimensionless gravitational-wave amplitude over the parameter space that we have searched. Depending on frequency, our upper limit ranges from $3.4 \times 10^{-23}$ to $1.3 \times 10^{-22}$. We have attempted a statistical verification of the hypotheses leading to our conclusions. We estimate that our upper limit is accurate to within 18%., Comment: LaTeX, 12 pages

Published
2008
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12. All-sky incoherent search for periodic signals with Explorer 2005 data

Author

Astone, P., Babusci, D., Bassan, M., Carelli, P., Cavallari, G., Chincarini, A., Coccia, E., D'Antonio, S., Emilio, M. Di Paolo, Fafone, V., Foffa, S., Gemme, G., Giordano, G., Maggiore, M., Marini, A., Minenkov, Y., Modena, I., Modestino, G., Moleti, A., Murtas, G. P., Pallottino, G. V., Parodi, R., Mortari, G. Piano, Pizzella, G., Quintieri, L., Rocchi, A., Ronga, F., Just, F. Saint, Sturani, R., Terenzi, R., Torrioli, G., Vaccarone, R., Vandoni, G., and Visco, M.

Subjects
General Relativity and Quantum Cosmology
Abstract

The data collected during 2005 by the resonant bar Explorer are divided into segments and incoherently summed in order to perform an all-sky search for periodic gravitational wave signals. The parameter space of the search spanned about 40 Hz in frequency, over 23927 positions in the sky. Neither source orbital corrections nor spindown parameters have been included, with the result that the search was sensible to isolated neutron stars with a frequency drift less than 6 X 10^{-11} Hz/s. No gravitational wave candidates have been found by means of the present analysis, which led to a best upper limit of 3.1 X 10^{-23} for the dimensionless strain amplitude., Comment: 9 pages, 5 figures

Published
2007
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13. CFT, Holography, and Causal Entropy Bound

Author

Brustein, R., Foffa, S., and Veneziano, G.

Subjects
High Energy Physics - Theory
Abstract

The causal entropy bound (CEB) is confronted with recent explicit entropy calculations in weakly and strongly coupled conformal field theories (CFTs) in arbitrary dimension $D$. For CFT's with a large number of fields, $N$, the CEB is found to be valid for temperatures not exceeding a value of order $M_P/N^{{1\over D-2}}$, in agreement with large $N$ bounds in generic cut-off theories of gravity, and with the generalized second law. It is also shown that for a large class of models including high-temperature weakly coupled CFT's and strongly coupled CFT's with AdS duals, the CEB, despite the fact that it relates extensive quantities, is equivalent to (a generalization of) a purely holographic entropy bound proposed by E. Verlinde., Comment: 14 pages, 2 figures

Published
2001
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14. Symmetry breaking aspects of the effective Lagrangian for quantum black holes

Author

Buonanno, A., Foffa, S., Maggiore, M., and Ungarelli, C.

Subjects
General Relativity and Quantum Cosmology
Abstract

The physical excitations entering the effective Lagrangian for quantum black holes are related to a Goldstone boson which is present in the Rindler limit and is due to the spontaneous breaking of the translation symmetry of the underlying Minkowski space. This physical interpretation, which closely parallels similar well-known results for the effective stringlike description of flux tubes in QCD, gives a physical insight into the problem of describing the quantum degrees of freedom of black holes. It also suggests that the recently suggested concept of 'black hole complementarity' emerges at the effective Lagrangian level rather than at the fundamental level., Comment: 11 pages, Latex,1 figure

Published
1996
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16. The Next Generation Global Gravitational Wave Observatory: The Science Book

Author

Kalogera, V., Sathyaprakash, B., Bailes, M., Bizouard, M., Buonanno, A., Burrows, A., Colpi, M., Evans, M., Fairhurst, S., Hild, S., Kasliwal, M., Lehner, L., Mandel, I., Mandic, V., Nissanke, S., Papa, M., Reddy, S., Rosswog, S., Broeck, C., Ajith, P., Anand, S., Andreoni, I., Arun, K., Barausse, E., Baryakhtar, M., Belgacem, E., Berry, C., Bertacca, D., Brito, R., Caprini, C., Chatziioannou, K., Coughlin, M., Cusin, G., Dietrich, T., Dirian, Y., East, W., Fan, X., Figueroa, D., Foffa, S., Ghosh, A., Hall, E., Harms, J., Harry, I., Hinderer, T., Janka, T., Justham, S., Kasen, D., Kotake, K., Lovelace, G., Maggiore, M., Mangiagli, A., Mapelli, M., Maselli, A., Matas, A., McIver, J., Messer, B., Mezzacappa, T., Mills, C., Mueller, B., Müller, E., Pürrer, M., Pani, P., Pratten, G., Regimbau, T., Sakellariadou, M., Schneider, R., Sesana, A., Shao, L., Sotiriou, P., Tamanini, N., Tauris, T., Thrane, E., Valiante, R., van de Meent, M., Varma, V., Vines, J., Vitale, S., Yang, H., Yunes, N., Zumalacarregui, M., Punturo, M., Reitze, D., Couvares, P., Katsanevas, S., Kajita, T., Lück, H., McClelland, D., Rowan, S., Sanders, G., Shoemaker, D., and Brand, J.

Abstract

The next generation of ground-based gravitational-wave detectors will observe coalescences of black holes and neutron stars throughout the cosmos, thousands of them with exceptional fidelity. The Science Book is the result of a 3-year effort to study the science capabilities of networks of next generation detectors. Such networks would make it possible to address unsolved problems in numerous areas of physics and astronomy, from Cosmology to Beyond the Standard Model of particle physics, and how they could provide insights into workings of strongly gravitating systems, astrophysics of compact objects and the nature of dense matter. It is inevitable that observatories of such depth and finesse will make new discoveries inaccessible to other windows of observation. In addition to laying out the rich science potential of the next generation of detectors, this report provides specific science targets in five different areas in physics and astronomy and the sensitivity requirements to accomplish those science goals. This report is the second in a six part series of reports by the GWIC 3G Subcommittee: i) Expanding the Reach of Gravitational Wave Observatories to the Edge of the Universe, ii) The Next Generation Global Gravitational Wave Observatory: The Science Book (this report), iii) 3G R&D: R&D for the Next Generation of Ground-based Gravitational Wave Detectors, iv) Gravitational Wave Data Analysis: Computing Challenges in the 3G Era, v) Future Ground-based Gravitational-wave Observatories: Synergies with Other Scientific Communities, and vi) An Exploration of Possible Governance Models for the Future Global Gravitational-Wave Observatory Network.

Published
2021

17. First joint gravitational waves search by the Auriga-Explorer-Nautilus-Virgo collaboration

Author

Acernese, F., Amico, P., Alshourbagy, M., Antonucci, F., Aoudia, S., Astone, P., Avino, S., Babusci, D., Baggio, L., Ballardin, G., Barone, F., Barsotti, L., Barsuglia, M., Bassan, M., Bauer, Th.S., Bignotto, M., Bigotta, S., Birindelli, S., Bizouard, M.A., Boccara, C., Bonaldi, M., Bondu, F., Bosi, L., Bradaschia, C., Braccini, S., van den Brand, J.F.J., Brillet, A., Brisson, V., Buskulic, D., Cagnoli, G., Calloni, E., Campagna, E., Camarda, M., Carbognani, F., Carelli, P., Cavalier, F., Cavalieri, R., Cavallari, G., Cavanna, Flavio, Cella, G., Cerdonio, M., Cesarini, E., Chassande-Mottin, E., Chincarini, A., Clapson, A.C., Cleva, F., Coccia, Eugenio, Conti, L., Corda, C., Corsi, A., Cottone, F., Coulon, J.P., Cuoco, E., D'Antonio, S., Dari, A., Dattilo, V., Davier, M., del Prete, M., De Rosa, R., Di Fiore, L., Di Lieto, A., Di Virgilio, A., Drago, M., Dubath, F., Dujardin, B., Evans, M., Fafone, V., Falferi, P., Ferrante, I., Fidecaro, Francesco, Fiori, I., Flaminio, R., Foffa, S., Fortini, P., Fournier, J.D., Frasca, S., Frasconi, F., Gammaitoni, L., Garufi, F., Gemme, Gianluca, Genin, E., Gennai, A., Giazotto, A., Giordano, G., Giordano, L., Granata, V., Greverie, C., Grosjean, D., Guidi, G., Hamdani, S., Hebri, S., Heitmann, H., Hello, P., Huet, D., Kreckelbergh, S., La Penna, P., Laval, M., Leroy, N., Letendre, N., Liguori, N., Longo, S., Lopez, B., Lorenzini, M., Loriette, V., Losurdo, G., Mackowski, J.M., Maggiore, M., Majorana, E., Marini, A., Man, C.N., Mantovani, M., Marchesoni, F., Marion, F., Marque, J., Martelli, F., Masserot, A., Menzinger, F., Mezzena, R., Minenkov, Y., Milano, L., Mion, A., Modena, I., Modestino, G., Moins, C., Moleti, A., Moreau, J., Morgado, N., Mosca, S., Mours, B., Murtas, G.P., Neri, I., Nocera, F., Ortolan, A., Pagliaroli, G., Palamara, O., Pallottino, G.V., Palomba, C., Paoletti, F., Pardi, S., Parodi, R., Pasqualetti, A., Passaquieti, R., Passuello, D., Piano Mortari, Giovanni, Piergiovanni, F., Pinard, L., Pizzella, G., Poggi, S., Poggiani, R., Prodi, G.A., Punturo, M., Puppo, P., van der Putten, S., Quintieri, L., Rapagnani, P., Re, V., Regimbau, T., Remillieux, A., Ricci, F., Ricciardi, I., Rocchi, A., Romano, R., Ronga, F., Ruggi, P., Russo, G., Salemi, F., Solimeno, S., Spallicci, A., Sturani, R., Taffarello, L., Tarallo, M., Terenzi, R., Tonelli, M., Toncelli, A., Torrioli, G., Tournefier, E., Travasso, F., Tremola, C., Vaccarone, R., Vajente, G., Vandoni, G., Vedovato, G., Verkindt, D., Vetrano, F., Vicere, A., Vinante, A., Vinet, J.Y., Visco, M., Vitale, S., Vocca, H., Yvert, M., Zendri, J.P., Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, ESPCI ParisTech, Virgo, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), AURIGA, VIRGO, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Laboratoire d'Annecy de Physique des Particules (LAPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Gravitation ( APC-Gravitation ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), F., Acernese, Avino, Saverio, Calloni, Enrico, DE ROSA, Rosario, L., DI FIORE, Garufi, Fabio, Giordano, Lara, Milano, Leopoldo, Mosca, Simona, Pardi, Silvio, Russo, Guido, Solimeno, Salvatore, Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Nice Sophia Antipolis (1965 - 2019) (UNS), and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
antenne risonanti, Physics and Astronomy (miscellaneous), Population, Onde gravitazionali, interferometri, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Constant false alarm rate, Coincident, 0103 physical sciences, DETECTORS, 010306 general physics, education, FILTER, RUN, Physics, education.field_of_study, AURIGA, General Relativity and Cosmology, 010308 nuclear & particles physics, Gravitational wave, Settore FIS/01 - Fisica Sperimentale, Detector, Galactic Center, Astronomy, Data set, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc]
Abstract

We present results of the search for coincident burst excitations over a 24 hours long data set collected by AURIGA, EXPLORER, NAUTILUS and Virgo detectors during September 2005. The search of candidate triggers was performed independently on each of the data sets from single detectors. We looked for two-fold time coincidences between these candidates using an algorithm optimized for a given population of sources and we calculated the efficiency of detection through injections of templated signal waveforms into the streams of data. To this purpose we have considered the case of signals shaped as damped sinusoids coming from the galactic center direction. In this framework our method targets an optimal balance between high efficiency and low false alarm rate, aiming at setting confidence intervals as stringent as possible in terms of the rate of the selected source models. We present results of the search for coincident burst excitations over a 24 hours long data set collected by AURIGA, EXPLORER, NAUTILUS and Virgo detectors during September 2005. The search of candidate triggers was performed independently on each of the data sets from single detectors. We looked for two-fold time coincidences between these candidates using an algorithm optimized for a given population of sources and we calculated the efficiency of detection through injections of templated signal waveforms into the streams of data. To this purpose we have considered the case of signals shaped as damped sinusoids coming from the galactic center direction. In this framework our method targets an optimal balance between high efficiency and low false alarm rate, aiming at setting confidence intervals as stringent as possible in terms of the rate of the selected source models.

Published
2008

18. New horizons for fundamental physics with LISA

Author

K. G. Arun, Enis Belgacem, Robert Benkel, Laura Bernard, Emanuele Berti, Gianfranco Bertone, Marc Besancon, Diego Blas, Christian G. Böhmer, Richard Brito, Gianluca Calcagni, Alejandro Cardenas-Avendaño, Katy Clough, Marco Crisostomi, Valerio De Luca, Daniela Doneva, Stephanie Escoffier, José María Ezquiaga, Pedro G. Ferreira, Pierre Fleury, Stefano Foffa, Gabriele Franciolini, Noemi Frusciante, Juan García-Bellido, Carlos Herdeiro, Thomas Hertog, Tanja Hinderer, Philippe Jetzer, Lucas Lombriser, Elisa Maggio, Michele Maggiore, Michele Mancarella, Andrea Maselli, Sourabh Nampalliwar, David Nichols, Maria Okounkova, Paolo Pani, Vasileios Paschalidis, Alvise Raccanelli, Lisa Randall, Sébastien Renaux-Petel, Antonio Riotto, Milton Ruiz, Alexander Saffer, Mairi Sakellariadou, Ippocratis D. Saltas, B. S. Sathyaprakash, Lijing Shao, Carlos F. Sopuerta, Thomas P. Sotiriou, Nikolaos Stergioulas, Nicola Tamanini, Filippo Vernizzi, Helvi Witek, Kinwah Wu, Kent Yagi, Stoytcho Yazadjiev, Nicolás Yunes, Miguel Zilhão, Niayesh Afshordi, Marie-Christine Angonin, Vishal Baibhav, Enrico Barausse, Tiago Barreiro, Nicola Bartolo, Nicola Bellomo, Ido Ben-Dayan, Eric A. Bergshoeff, Sebastiano Bernuzzi, Daniele Bertacca, Swetha Bhagwat, Béatrice Bonga, Lior M. Burko, Geoffrey Compére, Giulia Cusin, Antonio da Silva, Saurya Das, Claudia de Rham, Kyriakos Destounis, Ema Dimastrogiovanni, Francisco Duque, Richard Easther, Hontas Farmer, Matteo Fasiello, Stanislav Fisenko, Kwinten Fransen, Jörg Frauendiener, Jonathan Gair, László Árpád Gergely, Davide Gerosa, Leonardo Gualtieri, Wen-Biao Han, Aurelien Hees, Thomas Helfer, Jörg Hennig, Alexander C. Jenkins, Eric Kajfasz, Nemanja Kaloper, Vladimír Karas, Bradley J. Kavanagh, Sergei A. Klioner, Savvas M. Koushiappas, Macarena Lagos, Christophe Le Poncin-Lafitte, Francisco S. N. Lobo, Charalampos Markakis, Prado Martín-Moruno, C. J. A. P. Martins, Sabino Matarrese, Daniel R. Mayerson, José P. Mimoso, Johannes Noller, Nelson J. Nunes, Roberto Oliveri, Giorgio Orlando, George Pappas, Igor Pikovski, Luigi Pilo, Jiří Podolský, Geraint Pratten, Tomislav Prokopec, Hong Qi, Saeed Rastgoo, Angelo Ricciardone, Rocco Rollo, Diego Rubiera-Garcia, Olga Sergijenko, Stuart Shapiro, Deirdre Shoemaker, Alessandro Spallicci, Oleksandr Stashko, Leo C. Stein, Gianmassimo Tasinato, Andrew J. Tolley, Elias C. Vagenas, Stefan Vandoren, Daniele Vernieri, Rodrigo Vicente, Toby Wiseman, Valery I. Zhdanov, Miguel Zumalacárregui, UAM. Departamento de Física Teórica, Arun, K, Belgacem, E, Benkel, R, Bernard, L, Berti, E, Bertone, G, Besancon, M, Blas, D, Bohmer, C, Brito, R, Calcagni, G, Cardenas-Avendano, A, Clough, K, Crisostomi, M, De Luca, V, Doneva, D, Escoffier, S, Ezquiaga, J, Ferreira, P, Fleury, P, Foffa, S, Franciolini, G, Frusciante, N, Garcia-Bellido, J, Herdeiro, C, Hertog, T, Hinderer, T, Jetzer, P, Lombriser, L, Maggio, E, Maggiore, M, Mancarella, M, Maselli, A, Nampalliwar, S, Nichols, D, Okounkova, M, Pani, P, Paschalidis, V, Raccanelli, A, Randall, L, Renaux-Petel, S, Riotto, A, Ruiz, M, Saffer, A, Sakellariadou, M, Saltas, I, Sathyaprakash, B, Shao, L, Sopuerta, C, Sotiriou, T, Stergioulas, N, Tamanini, N, Vernizzi, F, Witek, H, Wu, K, Yagi, K, Yazadjiev, S, Yunes, N, Zilhao, M, Afshordi, N, Angonin, M, Baibhav, V, Barausse, E, Barreiro, T, Bartolo, N, Bellomo, N, Ben-Dayan, I, Bergshoeff, E, Bernuzzi, S, Bertacca, D, Bhagwat, S, Bonga, B, Burko, L, Compere, G, Cusin, G, da Silva, A, Das, S, de Rham, C, Destounis, K, Dimastrogiovanni, E, Duque, F, Easther, R, Farmer, H, Fasiello, M, Fisenko, S, Fransen, K, Frauendiener, J, Gair, J, Gergely, L, Gerosa, D, Gualtieri, L, Han, W, Hees, A, Helfer, T, Hennig, J, Jenkins, A, Kajfasz, E, Kaloper, N, Karas, V, Kavanagh, B, Klioner, S, Koushiappas, S, Lagos, M, Poncin-Lafitte, C, Lobo, F, Markakis, C, Martin-Moruno, P, Martins, C, Matarrese, S, Mayerson, D, Mimoso, J, Noller, J, Nunes, N, Oliveri, R, Orlando, G, Pappas, G, Pikovski, I, Pilo, L, Podolsky, J, Pratten, G, Prokopec, T, Qi, H, Rastgoo, S, Ricciardone, A, Rollo, R, Rubiera-Garcia, D, Sergijenko, O, Shapiro, S, Shoemaker, D, Spallicci, A, Stashko, O, Stein, L, Tasinato, G, Tolley, A, Vagenas, E, Vandoren, S, Vernieri, D, Vicente, R, Wiseman, T, Zhdanov, V, Zumalacarregui, M, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique [Palaiseau] (CPHT), École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des deux Infinis de Toulouse (L2IT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Systèmes de Référence Temps Espace (SYRTE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique et chimie de l'environnement (LPCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), LISA, Arun, K. G., Belgacem, Eni, Benkel, Robert, Bernard, Laura, Berti, Emanuele, Bertone, Gianfranco, Besancon, Marc, Blas, Diego, B??hmer, Christian G., Brito, Richard, Calcagni, Gianluca, Cardenas-Avenda??o, Alejandro, Clough, Katy, Crisostomi, Marco, De Luca, Valerio, Doneva, Daniela, Escoffier, Stephanie, Mar??a Ezquiaga, Jos??, Ferreira, Pedro G., Fleury, Pierre, Foffa, Stefano, Franciolini, Gabriele, Frusciante, Noemi, Garc??a-Bellido, Juan, Herdeiro, Carlo, Hertog, Thoma, Hinderer, Tanja, Jetzer, Philippe, Lombriser, Luca, Maggio, Elisa, Maggiore, Michele, Mancarella, Michele, Maselli, Andrea, Nampalliwar, Sourabh, Nichols, David, Okounkova, Maria, Pani, Paolo, Paschalidis, Vasileio, Raccanelli, Alvise, Randall, Lisa, Renaux-Petel, S??bastien, Riotto, Antonio, Ruiz, Milton, Saffer, Alexander, Sakellariadou, Mairi, Saltas, Ippocratis D., Sathyaprakash, B. S., Shao, Lijing, Sopuerta, Carlos F., Sotiriou, Thomas P., Stergioulas, Nikolao, Tamanini, Nicola, Vernizzi, Filippo, Witek, Helvi, Wu, Kinwah, Yagi, Kent, Yazadjiev, Stoytcho, Yunes, Nicol??, Zilh??o, Miguel, Afshordi, Niayesh, Angonin, Marie-Christine, Baibhav, Vishal, Barausse, Enrico, Barreiro, Tiago, Bartolo, Nicola, Bellomo, Nicola, Ben-Dayan, Ido, Bergshoeff, Eric A., Bernuzzi, Sebastiano, Bertacca, Daniele, Bhagwat, Swetha, Bonga, B??atrice, Burko, Lior M., Comp??re, Geoffrey, Cusin, Giulia, da Silva, Antonio, Das, Saurya, de Rham, Claudia, Destounis, Kyriako, Dimastrogiovanni, Ema, Duque, Francisco, Easther, Richard, Farmer, Honta, Fasiello, Matteo, Fisenko, Stanislav, Fransen, Kwinten, Frauendiener, J??rg, Gair, Jonathan, rp??d Gergely, L??szl??, Gerosa, Davide, Gualtieri, Leonardo, Han, Wen-Biao, Hees, Aurelien, Helfer, Thoma, Hennig, J??rg, Jenkins, Alexander C., Kajfasz, Eric, Kaloper, Nemanja, Karas, Vladim??r, Kavanagh, Bradley J., Klioner, Sergei A., Koushiappas, Savvas M., Lagos, Macarena, Le Poncin-Lafitte, Christophe, Lobo, Francisco S. N., Markakis, Charalampo, Mart??n-Moruno, Prado, Martins, C. J. A. P., Matarrese, Sabino, Mayerson, Daniel R., Mimoso, Jos?? P., Noller, Johanne, Nunes, Nelson J., Oliveri, Roberto, Orlando, Giorgio, Pappas, George, Pikovski, Igor, Pilo, Luigi, Podolsk??, Ji????, Pratten, Geraint, Prokopec, Tomislav, Qi, Hong, Rastgoo, Saeed, Ricciardone, Angelo, Rollo, Rocco, Rubiera-Garcia, Diego, Sergijenko, Olga, Shapiro, Stuart, Shoemaker, Deirdre, Spallicci, Alessandro, Stashko, Oleksandr, Stein, Leo C., Tasinato, Gianmassimo, Tolley, Andrew J., Vagenas, Elias C., Vandoren, Stefan, Vernieri, Daniele, Vicente, Rodrigo, Wiseman, Toby, Zhdanov, Valery I., Zumalac??rregui, Miguel, National Science Foundation (US), National Aeronautics and Space Administration (US), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Generalitat de Catalunya, European Research Council, European Commission, Fundação para a Ciência e a Tecnologia (Portugal), Ministero dell'Istruzione, dell'Università e della Ricerca, Fundación 'la Caixa', Czech Science Foundation, Science and Technology Facilities Council (UK), GRAPPA (ITFA, IoP, FNWI), and Astroparticle Physics (IHEF, IoP, FNWI)

Subjects
Astrofísica, PROTOPLANET MIGRATION, Física-Modelos matemáticos, Physics and Astronomy (miscellaneous), gr-qc, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), GRAVITATIONAL-WAVES, horizon, Fundamental physic, General Relativity and Quantum Cosmology, Physics, Particles & Fields, Gravitational waves, LIGO (Observatory), Tests of general relativity, Settore FIS/05 - Astronomia e Astrofisica, DARK-MATTER, Física matemática, KOZAI MECHANISM, High Energy Physics, GENERAL-RELATIVITY, Fundamental physics, LISA, PRIMORDIAL BLACK-HOLES, Science & Technology, General Relativity and Cosmology, 83CXX, Physics, gravitation: interaction, gravitational radiation, Física, Compact, QUANTUM-GRAVITY, Physical Sciences, Astronomia, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], fundamental physics, gravitational waves, test of general relativity, MODIFIED GRAVITY, Gravitational wave, MULTIPOLE MOMENTS, HUBBLE CONSTANT
Abstract

K. G. Arun et al., The Laser Interferometer Space Antenna (LISA) has the potential to reveal wonders about the fundamental theory of nature at play in the extreme gravity regime, where the gravitational interaction is both strong and dynamical. In this white paper, the Fundamental Physics Working Group of the LISA Consortium summarizes the current topics in fundamental physics where LISA observations of gravitational waves can be expected to provide key input. We provide the briefest of reviews to then delineate avenues for future research directions and to discuss connections between this working group, other working groups and the consortium work package teams. These connections must be developed for LISA to live up to its science potential in these areas., E. Berti is supported by NSF Grants No. PHY-1912550 and AST-2006538, NASA ATP Grants No. 17-ATP17-0225 and 19-ATP19-0051, NSF-XSEDE Grant No. PHY-090003, and NSF Grant PHY-20043. D. Blas is supported by a ‘Ayuda Beatriz Galindo Senior’ from the Spanish ‘Ministerio de Universidades’, grant BG20/00228. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. The research leading of to these results has received funding from the Spanish Ministry of Science and Innovation (PID2020-115845GB-I00/AEI/10.13039/501100011033). K. Clough is supported by funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 693024). A. Cárdenas-Avendaño acknowledges funding from the Fundación Universitaria Konrad Lorenz (Project 5INV1) and from Will and Kacie Snellings. M. Crisostomi and E. Barausse are supported by the European Union’s H2020 ERC Consolidator Grant “GRavity from Astrophysical to Microscopic Scales” (Grant No. GRAMS-815673). P. Fleury received the support of a fellowship from “la Caixa” Foundation (ID 100010434). The fellowship code is LCF/BQ/PI19/11690018. C. Herdeiro thanks the support of the Center for Research and Development in Mathematics and Applications (CIDMA) through the Portuguese Foundation for Science and Technology (FCT - Fundação para a Ciência e a Tecnologia), references UIDB/04106/2020 and UIDP/04106/2020, the projects PTDC/FIS-OUT/28407/2017, CERN/FIS-PAR/0027/2019, PTDC/FIS-AST/3041/2020 and the European Union’s Horizon 2020 research and innovation (RISE) programme H2020-MSCA-RISE-2017 Grant No. FunFiCO-777740. P. Pani and E. Maggio acknowledge financial support provided under the European Union’s H2020 ERC, Starting Grant agreement no. DarkGRA–757480, and under the MIUR PRIN and FARE programmes (GW-NEXT, CUP: B84I20000100001), and support from the Amaldi Research Center funded by the MIUR program “Dipartimento di Eccellenza” (CUP: B81I18001170001). N.Frusciante was supported by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-OUT/29048/2017, CERN/FIS-PAR/0037/2019, the FCT project “CosmoTests—Cosmological tests of gravity theories beyond General Relativity” with ref. number CEECIND/00017/2018 and the FCT project “BEYLA –BEYond LAmbda” with ref. number PTDC/FIS-AST/0054/2021. L.Lombriser was supported by a Swiss National Science Foundation Professorship grant (No. 170547). S.N. acknowledges support from the Alexander von Humboldt Foundation. D.N. acknowledges support from the NSF Grant No. PHY-2011784. R.B. acknowledges financial support from FCT – Fundação para a Ciência e a Tecnologia, I.P., under the Scientific Employment Stimulus - Individual Call - 2020.00470.CEECIND. V. Paschalidis acknowledges support from NSF Grant PHY-1912619 and NASA Grant 80NSSC20K1542 to the University of Arizona. B.S.S. is supported by NSF grants No. AST-2006384 and PHY-2012083. C.F.S. is supported by contracts ESP2017-90084-P and PID2019-106515GB-I00/AEI/10.13039/501100011033 (Spanish Ministry of Science and Innovation) and 2017-SGR-1469 (AGAUR, Generalitat de Catalunya). T. P. S. acknowledges partial support from the STFC Consolidated Grant No. ST/P000703/1. M. Ruiz acknowledges support from NASA Grant 80NSSC17K0070 to the University of Illinois at Urbana-Champaign. I.D. Saltas is supported by the Czech Science Foundation GAČR, Grant No. 21-16583M. N. Stergioulas is supported by the ESA Prodex grant PEA:4000132310 “LISA Stochastic Signals Analysis Pipeline”. F.V. acknowledges partial support from CNES. K.Y. acknowledges support from NSF Grant PHY-1806776, NASA Grant 80NSSC20K0523, a Sloan Foundation Research Fellowship and the Owens Family Foundation. K.Y. would like to also acknowledge support by the COST Action GWverse CA16104 and JSPS KAKENHI Grants No. JP17H06358. N. Yunes acknowledges support from NASA Grants No. NNX16AB98G, 80NSSC17M0041 and 80NSSC18K1352, NSF Award No. 1759615, and the Simons Foundation through MPS Award Number 896696. D.D. acknowledge financial support via an Emmy Noether Research Group funded by the German Research Foundation (DFG) under grant no. DO 1771/1-1.

Published
2022

19. Cosmology and modified gravity with dark sirens from GWTC-3

Author

Mancarella, Michele, Finke, Andreas, Foffa, Stefano, Genoud-Prachex, Edwin, Francesco Iacovelli, Maggiore, Michele, Augé, E, Dumarchez, J, Trân Thanh Vân, J, Mancarella, M, Finke, A, Foffa, S, Genoud-Prachex, E, Iacovelli, F, and Maggiore, M

Subjects
hubble parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Condensed Matter::Superconductivity, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), modified gravity, General Relativity and Quantum Cosmology, Gravitational wave, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the latest measurements of the Hubble parameter and of the parameter $\Xi_0$ describing modified gravitational wave propagation, obtained from the third gravitational wave transient catalog, GWTC-3, using the correlation with galaxy catalogs and information from the source-frame mass distribution of binary black holes. The latter leads to the tightest bound on $\Xi_0$ so far, i.e. $\Xi_0 = 1.2^{+0.7}_{-0.7}$ with a flat prior on $\Xi_0$, and $\Xi_0 = 1.0^{+0.4}_{-0.8}$ with a prior uniform in $\log\Xi_0$ (Max posterior and $68\%$ HDI). The measurement of $H_0$ is dominated by the single bright siren GW170817, resulting in $H_0=67^{+9}_{-6} \, \rm km \, s^{-1} \, Mpc$ when combined with the galaxy catalog., Comment: Contribution to the Gravitation session of the 56th Rencontres de Moriond 2022

Published
2022
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20. Gravitational-wave cosmology with dark sirens: state of the art and perspectives for 3G detectors

Author

Michele Mancarella, Nicola Borghi, Stefano Foffa, Edwin Genoud-Prachex, Francesco Iacovelli, Michele Maggiore, Michele Moresco, Matteo Schulz, Mancarella, M, Borghi, N, Foffa, S, Genoud-Prachex, E, Iacovelli, F, Maggiore, M, Moresco, M, and Schulz, M

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), hubble constant, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - High Energy Astrophysical Phenomena, gravitational wave, cosmology, modified gravity, General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A joint fit of the mass and redshift distributions of the population of Binary Black Holes detected with Gravitational-Wave observations can be used to obtain constraints on the Hubble parameter and on deviations from General Relativity in the propagation of Gravitational Waves. We first present applications of this technique to the latest catalog of Gravitational-Wave events, focusing on the comparison of different parametrizations for the source-frame mass distribution of Black Hole Binaries. We find that models with more than one feature are favourite by the data, as suggested by population studies, even when varying the cosmology. Then, we discuss perspectives for the use of this technique with third generation Gravitational-Wave detectors, exploiting the recently developed Fisher information matrix Python code GWFAST., 5 pages, 2 figures, Contribution to the ICHEP 2022 conference proceedings

Published
2022

21. Probing modified gravitational wave propagation with strongly lensed coalescing binaries

Author

Stefano Foffa, Francesco Iacovelli, Andreas Finke, Michele Mancarella, Michele Maggiore, Finke, A, Foffa, S, Iacovelli, F, Maggiore, M, and Mancarella, M

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Einstein Telescope, Gravitational wave, Detector, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, General Relativity and Quantum Cosmology, Galaxy, LIGO, Third generation, strong lensing, Sensitivity (control systems), KAGRA, dark energy, gravitational wave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

It has been recently shown that quadruply lensed gravitational-wave (GW) events due to coalescing binaries can be localized to one or just a few galaxies, even in the absence of an electromagnetic counterpart. We discuss how this can be used to extract information on modified GW propagation, which is a crucial signature of modifications of gravity at cosmological scales. We show that, using quadruply lensed systems, it is possible to constrain the parameter $\Xi_0$ that characterizes modified GW propagation, without the need of imposing a prior on $H_0$. A LIGO/Virgo/Kagra network at target sensitivity might already get a significant measurement of $\Xi_0$, while a third generation GW detector such as the Einstein Telescope could reach a very interesting accuracy., Comment: 11 pages, 5 figures

Published
2021

22. Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST

Author

Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore, Iacovelli, F, Mancarella, M, Foffa, S, and Maggiore, M

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), fisher information matrix, Astrophysics - High Energy Astrophysical Phenomena, Gravitational wave, General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We introduce $\texttt{GWFAST}$, a novel Fisher-matrix code for gravitational-wave studies, tuned toward third-generation gravitational-wave detectors such as Einstein Telescope (ET) and Cosmic Explorer (CE). We use it to perform a comprehensive study of the capabilities of ET alone, and of a network made by ET and two CE detectors, as well as to provide forecasts for the forthcoming O4 run of the LVK collaboration. We consider binary neutron stars, binary black holes and neutron star-black hole binaries, and compute basic metrics such as the distribution of signal-to-noise ratio (SNR), the accuracy in the reconstruction of various parameters (including distance, sky localization, masses, spins and, for neutron stars, tidal deformabilities), and the redshift distribution of the detections for different thresholds in SNR and different levels of accuracy in localization and distance measurement. We examine the expected distribution and properties of `golden events', with especially large values of the SNR. We also pay special attention to the dependence of the results on astrophysical uncertainties and on various technical details (such as choice of waveforms, or the threshold in SNR), and we compare with other Fisher codes in the literature. In a companion paper we discuss the technical aspects of the code. Together with this paper, we publicly release the code $\texttt{GWFAST}$ at https://github.com/CosmoStatGW/gwfast, and the library $\texttt{WF4Py}$ implementing state-of-the-art gravitational-wave waveforms in pure $\texttt{Python}$ at https://github.com/CosmoStatGW/WF4Py., 43 + 12 pages, 24 + 5 Figures, $\texttt{GWFAST}$ available at https://github.com/CosmoStatGW/gwfast, $\texttt{WF4Py}$ available at https://github.com/CosmoStatGW/WF4Py. v3: resubmitted to APJ, minor changes in results, Appendix C added

Published
2022

23. Modified gravitational wave propagation and the binary neutron star mass function

Author

Andreas Finke, Stefano Foffa, Francesco Iacovelli, Michele Maggiore, Michele Mancarella, Finke, A, Foffa, S, Iacovelli, F, Maggiore, M, and Mancarella, M

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Modified gravity, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Modified gravitational wave propagation, General Relativity and Quantum Cosmology, Space and Planetary Science, Einstein telescope, Astrophysics - High Energy Astrophysical Phenomena, Gravitational wave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Modified gravitational wave (GW) propagation is a generic phenomenon in modified gravity. It affects the reconstruction of the redshift of coalescing binaries from the luminosity distance measured by GW detectors, and therefore the reconstruction of the actual masses of the component compact stars from the observed (`detector-frame') masses. We show that, thanks to the narrowness of the mass distribution of binary neutron stars, this effect can provide a clear signature of modified gravity, particularly for the redshifts explored by third generation GW detectors such as Einstein Telescope and Cosmic Explorer., v2: expanded version, to appear in Physics of the Dark Universe

Published
2021

24. Cosmology with LIGO/Virgo dark sirens: Hubble parameter and modified gravitational wave propagation

Author

Andreas Finke, Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore, Finke, A, Foffa, S, Iacovelli, F, Maggiore, M, and Mancarella, M

Subjects
Physics, Modified gravity, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational wave, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Gravitational waves / theory, General Relativity and Quantum Cosmology (gr-qc), LIGO, Galaxy, Cosmology, General Relativity and Quantum Cosmology, law.invention, symbols.namesake, Binary black hole, law, symbols, Dark energy, Gravitational waves / experiment, Hubble's law, Flare, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a detailed study of the methodology for correlating `dark sirens' (compact binaries coalescences without electromagnetic counterpart) with galaxy catalogs. We propose several improvements on the current state of the art, and we apply them to the GWTC-2 catalog of LIGO/Virgo gravitational wave (GW) detections, and the GLADE galaxy catalog, performing a detailed study of several sources of systematic errors that, with the expected increase in statistics, will eventually become the dominant limitation. We provide a measurement of $H_0$ from dark sirens alone, finding as the best result $H_0=67.3^{+27.6}_{-17.9}\,\,{\rm km}\, {\rm s}^{-1}\, {\rm Mpc}^{-1}$ ($68\%$ c.l.) which is, currently, the most stringent constraint obtained using only dark sirens. Combining dark sirens with the counterpart for GW170817 we find $H_0= 72.2^{+13.9}_{-7.5} \,{\rm km}\, {\rm s}^{-1}\, {\rm Mpc}^{-1}$. We also study modified GW propagation, which is a smoking gun of dark energy and modifications of gravity at cosmological scales, and we show that current observations of dark sirens already start to provide interesting limits. From dark sirens alone, our best result for the parameter $\Xi_0$ that measures deviations from GR (with $\Xi_0=1$ in GR) is $\Xi_0=2.1^{+3.2}_{-1.2}$. We finally discuss limits on modified GW propagation under the tentative identification of the flare ZTF19abanrhr as the electromagnetic counterpart of the binary black hole coalescence GW190521, in which case our most stringent result is $\Xi_0=1.8^{+0.9}_{-0.6}$. We release the publicly available code $\tt{DarkSirensStat}$, which is available under open source license at \url{https://github.com/CosmoStatGW/DarkSirensStat}., Comment: v2: several significant technical improvements, results changed v3: minor changes, Fig 9 added. The version to appear in JCAP

Published
2021
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25. Conformal symmetry and nonlinear extensions of nonlocal gravity

Author

Stefano Foffa, Michele Maggiore, Giulia Cusin, Michele Mancarella, Cusin, G, Foffa, S, Maggiore, M, and Mancarella, M

Subjects
High Energy Physics - Theory, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Conformal anomaly, Inverse, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Square (algebra), General Relativity and Quantum Cosmology, Non-local gravity, De Sitter universe, Conformal symmetry, 0103 physical sciences, 010306 general physics, Effective action, Mathematical physics, Physics, 010308 nuclear & particles physics, Equation of state (cosmology), General Relativity and Cosmology, Operator (physics), Dark Energy, High Energy Physics - Theory (hep-th), Particle Physics - Theory, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study two nonlinear extensions of the nonlocal $R\,\Box^{-2}R$ gravity theory. We extend this theory in two different ways suggested by conformal symmetry, either replacing $\Box^{-2}$ with $(-\Box + R/6)^{-2}$, which is the operator that enters the action for a conformally-coupled scalar field, or replacing $\Box^{-2}$ with the inverse of the Paneitz operator, which is a four-derivative operator that enters in the effective action induced by the conformal anomaly. We show that the former modification gives an interesting and viable cosmological model, with a dark energy equation of state today $w_{\rm DE}\simeq -1.01$, which very closely mimics $\Lambda$CDM and evolves asymptotically into a de Sitter solution. The model based on the Paneitz operator seems instead excluded by the comparison with observations. We also review some issues about the causality of nonlocal theories, and we point out that these nonlocal models can be modified so to nicely interpolate between Starobinski inflation in the primordial universe and accelerated expansion in the recent epoch., Comment: 27 pages, 4 figures

Published
2016
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26. Non-local gravity with a Weyl-square term

Author

Stefano Foffa, Giulia Cusin, Michele Maggiore, Michele Mancarella, Cusin, G, Foffa, S, Maggiore, M, and Mancarella, M

Subjects
Weyl tensor, High Energy Physics - Theory, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Square (algebra), Local theory, General Relativity and Quantum Cosmology, symbols.namesake, Non-local gravity, Quantum mechanics, 0103 physical sciences, Tensor, 010306 general physics, Mathematical physics, Physics, 010308 nuclear & particles physics, General Relativity and Cosmology, Term (logic), Background level, High Energy Physics - Theory (hep-th), symbols, Particle Physics - Theory, Scalar curvature, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Recent work has shown that modifications of General Relativity based on the addition to the action of a non-local term $R\,\Box^{-2}R$, or on the addition to the equations of motion of a term involving $(g_{\mu\nu}\Box^{-1} R)$, produce dynamical models of dark energy which are cosmologically viable both at the background level and at the level of cosmological perturbations. We explore a more general class of models based on the addition to the action of terms proportional to $R_{\mu\nu}\,\Box^{-2}R^{\mu\nu}$ and $C_{\mu\nu\rho\sigma}\, \Box^{-2}C^{\mu\nu\rho\sigma}$, where $C_{\mu\nu\rho\sigma}$ is the Weyl tensor. We find that the term $R_{\mu\nu}\,\Box^{-2}R^{\mu\nu}$ does not give a viable background evolution. The non-local Weyl-square term, in contrast, does not contribute to the background evolution but we find that, at the level of cosmological perturbations, it gives instabilities in the tensor sector. Thus, only non-local terms which depend just on the Ricci scalar $R$ appear to be cosmologically viable. We discuss how these results can provide a hint for the mechanism that might generate these effective non-local terms from a fundamental local theory., Comment: 25 pages, 6 figures. v2: the version to appear in PRD

Published
2015

27. Stability issues of nonlocal gravity during primordial inflation

Author

Giulia Cusin, Stefano Foffa, Enis Belgacem, Michele Maggiore, Michele Mancarella, Belgacem, E, Cusin, G, Foffa, S, Maggiore, M, and Mancarella, M

Subjects
Inflation (cosmology), Physics, Modified gravity, Nuclear and High Energy Physics, Gravity (chemistry), 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Stability (probability), Atomic and Molecular Physics, and Optics, Cosmology, General Relativity and Quantum Cosmology, Theoretical physics, 0103 physical sciences, nonlocal gravity, Dark energy, 010306 general physics, cosmology, Mathematical physics
Abstract

We study the cosmological evolution of some nonlocal gravity models, when the initial conditions are set during a phase of primordial inflation. We examine in particular three models, the so-called RT, RR and [Formula: see text] models, previously introduced by our group. We find that, during inflation, the RT model has a viable background evolution, but at the level of cosmological perturbations develops instabilities that make it nonviable. In contrast, the RR and [Formula: see text] models have a viable evolution even when their initial conditions are set during a phase of primordial inflation.

Published
2018

28. Modified gravitational wave propagation: information from strongly lensed binaries and the BNS mass function

Author

Francesco Iacovelli, Finke, Andreas, Foffa, Stefano, Maggiore, Michele, Mancarella, Michele, Augé, E, Dumarchez, J, Trân Thanh Vân, J, Iacovelli, F, Finke, A, Foffa, S, Maggiore, M, and Mancarella, M

Subjects
General Relativity and Quantum Cosmology, Modified gravity, Cosmology and Nongalactic Astrophysics (astro-ph.CO), binary neutron stars, strong lensing, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), gravitational wave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Modified gravitational wave propagation is a smoking gun of modifications of gravity at cosmological scales, and can be the most promising observable for testing such theories. The observation of gravitational waves (GW) in recent years has allowed us to start probing this effect, and here we briefly review two promising ways of testing it. We will show that, already with the current network of detectors, it is possible to reach an interesting accuracy in the estimation of the $\Xi_0$ parameter (that characterizes modified gravitational wave propagation, with $\Xi_{0, {\rm GR}} = 1$) and with next generation facilities, such as the Einstein Telescope, we can get a sub-percent measurement., Comment: 4 pages, 2 figures, contribution to the 2022 Gravitation session of the 56th Rencontres de Moriond

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