New horizons for fundamental physics with LISA

Arun, K. G.; Belgacem, Enis; Benkel, Robert; Bernard, Laura; Berti, Emanuele; Bertone, Gianfranco; Besançon, M.; Blas, Diego; Böhmer, Christian G.; Brito, Richard; Calcagni, Gianluca; Cárdenas-Avendaño, Alejandro; Clough, Katy; Crisostomi, Marco; Luca, Valerio De; Doneva, Daniela D.; Escoffier, S.; Ezquiaga, José María; Ferreira, Pedro G.; Fleury, Pierre; Foffa, Stefano; Franciolini, Gabriele; Frusciante, Noemi; García-Bellido, J.; Herdeiro, Carlos; Hertog, Thomas; Hinderer, Tanja; Jetzer, Philippe; Lombriser, Lucas; Maggio, Elisa; Maggiore, Michele; Mancarella, Michele; Maselli, Andrea; Nampalliwar, Sourabh; Nichols, David A.; Okounkova, Maria; Pani, Paolo; Paschalidis, Vasileios; Raccanelli, Alvise; Randall, Lisa; Renaux‐Petel, Sébastien; Riotto, Antonio; Ruiz, Milton; Saffer, Alexander; Sakellariadou, Mairi; Saltas, Ippocratis D.; Sathyaprakash, B. S.; Shao, Lijing; Sopuerta, Carlos F.; Sotiriou, Thomas P.; Stergioulas, Nikolaos; Tamanini, Nicola; Vernizzi, Filippo; Witek, Helvi; Wu, Kinwah; Yagi, Kent; Yazadjiev, Stoytcho S.; Yunes, Nicolás; Zilhão, Miguel; Afshordi, Niayesh; Angonin, Marie-Christine; Baibhav, Vishal; Barausse, Enrico; Barreiro, Tiago; Bartolo, N.; Bellomo, Nicola; Ben-Dayan, Ido; Bergshoeff, Eric; Bernuzzi, Sebastiano; Bertacca, Daniele; Bhagwat, S.; Bonga, Béatrice; Burko, Lior M.; Compère, Geoffrey; Cusin, Giulia; Silva, Antônio da; Das, Saurya; Rham, Claudia de; Destounis, Kyriakos; Dimastrogiovanni, Emanuela; Duque, Francisco; Easther, Richard; Farmer, Hontas; Fasiello, Matteo; Fisenko, Stanislav; Fransen, Kwinten; Frauendiener, Jörg; Gair, J. R.; Gergely, L.; Gerosa, Davide; Gualtieri, Leonardo; Han, Wen-Biao; Hees, A.; Helfer, Thomas; Hennig, Jörg; Jenkins, A. C.; Kajfasz, E.; Kaloper, Nemanja; Karas, Vladimír; Kavanagh, Bradley J.; Klioner, Sergei A.; Koushiappas, Savvas M.; Lagos, Macarena; Poncin-Lafitte, Christophe Le; Lobo, Francisco S. N.; Markakis, C.; Martín–Moruno, Prado; Martins, C. J. A. P.; Matarrese, S.; Mayerson, Daniel R.; Mimoso, José P.; Noller, Johannes; Nunes, Nelson J.; Oliveri, Roberto; Orlando, Giorgio; Pappas, George J.; Pikovski, Igor; Pilo, Luigi; Podolský, Jiřı́; Pratten, G.; Prokopec, Tomislav; Qi, H.; Rastgoo, Saeed; Ricciardone, Angelo; Rollo, Rocco; Rubiera-García, Diego; Sergijenko, O.; Shapiro, Stuart L.; Shoemaker, D. H.; Spallicci, A.; Stashko, O. S.; Stein, Leo C.; Tasinato, Gianmassimo; Tolley, Andrew J.; Vagenas, Elias C.; Vandoren, Stefan; Vernieri, Daniele; Vicente, Rodrigo; Wiseman, Toby; Жданов, В. І.; Zumalacárregui, Miguel

doi:10.1007/s41114-022-00036-9

Cited by 130 publications

(46 citation statements)

References 1,254 publications

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“…in constant-roll model found in Ref. [117] (see (10) in [117]) is consistent with the dip in Starobinsky model given in (35), as…”

Section: Comparison With Constant-rollsupporting

confidence: 90%

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Primordial Black Hole Formation in Starobinsky's Linear Potential Model

Wang¹

2022

Preprint

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We study the power spectrum of the comoving curvature perturbation R in the model that glues two linear potentials of different slopes, originally proposed by Starobinsky. We find that the enhanced power spectrum reaches its maximum at the wavenumber which is π times the junction scale. The peak is ∼ 2.61 times larger than the ultraviolet plateau. We also show that its near-peak behavior can be well approximated by a constant-roll model, once we define the effective ultraslow-roll e-folding number appropriately by considering the contribution from nonsingle-clock phase only. Such an abrupt transition to non-attractor phase can leave some interesting characteristic features in the energy spectrum of the scalar-induced gravitational waves, which are detectable in the space-borne interferometers if the primordial black holes generated at such a high peak are all the dark matter.

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“…in constant-roll model found in Ref. [117] (see (10) in [117]) is consistent with the dip in Starobinsky model given in (35), as…”

Section: Comparison With Constant-rollsupporting

confidence: 90%

“…The existence and abundance of such asteroid-mass PBHs can be cross-checked by the GWs induced by the scalar perturbation that collapsed into such BHs [27][28][29][30][31][32][33], which are in the millihertz frequency band. This is an important scientific goal of the space-borne interferometers like LISA [34,35],…”

Section: Introductionmentioning

confidence: 99%

Primordial Black Hole Formation in Starobinsky's Linear Potential Model

Wang¹

2022

Preprint

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“…A few years after the first gravitational wave detection from a collision of two black holes (BHs) [1] and the first image of a BH resolving its horizon scale structure [2], there is a scientific consensus about the physical reality of BHs. Yet, both the inability to observationally proof the "BH hypothesis" [3][4][5][6] and its challenging and far-reaching theoretical consequences [7][8][9], demand a thorough scrutiny of its alternatives.…”

Section: Introductionmentioning

confidence: 99%

Exotic Compact Objects and the Fate of the Light-Ring Instability

Cunha¹,

Herdeiro²,

Radu³

et al. 2022

Preprint

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Ultracompact objects with light-rings (LRs) but without an event horizon could mimic black holes (BHs) in their strong gravity phenomenology. But are such objects dynamically viable? Stationary and axisymmetric ultracompact objects that can form from smooth, quasi-Minkowski initial data must have at least one stable LR, which has been argued to trigger a spacetime instability; but its development and fate have been unknown. Using fully non-linear numerical evolutions of ultracompact bosonic stars free of any other known instabilities and introducing a novel adiabatic effective potential technique, we confirm the LRs triggered instability, identifying two possible fates: migration to non-ultracompact configurations or collapse to BHs. In concrete examples we show that typical migration/collapse time scales are not larger than ∼ 10 3 light-crossing times, unless the stable LR potential well is very shallow. Our results show that the LR instability is effective in destroying horizonless ultracompact objects that could be plausible BH imitators.

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“…Among other sources, LISA will detect the coalescence of massive black hole binaries (MBHBs) in the entire Universe up to redshift z ∼ 20 before the epoch of re-ionization [2][3][4][5][6][7] and in the range of masses ∼ [10 4 , 10 8 ] M in the nearby Universe. Detecting GWs from these sources will allow to reconstruct the merger history of MBHBs, disentangling the astrophysical processes and mechanisms driving their formation and evolution [8][9][10][11][12][13][14], perform test of general relativity [15,16] and constrain cosmological scenarios [17][18][19][20][21][22] (see [23,24] for recent reviews on cosmological and fundamental physics implications of LISA). * mangiagli@apc.in2p3.fr Compact binaries emitting GWs can be considered "standard sirens", because they provide access to the source luminosity distance d L .…”

Section: Introductionmentioning

confidence: 99%

Massive black hole binaries in LISA: multimessenger prospects and electromagnetic counterparts

Mangiagli,

Caprini,

Volonteri

et al. 2022

Preprint

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In the next decade, the Laser Interferometer Space Antenna (LISA) will detect the coalescence of massive black hole binaries (MBHBs) in the range [10 4 , 10 8 ] M , up to z ∼ 10. Their gravitational wave (GW) signal is expected to be accompanied by an electromagnetic counterpart (EMcp), generated by the gas accreting on the binary or on the remnant BH. In this work, we present the number and characteristics (such as redshift and mass distribution, apparent magnitudes or fluxes) of EMcps detectable jointly by LISA and some representative EM telescopes. We combine state-of-the-art astrophysical models for the galaxies formation and evolution to build the MBHBs catalogues, with Bayesian tools to estimate the binary sky position uncertainty from the GW signal. Exploiting additional information from the astrophysical models, such as the amount of accreted gas and the BH spins, we evaluate the expected EM emission in the soft X-ray, optical and radio bands. Overall, we predict between 7 and 21 EMcps in 4 yrs of joint observations by LISA and the considered EM facilities, depending on the astrophysical model. We also explore the impact of the hydrogen and dust obscuration of the optical and X-ray emissions, as well as of the collimation of the radio emission: these effects reduce the number to EMcps to 2 or 3, depending on the astrophysical model, again in 4 yrs of observations. Most of the EMcps are characterised by faint EM emission, challenging the observational capabilities of future telescopes. Finally, we also find that systems with multi-modal sky position posterior distributions represent only a minority of cases and do not affect significantly the number of EMcps.

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New horizons for fundamental physics with LISA

Cited by 130 publications

References 1,254 publications

Primordial Black Hole Formation in Starobinsky's Linear Potential Model

Primordial Black Hole Formation in Starobinsky's Linear Potential Model

Exotic Compact Objects and the Fate of the Light-Ring Instability

Massive black hole binaries in LISA: multimessenger prospects and electromagnetic counterparts

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