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116 results on '"black hole physic"'

1. The second data release from the European Pulsar Timing Array: IV. Implications for massive black holes, dark matter, and the early Universe

Author: Antoniadis, J, Arumugam, P, Arumugam, S, Babak, S, Bagchi, M, Bak Nielsen, A, Bassa, C, Bathula, A, Berthereau, A, Bonetti, M, Bortolas, E, Brook, P, Burgay, M, Caballero, R, Chalumeau, A, Champion, D, Chanlaridis, S, Chen, S, Cognard, I, Dandapat, S, Deb, D, Desai, S, Desvignes, G, Dhanda-Batra, N, Dwivedi, C, Falxa, M, Ferdman, R, Franchini, A, Gair, J, Goncharov, B, Gopakumar, A, Graikou, E, Grießmeier, J, Gualandris, A, Guillemot, L, Guo, Y, Gupta, Y, Hisano, S, Hu, H, Iraci, F, Izquierdo Villalba, D, Jang, J, Jawor, J, Janssen, G, Jessner, A, Joshi, B, Kareem, F, Karuppusamy, R, Keane, E, Keith, M, Kharbanda, D, Kikunaga, T, Kolhe, N, Kramer, M, Krishnakumar, M, Lackeos, K, Lee, K, Liu, K, Liu, Y, Lyne, A, Mckee, J, Maan, Y, Main, R, Mickaliger, M, Niţu, I, Nobleson, K, Paladi, A, Parthasarathy, A, Perera, B, Perrodin, D, Petiteau, A, Porayko, N, Possenti, A, Prabu, T, Quelquejay Leclere, H, Rana, P, Samajdar, A, Sanidas, S, Sesana, A, Shaifullah, G, Singha, J, Speri, L, Spiewak, R, Srivastava, A, Stappers, B, Surnis, M, Susarla, S, Susobhanan, A, Takahashi, K, Tarafdar, P, Theureau, G, Tiburzi, C, Van Der Wateren, E, Vecchio, A, Venkatraman Krishnan, V, Verbiest, J, Wang, J, Wang, L, Wu, Z, Auclair, P, Antoniadis J., Arumugam P., Arumugam S., Babak S., Bagchi M., Bak Nielsen A. S., Bassa C. G., Bathula A., Berthereau A., Bonetti M., Bortolas E., Brook P. R., Burgay M., Caballero R. N., Chalumeau A., Champion D. J., Chanlaridis S., Chen S., Cognard I., Dandapat S., Deb D., Desai S., Desvignes G., Dhanda-Batra N., Dwivedi C., Falxa M., Ferdman R. D., Franchini A., Gair J. R., Goncharov B., Gopakumar A., Graikou E., Grießmeier J. M., Gualandris A., Guillemot L., Guo Y. J., Gupta Y., Hisano S., Hu H., Iraci F., Izquierdo Villalba D., Jang J., Jawor J., Janssen G. H., Jessner A., Joshi B. C., Kareem F., Karuppusamy R., Keane E. F., Keith M. J., Kharbanda D., Kikunaga T., Kolhe N., Kramer M., Krishnakumar M. A., Lackeos K., Lee K. J., Liu K., Liu Y., Lyne A. G., McKee J. W., Maan Y., Main R. A., Mickaliger M. B., Niţu I. C., Nobleson K., Paladi A. K., Parthasarathy A., Perera B. B. P., Perrodin D., Petiteau A., Porayko N. K., Possenti A., Prabu T., Quelquejay Leclere H., Rana P., Samajdar A., Sanidas S. A., Sesana A., Shaifullah G., Singha J., Speri L., Spiewak R., Srivastava A., Stappers B. W., Surnis M., Susarla S. C., Susobhanan A., Takahashi K., Tarafdar P., Theureau G., Tiburzi C., Van Der Wateren E., Vecchio A., Venkatraman Krishnan V., Verbiest J. P. W., Wang J., Wang L., Wu Z., Auclair P., Antoniadis, J, Arumugam, P, Arumugam, S, Babak, S, Bagchi, M, Bak Nielsen, A, Bassa, C, Bathula, A, Berthereau, A, Bonetti, M, Bortolas, E, Brook, P, Burgay, M, Caballero, R, Chalumeau, A, Champion, D, Chanlaridis, S, Chen, S, Cognard, I, Dandapat, S, Deb, D, Desai, S, Desvignes, G, Dhanda-Batra, N, Dwivedi, C, Falxa, M, Ferdman, R, Franchini, A, Gair, J, Goncharov, B, Gopakumar, A, Graikou, E, Grießmeier, J, Gualandris, A, Guillemot, L, Guo, Y, Gupta, Y, Hisano, S, Hu, H, Iraci, F, Izquierdo Villalba, D, Jang, J, Jawor, J, Janssen, G, Jessner, A, Joshi, B, Kareem, F, Karuppusamy, R, Keane, E, Keith, M, Kharbanda, D, Kikunaga, T, Kolhe, N, Kramer, M, Krishnakumar, M, Lackeos, K, Lee, K, Liu, K, Liu, Y, Lyne, A, Mckee, J, Maan, Y, Main, R, Mickaliger, M, Niţu, I, Nobleson, K, Paladi, A, Parthasarathy, A, Perera, B, Perrodin, D, Petiteau, A, Porayko, N, Possenti, A, Prabu, T, Quelquejay Leclere, H, Rana, P, Samajdar, A, Sanidas, S, Sesana, A, Shaifullah, G, Singha, J, Speri, L, Spiewak, R, Srivastava, A, Stappers, B, Surnis, M, Susarla, S, Susobhanan, A, Takahashi, K, Tarafdar, P, Theureau, G, Tiburzi, C, Van Der Wateren, E, Vecchio, A, Venkatraman Krishnan, V, Verbiest, J, Wang, J, Wang, L, Wu, Z, Auclair, P, Antoniadis J., Arumugam P., Arumugam S., Babak S., Bagchi M., Bak Nielsen A. S., Bassa C. G., Bathula A., Berthereau A., Bonetti M., Bortolas E., Brook P. R., Burgay M., Caballero R. N., Chalumeau A., Champion D. J., Chanlaridis S., Chen S., Cognard I., Dandapat S., Deb D., Desai S., Desvignes G., Dhanda-Batra N., Dwivedi C., Falxa M., Ferdman R. D., Franchini A., Gair J. R., Goncharov B., Gopakumar A., Graikou E., Grießmeier J. M., Gualandris A., Guillemot L., Guo Y. J., Gupta Y., Hisano S., Hu H., Iraci F., Izquierdo Villalba D., Jang J., Jawor J., Janssen G. H., Jessner A., Joshi B. C., Kareem F., Karuppusamy R., Keane E. F., Keith M. J., Kharbanda D., Kikunaga T., Kolhe N., Kramer M., Krishnakumar M. A., Lackeos K., Lee K. J., Liu K., Liu Y., Lyne A. G., McKee J. W., Maan Y., Main R. A., Mickaliger M. B., Niţu I. C., Nobleson K., Paladi A. K., Parthasarathy A., Perera B. B. P., Perrodin D., Petiteau A., Porayko N. K., Possenti A., Prabu T., Quelquejay Leclere H., Rana P., Samajdar A., Sanidas S. A., Sesana A., Shaifullah G., Singha J., Speri L., Spiewak R., Srivastava A., Stappers B. W., Surnis M., Susarla S. C., Susobhanan A., Takahashi K., Tarafdar P., Theureau G., Tiburzi C., Van Der Wateren E., Vecchio A., Venkatraman Krishnan V., Verbiest J. P. W., Wang J., Wang L., Wu Z., and Auclair P.
Abstract: The European Pulsar Timing Array (EPTA) and Indian Pulsar Timing Array (InPTA) collaborations have measured a low-frequency common signal in the combination of their second and first data releases, respectively, with the correlation properties of a gravitational wave background (GWB). Such a signal may have its origin in a number of physical processes including a cosmic population of inspiralling supermassive black hole binaries (SMBHBs); inflation, phase transitions, cosmic strings, and tensor mode generation by the non-linear evolution of scalar perturbations in the early Universe; and oscillations of the Galactic potential in the presence of ultra-light dark matter (ULDM). At the current stage of emerging evidence, it is impossible to discriminate among the different origins. Therefore, for this paper, we consider each process separately, and investigated the implications of the signal under the hypothesis that it is generated by that specific process. We find that the signal is consistent with a cosmic population of inspiralling SMBHBs, and its relatively high amplitude can be used to place constraints on binary merger timescales and the SMBH-host galaxy scaling relations. If this origin is confirmed, this would be the first direct evidence that SMBHBs merge in nature, adding an important observational piece to the puzzle of structure formation and galaxy evolution. As for early Universe processes, the measurement would place tight constraints on the cosmic string tension and on the level of turbulence developed by first-order phase transitions. Other processes would require non-standard scenarios, such as a blue-tilted inflationary spectrum or an excess in the primordial spectrum of scalar perturbations at large wavenumbers. Finally, a ULDM origin of the detected signal is disfavoured, which leads to direct constraints on the abundance of ULDM in our Galaxy.
Published: 2024

2. pAGN: the one-stop solution for AGN disc modelling

Author: Gangardt, D, Trani, A, Bonnerot, C, Gerosa, D, Trani, AA, Gangardt, D, Trani, A, Bonnerot, C, Gerosa, D, and Trani, AA
Abstract: Models of accretion discs surrounding active galactic nuclei (AGNs) find vast applications in high-energy astrophysics. The broad strategy is to parametrize some of the key disc properties such as gas density and temperature as a function of the radial coordinate from a given set of assumptions on the underlying physics. Two of the most popular approaches in this context were presented by Sirko & Goodman and Thompson et al. We present a critical reanalysis of these widely used models, detailing their assumptions and clarifying some steps in their derivation that were previously left unsaid. Our findings are implemented in the pAGN module for the Python programming language, which is the first public implementation of these accretion-disc models. We further apply pAGN to the evolution of stellar-mass black holes embedded in AGN discs, addressing the potential occurrence of migration traps.
Published: 2024

3. Mass-redshift dependency of supermassive black hole binaries for the gravitational wave background

Author: Kozhikkal, M, Chen, S, Theureau, G, Habouzit, M, Sesana, A, Kozhikkal M. M., Chen S., Theureau G., Habouzit M., Sesana A., Kozhikkal, M, Chen, S, Theureau, G, Habouzit, M, Sesana, A, Kozhikkal M. M., Chen S., Theureau G., Habouzit M., and Sesana A.
Abstract: Studying how the black hole (BH)-(galaxy) bulge mass relation evolves with redshift provides valuable insights into the co-evolution of supermassive black holes and their host galaxies. However, obtaining accurate measurement of BH masses is challenging due to the bias towards the most massive and luminous galaxies. Instead, we focus on the BH and bulge masses as they vary with redshift using the EAGLE, Illustris, TNG100, TNG300, Horizon-AGN, and SIMBA large-scale cosmological simulations. We use an analytical astrophysical model with galaxy stellar mass function, pair fraction, merger time-scale and BH-bulge mass relation extended to include redshift evolution. The model can predict the intensity of the gravitational wave background (GWB) produced by a population of supermassive black hole binary (SMBHB) as a function of the frequency. This allows us to compare the predictions of this model with the constraints of pulsar timing array observations. Here, we employ Bayesian analysis for the parameter inference. We find that all six simulations are consistent with a range of simulated GWB spectra. By fixing the BH-bulge mass parameters to the simulations we analyse the changes in the constraints on the other astrophysical parameters. Furthermore, we also examine the variation in SMBHB merger rate with mass and redshift between these large-scale simulations.
Published: 2024

4. Identifying heavy stellar black holes at cosmological distances with next-generation gravitational-wave observatories

Author: Fairhurst, S, Mills, C, Colpi, M, Schneider, R, Sesana, A, Trinca, A, Valiante, R, Fairhurst S., Mills C., Colpi M., Schneider R., Sesana A., Trinca A., Valiante R., Fairhurst, S, Mills, C, Colpi, M, Schneider, R, Sesana, A, Trinca, A, Valiante, R, Fairhurst S., Mills C., Colpi M., Schneider R., Sesana A., Trinca A., and Valiante R.
Abstract: We investigate the detectability of single-event coalescing black hole binaries with total mass of 100–600 M at cosmological distances (5 z 20) with the next generation of terrestrial gravitational wave observatories, specifically Einstein Telescope and Cosmic Explorer. Our ability to observe these binaries is limited by the low-frequency performance of the detectors. Higher order multipoles of the gravitational wave signal are observable in these systems, and detection of such multipoles serves to both extend the mass range over which black hole binaries are observable and improve the recovery of their individual masses and redshift. For high-redshift systems of ∼ 200 M we will be able to confidently infer that the redshift is at least z = 12, and for systems of ∼ 400 M we can infer a minimum redshift of at least z = 8. We discuss the impact that these observations will have in narrowing uncertainties on the existence of the pair-instability mass gap, and their implications on the formation of the first stellar black holes that could be seeds for the growth of supermassive black holes powering high-z quasars.
Published: 2024

5. REPEATING PARTIAL DISRUPTIONS AND TWO-BODY RELAXATION

Author: Broggi, L, Stone, N, Ryu, T, Bortolas, E, Dotti, M, Bonetti, M, Sesana, A, Broggi L., Stone N. C., Ryu T., Bortolas E., Dotti M., Bonetti M., Sesana A., Broggi, L, Stone, N, Ryu, T, Bortolas, E, Dotti, M, Bonetti, M, Sesana, A, Broggi L., Stone N. C., Ryu T., Bortolas E., Dotti M., Bonetti M., and Sesana A.
Abstract: Two-body relaxation may drive stars onto near-radial orbits around a massive black hole, resulting in a tidal disruption event (TDE). In some circumstances, stars are unlikely to undergo a single terminal disruption, but rather to have a sequence of many grazing encounters with the black hole. It has long been unclear what is the physical outcome of this sequence: each of these encounters can only liberate a small amount of stellar mass, but may significantly alter the orbit of the star. We study the phenomenon of repeating partial tidal disruptions (pTDEs) by building a semi-analytical model that accounts for mass loss and tidal excitation. In the empty loss cone regime, where two-body relaxation is weak, we estimate the number of consecutive partial disruptions that a star can undergo, on average, before being significantly affected by two-body encounters. We find that in this empty loss cone regime, a star will be destroyed in a sequence of weak pTDEs, possibly explaining the tension between the low observed TDE rate and its higher theoretical estimates.
Published: 2024

6. Neural networks unveiling the properties of gravitational wave background from supermassive black hole binaries

Author: Bonetti, M, Franchini, A, Galuzzi, B, Sesana, A, Bonetti M., Franchini A., Galuzzi B. G., Sesana A., Bonetti, M, Franchini, A, Galuzzi, B, Sesana, A, Bonetti M., Franchini A., Galuzzi B. G., and Sesana A.
Abstract: Supermassive black hole binaries (SMBHBs) are binary systems formed by black holes with masses exceeding millions of solar masses, and are expected to form and evolve in the nuclei of galaxies. The extremely compact nature of these objects leads to the intense and efficient emission of gravitational waves (GWs), which can be detected by the Pulsar Timing Array (PTA) experiment in the form of a gravitational wave background (GWB); that is, a superposition of GW signals coming from different sources. The modelling of the GWB requires some assumptions as to the binary population, and exploration of the whole parameter space involved is hindered by the great computational cost involved. We trained two neural networks (NN) on a semi-analytical modelling of the GWB generated by an eccentric population of MBHBs that interact with the stellar environment. We then used the NN to predict the characteristics of the GW signal in regions of the parameter space that we did not sample analytically. The developed framework allows us to quickly predict the amplitude, shape, and variance of the GWB signals produced in different realisations of the universe.
Published: 2024

7. Emission signatures from sub-parsec post-Newtonian binaries embedded in circumbinary discs

Author: Franchini, A, Bonetti, M, Lupi, A, Sesana, A, Franchini A., Bonetti M., Lupi A., Sesana A., Franchini, A, Bonetti, M, Lupi, A, Sesana, A, Franchini A., Bonetti M., Lupi A., and Sesana A.
Abstract: We studied the dynamical evolution of quasi-circular, equal-mass massive black hole binaries embedded in circumbinary discs from separations of ∼100 Rg down to the merger, following the post merger evolution. The binary orbit evolves owing to the presence of the gaseous disc and the addition of post-Newtonian (PN) corrections up to the 2.5 PN order, therefore including the dissipative gravitational wave back reaction. We investigated two cases of relatively cold and warm circumbinary discs, with aspect ratios of H/R = 0.03, 0.1, respectively, employing 3D hyper-Lagrangian resolution simulations with the GIZMO-MFM code. We extracted spectral energy distributions and light curves in different frequency bands (i.e. X-ray, optical, and UV) from the simulations. We find a clear two orders of magnitude drop in the X-ray flux right before merger if the disc is warm, while we identify a significant increase in the UV flux regardless of the disc temperature. The optical flux shows clear distinctive modulations on the binary orbital period and on the cavity edge period, regardless of the disc temperature. We find that the presence of a cold disc can accelerate the coalescence of the binary by up to 130 s over the last five days of inspiral, implying a phase shift accumulation of about 0.14 radians compared to the binary evolution in vacuum. These differences are triggered by the presence of the gaseous disc and might have implications on the waveforms that can be detected in principle. We discuss the implications that these distinctive signatures might have for existing and upcoming time domain surveys and for multi-messenger astronomy.
Published: 2024

8. Sustained super-Eddington accretion in high-redshift quasars

Author: Lupi, A, Quadri, G, Volonteri, M, Colpi, M, Regan, J, Lupi, Alessandro, Quadri, Giada, Volonteri, Marta, Colpi, Monica, Regan, John A., Lupi, A, Quadri, G, Volonteri, M, Colpi, M, Regan, J, Lupi, Alessandro, Quadri, Giada, Volonteri, Marta, Colpi, Monica, and Regan, John A.
Abstract: Observations of z ≳ 6 quasars provide information on the early evolution of the most massive black holes (MBHs) and galaxies. Current observations, able to trace both gas and stellar properties, reveal a population of MBHs that is significantly more massive than expected from the local MBH-stellar mass relation. The population lies on, but mostly above, the relation observed in the nearby Universe. This suggests that these objects grew very rapidly. To explain their presence when the Universe was less than 1 Gyr old and to assess the physical conditions for their rapid growth, we explored whether episodes of accretion above the Eddington limit can occur across cosmic epochs. By employing state-of-the-art high-resolution cosmological zoom-in simulations of a z ∼ 7 quasar, where different accretion regimes are included consistently, together with their associated radiative and kinetic feedback, we show that super-Eddington phases can be sustained for relatively long timescales (tens of millions of years). This allows the MBH to rapidly grow by up to three orders of magnitude, depending on the strength of the kinetic feedback. We also show by means of a semianalytic calculation that the MBH spin remains moderate and does not take on extremely high values during the super-Eddington phases. This results in a lower feedback efficiency, which may allow the rapid growth required to explain over-massive high-redshift MBHs.
Published: 2024

9. Eccentricity evolution of PTA sources from cosmological initial conditions

Author: Fastidio, F, Gualandris, A, Sesana, A, Bortolas, E, Dehnen, W, Fastidio F., Gualandris A., Sesana A., Bortolas E., Dehnen W., Fastidio, F, Gualandris, A, Sesana, A, Bortolas, E, Dehnen, W, Fastidio F., Gualandris A., Sesana A., Bortolas E., and Dehnen W.
Abstract: Recent results from pulsar timing arrays (PTAs) show evidence for a gravitational wave background (GWB) consistent with a population of unresolved supermassive black hole (SMBH) binaries (BHBs). While the data do not yet constrain the slope of the spectrum, this appears to flatten at the lowest frequencies, deviating from the power-law shape expected for circular binaries evolving solely due to gravitational wave (GW) emission. Interestingly, such flattening can be explained with a population of eccentric rather than circular binaries. The eccentricity of BHBs is notoriously difficult to predict based simply on the parameters of the host galaxies and the initial galactic orbit, as it is subject to stochastic effects. We study the evolution of the eccentricity of BHBs formed in galactic mergers with cosmological initial conditions from pairing to coalescence, with a focus on potential PTA sources. We select galactic mergers from the IllustrisTNG100-1 simulation and re-simulate them at high resolution with the N-body code griffin down to binary separations of the order of a parsec. We then estimate coalescence time-scales with a semi-analytical model of the evolution under the effects of GW emission and stellar hardening. We find that most mergers in IllustrisTNG100-1 occur on highly eccentric orbits, and that the eccentricity of BHBs at binary formation correlates with the initial eccentricity of the merger, if this is no larger than approximately 0.9. For extremely eccentric mergers, the binaries tend to form with modest eccentricities. We discuss the implications of these results on the interpretation of the observed GWB.
Published: 2024

10. Testing strengths, limitations, and biases of current pulsar timing arrays'detection analyses on realistic data

Author: Valtolina, S, Shaifullah, G, Samajdar, A, Sesana, A, Valtolina S., Shaifullah G., Samajdar A., Sesana A., Valtolina, S, Shaifullah, G, Samajdar, A, Sesana, A, Valtolina S., Shaifullah G., Samajdar A., and Sesana A.
Abstract: State-of-the-art searches for gravitational waves (GWs) in pulsar timing array (PTA) datasets model the signal as an isotropic, Gaussian, and stationary process described by a power law. In practice, none of these properties are expected to hold for an incoherent superposition of GWs generated by a cosmic ensemble of supermassive black hole binaries (SMBHBs). This stochastic signal is usually referred to as the GW background (GWB) and is expected to be the primary signal in the PTA band. We performed a systematic investigation of the performance of current search algorithms, using a simple power-law model to characterise GW signals in realistic datasets. We used, as the baseline dataset, synthetic realisations of timing residuals mimicking the European PTA (EPTA) second data release (DR2). Thus, we included in the dataset uneven time stamps, achromatic and chromatic red noise, and multi-frequency observations. We then injected timing residuals from an ideal isotropic, Gaussian, single power-law stochastic process and from a realistic population of SMBHBs, performing a methodical investigation of the recovered signal. We found that current search models are efficient at recovering the GW signal, but several biases can be identified due to the signal-template mismatch, which we identified via probability-probability (P- P) plots and quantified using Kolmogorov-Smirnov (KS) statistics. We discuss our findings in light of the signal observed in the EPTA DR2 and corroborate its consistency with a SMBHB origin.
Published: 2024

11. Multi-messenger prospects for black hole-neutron star mergers in the O4 and O5 runs

Author: Colombo, A, Duqué, R, Sharan Salafia, O, Broekgaarden, F, Iacovelli, F, Mancarella, M, Andreoni, I, Gabrielli, F, Ragosta, F, Ghirlanda, G, Fragos, T, Levan, A, Piranomonte, S, Melandri, A, Giacomazzo, B, Colpi, M, Alberto Colombo, Raphaël Duqué, Om Sharan Salafia, Floor S. Broekgaarden, Francesco Iacovelli, Michele Mancarella, Igor Andreoni, Francesco Gabrielli, Fabio Ragosta, Giancarlo Ghirlanda, Tassos Fragos, Andrew J. Levan, Silvia Piranomonte, Andrea Melandri, Bruno Giacomazzo, Monica Colpi, Colombo, A, Duqué, R, Sharan Salafia, O, Broekgaarden, F, Iacovelli, F, Mancarella, M, Andreoni, I, Gabrielli, F, Ragosta, F, Ghirlanda, G, Fragos, T, Levan, A, Piranomonte, S, Melandri, A, Giacomazzo, B, Colpi, M, Alberto Colombo, Raphaël Duqué, Om Sharan Salafia, Floor S. Broekgaarden, Francesco Iacovelli, Michele Mancarella, Igor Andreoni, Francesco Gabrielli, Fabio Ragosta, Giancarlo Ghirlanda, Tassos Fragos, Andrew J. Levan, Silvia Piranomonte, Andrea Melandri, Bruno Giacomazzo, and Monica Colpi
Abstract: The existence of merging black hole-neutron star (BHNS) binaries has been ascertained through the observation of their gravitational wave (GW) signals. However, to date, no definitive electromagnetic (EM) emission has been confidently associated with these mergers. Such an association could help unravel crucial information on these systems, for example, their BH spin distribution, the equation of state (EoS) of the neutron star and the rate of heavy element production. We modeled the multi-messenger (MM) emission from BHNS mergers detectable during the fourth (O4) and fifth (O5) observing runs of the LIGO-Virgo-KAGRA (LVK) GW detector network in order to provide detailed predictions that can help enhance the effectiveness of observational efforts and extract the highest possible scientific information from such remarkable events. Our methodology is based on a population synthesis approach, which includes the modeling of the signal-To-noise ratio of the GW signal in the detectors, the GW-inferred sky localization of the source, the kilonova (KN) optical and near-infrared light curves, the relativistic jet gamma-ray burst (GRB) prompt emission peak photon flux, and the GRB afterglow light curves in the radio, optical, and X-ray bands. The resulting prospects for BHNS MM detections during O4 are not promising, with an LVK GW detection rate of 15:0+15:48:8 yr-1, but joint MM rates of ∼10-1 yr-1 for the KN and 10-2 yr1 for the jet-related emission. In O5, we found an overall increase in expected detection rates by around an order of magnitude, owing to both the enhanced sensitivity of the GW detector network and the coming online of future EM facilities. Considering variations in the NS EoS and BH spin distribution, we find that the detection rates can increase further by up to a factor of several tens. Finally, we discuss direct searches for the GRB radio afterglow with large field-of-view instruments during O5 and beyond as a new possible follow-up strategy in the cont
Published: 2024

12. Dynamics of tidal disruptions and extreme mass ratio inspirals in galactic nuclei

Author: Broggi, L, SESANA, ALBERTO, DOTTI, MASSIMO, BROGGI, LUCA, Broggi, L, SESANA, ALBERTO, DOTTI, MASSIMO, and BROGGI, LUCA
Abstract: I buchi neri sono oggetti estremi e affascinanti dell'astrofisica contemporanea. Sono la fonte di gravità più potente che si possa trovare in natura e rivelano la loro presenza attraverso i stravolgenti effetti che hanno sull'ambiente che li circonda. Uno di questi effetti è la distruzione delle stelle che si avvicinano troppo all'orizzonte degli eventi. Questo è causato dalla forza mareale che un buco nero massiccio (MBH) esercita sulla struttura stellare, distruggendola e provocando la produzione di brillanti transienti luminosi, che durano da giorni a mesi. Questo fenomeno è noto come tidal disruption event (TDE). I buchi neri stellari e le stelle di neutroni possono resistere alle forze mareali, grazie alla loro struttura compatta, e possono avvicinarsi al buco nero fino al limite dell'ultima orbita stabile prescritto dalla relatività generale. Una volta raggiunto questo punto, vengono infine inghiottiti dal MBH in un evento noto come plunge. A seconda di come avviene, si può trattare di un direct plunge (DP) se la cattura avviene su poche orbite, oppure di una lunga fase di spiraleggiamento dell'oggetto stellare su molte orbite. Quest'ultimo tipo di eventi è noto come extreme mass ratio inspiral (EMRI), a causa della grande differenza di massa tra i due oggetti. La mia ricerca si concentra sulla costruzione di strumenti teorici e numerici avanzati per prevedere i tassi di TDE, DP e EMRI in galassie realistiche; questi possono essere successivamente trasformati in tassi di eventi dell'Universo osservabile e, in ultima analisi, in tassi di rilevamento previsti. Confrontando questi tassi con le osservazioni reali, si possono dedurre le proprietà della popolazione sottostante di MBH. Ho sviluppato il primo codice pubblico per risolvere l'evoluzione statistica dei nuclei galattici, gli ambienti densi e affollati in cui si produce la maggior parte di questi eventi. Con questo codice ho simulato una serie di nuclei galattici popolati da stelle e buchi neri st, Black holes are extreme and fascinating objects of contemporary astrophysics. They are the strongest source of gravity we can find in nature and they unveil their presence through the powerful effects they exert on the surrounding environment. One of these effects is represented by the disruption of those starts that got too close to the event horizon. This is caused by the strong tidal force that a massive black hole (MBH) exert on the stellar structure, ultimately tearing it apart and resulting in the production of luminous transient flares, lasting days to months. This phenomenon is known as tidal disruption event (TDE). Stellar black holes and neutron stars can withstand tidal forces, because of their compact structure, and can approach the black hole as close as the last stable orbit limit prescribed by general relativity. Once this point is reached, they are eventually swallowed by the MBH in a plunge event. Depending on how the plunge occurs, they can be direct plunges (DPs) if the capture happens over few orbits, or a long inspiralling of the stellar object over many orbits. This latter kind of events are known as extreme mass ratio inspiral (EMRI) due to the large difference in the mass of the two objects. My research is focused on building advanced theoretical and numerical tools to predict the rates of TDEs, DPs and EMRIs in realistic galaxies; these can be later turned into event rates of the observable Universe and ultimately expected detection rates. By comparing these rates with actual observations, one can infer properties of the underlying population of MBHs. I have developed the first public code to solve the statistical evolution of galactic nuclei, the dense and crowded environments where the majority of these events are produced. With this code, I have simulated a variety of galactic nuclei populated of stars and stellar black holes. This allowed me to fully characterize their evolution governed by mass segregation, and the formation rate of TDE
Published: 2024

13. Dynamical evolution of massive black hole pairs in the presence of spin-dependent radiative feedback

Author: Bollati, F, Lupi, A, Dotti, M, Haardt, F, Bollati F., Lupi A., Dotti M., Haardt F., Bollati, F, Lupi, A, Dotti, M, Haardt, F, Bollati F., Lupi A., Dotti M., and Haardt F.
Abstract: The putative ubiquity of massive black holes (MBHs) at the centre of galaxies, and the hierarchical progress of structure formation along the cosmic history, together necessarily imply the existence of a large population of cosmic MBH binaries. Such systems are understood to be the loudest sources of gravitational waves at MHz frequencies, the regime that will be probed by the next Laser Interferometer Space Antenna. It has been proposed that the rate at which MBHs pair and then bind to form binaries is critically dependent upon the feedback exerted by the MBHs on the surrounding gaseous environment. Using the publicly available code GIZMO, we perform a suite of simulations aimed at studying the dynamics of an MBH pair embedded in a gaseous disc on ∼100-pc scale. By means of dedicated modules, we follow the dynamics of MBHs in the presence of different spin-dependent radiative feedback models, and compare the results to a benchmark case with no feedback at all. Our main finding is that feedback causes the secondary MBH to shrink its orbit at a reduced pace, when compared with models where feedback is absent. Moreover, such slower inspiral occurs on eccentric orbits, as feedback has the net effect of hampering the circularization process. Though idealized in many aspects, our study highlights and quantities the importance of including spin-dependent feedback recipes in hydrodynamic simulations of MBH pairs, and ultimately in assessing the cosmological coalescence rate of such systems in view of their detection through gravitational waves.
Published: 2023

14. Partial stellar tidal disruption events and their rates

Author: Bortolas, E, Ryu, T, Broggi, L, Sesana, A, Elisa Bortolas, Taeho Ryu, Luca Broggi, Alberto Sesana, Bortolas, E, Ryu, T, Broggi, L, Sesana, A, Elisa Bortolas, Taeho Ryu, Luca Broggi, and Alberto Sesana
Abstract: Tidal disruption events (TDEs) of stars operated by massive black holes (MBHs) will be detected in thousands by upcoming facilities such as the Vera Rubin Observatory. In this work, we assess the rates of standard total TDEs, destroying the entire star, and partial TDEs, in which a stellar remnant survives the interaction, by solving 1D Fokker-Planck equations. Our rate estimates are based on a novel definition of the loss cone whose size is commensurate with the largest radius at which partial disruptions can occur, as motivated by relativistic hydrodynamical simulations. Our novel approach unveils two important results. First, partial TDEs can be more abundant than total disruptions by a factor of a few to a few tens. Second, the rates of complete stellar disruptions can be overestimated by a factor of a few to a few tens if one neglects partial TDEs, as we find that many of the events classified as total disruptions in the standard framework are in fact partial TDEs. Accounting for partial TDEs is particularly relevant for galaxies harbouring a nuclear stellar cluster featuring many events coming from the empty loss cone. Based on these findings, we stress that partial disruptions should be considered when constraining the luminosity function of TDE flares; accounting for this may reconcile the theoretically estimated TDE rates with the observed ones.
Published: 2023

15. Quasi-periodic eruptions from impacts between the secondary and a rigidly precessing accretion disc in an extreme mass-ratio inspiral system

Author: Franchini, A, Bonetti, M, Lupi, A, Miniutti, G, Bortolas, E, Giustini, M, Dotti, M, Sesana, A, Arcodia, R, Ryu, T, Franchini, A, Bonetti, M, Lupi, A, Miniutti, G, Bortolas, E, Giustini, M, Dotti, M, Sesana, A, Arcodia, R, and Ryu, T
Abstract: X-ray quasi-periodic eruptions (QPEs) represent a recently discovered example of extreme X-ray variability associated with supermassive black holes. These are high-amplitude bursts recurring every few hours that are detected in the soft X-ray band from the nuclei of nearby galaxies whose optical spectra lack the broad emission lines typically observed in unobscured active galaxies. The physical origin of this new X-ray variability phenomenon is still unknown and several theoretical models have been presented. However, no attempt has been made so far to account for the varying QPE recurrence time and luminosity in individual sources, nor for the diversity of the QPE phenomenology in the different known erupters. We present a semi-analytical model based on an extreme mass-ratio inspiral (EMRI) system where the secondary intersects, along its orbit, a rigidly precessing accretion disc surrounding the primary. We assume that QPEs result from emission from an adiabatically expanding, initially optically thick gas cloud expelled from the disc plane at each impact. We produced synthetic X-ray light curves, which we then compared with X-ray data from four QPE sources: GSN 069, eRO-QPE1, eRO-QPE2, and RX J1301.9+2747. Our model aptly reproduces the diversity of QPE properties between the considered objects and it is also able to naturally account for the varying QPE amplitudes and recurrence times in individual sources. Future implementations will enable us to refine the match with the data and to estimate the system parameters precisely, making additional use of multi-epoch QPE data. We briefly discuss the nature of the secondary object, as well as the possible implications of our findings for the EMRI population at large.
Published: 2023

16. Chasing supermassive black hole merging events with Athena and LISA

Author: Piro, L, Colpi, M, Aird, J, Mangiagli, A, Fabian, A, Guainazzi, M, Marsat, S, Sesana, A, Mcnamara, P, Bonetti, M, Rossi, E, Tanvir, N, Baker, J, Belanger, G, Dal Canton, T, Jennrich, O, Katz, M, Luetzgendorf, N, Piro L., Colpi M., Aird J., Mangiagli A., Fabian A. C., Guainazzi M., Marsat S., Sesana A., McNamara P., Bonetti M., Rossi E. M., Tanvir N. R., Baker J. G., Belanger G., Dal Canton T., Jennrich O., Katz M. L., Luetzgendorf N., Piro, L, Colpi, M, Aird, J, Mangiagli, A, Fabian, A, Guainazzi, M, Marsat, S, Sesana, A, Mcnamara, P, Bonetti, M, Rossi, E, Tanvir, N, Baker, J, Belanger, G, Dal Canton, T, Jennrich, O, Katz, M, Luetzgendorf, N, Piro L., Colpi M., Aird J., Mangiagli A., Fabian A. C., Guainazzi M., Marsat S., Sesana A., McNamara P., Bonetti M., Rossi E. M., Tanvir N. R., Baker J. G., Belanger G., Dal Canton T., Jennrich O., Katz M. L., and Luetzgendorf N.
Abstract: The European Space Agency is studying two large-class missions bound to operate in the decade of the 30s, and aiming at investigating the most energetic and violent phenomena in the Universe. Athena is poised to study the physical conditions of baryons locked in large-scale structures from the epoch of their formation, as well as to yield an accurate census of accreting supermassive black holes down to the epoch of reionization; LISA will extend the hunt for Gravitational Wave (GW) events to the hitherto unexplored mHz regime. We discuss in this paper the science that their concurrent operation could yield, and present possible Athena observational strategies. We focus on Supermassive (M≾ 107 M☉) Black Hole Mergers (SMBHMs), potentially accessible to Athena up to z ∼ 2. The simultaneous measurement of their electromagnetic (EM) and GW signals may enable unique experiments in the domains of astrophysics, fundamental physics, and cosmography, such as the magnetohydrodynamics of fluid flows in a rapidly variable space–time, the formation of coronae and jets in Active Galactic Nuclei, and the measurement of the speed of GW, among others. Key to achieve these breakthrough results will be the LISA capability of locating a SMBHM event with an error box comparable to, or better than the field-of-view of the Athena Wide Field Imager (≃ 0.4 deg2) and Athena capability to slew fast to detect the source during the inspiral phase and the post-merger phase. Together, the two observatories will open in principle the exciting possibility of truly concurrent EM and GW studies of the SMBHMs.
Published: 2023

17. Optical follow-up of the tick-tock massive black hole binary candidate

Author: Dotti, M, Bonetti, M, Rigamonti, F, Bortolas, E, Fossati, M, Decarli, R, Covino, S, Lupi, A, Franchini, A, Sesana, A, Calderone, G, Massimo Dotti, Matteo Bonetti, Fabio Rigamonti, Elisa Bortolas, Matteo Fossati, Roberto Decarli, Stefano Covino, Alessandro Lupi, Alessia Franchini, Alberto Sesana, Giorgio Calderone, Dotti, M, Bonetti, M, Rigamonti, F, Bortolas, E, Fossati, M, Decarli, R, Covino, S, Lupi, A, Franchini, A, Sesana, A, Calderone, G, Massimo Dotti, Matteo Bonetti, Fabio Rigamonti, Elisa Bortolas, Matteo Fossati, Roberto Decarli, Stefano Covino, Alessandro Lupi, Alessia Franchini, Alberto Sesana, and Giorgio Calderone
Abstract: The observation of a population of massive black hole binaries (MBHBs) is key for our complete understanding of galaxy mergers and for the characterization of the expected gravitational waves (GWs) signal. However, MBHBs still remain elusive with only a few candidates proposed to date. Among these, SDSSJ143016.05 + 230344.4 (’tick-tock’ hereafter) is the only candidate with a remarkably well sampled light curve showing a clear reduction of the modulation period and amplitude over three years of observations. This particular feature has been recently claimed to be the signature of a MBHB that is about to merge. In this paper, we provide an optical follow-up of the tick-tock source using the Rapid Eye Mount (REM) telescope. The decreasing luminosity observed in our follow up is hardly explained within the binary scenario. We speculate about an alternative scenario that might explain the observed light curve through relativistic Lense-Thirring precession of an accretion disc around a single massive black hole.
Published: 2023

18. Unveiling the hosts of parsec-scale massive black hole binaries: morphology and electromagnetic signatures

Author: IZQUIERDO VILLALBA, D, Sesana, A, Colpi, M, David Izquierdo-Villalba, Alberto Sesana, Monica Colpi, IZQUIERDO VILLALBA, D, Sesana, A, Colpi, M, David Izquierdo-Villalba, Alberto Sesana, and Monica Colpi
Abstract: Parsec-scale massive black hole binaries (MBHBs) are expected to form in hierarchical models of structure formation. Even though different observational strategies have been designed to detect these systems, a theoretical study is a further guide for their search and identification. In this work, we investigate the hosts properties and the electromagnetic signatures of massive black holes gravitationally bound on parsec-scales with primary mass > 107 M☉. For that, we construct a full-sky light-cone by the use of the semi-analytical model L-Galaxies in which physically motivated prescriptions for the formation and evolution of MBHBs have been included. Our predictions show that the large majority of the MBHBs are placed either in spiral galaxies with a classical bulge structure or in elliptical galaxies. Besides, the scaling relations followed by MBHBs are indistinguishable from the ones of single massive black holes. We find that the occupation fraction of parsec-scale MBHBs reaches up to ∼ 50 per cent in galaxies with Mstellar > 1011 M☉ and drops below 10 per cent for Mstellar < 1011 M☉. Our model anticipates that the majority of parsec-scale MBHBs are unequal mass systems and lie at z ∼ 0.5, with ∼ 20 objects per deg2 in the sky. However, most of these systems are inactive, and only 1–0.1 objects per deg2 have an electromagnetic counterpart with a bolometric luminosity in excess of 1043 erg s−1. Very luminous phases of parsec-scale MBHBs are more common at z > 1, but the number of binaries per deg2 is ≤ 0.01 at Lbol > 1045 erg s−1.
Published: 2023

19. Galaxy fields of LISA massive black hole mergers in a simulated universe

Author: Lops, G, Izquierdo-Villalba, D, Colpi, M, Bonoli, S, Sesana, A, Mangiagli, A, Lops G., Izquierdo-Villalba D., Colpi M., Bonoli S., Sesana A., Mangiagli A., Lops, G, Izquierdo-Villalba, D, Colpi, M, Bonoli, S, Sesana, A, Mangiagli, A, Lops G., Izquierdo-Villalba D., Colpi M., Bonoli S., Sesana A., and Mangiagli A.
Abstract: Laser Interferometer Space Antenna (LISA) will extend the search for gravitational waves (GWs) at 0.1 − 100 mHz where loud signals from coalescing binary black holes of 104 − 107 M are expected. Depending on their mass and luminosity distance, the uncertainty in the LISA sky-localization decreases from hundreds of deg2 during the inspiral phase to fractions of a deg2 after the merger. By using the semi-analytical model L-Galaxies applied to the Millennium-I merger trees, we generate a simulated universe to identify the hosts of z ≤ 3 coalescing binaries with total mass of 3 × 105, 3 × 106, and 3 × 107 M, and varying mass ratio. We find that, even at the time of merger, the number of galaxies around the LISA sources is too large (<~ 102) to allow direct host identification. However, if an X-ray counterpart is associated to the GW sources at z < 1, all LISA fields at merger are populated by <~ 10 active galactic nuclei (AGNs) emitting above ∼ 10−17 erg cm−2 s−1. For sources at higher redshifts, the poorer sky-localization causes this number to increase up to ∼ 103. Archival data from eRosita will allow discarding ∼ 10 per cent of these AGNs, being too shallow to detect the dim X-ray luminosity of the GW sources. Inspiralling binaries in an active phase with masses <~ 106 M at z ≤ 0.3 can be detected, as early as 10 h before the merger, by future X-ray observatories in less than a few minutes. For these systems, <~ 10 AGNs are within the LISA sky-localization area. Finally, the LISA-Taiji network would guarantee the identification of an X-ray counterpart 10 h before merger for all binaries at z <~ 1.
Published: 2023

20. Revised event rates for extreme and extremely large mass-ratio inspirals

Author: Vazquez-Aceves, V, Zwick, L, Bortolas, E, Capelo, P, Amaro Seoane, P, Mayer, L, Chen, X, Vazquez-Aceves V., Zwick L., Bortolas E., Capelo P. R., Amaro Seoane P., Mayer L., Chen X., Vazquez-Aceves, V, Zwick, L, Bortolas, E, Capelo, P, Amaro Seoane, P, Mayer, L, Chen, X, Vazquez-Aceves V., Zwick L., Bortolas E., Capelo P. R., Amaro Seoane P., Mayer L., and Chen X.
Abstract: One of the main targets of the Laser Interferometer Space Antenna (LISA) is the detection of extreme mass-ratio inspirals (EMRIs) and extremely large mass-ratio inspirals (X-MRIs). Their orbits are expected to be highly eccentric and relativistic when entering the LISA band. Under these circumstances, the inspiral time-scale given by Peters' formula loses precision and the shift of the last-stable orbit (LSO) caused by the massive black hole spin could influence the event rates estimate. We re-derive EMRIs and X-MRIs event rates by implementing two different versions of a Kerr loss-cone angle that includes the shift in the LSO, and a corrected version of Peters' time-scale that accounts for eccentricity evolution, 1.5 post-Newtonian hereditary fluxes, and spin-orbit coupling. The main findings of our study are summarized as follows: (1) implementing a Kerr loss-cone changes the event rates by a factor ranging between 0.9 and 1.1; (2) the high-eccentricity limit of Peters' formula offers a reliable inspiral time-scale for EMRIs and X-MRIs, resulting in an event-rate estimate that deviates by a factor of about 0.9-3 when compared to event rates computed with the corrected version of Peters' time-scale and the usual loss-cone definition. (3) Event-rate estimates for systems with a wide range of eccentricities should be revised. Peters' formula overestimates the inspiral rates of highly eccentric systems by a factor of about 8-30 compared to the corrected values. Besides, for e0 ≲ 0.8, implementing the corrected version of Peters' formula is necessary to obtain accurate estimates.
Published: 2022

21. Tidal disruption events in post-starburst galaxies: The importance of a complete stellar mass function

Author: Bortolas, E, Bortolas E., Bortolas, E, and Bortolas E.
Abstract: A tidal disruption event (TDE) occurs when a star is destroyed by the strong tidal shear of a massive black hole (MBH). The accumulation of TDE observations over the last years has revealed that post-starburst galaxies are significantly overrepresented in the sample of TDE hosts. Here we address the post-starburst preference by investigating the decline of TDE rates in a Milky-Way like nuclear stellar cluster featuring either a monochromatic (1 M⊙) or a complete, evolved stellar mass function. In the former case, the decline of TDE rates with time is very mild, and generally up to a factor of a few in 10 Gyr. Conversely, if a complete mass function is considered, a strong TDE burst over the first 0.1-1 Gyr is followed by a considerable rate drop, by at least an order of magnitude over 10 Gyr. The decline starts after a mass segregation time-scale, and it is more pronounced assuming a more top-heavy initial mass function and/or an initially denser nucleus. Our results thus suggest that the post-starburst preference can be accounted for in realistic systems featuring a complete stellar mass function, even in moderately dense galactic nuclei. Overall, our findings support the idea that starbursting galactic nuclei are characterized by a top-heavy initial mass function; we speculate that accounting for this can reconcile the discrepancy between observed and theoretically predicted TDE rates even in quiescent galaxies.
Published: 2022

22. Search for intermediate-mass black hole binaries in the third observing run of Advanced LIGO and Advanced Virgo

Author: Abbott, R, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adhikari, N, Adhikari, R, Adya, V, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Ando, M, Andrade, T, Andres, N, Andric, T, Angelova, S, Ansoldi, S, Antelis, J, Antier, S, Appert, S, Arai, K, Arai, Y, Araki, S, Araya, A, Araya, M, Areeda, J, Arene, M, Aritomi, N, Arnaud, N, Aronson, S, Arun, K, Asada, H, Asali, Y, Ashton, G, Aso, Y, Assiduo, M, Aston, S, Astone, P, Aubin, F, Austin, C, Babak, S, Badaracco, F, Bader, M, Badger, C, Bae, S, Bae, Y, Baer, A, Bagnasco, S, Bai, Y, Baiotti, L, Baird, J, Bajpai, R, Ball, M, Ballardin, G, Ballmer, S, Balsamo, A, Baltus, G, Banagiri, S, Bankar, D, Barayoga, J, Barbieri, C, Barish, B, Barker, D, Barneo, P, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, M, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Baylor, A, Bazzan, M, Becsy, B, Bedakihale, V, Bejger, M, Belahcene, I, Benedetto, V, Beniwal, D, Bennett, T, Bentley, J, Benyaala, M, Bergamin, F, Berger, B, Bernuzzi, S, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Beveridge, D, Bhandare, R, Bhardwaj, U, Bhattacharjee, D, Bhaumik, S, Bilenko, I, Billingsley, G, Bini, S, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Biswas, B, Bitossi, M, Bizouard, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Bobba, F, Bode, N, Boer, M, Bogaert, G, Boldrini, M, Bonavena, L, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, N, Bose, S, Bossilkov, V, Boudart, V, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branch, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Bruno, G, Bruntz, R, Bryant, J, Bulik, T, Bulten, H, Buonanno, A, Buscicchio, R, Buskulic, D, Buy, C, Byer, R, Cadonati, L, Cagnoli, G, Cahillane, C, Calderon Bustillo, J, Callaghan, J, Callister, T, Calloni, E, Cameron, J, Camp, J, Canepa, M, Canevarolo, S, Cannavacciuolo, M, Cannon, K, Cao, H, Cao, Z, Capocasa, E, Capote, E, Carapella, G, Carbognani, F, Carlin, J, Carney, M, Carpinelli, M, Carrillo, G, Carullo, G, Carver, T, Casanueva Diaz, J, Casentini, C, Castaldi, G, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Ceasar, M, Cella, G, Cerda-Duran, P, Cesarini, E, Chaibi, W, Chakravarti, K, Chalathadka Subrahmanya, S, Champion, E, Chan, C, Chan, K, Chan, M, Chandra, K, Chanial, P, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, C, Chatterjee, D, Chaturvedi, M, Chaty, S, Chatziioannou, K, Chen, C, Chen, H, Chen, J, Chen, K, Chen, X, Chen, Y, Chen, Z, Cheng, H, Cheong, C, Cheung, H, Chia, H, Chiadini, F, Chiang, C, Chiarini, G, Chierici, R, Chincarini, A, Chiofalo, M, Chiummo, A, Cho, G, Cho, H, Choudhary, R, Choudhary, S, Christensen, N, Chu, H, Chu, Q, Chu, Y, Chua, S, Chung, K, Ciani, G, Ciecielag, P, Cieslar, M, Cifaldi, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, E, Clark, J, Clarke, L, Clearwater, P, Clesse, S, Cleva, F, Coccia, E, Codazzo, E, Cohadon, P, Cohen, D, Cohen, L, Colleoni, M, Collette, C, Colombo, A, Colpi, M, Compton, C, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrion, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coulon, J, Countryman, S, Cousins, B, Couvares, P, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Criswell, A, Croquette, M, Crowder, S, Cudell, J, Cullen, T, Cumming, A, Cummings, R, Cunningham, L, Cuoco, E, Curylo, M, Dabadie, P, Dal Canton, T, Dall'Osso, S, Dalya, G, Dana, A, Daneshgaran Bajastani, L, D'Angelo, B, Danilishin, S, D'Antonio, S, Danzmann, K, Darsow-Fromm, C, Dasgupta, A, Datrier, L, Datta, S, Dattilo, V, Dave, I, Davier, M, Davies, G, Davis, D, Davis, M, Daw, E, Dean, R, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Favero, V, De Lillo, F, De Lillo, N, Del Pozzo, W, De Marchi, L, De Matteis, F, D'Emilio, V, Demos, N, Dent, T, Depasse, A, De Pietri, R, De Rosa, R, De Rossi, C, De Salvo, R, De Simone, R, Dhurandhar, S, Diaz, M, Diaz-Ortiz, M, Didio, N, Dietrich, T, Di Fiore, L, Di Fronzo, C, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, D'Onofrio, L, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Drago, M, Driggers, J, Drori, Y, Ducoin, J, Dupej, P, Durante, O, D'Urso, D, Duverne, P, Dwyer, S, Eassa, C, Easter, P, Ebersold, M, Eckhardt, T, Eddolls, G, Edelman, B, Edo, T, Edy, O, Effler, A, Eguchi, S, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Ejlli, A, Engelby, E, Enomoto, Y, Errico, L, Essick, R, Estelles, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Ewing, B, Fafone, 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J., Kapasi D. P., Karat S., Karathanasis C., Karki S., Kashyap R., Kasprzack M., Kastaun W., Katsanevas S., Katsavounidis E., Katzman W., Kaur T., Kawabe K., Kawaguchi K., Kawai N., Kawasaki T., Kefelian F., Keitel D., Key J. S., Khadka S., Khalili F. Y., Khan S., Khazanov E. A., Khetan N., Khursheed M., Kijbunchoo N., Kim C., Kim J. C., Kim J., Kim K., Kim W. S., Kim Y. -M., Kimball C., Kimura N., Kinley-Hanlon M., Kirchhoff R., Kissel J. S., Kita N., Kitazawa H., Kleybolte L., Klimenko S., Knee A. M., Knowles T. D., Knyazev E., Koch P., Koekoek G., Kojima Y., Kokeyama K., Koley S., Kolitsidou P., Kolstein M., Komori K., Kondrashov V., Kong A. K. H., Kontos A., Koper N., Korobko M., Kotake K., Kovalam M., Kozak D. B., Kozakai C., Kozu R., Kringel V., Krishnendu N. V., Krolak A., Kuehn G., Kuei F., Kuijer P., Kumar A., Kumar P., Kumar R., Kume J., Kuns K., Kuo C., Kuo H. -S., Kuromiya Y., Kuroyanagi S., Kusayanagi K., Kuwahara S., Kwak K., Lagabbe P., Laghi D., Lalande E., Lam T. 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M., Maggiore R., Magnozzi M., Mahesh S., Majorana E., Makarem C., Maksimovic I., Maliakal S., Malik A., Man N., Mandic V., Mangano V., Mango J. L., Mansell G. L., Manske M., Mantovani M., Mapelli M., Marchesoni F., Marchio M., Marion F., Mark Z., Marka S., Marka Z., Markakis C., Markosyan A. S., Markowitz A., Maros E., Marquina A., Marsat S., Martelli F., Martin I. W., Martin R. M., Martinez M., Martinez V. A., Martinez V., Martinovic K., Martynov D. V., Marx E. J., Masalehdan H., Mason K., Massera E., Masserot A., Massinger T. J., Masso-Reid M., Mastrogiovanni S., Matas A., Mateu-Lucena M., Matichard F., Matiushechkina M., Mavalvala N., McCann J. J., McCarthy R., McClelland D. E., McClincy P. K., McCormick S., McCuller L., McGhee G. I., McGuire S. C., McIsaac C., McIver J., McRae T., McWilliams S. T., Meacher D., Mehmet M., Mehta A. K., Meijer Q., Melatos A., Melchor D. A., Mendell G., Menendez-Vazquez A., Menoni C. S., Mercer R. A., Mereni L., Merfeld K., Merilh E. L., Merritt J. D., Merzougui M., Meshkov S., Messenger C., Messick C., Meyers P. M., Meylahn F., Mhaske A., Miani A., Miao H., Michaloliakos I., Michel C., Michimura Y., Middleton H., Milano L., Miller A. L., Miller A., Miller B., Millhouse M., Mills J. C., Milotti E., Minazzoli O., Minenkov Y., Mio N., Mir L. M., Miravet-Tenes M., Mishra C., Mishra T., Mistry T., Mitra S., Mitrofanov V. P., Mitselmakher G., Mittleman R., Miyakawa O., Miyamoto A., Miyazaki Y., Miyo K., Miyoki S., Mo G., Moguel E., Mogushi K., Mohapatra S. R. P., Mohite S. R., Molina I., Molina-Ruiz M., Mondin M., Montani M., Moore C. J., Moraru D., Morawski F., More A., Moreno C., Moreno G., Mori Y., Morisaki S., Moriwaki Y., Mours B., Mow-Lowry C. M., Mozzon S., Muciaccia F., Mukherjee A., Mukherjee D., Mukherjee S., Mukund N., Mullavey A., Munch J., Muniz E. A., Murray P. G., Musenich R., Muusse S., Nadji S. L., Nagano K., Nagano S., Nagar A., Nakamura K., Nakano H., Nakano M., Nakashima R., Nakayama Y., Napolano V., Nardecchia I., Narikawa T., Naticchioni L., Nayak B., Nayak R. K., Negishi R., Neil B. F., Neilson J., Nelemans G., Nelson T. J. N., Nery M., Neubauer P., Neunzert A., Ng K. Y., Ng S. W. S., Nguyen C., Nguyen P., Nguyen T., Nguyen Quynh L., Ni W. -T., Nichols S. A., Nishizawa A., Nissanke S., Nitoglia E., Nocera F., Norman M., North C., Nozaki S., Nuttall L. K., Oberling J., O'Brien B. D., Obuchi Y., O'Dell J., Oelker E., Ogaki W., Oganesyan G., Oh J. J., Oh K., Oh S. H., Ohashi M., Ohishi N., Ohkawa M., Ohme F., Ohta H., Okada M. A., Okutani Y., Okutomi K., Olivetto C., Oohara K., Ooi C., Oram R., O'Reilly B., Ormiston R. G., Ormsby N. D., Ortega L. F., O'Shaughnessy R., O'Shea E., Oshino S., Ossokine S., Osthelder C., Otabe S., Ottaway D. J., Overmier H., Pace A. E., Pagano G., Page M. A., Pagliaroli G., Pai A., Pai S. A., Palamos J. 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K., Prasai K., Prasanna R., Pratten G., Principe M., Prodi G. A., Prokhorov L., Prosposito P., Prudenzi L., Puecher A., Punturo M., Puosi F., Puppo P., Purrer M., Qi H., Quetschke V., Quitzow-James R., Raab F. J., Raaijmakers G., Radkins H., Radulesco N., Raffai P., Rail S. X., Raja S., Rajan C., Ramirez K. E., Ramirez T. D., Ramos-Buades A., Rana J., Rapagnani P., Rapol U. D., Ray A., Raymond V., Raza N., Razzano M., Read J., Rees L. A., Regimbau T., Rei L., Reid S., Reid S. W., Reitze D. H., Relton P., Renzini A., Rettegno P., Rezac M., Ricci F., Richards D., Richardson J. W., Richardson L., Riemenschneider G., Riles K., Rinaldi S., Rink K., Rizzo M., Robertson N. A., Robie R., Robinet F., Rocchi A., Rodriguez S., Rolland L., Rollins J. G., Romanelli M., Romano R., Romel C. L., Romero-Rodriguez A., Romero-Shaw I. M., Romie J. H., Ronchini S., Rosa L., Rose C. A., Rosinska D., Ross M. P., Rowan S., Rowlinson S. 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L., Nagano K., Nagano S., Nagar A., Nakamura K., Nakano H., Nakano M., Nakashima R., Nakayama Y., Napolano V., Nardecchia I., Narikawa T., Naticchioni L., Nayak B., Nayak R. K., Negishi R., Neil B. F., Neilson J., Nelemans G., Nelson T. J. N., Nery M., Neubauer P., Neunzert A., Ng K. Y., Ng S. W. S., Nguyen C., Nguyen P., Nguyen T., Nguyen Quynh L., Ni W. -T., Nichols S. A., Nishizawa A., Nissanke S., Nitoglia E., Nocera F., Norman M., North C., Nozaki S., Nuttall L. K., Oberling J., O'Brien B. D., Obuchi Y., O'Dell J., Oelker E., Ogaki W., Oganesyan G., Oh J. J., Oh K., Oh S. H., Ohashi M., Ohishi N., Ohkawa M., Ohme F., Ohta H., Okada M. A., Okutani Y., Okutomi K., Olivetto C., Oohara K., Ooi C., Oram R., O'Reilly B., Ormiston R. G., Ormsby N. D., Ortega L. F., O'Shaughnessy R., O'Shea E., Oshino S., Ossokine S., Osthelder C., Otabe S., Ottaway D. J., Overmier H., Pace A. E., Pagano G., Page M. A., Pagliaroli G., Pai A., Pai S. A., Palamos J. R., Palashov O., Palomba C., Pan H., Pan K., Panda P. K., Pang H., Pang P. T. H., Pankow C., Pannarale F., Pant B. C., Panther F. H., Paoletti F., Paoli A., Paolone A., Parisi A., Park H., Park J., Parker W., Pascucci D., Pasqualetti A., Passaquieti R., Passuello D., Patel M., Pathak M., Patricelli B., Patron A. S., Patrone S., Paul S., Payne E., Pedraza M., Pegoraro M., Pele A., Pena Arellano F. E., Penn S., Perego A., Pereira A., Pereira T., Perez C. J., Perigois C., Perkins C. C., Perreca A., Perries S., Petermann J., Petterson D., Pfeiffer H. P., Pham K. A., Phukon K. S., Piccinni O. J., Pichot M., Piendibene M., Piergiovanni F., Pierini L., Pierro V., Pillant G., Pillas M., Pilo F., Pinard L., Pinto I. M., Pinto M., Piotrzkowski K., Pirello M., Pitkin M. D., Placidi E., Planas L., Plastino W., Pluchar C., Poggiani R., Polini E., Pong D. Y. T., Ponrathnam S., Popolizio P., Porter E. K., Poulton R., Powell J., Pracchia M., Pradier T., Prajapati A. K., Prasai K., Prasanna R., Pratten G., Principe M., Prodi G. A., Prokhorov L., Prosposito P., Prudenzi L., Puecher A., Punturo M., Puosi F., Puppo P., Purrer M., Qi H., Quetschke V., Quitzow-James R., Raab F. J., Raaijmakers G., Radkins H., Radulesco N., Raffai P., Rail S. X., Raja S., Rajan C., Ramirez K. E., Ramirez T. D., Ramos-Buades A., Rana J., Rapagnani P., Rapol U. D., Ray A., Raymond V., Raza N., Razzano M., Read J., Rees L. A., Regimbau T., Rei L., Reid S., Reid S. W., Reitze D. H., Relton P., Renzini A., Rettegno P., Rezac M., Ricci F., Richards D., Richardson J. W., Richardson L., Riemenschneider G., Riles K., Rinaldi S., Rink K., Rizzo M., Robertson N. A., Robie R., Robinet F., Rocchi A., Rodriguez S., Rolland L., Rollins J. G., Romanelli M., Romano R., Romel C. L., Romero-Rodriguez A., Romero-Shaw I. M., Romie J. H., Ronchini S., Rosa L., Rose C. A., Rosinska D., Ross M. P., Rowan S., Rowlinson S. J., Roy S., Rozza D., Ruggi P., Ryan K., Sachdev S., Sadecki T., Sadiq J., Sago N., Saito S., Saito Y., Sakai K., Sakai Y., Sakellariadou M., Sakuno Y., Salafia O. S., Salconi L., Saleem M., Salemi F., Samajdar A., Sanchez E. J., Sanchez J. H., Sanchez L. E., Sanchis-Gual N., Sanders J. R., Sanuy A., Saravanan T. R., Sarin N., Sassolas B., Satari H., Sathyaprakash B. S., Sato S., Sato T., Sauter O., Savage R. L., Sawada T., Sawant D., Sawant H. L., Sayah S., Schaetzl D., Scheel M., Scheuer J., Schiworski M., Schmidt P., Schmidt S., Schnabel R., Schneewind M., Schofield R. M. S., Schonbeck A., Schulte B. W., Schutz B. F., Schwartz E., Scott J., Scott S. M., Seglar-Arroyo M., Sekiguchi T., Sekiguchi Y., Sellers D., Sengupta A. S., Sentenac D., Seo E. G., Sequino V., Sergeev A., Setyawati Y., Shaffer T., Shahriar M. S., Shams B., Shao L., Sharma A., Sharma P., Shawhan P., Shcheblanov N. S., Shibagaki S., Shikauchi M., Shimizu R., Shimoda T., Shimode K., Shinkai H., Shishido T., Shoda A., Shoemaker D. H., Shoemaker D. M., Shyamsundar S., Sieniawska M., Sigg D., Singer L. P., Singh D., Singh N., Singha A., Sintes A. M., Sipala V., Skliris V., Slagmolen B. J. J., Slaven-Blair T. J., Smetana J., Smith J. R., Smith R. J. E., Soldateschi J., Somala S. N., Somiya K., Son E. J., Soni K., Soni S., Sordini V., Sorrentino F., Sorrentino N., Sotani H., Soulard R., Souradeep T., Sowell E., Spagnuolo V., Spencer A. P., Spera M., Srinivasan R., Srivastava A. K., Srivastava V., Staats K., Stachie C., Steer D. A., Steinlechner J., Steinlechner S., Stops D. J., Stover M., Strain K. A., Strang L. C., Stratta G., Strunk A., Sturani R., Stuver A. L., Sudhagar S., Sudhir V., Sugimoto R., Suh H. G., Summerscales T. Z., Sun H., Sun L., Sunil S., Sur A., Suresh J., Sutton P. J., Suzuki T., Swinkels B. L., Szczepanczyk M. J., Szewczyk P., Tacca M., Vtagoshi H., Tait S. C., Takahashi H., Takahashi R., Takamori A., Takano S., Takeda H., Takeda M., Talbot C. J., Talbot C., Tanaka H., Tanaka K., Tanaka T., Tanasijczuk A. J., Tanioka S., Tanner D. B., Tao D., Tao L., Tapia San Martin E. N., Taranto C., Tasson J. D., Telada S., Tenorio R., Terhune J. E., Terkowski L., Thirugnanasambandam M. P., Thomas M., Thomas P., Thompson J. E., Thondapu S. R., Thorne K. A., Thrane E., Tiwari S., Tiwari V., Toivonen A. M., Toland K., Tolley A. E., Tomaru T., Tomigami Y., Tomura T., Tonelli M., Torres-Forne A., Torrie C. I., Tosta E Melo I., Toyra D., Trapananti A., Travasso F., Traylor G., Trevor M., Tringali M. C., Tripathee A., Troiano L., Trovato A., Trozzo L., Trudeau R. J., Tsai D. S., Tsai D., Tsang K. W., Tsang T., Tsao J. -S., Tse M., Tso R., Tsubono K., Tsuchida S., Tsukada L., Tsuna D., Tsutsui T., Tsuzuki T., Turbang K., Turconi M., Tuyenbayev D., Ubhi A. S., Uchikata N., Uchiyama T., Udall R. P., Ueda A., Uehara T., Ueno K., Ueshima G., Unnikrishnan C. S., Uraguchi F., Urban A. L., Ushiba T., Utina A., Vahlbruch H., Vajente G., Vajpeyi A., Valdes G., Valentini M., Valsan V., Van Bakel N., Van Beuzekom M., Van Den Brand J. F. J., Van Den Broeck C., Vander-Hyde D. C., Van Der Schaaf L., Van Heijningen J. V., Vanosky J., Van Putten M. H. P. M., Van Remortel N., Vardaro M., Vargas A. F., Varma V., Vasuth M., Vecchio A., Vedovato G., Veitch J., Veitch P. J., Venneberg J., Venugopalan G., Verkindt D., Verma P., Verma Y., Veske D., Vetrano F., Vicere A., Vidyant S., Viets A. D., Vijaykumar A., Villa-Ortega V., Vinet J. -Y., Virtuoso A., Vitale S., Vo T., Vocca H., Von Reis E. R. G., Von Wrangel J. S. A., Vorvick C., Vyatchanin S. P., Wade L. E., Wade M., Wagner K. J., Walet R. C., Walker M., Wallace G. S., Wallace L., Walsh S., Wang J., Wang J. Z., Wang W. H., Ward R. L., Warner J., Was M., Washimi T., Washington N. Y., Watchi J., Weaver B., Webster S. A., Weinert M., Weinstein A. J., Weiss R., Weller C. M., Wellmann F., Wen L., Weaels P., Wette K., Whelan J. T., White D. D., Whiting B. F., Whittle C., Wilken D., Williams D., Williams M. J., Williamson A. R., Willis J. L., Willke B., Wilson D. J., Winkler W., Wipf C. C., Wlodarczyk T., Woan G., Woehler J., Wofford J. K., Wong I. C. F., Wu C., Wu D. S., Wu H., Wu S., Wysocki D. M., Xiao L., Xu W. -R., Yamada T., Yamamoto H., Yamamoto K., Yamamoto T., Yamashita K., Yamazaki R., Yang F. W., Yang L., Yang Y., Yang Z., Yap M. J., Yeeles D. W., Yelikar A. B., Ying M., Yokogawa K., Yokoyama J., Yokozawa T., Yoo J., Yoshioka T., Yu H., Yuzurihara H., Zadrozny A., Zanolin M., Zeidler S., Zelenova T., Zendri J. -P., Zevin M., Zhan M., Zhang H., Zhang J., Zhang L., Zhang T., Zhang Y., Zhao C., Zhao G., Zhao Y., Zhou R., Zhou Z., Zhu X. J., Zhu Z. -H., Zimmerman A. B., Zucker M. E., and Zweizig J.
Abstract: Intermediate-mass black holes (IMBHs) span the approximate mass range 100-105 M· , between black holes (BHs) that formed by stellar collapse and the supermassive BHs at the centers of galaxies. Mergers of IMBH binaries are the most energetic gravitational-wave sources accessible by the terrestrial detector network. Searches of the first two observing runs of Advanced LIGO and Advanced Virgo did not yield any significant IMBH binary signals. In the third observing run (O3), the increased network sensitivity enabled the detection of GW190521, a signal consistent with a binary merger of mass ∼150 M· providing direct evidence of IMBH formation. Here, we report on a dedicated search of O3 data for further IMBH binary mergers, combining both modeled (matched filter) and model-independent search methods. We find some marginal candidates, but none are sufficiently significant to indicate detection of further IMBH mergers. We quantify the sensitivity of the individual search methods and of the combined search using a suite of IMBH binary signals obtained via numerical relativity, including the effects of spins misaligned with the binary orbital axis, and present the resulting upper limits on astrophysical merger rates. Our most stringent limit is for equal mass and aligned spin BH binary of total mass 200 M· and effective aligned spin 0.8 at 0.056 Gpc-3 yr-1 (90% confidence), a factor of 3.5 more constraining than previous LIGO-Virgo limits. We also update the estimated rate of mergers similar to GW190521 to 0.08 Gpc-3 yr-1.
Published: 2022

23. Extreme mass ratio inspirals and tidal disruption events in nuclear clusters. I. Time dependent rates

Author: Broggi, L, Bortolas, E, Bonetti, M, Sesana, A, Dotti, M, Luca Broggi, Elisa Bortolas, Matteo Bonetti, Alberto Sesana, Massimo Dotti, Broggi, L, Bortolas, E, Bonetti, M, Sesana, A, Dotti, M, Luca Broggi, Elisa Bortolas, Matteo Bonetti, Alberto Sesana, and Massimo Dotti
Abstract: In this paper, we develop a computationally efficient, two-population, time-dependent Fokker-Plank approach in the two dimensions of energy and angular momentum to study the rates of tidal disruption events (TDEs), extreme mass ratio inspirals (EMRIs), and direct plunges occurring around massive black holes (MBHs) in galactic nuclei. We test our code by exploring a wide range of the astrophysically relevant parameter space, including MBH masses, galaxy central densities, and inner density slopes. We find that mass segregation and, more in general, the time dependency of the distribution function regulate the event rate: TDEs always decline with time, whereas EMRIs and plunges reach a maximum and undergo a subsequent nearly exponential decay. Once suitably normalized, the rates associated to different choices of MBH mass and galaxy density overlap nearly perfectly. Based on this, we provide a simple scaling that allows to reproduce the time-dependent event rates for any MBH mass and underlying galactic nucleus. Although our peak rates are in general agreement with the literature relying on the steady-state (non-time-dependent) assumption, those can be sustained on a time-scale that strongly depends on the properties of the system. In particular, this can be much shorter than a Gyr for relatively light MBHs residing in dense systems. This warns against using steady-state models to compute global TDE, EMRI, and plunge rates and calls for a more sophisticated, time-dependent treatment of the problem.
Published: 2022

24. Extreme mass ratio inspirals triggered by massive black hole binaries: from relativistic dynamics to cosmological rates

Author: Mazzolari, G, Bonetti, M, Sesana, A, Colombo, R, Dotti, M, Lodato, G, Izquierdo-Villalba, D, Colombo, RM, Mazzolari, G, Bonetti, M, Sesana, A, Colombo, R, Dotti, M, Lodato, G, Izquierdo-Villalba, D, and Colombo, RM
Abstract: Extreme mass ratio inspirals (EMRIs) are compact binary systems characterized by a mass ratio q = m/M in the range 10−9–10−4 and represent primary gravitational wave (GW) sources for the forthcoming Laser Interferometer Space Antenna (LISA). While their standard formation channel involves relaxation processes deflecting compact objects on very low angular momentum orbits around the central massive black hole, a number of alternative formation channels has been proposed, including binary tidal break-up, migration in accretion discs and secular and chaotic dynamics around a massive black hole binary (MBHB). In this work, we take an extensive closer look at this latter scenario, investigating how EMRIs can be triggered by MBHBs, formed in the aftermath of galaxy mergers. By employing a suite of relativistic three-body simulations, we evaluate the efficiency of EMRI formation for different parameters of the MBHB, assessing the importance of both secular and chaotic dynamics. By modelling the distribution of compact objects in galaxy nuclei, we estimate the resulting EMRI formation rate, finding that EMRI are produced in a sharp burst, with peak rates that are 10–100 times higher than the standard two-body relaxation channel, lasting for 106–108 yr. By coupling our results with an estimate of the cosmic MBHB merger rate, we finally forecast that LISA could observe O(10) EMRIs per year formed by this channel.
Published: 2022

25. Eccentricity evolution of massive black hole binaries from formation to coalescence

Author: Gualandris, A, Khan, F, Bortolas, E, Bonetti, M, Sesana, A, Berczik, P, Holley-Bockelmann, K, Gualandris A., Khan F. M., Bortolas E., Bonetti M., Sesana A., Berczik P., Holley-Bockelmann K., Gualandris, A, Khan, F, Bortolas, E, Bonetti, M, Sesana, A, Berczik, P, Holley-Bockelmann, K, Gualandris A., Khan F. M., Bortolas E., Bonetti M., Sesana A., Berczik P., and Holley-Bockelmann K.
Abstract: Coalescing supermassive black hole binaries (BHBs) are expected to be the loudest sources of gravitational waves (GWs) in the Universe. Detection rates for ground or space-based detectors based on cosmological simulations and semi-analytic models are highly uncertain. A major difficulty stems from the necessity to model the BHB from the scale of the merger to that of inspiral. Of particular relevance to the GW merger time-scale is the binary eccentricity. Here, we present a self-consistent numerical study of the eccentricity of BHBs formed in massive gas-free mergers from the early stages of the merger to the hardening phase, followed by a semi-analytical model down to coalescence. We find that the early eccentricity of the unbound black hole pair is largely determined by the initial orbit. It systematically decreases during the dynamical friction phase. The eccentricity at binary formation is affected by stochasticity and noise owing to encounters with stars, but preserves a strong correlation with the initial orbital eccentricity. Binding of the black holes is a phase characterized by strong perturbations; and we present a quantitative definition of the time of binary formation. During hardening the eccentricity increases in minor mergers, unless the binary is approximately circular, but remains largely unchanged in major mergers, in agreement with predictions from semi-analytical models based on isotropic scattering experiments. Coalescence times due to hardening and GW emission in gas-poor non-rotating ellipticals are 0.5 Gyr for the large initial eccentricities (0.5 ≤ e ≤ 0.9) typical of galaxy mergers in cosmological simulations.
Published: 2022

26. Massive black hole evolution models confronting the n-Hz amplitude of the stochastic gravitational wave background

Author: Izquierdo-Villalba, D, Sesana, A, Bonoli, S, Colpi, M, Izquierdo-Villalba David, Sesana Alberto, Bonoli Silvia, Colpi Monica, Izquierdo-Villalba, D, Sesana, A, Bonoli, S, Colpi, M, Izquierdo-Villalba David, Sesana Alberto, Bonoli Silvia, and Colpi Monica
Abstract: We estimate the amplitude of the nano-Hz stochastic gravitational wave background (GWB) resulting from an unresolved population of inspiralling massive black hole binaries (MBHBs). To this aim, we use the L-Galaxies semi-analytical model applied on top of the Millennium merger trees. The dynamical evolution of MBHBs includes dynamical friction, stellar and gas binary hardening, and gravitational wave (GW) feedback. At the frequencies proved by the Pulsar Timing Array experiments, our model predicts an amplitude of 1.2 × 10-15} at 3 × 10-8, Hz in agreement with current estimations. The contribution to the background comes primarily from equal-mass binaries with chirp masses above 108, M\odot. We then consider the recently detected common red noise in NANOGrav, PPTA, and EPTA data, working under the hypothesis that it is indeed a stochastic GWB coming from MBHBs. By boosting the massive black hole growth via gas accretion, we show that our model can produce a signal with an amplitude A ≈ (2-3) × 10-15. There are, however, difficulties in predicting this background level without mismatching key observational constraints such as the quasar bolometric luminosity functions or the local black hole mass function. This highlights how current and forthcoming GW observations can, for the first time, confront galaxy and black hole evolution models.
Published: 2022

27. Search for intermediate-mass black hole binaries in the third observing run of Advanced LIGO and Advanced Virgo

Author: Abbott, R, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adhikari, N, Adhikari, R, Adya, V, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Ando, M, Andrade, T, Andres, N, Andric, T, Angelova, S, Ansoldi, S, Antelis, J, Antier, S, Appert, S, Arai, K, Arai, Y, Araki, S, Araya, A, Araya, M, Areeda, J, Arene, M, Aritomi, N, Arnaud, N, Aronson, S, Arun, K, Asada, H, Asali, Y, Ashton, G, Aso, Y, Assiduo, M, Aston, S, Astone, P, Aubin, F, Austin, C, Babak, S, Badaracco, F, Bader, M, Badger, C, Bae, S, Bae, Y, Baer, A, Bagnasco, S, Bai, Y, Baiotti, L, Baird, J, Bajpai, R, Ball, M, Ballardin, G, Ballmer, S, Balsamo, A, Baltus, G, Banagiri, S, Bankar, D, Barayoga, J, Barbieri, C, Barish, B, Barker, D, Barneo, P, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, M, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Baylor, A, Bazzan, M, Becsy, B, Bedakihale, V, Bejger, M, Belahcene, I, Benedetto, V, Beniwal, D, Bennett, T, Bentley, J, Benyaala, M, Bergamin, F, Berger, B, Bernuzzi, S, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Beveridge, D, Bhandare, R, Bhardwaj, U, Bhattacharjee, D, Bhaumik, S, Bilenko, I, Billingsley, G, Bini, S, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Biswas, B, Bitossi, M, Bizouard, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Bobba, F, Bode, N, Boer, M, Bogaert, G, Boldrini, M, Bonavena, L, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, N, Bose, S, Bossilkov, V, Boudart, V, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branch, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Bruno, G, Bruntz, R, Bryant, J, Bulik, T, Bulten, H, Buonanno, A, Buscicchio, R, Buskulic, D, Buy, C, Byer, R, Cadonati, L, Cagnoli, G, Cahillane, C, Calderon Bustillo, J, Callaghan, J, Callister, T, Calloni, E, Cameron, J, Camp, J, Canepa, M, Canevarolo, S, Cannavacciuolo, M, Cannon, K, Cao, H, Cao, Z, Capocasa, E, Capote, E, Carapella, G, Carbognani, F, Carlin, J, Carney, M, Carpinelli, M, Carrillo, G, Carullo, G, Carver, T, Casanueva Diaz, J, Casentini, C, Castaldi, G, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Ceasar, M, Cella, G, Cerda-Duran, P, Cesarini, E, Chaibi, W, Chakravarti, K, Chalathadka Subrahmanya, S, Champion, E, Chan, C, Chan, K, Chan, M, Chandra, K, Chanial, P, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, C, Chatterjee, D, Chaturvedi, M, Chaty, S, Chatziioannou, K, Chen, C, Chen, H, Chen, J, Chen, K, Chen, X, Chen, Y, Chen, Z, Cheng, H, Cheong, C, Cheung, H, Chia, H, Chiadini, F, Chiang, C, Chiarini, G, Chierici, R, Chincarini, A, Chiofalo, M, Chiummo, A, Cho, G, Cho, H, Choudhary, R, Choudhary, S, Christensen, N, Chu, H, Chu, Q, Chu, Y, Chua, S, Chung, K, Ciani, G, Ciecielag, P, Cieslar, M, Cifaldi, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, E, Clark, J, Clarke, L, Clearwater, P, Clesse, S, Cleva, F, Coccia, E, Codazzo, E, Cohadon, P, Cohen, D, Cohen, L, Colleoni, M, Collette, C, Colombo, A, Colpi, M, Compton, C, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrion, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coulon, J, Countryman, S, Cousins, B, Couvares, P, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Criswell, A, Croquette, M, Crowder, S, Cudell, J, Cullen, T, Cumming, A, Cummings, R, Cunningham, L, Cuoco, E, Curylo, M, Dabadie, P, Dal Canton, T, Dall'Osso, S, Dalya, G, Dana, A, Daneshgaran Bajastani, L, D'Angelo, B, Danilishin, S, D'Antonio, S, Danzmann, K, Darsow-Fromm, C, Dasgupta, A, Datrier, L, Datta, S, Dattilo, V, Dave, I, Davier, M, Davies, G, Davis, D, Davis, M, Daw, 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L., Nagano K., Nagano S., Nagar A., Nakamura K., Nakano H., Nakano M., Nakashima R., Nakayama Y., Napolano V., Nardecchia I., Narikawa T., Naticchioni L., Nayak B., Nayak R. K., Negishi R., Neil B. F., Neilson J., Nelemans G., Nelson T. J. N., Nery M., Neubauer P., Neunzert A., Ng K. Y., Ng S. W. S., Nguyen C., Nguyen P., Nguyen T., Nguyen Quynh L., Ni W. -T., Nichols S. A., Nishizawa A., Nissanke S., Nitoglia E., Nocera F., Norman M., North C., Nozaki S., Nuttall L. K., Oberling J., O'Brien B. D., Obuchi Y., O'Dell J., Oelker E., Ogaki W., Oganesyan G., Oh J. J., Oh K., Oh S. H., Ohashi M., Ohishi N., Ohkawa M., Ohme F., Ohta H., Okada M. A., Okutani Y., Okutomi K., Olivetto C., Oohara K., Ooi C., Oram R., O'Reilly B., Ormiston R. G., Ormsby N. D., Ortega L. F., O'Shaughnessy R., O'Shea E., Oshino S., Ossokine S., Osthelder C., Otabe S., Ottaway D. J., Overmier H., Pace A. E., Pagano G., Page M. A., Pagliaroli G., Pai A., Pai S. A., Palamos J. R., Palashov O., Palomba C., Pan H., Pan K., Panda P. K., Pang H., Pang P. T. H., Pankow C., Pannarale F., Pant B. C., Panther F. H., Paoletti F., Paoli A., Paolone A., Parisi A., Park H., Park J., Parker W., Pascucci D., Pasqualetti A., Passaquieti R., Passuello D., Patel M., Pathak M., Patricelli B., Patron A. S., Patrone S., Paul S., Payne E., Pedraza M., Pegoraro M., Pele A., Pena Arellano F. E., Penn S., Perego A., Pereira A., Pereira T., Perez C. J., Perigois C., Perkins C. C., Perreca A., Perries S., Petermann J., Petterson D., Pfeiffer H. P., Pham K. A., Phukon K. S., Piccinni O. J., Pichot M., Piendibene M., Piergiovanni F., Pierini L., Pierro V., Pillant G., Pillas M., Pilo F., Pinard L., Pinto I. M., Pinto M., Piotrzkowski K., Pirello M., Pitkin M. D., Placidi E., Planas L., Plastino W., Pluchar C., Poggiani R., Polini E., Pong D. Y. T., Ponrathnam S., Popolizio P., Porter E. K., Poulton R., Powell J., Pracchia M., Pradier T., Prajapati A. K., Prasai K., Prasanna R., Pratten G., Principe M., Prodi G. A., Prokhorov L., Prosposito P., Prudenzi L., Puecher A., Punturo M., Puosi F., Puppo P., Purrer M., Qi H., Quetschke V., Quitzow-James R., Raab F. J., Raaijmakers G., Radkins H., Radulesco N., Raffai P., Rail S. X., Raja S., Rajan C., Ramirez K. E., Ramirez T. D., Ramos-Buades A., Rana J., Rapagnani P., Rapol U. D., Ray A., Raymond V., Raza N., Razzano M., Read J., Rees L. A., Regimbau T., Rei L., Reid S., Reid S. W., Reitze D. H., Relton P., Renzini A., Rettegno P., Rezac M., Ricci F., Richards D., Richardson J. W., Richardson L., Riemenschneider G., Riles K., Rinaldi S., Rink K., Rizzo M., Robertson N. A., Robie R., Robinet F., Rocchi A., Rodriguez S., Rolland L., Rollins J. G., Romanelli M., Romano R., Romel C. L., Romero-Rodriguez A., Romero-Shaw I. M., Romie J. H., Ronchini S., Rosa L., Rose C. A., Rosinska D., Ross M. P., Rowan S., Rowlinson S. J., Roy S., Rozza D., Ruggi P., Ryan K., Sachdev S., Sadecki T., Sadiq J., Sago N., Saito S., Saito Y., Sakai K., Sakai Y., Sakellariadou M., Sakuno Y., Salafia O. S., Salconi L., Saleem M., Salemi F., Samajdar A., Sanchez E. J., Sanchez J. H., Sanchez L. E., Sanchis-Gual N., Sanders J. R., Sanuy A., Saravanan T. R., Sarin N., Sassolas B., Satari H., Sathyaprakash B. S., Sato S., Sato T., Sauter O., Savage R. L., Sawada T., Sawant D., Sawant H. L., Sayah S., Schaetzl D., Scheel M., Scheuer J., Schiworski M., Schmidt P., Schmidt S., Schnabel R., Schneewind M., Schofield R. M. S., Schonbeck A., Schulte B. W., Schutz B. F., Schwartz E., Scott J., Scott S. M., Seglar-Arroyo M., Sekiguchi T., Sekiguchi Y., Sellers D., Sengupta A. S., Sentenac D., Seo E. G., Sequino V., Sergeev A., Setyawati Y., Shaffer T., Shahriar M. S., Shams B., Shao L., Sharma A., Sharma P., Shawhan P., Shcheblanov N. S., Shibagaki S., Shikauchi M., Shimizu R., Shimoda T., Shimode K., Shinkai H., Shishido T., Shoda A., Shoemaker D. H., Shoemaker D. M., Shyamsundar S., Sieniawska M., Sigg D., Singer L. P., Singh D., Singh N., Singha A., Sintes A. M., Sipala V., Skliris V., Slagmolen B. J. J., Slaven-Blair T. J., Smetana J., Smith J. R., Smith R. J. E., Soldateschi J., Somala S. N., Somiya K., Son E. J., Soni K., Soni S., Sordini V., Sorrentino F., Sorrentino N., Sotani H., Soulard R., Souradeep T., Sowell E., Spagnuolo V., Spencer A. P., Spera M., Srinivasan R., Srivastava A. K., Srivastava V., Staats K., Stachie C., Steer D. A., Steinlechner J., Steinlechner S., Stops D. J., Stover M., Strain K. A., Strang L. C., Stratta G., Strunk A., Sturani R., Stuver A. L., Sudhagar S., Sudhir V., Sugimoto R., Suh H. G., Summerscales T. Z., Sun H., Sun L., Sunil S., Sur A., Suresh J., Sutton P. J., Suzuki T., Swinkels B. L., Szczepanczyk M. J., Szewczyk P., Tacca M., Vtagoshi H., Tait S. C., Takahashi H., Takahashi R., Takamori A., Takano S., Takeda H., Takeda M., Talbot C. J., Talbot C., Tanaka H., Tanaka K., Tanaka T., Tanasijczuk A. J., Tanioka S., Tanner D. B., Tao D., Tao L., Tapia San Martin E. N., Taranto C., Tasson J. D., Telada S., Tenorio R., Terhune J. E., Terkowski L., Thirugnanasambandam M. P., Thomas M., Thomas P., Thompson J. E., Thondapu S. R., Thorne K. A., Thrane E., Tiwari S., Tiwari V., Toivonen A. M., Toland K., Tolley A. E., Tomaru T., Tomigami Y., Tomura T., Tonelli M., Torres-Forne A., Torrie C. I., Tosta E Melo I., Toyra D., Trapananti A., Travasso F., Traylor G., Trevor M., Tringali M. C., Tripathee A., Troiano L., Trovato A., Trozzo L., Trudeau R. J., Tsai D. S., Tsai D., Tsang K. W., Tsang T., Tsao J. -S., Tse M., Tso R., Tsubono K., Tsuchida S., Tsukada L., Tsuna D., Tsutsui T., Tsuzuki T., Turbang K., Turconi M., Tuyenbayev D., Ubhi A. S., Uchikata N., Uchiyama T., Udall R. P., Ueda A., Uehara T., Ueno K., Ueshima G., Unnikrishnan C. S., Uraguchi F., Urban A. L., Ushiba T., Utina A., Vahlbruch H., Vajente G., Vajpeyi A., Valdes G., Valentini M., Valsan V., Van Bakel N., Van Beuzekom M., Van Den Brand J. F. J., Van Den Broeck C., Vander-Hyde D. C., Van Der Schaaf L., Van Heijningen J. V., Vanosky J., Van Putten M. H. P. M., Van Remortel N., Vardaro M., Vargas A. F., Varma V., Vasuth M., Vecchio A., Vedovato G., Veitch J., Veitch P. J., Venneberg J., Venugopalan G., Verkindt D., Verma P., Verma Y., Veske D., Vetrano F., Vicere A., Vidyant S., Viets A. D., Vijaykumar A., Villa-Ortega V., Vinet J. -Y., Virtuoso A., Vitale S., Vo T., Vocca H., Von Reis E. R. G., Von Wrangel J. S. A., Vorvick C., Vyatchanin S. P., Wade L. E., Wade M., Wagner K. J., Walet R. C., Walker M., Wallace G. S., Wallace L., Walsh S., Wang J., Wang J. Z., Wang W. H., Ward R. L., Warner J., Was M., Washimi T., Washington N. Y., Watchi J., Weaver B., Webster S. A., Weinert M., Weinstein A. J., Weiss R., Weller C. M., Wellmann F., Wen L., Weaels P., Wette K., Whelan J. T., White D. D., Whiting B. F., Whittle C., Wilken D., Williams D., Williams M. J., Williamson A. R., Willis J. L., Willke B., Wilson D. J., Winkler W., Wipf C. C., Wlodarczyk T., Woan G., Woehler J., Wofford J. K., Wong I. C. F., Wu C., Wu D. S., Wu H., Wu S., Wysocki D. M., Xiao L., Xu W. -R., Yamada T., Yamamoto H., Yamamoto K., Yamamoto T., Yamashita K., Yamazaki R., Yang F. W., Yang L., Yang Y., Yang Z., Yap M. J., Yeeles D. W., Yelikar A. B., Ying M., Yokogawa K., Yokoyama J., Yokozawa T., Yoo J., Yoshioka T., Yu H., Yuzurihara H., Zadrozny A., Zanolin M., Zeidler S., Zelenova T., Zendri J. -P., Zevin M., Zhan M., Zhang H., Zhang J., Zhang L., Zhang T., Zhang Y., Zhao C., Zhao G., Zhao Y., Zhou R., Zhou Z., Zhu X. J., Zhu Z. -H., Zimmerman A. B., Zucker M. E., and Zweizig J.
Abstract: Intermediate-mass black holes (IMBHs) span the approximate mass range 100-105 M· , between black holes (BHs) that formed by stellar collapse and the supermassive BHs at the centers of galaxies. Mergers of IMBH binaries are the most energetic gravitational-wave sources accessible by the terrestrial detector network. Searches of the first two observing runs of Advanced LIGO and Advanced Virgo did not yield any significant IMBH binary signals. In the third observing run (O3), the increased network sensitivity enabled the detection of GW190521, a signal consistent with a binary merger of mass ∼150 M· providing direct evidence of IMBH formation. Here, we report on a dedicated search of O3 data for further IMBH binary mergers, combining both modeled (matched filter) and model-independent search methods. We find some marginal candidates, but none are sufficiently significant to indicate detection of further IMBH mergers. We quantify the sensitivity of the individual search methods and of the combined search using a suite of IMBH binary signals obtained via numerical relativity, including the effects of spins misaligned with the binary orbital axis, and present the resulting upper limits on astrophysical merger rates. Our most stringent limit is for equal mass and aligned spin BH binary of total mass 200 M· and effective aligned spin 0.8 at 0.056 Gpc-3 yr-1 (90% confidence), a factor of 3.5 more constraining than previous LIGO-Virgo limits. We also update the estimated rate of mergers similar to GW190521 to 0.08 Gpc-3 yr-1.
Published: 2022

28. Improved gravitational radiation time-scales II: Spin–orbit contributions and environmental perturbations

Author: Zwick, L, Capelo, P, Bortolas, E, Vazquez-Aceves, V, Mayer, L, Amaro-Seoane, P, Zwick L., Capelo P. R., Bortolas E., Vazquez-Aceves V., Mayer L., Amaro-Seoane P., Zwick, L, Capelo, P, Bortolas, E, Vazquez-Aceves, V, Mayer, L, Amaro-Seoane, P, Zwick L., Capelo P. R., Bortolas E., Vazquez-Aceves V., Mayer L., and Amaro-Seoane P.
Abstract: Peters’ formula is an analytical estimate of the time-scale of gravitational wave (GW)-induced coalescence of binary systems. It is used in countless applications, where the convenience of a simple formula outweighs the need for precision. However, many promising sources of the Laser Interferometer Space Antenna (LISA), such as supermassive black hole binaries and extreme mass-ratio inspirals (EMRIs), are expected to enter the LISA band with highly eccentric (e ≳ 0.9) and highly relativistic orbits. These are exactly the two limits in which Peters’ estimate performs the worst. In this work, we expand upon previous results and give simple analytical fits to quantify how the inspiral time-scale is affected by the relative 1.5 post-Newtonian (PN) hereditary fluxes and spin–orbit couplings. We discuss several cases that demand a more accurate GW time-scale. We show how this can have a major influence on quantities that are relevant for LISA event-rate estimates, such as the EMRI critical semimajor axis. We further discuss two types of environmental perturbations that can play a role in the inspiral phase: the gravitational interaction with a third massive body and the energy loss due to dynamical friction and torques from a surrounding gas medium ubiquitous in galactic nuclei. With the aid of PN corrections to the time-scale in vacuum, we find simple analytical expressions for the regions of phase space in which environmental perturbations are of comparable strength to the effects of any particular PN order, being able to qualitatively reproduce the results of much more sophisticated analyses.
Published: 2021

29. Black Hole Science With the Laser Interferometer Space Antenna

Author: Sesana, A, Sesana A., Sesana, A, and Sesana A.
Abstract: The author reviews the scientific potential of the Laser Interferometer Space Antenna (LISA), a space-borne gravitational wave (GW) observatory to be launched in the early 30s. Thanks to its sensitivity in the milli-Hz frequency range, LISA will reveal a variety of GW sources across the Universe, from our Solar neighborhood potentially all the way back to the Big Bang, promising to be a game changer in our understanding of astrophysics, cosmology, and fundamental physics. This review dives in the LISA Universe, with a specific focus on black hole science, including the formation and evolution of massive black holes in galaxy centers, the dynamics of dense nuclei and formation of extreme mass ratio inspirals, and the astrophysics of stellar-origin black hole binaries.
Published: 2021

30. Stellar hardening of massive black hole binaries: The impact of the host rotation

Author: Varisco, L, Bortolas, E, Dotti, M, Sesana, A, Varisco L., Bortolas E., Dotti M., Sesana A., Varisco, L, Bortolas, E, Dotti, M, Sesana, A, Varisco L., Bortolas E., Dotti M., and Sesana A.
Abstract: Massive black hole binaries (MBHBs) with masses of ∼104 to ∼1010, M⊙ are one of the main targets for currently operating and forthcoming space-borne gravitational wave observatories. In this paper, we explore the effect of the stellar host rotation on the bound binary hardening efficiency, driven by three-body stellar interactions. As seen in previous studies, we find that the centre of mass (CoM) of a prograde MBHB embedded in a rotating environment starts moving on a nearly circular orbit about the centre of the system shortly after the MBHB binding. In our runs, the oscillation radius is ≈ 0.25 (≈ 0.1) times the binary influence radius for equal mass MBHBs (MBHBs with mass ratio 1:4). Conversely, retrograde binaries remain anchored about the centre of the host. The binary shrinking rate is twice as fast when the binary CoM exhibits a net orbital motion, owing to a more efficient loss cone repopulation even in our spherical stellar systems. We develop a model that captures the CoM oscillations of prograde binaries; we argue that the CoM angular momentum gain per time unit scales with the internal binary angular momentum, so that most of the displacement is induced by stellar interactions occurring around the time of MBHB binding, while the subsequent angular momentum enhancement gets eventually quashed by the effect of dynamical friction. The effect of the background rotation on the MBHB evolution may be relevant for LISA sources, that are expected to form in significantly rotating stellar systems.
Published: 2021

31. A possible sub-kiloparsec dual AGN buried behind the galaxy curtain

Author: Severgnini, P, Braito, V, Cicone, C, Saracco, P, Vignali, C, Serafinelli, R, Della Ceca, R, Dotti, M, Cusano, F, Paris, D, Pruto, G, Zaino, A, Ballo, L, Landoni, M, Severgnini P., Braito V., Cicone C., Saracco P., Vignali C., Serafinelli R., Della Ceca R., Dotti M., Cusano F., Paris D., Pruto G., Zaino A., Ballo L., Landoni M., Severgnini, P, Braito, V, Cicone, C, Saracco, P, Vignali, C, Serafinelli, R, Della Ceca, R, Dotti, M, Cusano, F, Paris, D, Pruto, G, Zaino, A, Ballo, L, Landoni, M, Severgnini P., Braito V., Cicone C., Saracco P., Vignali C., Serafinelli R., Della Ceca R., Dotti M., Cusano F., Paris D., Pruto G., Zaino A., Ballo L., and Landoni M.
Abstract: Although thousands of galaxy mergers are known, only a handful of sub-kiloparsec-scale supermassive black hole (SMBH) pairs have been confirmed so far, leaving a huge gap between the observed and predicted numbers of such objects. In this work, we present a detailed analysis of the Sloan Digital Sky Survey optical spectrum and of near-infrared (NIR) diffraction limited imaging of SDSS J1431+4358. This object is a local radio-quiet type 2 active galactic nucleus (AGN) previously selected as a double AGN candidate on the basis of the double-peaked [OIII] emission line. The NIR adaptive optics-assisted observations were obtained at the Large Binocular Telescope with the LUCI+FLAO camera. We found that most of the prominent optical emission lines are characterized by a double-peaked profile, mainly produced by AGN photoionization. Our spectroscopical analysis disfavors the hypothesis that the double-peaked emission lines in the source are the signatures of outflow kinematics, leaving open the possibility that we are detecting either the rotation of a single narrow-line region or the presence of two SMBHs orbiting around a common central potential. The latter scenario is further supported by the high-spatial resolution NIR imaging: After subtracting the dominant contribution of the stellar bulge component in the host galaxy, we detect two faint nuclear sources at r < 0.5 kpc projected separation. Interestingly, the two sources have a position angle consistent with that defined by the two regions where the [OIII] double peaks most likely originate. Aside from the discovery of a promising sub-kiloparsec scale dual AGN, our analysis shows the importance of an appropriate host galaxy subtraction in order to achieve a reliable estimate of the incidence of dual AGNs at small projected separations.
Published: 2021

32. Black Hole Science With the Laser Interferometer Space Antenna

Author: Sesana, A, Sesana A., Sesana, A, and Sesana A.
Abstract: The author reviews the scientific potential of the Laser Interferometer Space Antenna (LISA), a space-borne gravitational wave (GW) observatory to be launched in the early 30s. Thanks to its sensitivity in the milli-Hz frequency range, LISA will reveal a variety of GW sources across the Universe, from our Solar neighborhood potentially all the way back to the Big Bang, promising to be a game changer in our understanding of astrophysics, cosmology, and fundamental physics. This review dives in the LISA Universe, with a specific focus on black hole science, including the formation and evolution of massive black holes in galaxy centers, the dynamics of dense nuclei and formation of extreme mass ratio inspirals, and the astrophysics of stellar-origin black hole binaries.
Published: 2021

33. Non-isotropic feedback from accreting spinning black holes

Author: Sala, L, Cenci, E, R Capelo, P, Lupi, A, Dotti, M, Luca Sala, Elia Cenci, Pedro R Capelo, Alessandro Lupi, Massimo Dotti, Sala, L, Cenci, E, R Capelo, P, Lupi, A, Dotti, M, Luca Sala, Elia Cenci, Pedro R Capelo, Alessandro Lupi, and Massimo Dotti
Abstract: Active galactic nuclei (AGNs) are massive black holes (BHs) caught in the act of accreting gas at the centre of their host galaxies. Part of the accreting mass is converted to energy and released into the surrounding medium, in a process loosely referred to as AGN feedback. Most numerical simulations include AGN feedback as a sub-grid model, wherein energy or momentum (or both) is coupled to the nearby gas. In this work, we implement a new momentum-driven model in the hydrodynamics code GIZMO, in which accretion from large scales is mediated by a sub-grid accretion disc model, and gas particles are stochastically kicked over a bi-conical region, to mimic observed kinetic winds. The feedback cone’s axis can be set parallel either to the angular momentum of the gas surrounding the BH or to the BH spin direction, which is self-consistently evolved within the accretion-disc model. Using a circumnuclear disc (CND) as a test bed, we find that (i) the conical shape of the outflow is always visible and is weakly dependent on the launching orientation and aperture, resulting in comparable mass inflows and outflows; (ii) the cone’s orientation is also similar amongst our tests, and it is not always the same as the initial value, due to the interaction with the CND playing a crucial role in shaping the outflow; and (iii) the velocity of the outflow, instead, differs and strongly depends on the interplay with the CND.
Published: 2021

34. Massive black hole binary systems and the NANOGrav 12.5 yr results

Author: Middleton, H, Sesana, A, Chen, S, Vecchio, A, Del Pozzo, W, Rosado, P, Middleton H., Sesana A., Chen S., Vecchio A., Del Pozzo W., Rosado P. A., Middleton, H, Sesana, A, Chen, S, Vecchio, A, Del Pozzo, W, Rosado, P, Middleton H., Sesana A., Chen S., Vecchio A., Del Pozzo W., and Rosado P. A.
Abstract: The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) recently reported evidence for the presence of a common stochastic signal across their array of pulsars. The origin of this signal is still unclear. One possibility is that it is due to a stochastic gravitational-wave background (SGWB) in the ∼1-10 nHz frequency region. Taking the NANOGrav observational result at face value, we show that this signal would be fully consistent with an SGWB produced by an unresolved population of in-spiralling massive black hole binaries (MBHBs) predicted by current theoretical models. Considering an astrophysically agnostic model, the MBHB merger rate is loosely constrained. Including additional constraints from galaxy pairing fraction and MBH-bulge scaling relations, we find that the MBHB merger rate is 1.2 × 10-5 -4.5 × 10-4, Mpc-3, Gyr-1, the MBHB merger time-scale is ≤ 2.7, Gyr, and the norm of the MBH-Mbulge relation is ≥ 1.2 × 108, M⊙ (all quoted at 90 per cent credible intervals). Regardless of the astrophysical details of MBHB assembly, the NANOGrav result would imply that a sufficiently large population of massive black holes pair up, form binaries and merge within a Hubble time.
Published: 2021

35. Improved gravitational radiation time-scales: Significance for LISA and LIGO-Virgo sources

Author: Zwick, L, Capelo, P, Bortolas, E, Mayer, L, Amaro-Seoane, P, Zwick L., Capelo P. R., Bortolas E., Mayer L., Amaro-Seoane P., Zwick, L, Capelo, P, Bortolas, E, Mayer, L, Amaro-Seoane, P, Zwick L., Capelo P. R., Bortolas E., Mayer L., and Amaro-Seoane P.
Abstract: We present a revised version of Peters' time-scale for the gravitational wave (GW)-induced decay of two point masses. The new formula includes the effects of the first-order post- Newtonian perturbation and additionally provides a simple fit to account for the Newtonian self-consistent evolution of the eccentricity. The revised time-scale is found by multiplying Peters' estimate by two factors, R(e0) = 81- √ 1-e0 and Qf(p0) = exp (2.5(rS/p0)), where e0 and p0 are the initial eccentricity and periapsis, respectively, and rS the Schwarzschild radius of the system. Their use can correct errors of a factor of 1-10 that arise from using the original Peters' formula.We apply the revised time-scales to a set of typical sources for existing ground-based laser interferometers and for the future Laser Interferometer Space Antenna (LISA), at the onset of theirGW-driven decay.We argue that our more accuratemodel for the orbital evolution will affect current event- and detection-rate estimates for mergers of compact object binaries, with stronger deviations for eccentric LISA sources, such as extreme and intermediate massratio inspirals.We propose the correction factors R and Qf as a simple prescription to quantify decay time-scales more accurately in future population synthesis models.We also suggest that the corrected time-scale may be used as a computationally efficient alternative to numerical integration in other applications that include the modelling of radiation reaction for eccentric sources.
Published: 2020

36. Improved constraints from ultra-faint dwarf galaxies on primordial black holes as dark matter

Author: Stegmann, J, Capelo, P, Bortolas, E, Mayer, L, Stegmann J., Capelo P. R., Bortolas E., Mayer L., Stegmann, J, Capelo, P, Bortolas, E, Mayer, L, Stegmann J., Capelo P. R., Bortolas E., and Mayer L.
Abstract: Soon after the recent first ever detection of gravitational waves from merging black holes it has been suggested that their origin is primordial. Appealingly, a sufficient number of primordial black holes (PBHs) could also partially or entirely constitute the dark matter (DM) in our Universe. However, recent studies on PBHs in ultra-faint dwarf galaxies (UFDGs) suggest that they would dynamically heat up the stellar component due to two-body relaxation processes. From the comparison with the observed stellar velocity dispersions and the stellar half-light radii, it was claimed that only PBHs with masses ≲ 10 M⊙ can significantly contribute to the DM. In this work, we improve the latter constraints by considering the largest observational sample of UFDGs and by allowing the PBH masses to follow an extended (lognormal) distribution. By means of collisional Fokker–Planck simulations, we explore a wide parameter space of UFDGs containing PBHs. The analysis of the half-light radii and velocity dispersions resulting from the simulations leads to three general findings that exclude PBHs with masses ∼ O(1 - 100) M⊙ from constituting all of the DM: (i) we identify a critical sub-sample of UFDGs that only allows for ∼ O(1) M⊙ PBH masses; (ii) for any PBH mass, there is an UFDG in our sample that disfavours it; (iii) the spatial extensions of a majority of simulated UFDGs containing PBHs are too large to match the observed.
Published: 2020

37. Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes

Author: Belczynski, K, Klencki, J, Fields, C, Olejak, A, Berti, E, Meynet, G, Fryer, C, Holz, D, O'Shaughnessy, R, Brown, D, Bulik, T, Leung, S, Nomoto, K, Madau, P, Hirschi, R, Kaiser, E, Jones, S, Mondal, S, Chruslinska, M, Drozda, P, Gerosa, D, Doctor, Z, Giersz, M, Ekstrom, S, Georgy, C, Askar, A, Baibhav, V, Wysocki, D, Natan, T, Farr, W, Wiktorowicz, G, Coleman Miller, M, Farr, B, Lasota, J, Belczynski K., Klencki J., Fields C. E., Olejak A., Berti E., Meynet G., Fryer C. L., Holz D. E., O'Shaughnessy R., Brown D. A., Bulik T., Leung S. C., Nomoto K., Madau P., Hirschi R., Kaiser E., Jones S., Mondal S., Chruslinska M., Drozda P., Gerosa D., Doctor Z., Giersz M., Ekstrom S., Georgy C., Askar A., Baibhav V., Wysocki D., Natan T., Farr W. M., Wiktorowicz G., Coleman Miller M., Farr B., Lasota J. -P., Belczynski, K, Klencki, J, Fields, C, Olejak, A, Berti, E, Meynet, G, Fryer, C, Holz, D, O'Shaughnessy, R, Brown, D, Bulik, T, Leung, S, Nomoto, K, Madau, P, Hirschi, R, Kaiser, E, Jones, S, Mondal, S, Chruslinska, M, Drozda, P, Gerosa, D, Doctor, Z, Giersz, M, Ekstrom, S, Georgy, C, Askar, A, Baibhav, V, Wysocki, D, Natan, T, Farr, W, Wiktorowicz, G, Coleman Miller, M, Farr, B, Lasota, J, Belczynski K., Klencki J., Fields C. E., Olejak A., Berti E., Meynet G., Fryer C. L., Holz D. E., O'Shaughnessy R., Brown D. A., Bulik T., Leung S. C., Nomoto K., Madau P., Hirschi R., Kaiser E., Jones S., Mondal S., Chruslinska M., Drozda P., Gerosa D., Doctor Z., Giersz M., Ekstrom S., Georgy C., Askar A., Baibhav V., Wysocki D., Natan T., Farr W. M., Wiktorowicz G., Coleman Miller M., Farr B., and Lasota J. -P.
Abstract: All ten LIGO/Virgo binary black hole (BH-BH) coalescences reported following the O1/O2 runs have near-zero effective spins. There are only three potential explanations for this. If the BH spin magnitudes are large, then: (i) either both BH spin vectors must be nearly in the orbital plane or (ii) the spin angular momenta of the BHs must be oppositely directed and similar in magnitude. Then there is also the possibility that (iii) the BH spin magnitudes are small. We consider the third hypothesis within the framework of the classical isolated binary evolution scenario of the BH-BH merger formation. We test three models of angular momentum transport in massive stars: A mildly efficient transport by meridional currents (as employed in the Geneva code), an efficient transport by the Tayler-Spruit magnetic dynamo (as implemented in the MESA code), and a very-efficient transport (as proposed by Fuller et al.) to calculate natal BH spins. We allow for binary evolution to increase the BH spins through accretion and account for the potential spin-up of stars through tidal interactions. Additionally, we update the calculations of the stellar-origin BH masses, including revisions to the history of star formation and to the chemical evolution across cosmic time. We find that we can simultaneously match the observed BH-BH merger rate density and BH masses and BH-BH effective spins. Models with efficient angular momentum transport are favored. The updated stellar-mass weighted gas-phase metallicity evolution now used in our models appears to be key for obtaining an improved reproduction of the LIGO/Virgo merger rate estimate. Mass losses during the pair-instability pulsation supernova phase are likely to be overestimated if the merger GW170729 hosts a BH more massive than 50âMâŠ. We also estimate rates of black hole-neutron star (BH-NS) mergers from recent LIGO/Virgo observations. If, in fact. angular momentum transport in massive stars is efficient, then any (electromagnetic o
Published: 2020

38. Global torques and stochasticity as the drivers of massive black hole pairing in the young Universe

Author: Bortolas, E, Capelo, P, Zana, T, Mayer, L, Bonetti, M, Dotti, M, Davies, M, Madau, P, Bortolas, Elisa, Capelo, Pedro R, Zana, Tommaso, Mayer, Lucio, Bonetti, Matteo, Dotti, Massimo, Davies, Melvyn B, Madau, Piero, Bortolas, E, Capelo, P, Zana, T, Mayer, L, Bonetti, M, Dotti, M, Davies, M, Madau, P, Bortolas, Elisa, Capelo, Pedro R, Zana, Tommaso, Mayer, Lucio, Bonetti, Matteo, Dotti, Massimo, Davies, Melvyn B, and Madau, Piero
Abstract: The forthcoming Laser Interferometer Space Antenna (LISA) will probe the population of coalescing massive black hole (MBH) binaries up to the onset of structure formation. Here, we simulate the galactic-scale pairing of ∼106 M⊙ MBHs in a typical, non-clumpy main-sequence galaxy embedded in a cosmological environment at z = 7–6. In order to increase our statistical sample, we adopt a strategy that allows us to follow the evolution of six secondary MBHs concomitantly. We find that the magnitude of the dynamical-friction-induced torques is significantly smaller than that of the large-scale, stochastic gravitational torques arising from the perturbed and morphologically evolving galactic disc, suggesting that the standard dynamical friction treatment is inadequate for realistic galaxies at high redshift. The dynamical evolution of MBHs is very stochastic, and a variation in the initial orbital phase can lead to a drastically different time-scale for the inspiral. Most remarkably, the development of a galactic bar in the host system either significantly accelerates the inspiral by dragging a secondary MBH into the centre, or ultimately hinders the orbital decay by scattering the MBH in the galaxy outskirts. The latter occurs more rarely, suggesting that galactic bars overall promote MBH inspiral and binary coalescence. The orbital decay time can be an order of magnitude shorter than what would be predicted relying on dynamical friction alone. The stochasticity and the important role of global torques have crucial implications for the rates of MBH coalescences in the early Universe: both have to be accounted for when making predictions for the upcoming LISA observatory.
Published: 2020

39. On the eccentricity evolution of massive black hole binaries in stellar backgrounds

Author: Bonetti, M, Rasskazov, A, Sesana, A, Dotti, M, Haardt, F, Leigh, N, Arca Sedda, M, Fragione, G, Rossi, E, Bonetti M., Rasskazov A., Sesana A., Dotti M., Haardt F., Leigh N. W. C., Arca Sedda M., Fragione G., Rossi E., Bonetti, M, Rasskazov, A, Sesana, A, Dotti, M, Haardt, F, Leigh, N, Arca Sedda, M, Fragione, G, Rossi, E, Bonetti M., Rasskazov A., Sesana A., Dotti M., Haardt F., Leigh N. W. C., Arca Sedda M., Fragione G., and Rossi E.
Abstract: We study the dynamical evolution of eccentric massive black hole binaries (MBHBs) interacting with unbound stars by means of an extensive set of three-body scattering experiments. Compared to previous studies, we extend the investigation down to a MBHB mass ratio of q = m2/m1 = 10-4, where m1 and m2 are the masses of the primary and secondary hole, respectively. Contrary to a simple extrapolation from higher mass ratios, we find that for q ? 10-3 the eccentricity growth rate becomes negative, i.e. the binary circularizes as it shrinks. This behaviour is due to the subset of interacting stars captured in metastable counter-rotating orbits; those stars tend to extract angular momentum from the binary, promoting eccentricity growth for q > 10-3, but tend to inject angular momentum into the binary driving it towards circularization for q < 10-3. The physical origin of this behaviour requires a detailed study of the orbits of this subset of stars and is currently under investigation. Our findings might have important consequences for intermediate massive black holes (IMBHs) inspiralling on to MBHs (e.g. a putative $10^3, m M-{odot }$ black hole inspiralling on to Sgr A∗).
Published: 2020

40. Can supernova kicks trigger EMRIs in the Galactic Centre?

Author: Bortolas, E, Mapelli, M, Bortolas E., Mapelli M., Bortolas, E, Mapelli, M, Bortolas E., and Mapelli M.
Abstract: One of the most promising gravitational wave (GW) sources detectable by the forthcoming LISA observatory are the so-called extreme-mass ratio inspirals (EMRIs), i.e. GW-driven inspirals of stellar-mass compact objects on to supermassive black holes (SMBHs). In this paper, we suggest that supernova (SN) kicks may trigger EMRIs in galactic nuclei by scattering newborn stellar black holes and neutron stars on extremely eccentric orbits; as a consequence, the time-scale over which these compact objects are expected to inspiral on to the central SMBH via GW emission may become shorter than the time-scale for other orbital perturbations to occur. By applying this argument to the Galactic Centre, we show that the S-cluster and the clockwise disc are optimal regions for the generation of such events: one SN out of ∼104 (∼105) occurring in the S-cluster (clockwise disc) is expected to induce an EMRI. If we assume that the natal kicks affecting stellar black holes are significantly slower than those experienced by neutron stars, we find that most SN-driven EMRIs involve neutron stars. We further estimate the time spanning from the SN to the final plunge on to the SMBH to be of the order of few Myr. Finally, we extrapolate the rate of SN-driven EMRIs per Milky Way to be up to 10−8 yr−1, thus we expect that LISA will detect up to a few tens of SN-driven EMRIs every year.
Published: 2019

41. The host galaxies of double compact objects across cosmic time

Author: Toffano, M, Mapelli, M, Giacobbo, N, Artale, M, Ghirlanda, G, Toffano M., Mapelli M., Giacobbo N., Artale M. C., Ghirlanda G., Toffano, M, Mapelli, M, Giacobbo, N, Artale, M, Ghirlanda, G, Toffano M., Mapelli M., Giacobbo N., Artale M. C., and Ghirlanda G.
Abstract: We explore the host galaxies of compact-object binaries (black hole–black hole binaries, BHBs; neutron star–black hole binaries, NSBHs; double–neutron stars; DNSs) across cosmic time, by means of population-synthesis simulations combined with the Illustris cosmological simulation. At high redshift (z 4), the host galaxies of BHBs, NSBHs, and DNSs are very similar and are predominantly low-mass galaxies (stellar mass M < 1011 M). If z 4, most compact objects form and merge in the same galaxy, with a short delay time. At low redshift (z ≤ 2), the host galaxy populations of DNSs differ significantly from the host galaxies of both BHBs and NSBHs. DNSs merging at low redshift tend to form and merge in the same galaxy, with relatively short delay time. The stellar mass of DNS hosts peaks around ∼1010–1011 M. In contrast, BHBs and NSBHs merging at low redshift tend to form in rather small galaxies at high redshift and then to merge in larger galaxies with long delay times. This difference between DNSs and black hole binaries is a consequence of their profoundly different metallicity dependence.
Published: 2019

42. The host galaxies of double compact objects across cosmic time

Author: Toffano, M, Mapelli, M, Giacobbo, N, Artale, M, Ghirlanda, G, Toffano M., Mapelli M., Giacobbo N., Artale M. C., Ghirlanda G., Toffano, M, Mapelli, M, Giacobbo, N, Artale, M, Ghirlanda, G, Toffano M., Mapelli M., Giacobbo N., Artale M. C., and Ghirlanda G.
Abstract: We explore the host galaxies of compact-object binaries (black hole–black hole binaries, BHBs; neutron star–black hole binaries, NSBHs; double–neutron stars; DNSs) across cosmic time, by means of population-synthesis simulations combined with the Illustris cosmological simulation. At high redshift (z 4), the host galaxies of BHBs, NSBHs, and DNSs are very similar and are predominantly low-mass galaxies (stellar mass M < 1011 M). If z 4, most compact objects form and merge in the same galaxy, with a short delay time. At low redshift (z ≤ 2), the host galaxy populations of DNSs differ significantly from the host galaxies of both BHBs and NSBHs. DNSs merging at low redshift tend to form and merge in the same galaxy, with relatively short delay time. The stellar mass of DNS hosts peaks around ∼1010–1011 M. In contrast, BHBs and NSBHs merging at low redshift tend to form in rather small galaxies at high redshift and then to merge in larger galaxies with long delay times. This difference between DNSs and black hole binaries is a consequence of their profoundly different metallicity dependence.
Published: 2019

43. Black hole formation in the context of dissipative dark matter

Author: Latif, M, Lupi, A, Schleicher, D, D'Amico, G, Panci, P, Bovino, S, Latif M. A., Lupi A., Schleicher D. R. G., D'Amico G., Panci P., Bovino S., Latif, M, Lupi, A, Schleicher, D, D'Amico, G, Panci, P, Bovino, S, Latif M. A., Lupi A., Schleicher D. R. G., D'Amico G., Panci P., and Bovino S.
Abstract: Black holes with masses of 106-109 M dwell in the centres of most galaxies, but their formation mechanisms are not well known. A subdominant dissipative component of dark matter with similar properties to the ordinary baryons, known as mirror dark matter, may collapse to form massive black holes during the epoch of first galaxies formation. In this study, we explore the possibility of massive black hole formation via this alternative scenario. We perform three-dimensional cosmological simulations for four distinct haloes and compare their thermal, chemical, and dynamical evolution in both the ordinary and the mirror sectors. We find that the collapse of haloes is significantly delayed in the mirror sector due to the lack of H2 cooling and only haloes with masses above ≥107 M are formed. Overall, the mass inflow rates are ≥10−2 M yr−1 and there is less fragmentation. This suggests that the conditions for the formation of massive objects, including black holes, are more favourable in the mirror sector.
Published: 2019

44. Associating host galaxy candidates to massive black hole binaries resolved by pulsar timing arrays

Author: Goldstein, J, Sesana, A, Holgado, A, Veitch, J, Goldstein J. M., Sesana A., Holgado A. M., Veitch J., Goldstein, J, Sesana, A, Holgado, A, Veitch, J, Goldstein J. M., Sesana A., Holgado A. M., and Veitch J.
Abstract: We propose a novel methodology to select host galaxy candidates of future pulsar timing array (PTA) detections of resolved gravitational waves (GWs) from massive black hole binaries (MBHBs). The method exploits the physical dependence of the GW amplitude on the MBHB chirp mass and distance to the observer, together with empirical MBH mass-host galaxy correlations, to rank potential host galaxies in the mass-redshift plane. This is coupled to a null-stream-based likelihood evaluation of the GW amplitude and sky position in a Bayesian framework that assigns to each galaxy a probability of hosting the MBHB generating the GW signal. We test our algorithm on a set of realistic simulations coupling the likely properties of the first PTA resolved GW signal to synthetic all-sky galaxy maps. For a foreseeable PTA sky-localization precision of 100 deg2, we find that the GW source is hosted with 50 per cent (90 per cent) probability within a restricted number of ≤ 50(≤ 500) potential hosts. These figures are orders of magnitude smaller than the total number of galaxies within the PTA sky error-box, enabling extensive electromagnetic follow-up campaigns on a limited number of targets.
Published: 2019

45. Post-Newtonian evolution of massive black hole triplets in galactic nuclei – IV. Implications for LISA

Author: Bonetti, M, Sesana, A, Haardt, F, Barausse, E, Colpi, M, Bonetti, Matteo, Sesana, Alberto, Haardt, Francesco, Barausse, Enrico, Colpi, Monica, Bonetti, M, Sesana, A, Haardt, F, Barausse, E, Colpi, M, Bonetti, Matteo, Sesana, Alberto, Haardt, Francesco, Barausse, Enrico, and Colpi, Monica
Abstract: Coalescing massive black hole binaries (MBHBs) of 104-7M⊙, forming in the aftermath of galaxy mergers, are primary targets of the space mission LISA, the Laser Interferometer Space Antenna. An assessment of LISA detection prospects requires an estimate of the abundance and properties of MBHBs that form and evolve during the assembly of cosmic structures. To this aim, we employ a semi-analytic model to follow the co-evolution of MBHBs within their host galaxies. We identify three major evolutionary channels driving the binaries to coalescence: two standard paths along which the binary evolution is driven by interactions with the stellar and/or gaseous environment, and a novel channel where MBHB coalescence occurs during the interaction with a third black hole. For each channel, we follow the orbital evolution of MBHBs with physically motivated models that include a self-consistent treatment of the orbital eccentricity. We find that LISA will detect between ≈25 and ≈75 events per year depending on the seed model. We show that triple-induced coalescences can range from a few detected events up to ∼30 per cent of the total detected mergers. Moreover, even if the standard gas/stars-driven evolutionary channels should fail and MBHBs were to stall, triple interactions would still occur as a result of the hierarchical nature of galaxy formation, resulting in about ≈10 to ≈20 LISA detections per year. Remarkably, triple interactions among the black holes can produce coalescing binaries with large eccentricities (≥ 0.9) upon entrance into the LISA band. This eccentricity will remain significant (∼0.1) also at merger, requiring suitable templates for parameter estimation.
Published: 2019

46. The lifetime of binary black holes in Sérsic galaxy models

Author: Biava, N, Colpi, M, Capelo, P, Bonetti, M, Volonteri, M, Tamfal, T, Mayer, L, Sesana, A, Biava, Nadia, Colpi, Monica, Capelo, Pedro R, Bonetti, Matteo, Volonteri, Marta, Tamfal, Tomas, Mayer, Lucio, Sesana, Alberto, Biava, N, Colpi, M, Capelo, P, Bonetti, M, Volonteri, M, Tamfal, T, Mayer, L, Sesana, A, Biava, Nadia, Colpi, Monica, Capelo, Pedro R, Bonetti, Matteo, Volonteri, Marta, Tamfal, Tomas, Mayer, Lucio, and Sesana, Alberto
Abstract: In the local Universe, black holes of are hosted in galaxies displaying a variety of stellar profiles and morphologies. These black holes are the anticipated targets of LISA, the Laser Interferometer Space Antenna that will detect the low-frequency gravitational-wave signal emitted by binary black holes in this mass interval. In this paper, we infer upper limits on the lifetime of binary black holes of and up to , forming in galaxy mergers, exploring two underlying stellar density profiles, by Dehnen and by Prugniel & Simien, and by exploiting local scaling relations between the mass of the black holes and several quantities of their hosts. We focus on the phase of the dynamical evolution when the binary is transitioning from the hardening phase ruled by the interaction with single stars to the phase driven by the emission of gravitational waves. We find that different stellar profiles predict very distinct trends with binary mass, with lifetimes ranging between fractions of a Gyr to more than 10Gyr, and with a spread of about one order of magnitude, given by the uncertainties in the observed correlations, which are larger in the low-mass tail of the observed black hole population
Published: 2019

47. Star cluster disruption by a massive black hole binary

Author: Bortolas, E, Mapelli, M, Spera, M, Bortolas E., Mapelli M., Spera M., Bortolas, E, Mapelli, M, Spera, M, Bortolas E., Mapelli M., and Spera M.
Abstract: Massive black hole binaries (BHBs) are expected to form as the result of galaxy mergers; they shrink via dynamical friction and stellar scatterings, until gravitational waves (GWs) bring them to the final coalescence. It has been argued that BHBs may stall at a parsec scale and never enter the GW stage if stars are not continuously supplied to the BHB loss cone. Here, we perform several N-body experiments to study the effect of an 8 × 104M⊙ stellar cluster (SC) infalling on a parsec-scale BHB. We explore different orbital elements for the SC, and we perform runs both with and without accounting for the influence of a rigid stellar cusp (modelled as a rigid Dehnen potential). We find that the semimajor axis of the BHB shrinks by ≳ 10 per cent if the SC is on a nearly radial orbit; the shrinking is more efficient when a Dehnen potential is included and the orbital plane of the SC coincides with that of the BHB. In contrast, if the SC orbit has non-zero angular momentum, only few stars enter the BHB loss cone and the resulting BHB shrinking is negligible. Our results indicate that SC disruption might significantly contribute to the shrinking of a parsec-scale BHB only if the SC approaches the BHB on a nearly radial orbit.
Published: 2018

48. AGN mass estimates in large spectroscopic surveys: The effect of host galaxy light

Author: Varisco, L, Sbarrato, T, Calderone, G, Dotti, M, VARISCO, LUDOVICA, Varisco, L, Sbarrato, T, Calderone, G, Dotti, M, and VARISCO, LUDOVICA
Abstract: Virial-based methods for estimating active supermassive black hole masses are now commonly used on extremely large spectroscopic quasar catalogs. Most spectral analyses, though, do not pay enough attention to the detailed continuum decomposition. To understand how this affects virial mass estimates, we test the influence of host galaxy light on them, along with a Balmer continuum component. A detailed fit with the new spectroscopic analysis software QSFIT demonstrates that the presence or absence of continuum components does not significantly affect the virial-based results for our sample. Taking a host galaxy component into consideration or not, instead, affects the emission line fitting in a more pronounced way at lower redshifts, where in fact we observe dimmer quasars and more visible host galaxies.
Published: 2018

49. Study of the orientation of narrow-line Seyfert i

Author: Sbarrato, T, Dotti, M, Ghirlanda, G, Tavecchio, F, Sbarrato, T, Dotti, M, Ghirlanda, G, and Tavecchio, F
Abstract: We study a sample of narrow-line Seyfert 1 galaxies (NLS1) in their optical and radio features to understand the differences between their radio silent, radio-loud, and radio-quiet subclasses. We first show that the different redshift and mass distributions of radio-loud and radio-quiet NLS1s could be ascribed to observational biases. We then present a geometrical model according to which most of the different observational features of radio-loud and radio-quiet NLS1s are ascribed to the orientation of an intrinsically structured jet. We estimate the fraction of intrinsically jetted sources among NLS1s that justifies the observed radio-detected population. Noticeably, under the assumptions of the geometrical model, we derive a fraction of jetted sources significantly larger than in standard AGN.
Published: 2018

50. Study of the orientation of narrow-line Seyfert i

Author: Sbarrato, T, Dotti, M, Ghirlanda, G, Tavecchio, F, Sbarrato, T, Dotti, M, Ghirlanda, G, and Tavecchio, F
Abstract: We study a sample of narrow-line Seyfert 1 galaxies (NLS1) in their optical and radio features to understand the differences between their radio silent, radio-loud, and radio-quiet subclasses. We first show that the different redshift and mass distributions of radio-loud and radio-quiet NLS1s could be ascribed to observational biases. We then present a geometrical model according to which most of the different observational features of radio-loud and radio-quiet NLS1s are ascribed to the orientation of an intrinsically structured jet. We estimate the fraction of intrinsically jetted sources among NLS1s that justifies the observed radio-detected population. Noticeably, under the assumptions of the geometrical model, we derive a fraction of jetted sources significantly larger than in standard AGN.
Published: 2018

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