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1. Comparing recent PTA results on the nanohertz stochastic gravitational wave background

Author

The International Pulsar Timing Array Collaboration, Agazie, G., Antoniadis, J., Anumarlapudi, A., Archibald, A. M., Arumugam, P., Arumugam, S., Arzoumanian, Z., Askew, J., Babak, S., Bagchi, M., Bailes, M., Nielsen, A. -S. Bak, Baker, P. T., Bassa, C. G., Bathula, A., Bécsy, B., Berthereau, A., Bhat, N. D. R., Blecha, L., Bonetti, M., Bortolas, E., Brazier, A., Brook, P. R., Burgay, M., Burke-Spolaor, S., Burnette, R., Caballero, R. N., Cameron, A., Case, R., Chalumeau, A., Champion, D. J., Chanlaridis, S., Charisi, M., Chatterjee, S., Chatziioannou, K., Cheeseboro, B. D., Chen, S., Chen, Z. -C., Cognard, I., Cohen, T., Coles, W. A., Cordes, J. M., Cornish, N. J., Crawford, F., Cromartie, H. T., Crowter, K., Curyło, M., Cutler, C. J., Dai, S., Dandapat, S., Deb, D., DeCesar, M. E., DeGan, D., Demorest, P. B., Deng, H., Desai, S., Desvignes, G., Dey, L., Dhanda-Batra, N., Di Marco, V., Dolch, T., Drachler, B., Dwivedi, C., Ellis, J. A., Falxa, M., Feng, Y., Ferdman, R. D., Ferrara, E. C., Fiore, W., Fonseca, E., Franchini, A., Freedman, G. E., Gair, J. R., Garver-Daniels, N., Gentile, P. A., Gersbach, K. A., Glaser, J., Good, D. C., Goncharov, B., Gopakumar, A., Graikou, E., Grießmeier, J. -M., Guillemot, L., Gültekin, K., Guo, Y. J., Gupta, Y., Grunthal, K., Hazboun, J. S., Hisano, S., Hobbs, G. B., Hourihane, S., Hu, H., Iraci, F., Islo, K., Izquierdo-Villalba, D., Jang, J., Jawor, J., Janssen, G. H., Jennings, R. J., Jessner, A., Johnson, A. D., Jones, M. L., Joshi, B. C., Kaiser, A. R., Kaplan, D. L., Kapur, A., Kareem, F., Karuppusamy, R., Keane, E. F., Keith, M. J., Kelley, L. Z., Kerr, M., Key, J. S., Kharbanda, D., Kikunaga, T., Klein, T. C., Kolhe, N., Kramer, M., Krishnakumar, M. A., Kulkarni, A., Laal, N., Lackeos, K., Lam, M. T., Lamb, W. G., Larsen, B. B., Lazio, T. J. W., Lee, K. J., Levin, Y., Lewandowska, N., Littenberg, T. B., Liu, K., Liu, T., Liu, Y., Lommen, A., Lorimer, D. R., Lower, M. E., Luo, J., Luo, R., Lynch, R. S., Lyne, A. G., Ma, C. -P., Maan, Y., Madison, D. R., Main, R. A., Manchester, R. N., Mandow, R., Mattson, M. A., McEwen, A., McKee, J. W., McLaughlin, M. A., McMann, N., Meyers, B. W., Meyers, P. M., Mickaliger, M. B., Miles, M., Mingarelli, C. M. F., Mitridate, A., Natarajan, P., Nathan, R. S., Ng, C., Nice, D. J., Niţu, I. C., Nobleson, K., Ocker, S. K., Olum, K. D., Osłowski, S., Paladi, A. K., Parthasarathy, A., Pennucci, T. T., Perera, B. B. P., Perrodin, D., Petiteau, A., Petrov, P., Pol, N. S., Porayko, N. K., Possenti, A., Prabu, T., Leclere, H. Quelquejay, Radovan, H. A., Rana, P., Ransom, S. M., Ray, P. S., Reardon, D. J., Rogers, A. F., Romano, J. D., Russell, C. J., Samajdar, A., Sanidas, S. A., Sardesai, S. C., Schmiedekamp, A., Schmiedekamp, C., Schmitz, K., Schult, L., Sesana, A., Shaifullah, G., Shannon, R. M., Shapiro-Albert, B. J., Siemens, X., Simon, J., Singha, J., Siwek, M. S., Speri, L., Spiewak, R., Srivastava, A., Stairs, I. H., Stappers, B. W., Stinebring, D. R., Stovall, K., Sun, J. P., Surnis, M., Susarla, S. C., Susobhanan, A., Swiggum, J. K., Takahashi, K., Tarafdar, P., Taylor, J., Taylor, S. R., Theureau, G., Thrane, E., Thyagarajan, N., Tiburzi, C., Toomey, L., Turner, J. E., Unal, C., Vallisneri, M., van der Wateren, E., van Haasteren, R., Vecchio, A., Krishnan, V. Venkatraman, Verbiest, J. P. W., Vigeland, S. J., Wahl, H. M., Wang, S., Wang, Q., Witt, C. A., Wang, J., Wang, L., Wayt, K. E., Wu, Z., Young, O., Zhang, L., Zhang, S., Zhu, X. -J., and Zic, A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

The Australian, Chinese, European, Indian, and North American pulsar timing array (PTA) collaborations recently reported, at varying levels, evidence for the presence of a nanohertz gravitational wave background (GWB). Given that each PTA made different choices in modeling their data, we perform a comparison of the GWB and individual pulsar noise parameters across the results reported from the PTAs that constitute the International Pulsar Timing Array (IPTA). We show that despite making different modeling choices, there is no significant difference in the GWB parameters that are measured by the different PTAs, agreeing within $1\sigma$. The pulsar noise parameters are also consistent between different PTAs for the majority of the pulsars included in these analyses. We bridge the differences in modeling choices by adopting a standardized noise model for all pulsars and PTAs, finding that under this model there is a reduction in the tension in the pulsar noise parameters. As part of this reanalysis, we "extended" each PTA's data set by adding extra pulsars that were not timed by that PTA. Under these extensions, we find better constraints on the GWB amplitude and a higher signal-to-noise ratio for the Hellings and Downs correlations. These extensions serve as a prelude to the benefits offered by a full combination of data across all pulsars in the IPTA, i.e., the IPTA's Data Release 3, which will involve not just adding in additional pulsars, but also including data from all three PTAs where any given pulsar is timed by more than as single PTA., Comment: 21 pages, 9 figures, submitted to ApJ

Published
2023

2. Searching for continuous Gravitational Waves in the second data release of the International Pulsar Timing Array

Author

Falxa, M., Babak, S., Baker, P. T., Bécsy, B., Chalumeau, A., Chen, S., Chen, Z., Cornish, N. J., Guillemot, L., Hazboun, J. S., Mingarelli, C. M. F., Parthasarathy, A., Petiteau, A., Pol, N. S., Sesana, A., Spolaor, S. B., Taylor, S. R., Theureau, G., Vallisneri, M., Vigeland, S. J., Witt, C. A., Zhu, X., Antoniadis, J., Arzoumanian, Z., Bailes, M., Bhat, N. D. R., Blecha, L., Brazier, A., Brook, P. R., Caballero, N., Cameron, A. D., Casey-Clyde, J. A., Champion, D., Charisi, M., Chatterjee, S., Cognard, I., Cordes, J. M., Crawford, F., Cromartie, H. T., Crowter, K., Dai, S., DeCesar, M. E., Demorest, P. B., Desvignes, G., Dolch, T., Drachler, B., Feng, Y., Ferrara, E. C., Fiore, W., Fonseca, E., Garver-Daniels, N., Glaser, J., Goncharov, B., Good, D. C., Griessmeier, J., Guo, Y. J., Gültekin, K., Hobbs, G., Hu, H., Islo, K., Jang, J., Jennings, R. J., Johnson, A. D., Jones, M. L., Kaczmarek, J., Kaiser, A. R., Kaplan, D. L., Keith, M., Kelley, L. Z., Kerr, M., Key, J. S., Laal, N., Lam, M. T., Lamb, W. G., Lazio, T. J. W., Liu, K., Liu, T., Luo, J., Lynch, R. S., Madison, D. R., Main, R., Manchester, R., McEwen, A., McKee, J., McLaughlin, M. A., Ng, C., Nice, D. J., Ocker, S., Olum, K. D., Osłowski, S., Pennucci, T. T., Perera, B. B. P., Perrodin, D., Porayko, N., Possenti, A., Quelquejay-Leclere, H., Ransom, S. M., Ray, P. S., Reardon, D. J., Russell, C. J., Samajdar, A., Sarkissian, J., Schult, L., Shaifullah, G., Shannon, R. M., Shapiro-Albert, B. J., Siemens, X., Simon, J. J., Siwek, M., Smith, T. L., Speri, L., Spiewak, R., Stairs, I. H., Stappers, B., Stinebring, D. R., Swiggum, J. K., Tiburzi, C., Turner, J., Vecchio, A., Verbiest, J. P. W., Wahl, H., Wang, S. Q., Wang, J., Wu, Z., Zhang, L., and Zhang, S.

Subjects
General Relativity and Quantum Cosmology, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The International Pulsar Timing Array 2nd data release is the combination of datasets from worldwide collaborations. In this study, we search for continuous waves: gravitational wave signals produced by individual supermassive black hole binaries in the local universe. We consider binaries on circular orbits and neglect the evolution of orbital frequency over the observational span. We find no evidence for such signals and set sky averaged 95% upper limits on their amplitude h 95 . The most sensitive frequency is 10nHz with h 95 = 9.1 10-15 . We achieved the best upper limit to date at low and high frequencies of the PTA band thanks to improved effective cadence of observations. In our analysis, we have taken into account the recently discovered common red noise process, which has an impact at low frequencies. We also find that the peculiar noise features present in some pulsars data must be taken into account to reduce the false alarm. We show that using custom noise models is essential in searching for continuous gravitational wave signals and setting the upper limit.

Published
2023
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3. The International Pulsar Timing Array second data release: Search for an isotropic Gravitational Wave Background

Author

Antoniadis, J., Arzoumanian, Z., Babak, S., Bailes, M., Nielsen, A. -S. Bak, Baker, P. T., Bassa, C. G., Becsy, B., Berthereau, A., Bonetti, M., Brazier, A., Brook, P. R., Burgay, M., Burke-Spolaor, S., Caballero, R. N., Casey-Clyde, J. A., Chalumeau, A., Champion, D. J., Charisi, M., Chatterjee, S., Chen, S., Cognard, I., Cordes, J. M., Cornish, N. J., Crawford, F., Cromartie, H. T., Crowter, K., Dai, S., DeCesar, M. E., Demorest, P. B., Desvignes, G., Dolch, T., Drachler, B., Falxa, M., Ferrara, E. C., Fiore, W., Fonseca, E., Gair, J. R., Garver-Daniels, N., Goncharov, B., Good, D. C., Graikou, E., Guillemot, L., Guo, Y. J., Hazboun, J. S., Hobbs, G., Hu, H., Islo, K., Janssen, G. H., Jennings, R. J., Johnson, A. D., Jones, M. L., Kaiser, A. R., Kaplan, D. L., Karuppusamy, R., Keith, M. J., Kelley, L. Z., Kerr, M., Key, J. S., Kramer, M., Lam, M. T., Lamb, W. G., Lazio, T. J. W., Lee, K. J., Lentati, L., Liu, K., Luo, J., Lynch, R. S., Lyne, A. G., Madison, D. R., Main, R. A., Manchester, R. N., McEwen, A., McKee, J. W., McLaughlin, M. A., Mickaliger, M. B., Mingarelli, C. M. F., Ng, C., Nice, D. J., lowski, S. Os, Parthasarathy, A., Pennucci, T. T., Perera, B. B. P., Perrodin, D., Petiteau, A., Pol, N. S., Porayko, N. K., Possenti, A., Ransom, S. M., Ray, P. S., Reardon, D. J., Russell, C. J., Samajdar, A., Sampson, L. M., Sanidas, S., Sarkissian, J. M., Schmitz, K., Schult, L., Sesana, A., Shaifullah, G., Shannon, R. M., Shapiro-Albert, B. J., Siemens, X., Simon, J., Smith, T. L., Speri, L., Spiewak, R., Stairs, I. H., Stappers, B. W., Stinebring, D. R., Swiggum, J. K., Taylor, S. R., Theureau, G., Tiburzi, C., Vallisneri, M., van der Wateren, E., Vecchio, A., Verbiest, J. P. W., Vigeland, S. J., Wahl, H., Wang, J. B., Wang, J., Wang, L., Witt, C. A., Zhang, S., and Zhu, X. J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We searched for an isotropic stochastic gravitational wave background in the second data release of the International Pulsar Timing Array, a global collaboration synthesizing decadal-length pulsar-timing campaigns in North America, Europe, and Australia. In our reference search for a power law strain spectrum of the form $h_c = A(f/1\,\mathrm{yr}^{-1})^{\alpha}$, we found strong evidence for a spectrally-similar low-frequency stochastic process of amplitude $A = 3.8^{+6.3}_{-2.5}\times10^{-15}$ and spectral index $\alpha = -0.5 \pm 0.5$, where the uncertainties represent 95\% credible regions, using information from the auto- and cross-correlation terms between the pulsars in the array. For a spectral index of $\alpha = -2/3$, as expected from a population of inspiralling supermassive black hole binaries, the recovered amplitude is $A = 2.8^{+1.2}_{-0.8}\times10^{-15}$. Nonetheless, no significant evidence of the Hellings-Downs correlations that would indicate a gravitational-wave origin was found. We also analyzed the constituent data from the individual pulsar timing arrays in a consistent way, and clearly demonstrate that the combined international data set is more sensitive. Furthermore, we demonstrate that this combined data set produces comparable constraints to recent single-array data sets which have more data than the constituent parts of the combination. Future international data releases will deliver increased sensitivity to gravitational wave radiation, and significantly increase the detection probability., Comment: 17 pages, 12 figures, accepted in MNRAS

Published
2022
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4. Testing the relativistic Doppler boost hypothesis for supermassive black hole binary candidates

Author

Charisi, M., Haiman, Z., Schiminovich, D., and D'Orazio, D. J.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Supermassive black hole binaries (SMBHBs) should be common in galactic nuclei as a result of frequent galaxy mergers. Recently, a large sample of sub-parsec SMBHB candidates was identified as bright periodically variable quasars in optical surveys. If the observed periodicity corresponds to the redshifted binary orbital period, the inferred orbital velocities are relativistic (v/c~0.1). The optical and UV luminosities are expected to arise from gas bound to the individual BHs, and would be modulated by the relativistic Doppler effect. The optical and UV light curves should vary in tandem with relative amplitudes which depend on the respective spectral slopes. We constructed a control sample of 42 quasars with aperiodic variability, to test whether this Doppler colour signature can be distinguished from intrinsic chromatic variability. We found that the Doppler signature can arise by chance in ~20% (~37%) of quasars in the nUV (fUV) band. These probabilities reflect the limited quality of the control sample and represent upper limits on how frequently quasars mimic the Doppler brightness+colour variations. We performed separate tests on the periodic quasar candidates, and found that for the majority, the Doppler boost hypothesis requires an unusually steep UV spectrum or an unexpectedly large BH mass and orbital velocity. We conclude that at most ~1/3rd of these periodic candidates can harbor Doppler-modulated SMBHBs., Comment: submitted in MNRAS

Published
2018
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5. A Population of Short-Period Variable Quasars from PTF as Supermassive Black Hole Binary Candidates

Author

Charisi, M., Bartos, I., Haiman, Z., Price-Whelan, A. M., Graham, M. J., Bellm, E. C., Laher, R. R., and Marka, S.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Supermassive black hole binaries (SMBHBs) at sub-parsec separations should be common in galactic nuclei, as a result of frequent galaxy mergers. Hydrodynamical simulations of circumbinary discs predict strong periodic modulation of the mass accretion rate on time-scales comparable to the orbital period of the binary. As a result, SMBHBs may be recognized by the periodic modulation of their brightness. We conducted a statistical search for periodic variability in a sample of 35,383 spectroscopically confirmed quasars in the photometric database of the Palomar Transient Factory (PTF). We analysed Lomb-Scargle periodograms and assessed the significance of our findings by modeling each individual quasar's variability as a damped random walk (DRW). We identified 50 quasars with significant periodicity beyond the DRW model, typically with short periods of a few hundred days. We find 33 of these to remain significant after a re-analysis of their periodograms including additional optical data from the intermediate-PTF and the Catalina Real-Time Transient Survey (CRTS). Assuming that the observed periods correspond to the redshifted orbital periods of SMBHBs, we conclude that our findings are consistent with a population of unequal-mass SMBHBs, with a typical mass ratio as low as q = M2/M1 ~ 0.01., Comment: MNRAS (accepted), new section 4.7

Published
2016
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6. NANOGrav 15-year gravitational-wave background methods

Author

Johnson, AD, Meyers, PM, Baker, PT, Cornish, NJ, Hazboun, JS, Littenberg, TB, Romano, JD, Taylor, SR, Vallisneri, M, Vigeland, SJ, Olum, KD, Siemens, X, Ellis, JA, Van Haasteren, R, Hourihane, S, Agazie, G, Anumarlapudi, A, Archibald, AM, Arzoumanian, Z, Blecha, L, Brazier, A, Brook, PR, Burke-Spolaor, S, Bécsy, B, Casey-Clyde, JA, Charisi, M, Chatterjee, S, Chatziioannou, K, Cohen, T, Cordes, JM, Crawford, F, Cromartie, HT, Crowter, K, Decesar, ME, Demorest, PB, Dolch, T, Drachler, B, Ferrara, EC, Fiore, W, Fonseca, E, Freedman, GE, Garver-Daniels, N, Gentile, PA, Glaser, J, Good, DC, Gültekin, K, Jennings, RJ, Jones, ML, Kaiser, AR, Kaplan, DL, Kelley, LZ, Kerr, M, Key, JS, Laal, N, Lam, MT, Lamb, WG, Lazio, TJW, Lewandowska, N, Liu, T, Lorimer, DR, Luo, J, Lynch, RS, Ma, CP, Madison, DR, McEwen, A, McKee, JW, McLaughlin, MA, McMann, N, Meyers, BW, Mingarelli, CMF, Mitridate, A, Ng, C, Nice, DJ, Ocker, SK, Pennucci, TT, Perera, BBP, Pol, NS, Radovan, HA, Ransom, SM, Ray, PS, Sardesai, SC, Schmiedekamp, C, Schmiedekamp, A, Schmitz, K, Shapiro-Albert, BJ, Simon, J, Siwek, MS, Stairs, IH, Stinebring, DR, Stovall, K, Susobhanan, A, Swiggum, JK, Turner, JE, Unal, C, Wahl, HM, Witt, CA, Young, O, Johnson, AD, Meyers, PM, Baker, PT, Cornish, NJ, Hazboun, JS, Littenberg, TB, Romano, JD, Taylor, SR, Vallisneri, M, Vigeland, SJ, Olum, KD, Siemens, X, Ellis, JA, Van Haasteren, R, Hourihane, S, Agazie, G, Anumarlapudi, A, Archibald, AM, Arzoumanian, Z, Blecha, L, Brazier, A, Brook, PR, Burke-Spolaor, S, Bécsy, B, Casey-Clyde, JA, Charisi, M, Chatterjee, S, Chatziioannou, K, Cohen, T, Cordes, JM, Crawford, F, Cromartie, HT, Crowter, K, Decesar, ME, Demorest, PB, Dolch, T, Drachler, B, Ferrara, EC, Fiore, W, Fonseca, E, Freedman, GE, Garver-Daniels, N, Gentile, PA, Glaser, J, Good, DC, Gültekin, K, Jennings, RJ, Jones, ML, Kaiser, AR, Kaplan, DL, Kelley, LZ, Kerr, M, Key, JS, Laal, N, Lam, MT, Lamb, WG, Lazio, TJW, Lewandowska, N, Liu, T, Lorimer, DR, Luo, J, Lynch, RS, Ma, CP, Madison, DR, McEwen, A, McKee, JW, McLaughlin, MA, McMann, N, Meyers, BW, Mingarelli, CMF, Mitridate, A, Ng, C, Nice, DJ, Ocker, SK, Pennucci, TT, Perera, BBP, Pol, NS, Radovan, HA, Ransom, SM, Ray, PS, Sardesai, SC, Schmiedekamp, C, Schmiedekamp, A, Schmitz, K, Shapiro-Albert, BJ, Simon, J, Siwek, MS, Stairs, IH, Stinebring, DR, Stovall, K, Susobhanan, A, Swiggum, JK, Turner, JE, Unal, C, Wahl, HM, Witt, CA, and Young, O

Published
2024

7. Astrophysics with the Laser Interferometer Space Antenna

Author

Amaro-Seoane, P, Andrews, J, Arca Sedda, M, Askar, A, Baghi, Q, Balasov, R, Bartos, I, Bavera, S, Bellovary, J, Berry, C, Berti, E, Bianchi, S, Blecha, L, Blondin, S, Bogdanović, T, Boissier, S, Bonetti, M, Bonoli, S, Bortolas, E, Breivik, K, Capelo, P, Caramete, L, Cattorini, F, Charisi, M, Chaty, S, Chen, X, Chruślińska, M, Chua, A, Church, R, Colpi, M, D’Orazio, D, Danielski, C, Davies, M, Dayal, P, De Rosa, A, Derdzinski, A, Destounis, K, Dotti, M, Duţan, I, Dvorkin, I, Fabj, G, Foglizzo, T, Ford, S, Fouvry, J, Franchini, A, Fragos, T, Fryer, C, Gaspari, M, Gerosa, D, Graziani, L, Groot, P, Habouzit, M, Haggard, D, Haiman, Z, Han, W, Istrate, A, Johansson, P, Khan, F, Kimpson, T, Kokkotas, K, Kong, A, Korol, V, Kremer, K, Kupfer, T, Lamberts, A, Larson, S, Lau, M, Liu, D, Lloyd-Ronning, N, Lodato, G, Lupi, A, Ma, C, Maccarone, T, Mandel, I, Mangiagli, A, Mapelli, M, Mathis, S, Mayer, L, Mcgee, S, Mckernan, B, Miller, M, Mota, D, Mumpower, M, Nasim, S, Nelemans, G, Noble, S, Pacucci, F, Panessa, F, Paschalidis, V, Pfister, H, Porquet, D, Quenby, J, Ricarte, A, Röpke, F, Regan, J, Rosswog, S, Ruiter, A, Ruiz, M, Runnoe, J, Schneider, R, Amaro-Seoane P., Andrews J., Arca Sedda M., Askar A., Baghi Q., Balasov R., Bartos I., Bavera S. S., Bellovary J., Berry C. P. L., Berti E., Bianchi S., Blecha L., Blondin S., Bogdanović T., Boissier S., Bonetti M., Bonoli S., Bortolas E., Breivik K., Capelo P. R., Caramete L., Cattorini F., Charisi M., Chaty S., Chen X., Chruślińska M., Chua A. J. K., Church R., Colpi M., D’Orazio D., Danielski C., Davies M. B., Dayal P., De Rosa A., Derdzinski A., Destounis K., Dotti M., Duţan I., Dvorkin I., Fabj G., Foglizzo T., Ford S., Fouvry J. B., Franchini A., Fragos T., Fryer C., Gaspari M., Gerosa D., Graziani L., Groot P., Habouzit M., Haggard D., Haiman Z., Han W. B., Istrate A., Johansson P. H., Khan F. M., Kimpson T., Kokkotas K., Kong A., Korol V., Kremer K., Kupfer T., Lamberts A., Larson S., Lau M., Liu D., Lloyd-Ronning N., Lodato G., Lupi A., Ma C. P., Maccarone T., Mandel I., Mangiagli A., Mapelli M., Mathis S., Mayer L., McGee S., McKernan B., Miller M. C., Mota D. F., Mumpower M., Nasim S. S., Nelemans G., Noble S., Pacucci F., Panessa F., Paschalidis V., Pfister H., Porquet D., Quenby J., Ricarte A., Röpke F. K., Regan J., Rosswog S., Ruiter A., Ruiz M., Runnoe J., Schneider R., Amaro-Seoane, P, Andrews, J, Arca Sedda, M, Askar, A, Baghi, Q, Balasov, R, Bartos, I, Bavera, S, Bellovary, J, Berry, C, Berti, E, Bianchi, S, Blecha, L, Blondin, S, Bogdanović, T, Boissier, S, Bonetti, M, Bonoli, S, Bortolas, E, Breivik, K, Capelo, P, Caramete, L, Cattorini, F, Charisi, M, Chaty, S, Chen, X, Chruślińska, M, Chua, A, Church, R, Colpi, M, D’Orazio, D, Danielski, C, Davies, M, Dayal, P, De Rosa, A, Derdzinski, A, Destounis, K, Dotti, M, Duţan, I, Dvorkin, I, Fabj, G, Foglizzo, T, Ford, S, Fouvry, J, Franchini, A, Fragos, T, Fryer, C, Gaspari, M, Gerosa, D, Graziani, L, Groot, P, Habouzit, M, Haggard, D, Haiman, Z, Han, W, Istrate, A, Johansson, P, Khan, F, Kimpson, T, Kokkotas, K, Kong, A, Korol, V, Kremer, K, Kupfer, T, Lamberts, A, Larson, S, Lau, M, Liu, D, Lloyd-Ronning, N, Lodato, G, Lupi, A, Ma, C, Maccarone, T, Mandel, I, Mangiagli, A, Mapelli, M, Mathis, S, Mayer, L, Mcgee, S, Mckernan, B, Miller, M, Mota, D, Mumpower, M, Nasim, S, Nelemans, G, Noble, S, Pacucci, F, Panessa, F, Paschalidis, V, Pfister, H, Porquet, D, Quenby, J, Ricarte, A, Röpke, F, Regan, J, Rosswog, S, Ruiter, A, Ruiz, M, Runnoe, J, Schneider, R, Amaro-Seoane P., Andrews J., Arca Sedda M., Askar A., Baghi Q., Balasov R., Bartos I., Bavera S. S., Bellovary J., Berry C. P. L., Berti E., Bianchi S., Blecha L., Blondin S., Bogdanović T., Boissier S., Bonetti M., Bonoli S., Bortolas E., Breivik K., Capelo P. R., Caramete L., Cattorini F., Charisi M., Chaty S., Chen X., Chruślińska M., Chua A. J. K., Church R., Colpi M., D’Orazio D., Danielski C., Davies M. B., Dayal P., De Rosa A., Derdzinski A., Destounis K., Dotti M., Duţan I., Dvorkin I., Fabj G., Foglizzo T., Ford S., Fouvry J. B., Franchini A., Fragos T., Fryer C., Gaspari M., Gerosa D., Graziani L., Groot P., Habouzit M., Haggard D., Haiman Z., Han W. B., Istrate A., Johansson P. H., Khan F. M., Kimpson T., Kokkotas K., Kong A., Korol V., Kremer K., Kupfer T., Lamberts A., Larson S., Lau M., Liu D., Lloyd-Ronning N., Lodato G., Lupi A., Ma C. P., Maccarone T., Mandel I., Mangiagli A., Mapelli M., Mathis S., Mayer L., McGee S., McKernan B., Miller M. C., Mota D. F., Mumpower M., Nasim S. S., Nelemans G., Noble S., Pacucci F., Panessa F., Paschalidis V., Pfister H., Porquet D., Quenby J., Ricarte A., Röpke F. K., Regan J., Rosswog S., Ruiter A., Ruiz M., Runnoe J., and Schneider R.

Abstract

The Laser Interferometer Space Antenna (LISA) will be a transformative experiment for gravitational wave astronomy, and, as such, it will offer unique opportunities to address many key astrophysical questions in a completely novel way. The synergy with ground-based and space-born instruments in the electromagnetic domain, by enabling multi-messenger observations, will add further to the discovery potential of LISA. The next decade is crucial to prepare the astrophysical community for LISA’s first observations. This review outlines the extensive landscape of astrophysical theory, numerical simulations, and astronomical observations that are instrumental for modeling and interpreting the upcoming LISA datastream. To this aim, the current knowledge in three main source classes for LISA is reviewed; ultra-compact stellar-mass binaries, massive black hole binaries, and extreme or interme-diate mass ratio inspirals. The relevant astrophysical processes and the established modeling techniques are summarized. Likewise, open issues and gaps in our understanding of these sources are highlighted, along with an indication of how LISA could help making progress in the different areas. New research avenues that LISA itself, or its joint exploitation with upcoming studies in the electromagnetic domain, will enable, are also illustrated. Improvements in modeling and analysis approaches, such as the combination of numerical simulations and modern data science techniques, are discussed. This review is intended to be a starting point for using LISA as a new discovery tool for understanding our Universe.

Published
2023

8. Searching for continuous Gravitational Waves in the second data release of the International Pulsar Timing Array

Author

Falxa, M, Babak, S, Baker, P T, Bécsy, B, Chalumeau, A, Chen, S, Chen, Z, Cornish, N J, Guillemot, L, Hazboun, J S, Mingarelli, C M F, Parthasarathy, A, Petiteau, A, Pol, N S, Sesana, A, Spolaor, S B, Taylor, S R, Theureau, G, Vallisneri, M, Vigeland, S J, Witt, C A, Zhu, X, Antoniadis, J, Arzoumanian, Z, Bailes, M, Bhat, N D R, Blecha, L, Brazier, A, Brook, P R, Caballero, N, Cameron, A D, Casey-Clyde, J A, Champion, D, Charisi, M, Chatterjee, S, Cognard, I, Cordes, J M, Crawford, F, Cromartie, H T, Crowter, K, Dai, S, DeCesar, M E, Demorest, P B, Desvignes, G, Dolch, T, Drachler, B, Feng, Y, Ferrara, E C, Fiore, W, Fonseca, E, Garver-Daniels, N, Glaser, J, Goncharov, B, Good, D C, Griessmeier, J, Guo, Y J, Gültekin, K, Hobbs, G, Hu, H, Islo, K, Jang, J, Jennings, R J, Johnson, A D, Jones, M L, Kaczmarek, J, Kaiser, A R, Kaplan, D L, Keith, M, Kelley, L Z, Kerr, M, Key, J S, Laal, N, Lam, M T, Lamb, W G, Lazio, T J W, Liu, K, Liu, T, Luo, J, Lynch, R S, Madison, D R, Main, R, Manchester, R, McEwen, A, McKee, J, McLaughlin, M A, Ng, C, Nice, D J, Ocker, S, Olum, K D, Osłowski, S, Pennucci, T T, Perera, B B P, Perrodin, D, Porayko, N, Possenti, A, Quelquejay-Leclere, H, Ransom, S M, Ray, P S, Reardon, D J, Russell, C J, Samajdar, A, Sarkissian, J, Schult, L, Shaifullah, G, Shannon, R M, Shapiro-Albert, B J, Siemens, X, Simon, J J, Siwek, M, Smith, T L, Speri, L, Spiewak, R, Stairs, I H, Stappers, B, Stinebring, D R, Swiggum, J K, Tiburzi, C, Turner, J, Vecchio, A, Verbiest, Joris, Wahl, H, Wang, S Q, Wang, J, Wang, Jun, Wu, Ziwei, Zhang, L, Zhang, S, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), and IPTA

Subjects
noise, data analysis method, gravitational radiation, orbit: circle, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), sensitivity, frequency: high, General Relativity and Quantum Cosmology, confidence limit, frequency: low, black hole: binary, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), pulsar
Abstract

The International Pulsar Timing Array 2nd data release is the combination ofdatasets from worldwide collaborations. In this study, we search for continuouswaves: gravitational wave signals produced by individual supermassive blackhole binaries in the local universe. We consider binaries on circular orbitsand neglect the evolution of orbital frequency over the observational span. Wefind no evidence for such signals and set sky averaged 95% upper limits ontheir amplitude h 95 . The most sensitive frequency is 10nHz with h 95 = 9.110-15 . We achieved the best upper limit to date at low and high frequencies ofthe PTA band thanks to improved effective cadence of observations. In ouranalysis, we have taken into account the recently discovered common red noiseprocess, which has an impact at low frequencies. We also find that the peculiarnoise features present in some pulsars data must be taken into account toreduce the false alarm. We show that using custom noise models is essential insearching for continuous gravitational wave signals and setting the upperlimit.

Published
2023

9. Searching for continuous Gravitational Waves in the second data release of the International Pulsar Timing Array

Author

Falxa, M, primary, Babak, S, additional, Baker, P T, additional, Bécsy, B, additional, Chalumeau, A, additional, Chen, S, additional, Chen, Z, additional, Cornish, N J, additional, Guillemot, L, additional, Hazboun, J S, additional, Mingarelli, C M F, additional, Parthasarathy, A, additional, Petiteau, A, additional, Pol, N S, additional, Sesana, A, additional, Spolaor, S B, additional, Taylor, S R, additional, Theureau, G, additional, Vallisneri, M, additional, Vigeland, S J, additional, Witt, C A, additional, Zhu, X, additional, Antoniadis, J, additional, Arzoumanian, Z, additional, Bailes, M, additional, Bhat, N D R, additional, Blecha, L, additional, Brazier, A, additional, Brook, P R, additional, Caballero, N, additional, Cameron, A D, additional, Casey-Clyde, J A, additional, Champion, D, additional, Charisi, M, additional, Chatterjee, S, additional, Cognard, I, additional, Cordes, J M, additional, Crawford, F, additional, Cromartie, H T, additional, Crowter, K, additional, Dai, S, additional, DeCesar, M E, additional, Demorest, P B, additional, Desvignes, G, additional, Dolch, T, additional, Drachler, B, additional, Feng, Y, additional, Ferrara, E C, additional, Fiore, W, additional, Fonseca, E, additional, Garver-Daniels, N, additional, Glaser, J, additional, Goncharov, B, additional, Good, D C, additional, Griessmeier, J, additional, Guo, Y J, additional, Gültekin, K, additional, Hobbs, G, additional, Hu, H, additional, Islo, K, additional, Jang, J, additional, Jennings, R J, additional, Johnson, A D, additional, Jones, M L, additional, Kaczmarek, J, additional, Kaiser, A R, additional, Kaplan, D L, additional, Keith, M, additional, Kelley, L Z, additional, Kerr, M, additional, Key, J S, additional, Laal, N, additional, Lam, M T, additional, Lamb, W G, additional, Lazio, T J W, additional, Liu, K, additional, Liu, T, additional, Luo, J, additional, Lynch, R S, additional, Madison, D R, additional, Main, R, additional, Manchester, R, additional, McEwen, A, additional, McKee, J, additional, McLaughlin, M A, additional, Ng, C, additional, Nice, D J, additional, Ocker, S, additional, Olum, K D, additional, Osłowski, S, additional, Pennucci, T T, additional, Perera, B B P, additional, Perrodin, D, additional, Porayko, N, additional, Possenti, A, additional, Quelquejay-Leclere, H, additional, Ransom, S M, additional, Ray, P S, additional, Reardon, D J, additional, Russell, C J, additional, Samajdar, A, additional, Sarkissian, J, additional, Schult, L, additional, Shaifullah, G, additional, Shannon, R M, additional, Shapiro-Albert, B J, additional, Siemens, X, additional, Simon, J J, additional, Siwek, M, additional, Smith, T L, additional, Speri, L, additional, Spiewak, R, additional, Stairs, I H, additional, Stappers, B, additional, Stinebring, D R, additional, Swiggum, J K, additional, Tiburzi, C, additional, Turner, J, additional, Vecchio, A, additional, Verbiest, J P W, additional, Wahl, H, additional, Wang, S Q, additional, Wang, J, additional, Wu, Z, additional, Zhang, L, additional, and Zhang, S, additional

Published
2023
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10. Multi-messenger Astrophysics with Pulsar Timing Arrays: Astro2020 Science White Paper

Author

Kelley, L. Z, Charisi, M, Burke-Spolaor, S, Simon, J, Blecha, L, Bogdanovic, T, Colpi, M, Comerford, J, D'Orazio, D, Dotti, M, Eracleous, M, Graham, M, Greene, J, Haiman, Z, Holley-Bockelmann, K, Kara, E, Kelly, Bernard J, Komossa, S, Larson, S, Liu, X, Ma, C. -P, Noble, Scott C, Paschalidis, V, Rafikov, R, Ravi, V, Runnoe, J, Sesana, A, Stern, D, Strauss, M. A, U, V, and Volonteri, M

Subjects
Astrophysics
Abstract

Pulsar timing arrays (PTAs) are on the verge of detecting low-frequency gravitational waves (GWs)from supermassive black hole binaries (SMBHBs). With continued observations of a large sampleof millisecond pulsars, PTAs will reach this major milestone within the next decade. Already,SMBHB candidates are being identied by electromagnetic surveys in ever-increasing numbers;upcoming surveys will enhance our ability to detect and verify candidates, and will be instrumentalin identifying the host galaxies of GW sources. Multi-messenger (GW and electromagnetic) obser-vations of SMBHBs will revolutionize our understanding of the co-evolution of SMBHs with theirhost galaxies, the dynamical interactions between binaries and their galactic environments, and thefundamental physics of accretion. Multi-messenger observations can also make SMBHBs `standardsirens' for cosmological distance measurements out to z ~ 0.5 LIGO has already ushered in break-through insights in our knowledge of black holes. The multi-messenger detection of SMBHBs withPTAs will be a breakthrough in the years 2020-2030 and beyond, and prepare us for LISA to helpcomplete our views of black hole demographics and evolution at higher redshifts.

Published
2019

11. The International Pulsar Timing Array second data release: Search for an isotropic gravitational wave background

Author

Antoniadis, J, primary, Arzoumanian, Z, additional, Babak, S, additional, Bailes, M, additional, Bak Nielsen, A-S, additional, Baker, P T, additional, Bassa, C G, additional, Bécsy, B, additional, Berthereau, A, additional, Bonetti, M, additional, Brazier, A, additional, Brook, P R, additional, Burgay, M, additional, Burke-Spolaor, S, additional, Caballero, R N, additional, Casey-Clyde, J A, additional, Chalumeau, A, additional, Champion, D J, additional, Charisi, M, additional, Chatterjee, S, additional, Chen, S, additional, Cognard, I, additional, Cordes, J M, additional, Cornish, N J, additional, Crawford, F, additional, Cromartie, H T, additional, Crowter, K, additional, Dai, S, additional, DeCesar, M E, additional, Demorest, P B, additional, Desvignes, G, additional, Dolch, T, additional, Drachler, B, additional, Falxa, M, additional, Ferrara, E C, additional, Fiore, W, additional, Fonseca, E, additional, Gair, J R, additional, Garver-Daniels, N, additional, Goncharov, B, additional, Good, D C, additional, Graikou, E, additional, Guillemot, L, additional, Guo, Y J, additional, Hazboun, J S, additional, Hobbs, G, additional, Hu, H, additional, Islo, K, additional, Janssen, G H, additional, Jennings, R J, additional, Johnson, A D, additional, Jones, M L, additional, Kaiser, A R, additional, Kaplan, D L, additional, Karuppusamy, R, additional, Keith, M J, additional, Kelley, L Z, additional, Kerr, M, additional, Key, J S, additional, Kramer, M, additional, Lam, M T, additional, Lamb, W G, additional, Lazio, T J W, additional, Lee, K J, additional, Lentati, L, additional, Liu, K, additional, Luo, J, additional, Lynch, R S, additional, Lyne, A G, additional, Madison, D R, additional, Main, R A, additional, Manchester, R N, additional, McEwen, A, additional, McKee, J W, additional, McLaughlin, M A, additional, Mickaliger, M B, additional, Mingarelli, C M F, additional, Ng, C, additional, Nice, D J, additional, Osłowski, S, additional, Parthasarathy, A, additional, Pennucci, T T, additional, Perera, B B P, additional, Perrodin, D, additional, Petiteau, A, additional, Pol, N S, additional, Porayko, N K, additional, Possenti, A, additional, Ransom, S M, additional, Ray, P S, additional, Reardon, D J, additional, Russell, C J, additional, Samajdar, A, additional, Sampson, L M, additional, Sanidas, S, additional, Sarkissian, J M, additional, Schmitz, K, additional, Schult, L, additional, Sesana, A, additional, Shaifullah, G, additional, Shannon, R M, additional, Shapiro-Albert, B J, additional, Siemens, X, additional, Simon, J, additional, Smith, T L, additional, Speri, L, additional, Spiewak, R, additional, Stairs, I H, additional, Stappers, B W, additional, Stinebring, D R, additional, Swiggum, J K, additional, Taylor, S R, additional, Theureau, G, additional, Tiburzi, C, additional, Vallisneri, M, additional, van der Wateren, E, additional, Vecchio, A, additional, Verbiest, J P W, additional, Vigeland, S J, additional, Wahl, H, additional, Wang, J B, additional, Wang, J, additional, Wang, L, additional, Witt, C A, additional, Zhang, S, additional, and Zhu, X J, additional

Published
2022
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12. The quest for dual and binary supermassive black holes: A multi-messenger view

Author

De Rosa, A, Vignali, C, Bogdanovic, T, Capelo, P, Charisi, M, Dotti, M, Husemann, B, Lusso, E, Mayer, L, Paragi, Z, Runnoe, J, Sesana, A, Steinborn, L, Bianchi, S, Colpi, M, del Valle, L, Frey, S, Gabanyi, K, Giustini, M, Guainazzi, M, Haiman, Z, Herrera Ruiz, N, Herrero-Illana, R, Iwasawa, K, Komossa, S, Lena, D, Loiseau, N, Perez-Torres, M, Piconcelli, E, Volonteri, M, De Rosa A., Vignali C., Bogdanovic T., Capelo P. R., Charisi M., Dotti M., Husemann B., Lusso E., Mayer L., Paragi Z., Runnoe J., Sesana A., Steinborn L., Bianchi S., Colpi M., del Valle L., Frey S., Gabanyi K. E., Giustini M., Guainazzi M., Haiman Z., Herrera Ruiz N., Herrero-Illana R., Iwasawa K., Komossa S., Lena D., Loiseau N., Perez-Torres M., Piconcelli E., Volonteri M., De Rosa, A, Vignali, C, Bogdanovic, T, Capelo, P, Charisi, M, Dotti, M, Husemann, B, Lusso, E, Mayer, L, Paragi, Z, Runnoe, J, Sesana, A, Steinborn, L, Bianchi, S, Colpi, M, del Valle, L, Frey, S, Gabanyi, K, Giustini, M, Guainazzi, M, Haiman, Z, Herrera Ruiz, N, Herrero-Illana, R, Iwasawa, K, Komossa, S, Lena, D, Loiseau, N, Perez-Torres, M, Piconcelli, E, Volonteri, M, De Rosa A., Vignali C., Bogdanovic T., Capelo P. R., Charisi M., Dotti M., Husemann B., Lusso E., Mayer L., Paragi Z., Runnoe J., Sesana A., Steinborn L., Bianchi S., Colpi M., del Valle L., Frey S., Gabanyi K. E., Giustini M., Guainazzi M., Haiman Z., Herrera Ruiz N., Herrero-Illana R., Iwasawa K., Komossa S., Lena D., Loiseau N., Perez-Torres M., Piconcelli E., and Volonteri M.

Abstract

The quest for binary and dual supermassive black holes (SMBHs) at the dawn of the multi-messenger era is compelling. Detecting dual active galactic nuclei (AGN) – active SMBHs at projected separations larger than several parsecs – and binary AGN – probing the scale where SMBHs are bound in a Keplerian binary – is an observational challenge. The study of AGN pairs (either dual or binary) also represents an overarching theoretical problem in cosmology and astrophysics. The AGN triggering calls for detailed knowledge of the hydrodynamical conditions of gas in the imminent surroundings of the SMBHs and, at the same time, their duality calls for detailed knowledge on how galaxies assemble through major and minor mergers and grow fed by matter along the filaments of the cosmic web. This review describes the techniques used across the electromagnetic spectrum to detect dual and binary AGN candidates and proposes new avenues for their search. The current observational status is compared with the state-of-the-art numerical simulations and models for formation of dual and binary AGN. Binary SMBHs are among the loudest sources of gravitational waves (GWs) in the Universe. The search for a background of GWs at nHz frequencies from inspiralling SMBHs at low redshifts, and the direct detection of signals from their coalescence by the Laser Interferometer Space Antenna in the next decade, make this a theme of major interest for multi-messenger astrophysics. This review discusses the future facilities and observational strategies that are likely to significantly advance this fascinating field.

Published
2019

13. International Pulsar Timing Array second data release: Search for an isotropic gravitational wave background.

Author

Antoniadis, J, Arzoumanian, Z, Babak, S, Bailes, M, Bak Nielsen, A-S, Baker, P T, Bassa, C G, Bécsy, B, Berthereau, A, Bonetti, M, Brazier, A, Brook, P R, Burgay, M, Burke-Spolaor, S, Caballero, R N, Casey-Clyde, J A, Chalumeau, A, Champion, D J, Charisi, M, and Chatterjee, S

Subjects
DATA release, PULSARS, BINARY black holes, SUPERMASSIVE black holes, GRAVITATIONAL waves, STOCHASTIC processes
Abstract

We searched for an isotropic stochastic gravitational wave background in the second data release of the International Pulsar Timing Array, a global collaboration synthesizing decadal-length pulsar-timing campaigns in North America, Europe, and Australia. In our reference search for a power-law strain spectrum of the form |$h_c = A(f/1\, \mathrm{yr}^{-1})^{\alpha }$|⁠ , we found strong evidence for a spectrally similar low-frequency stochastic process of amplitude |$A = 3.8^{+6.3}_{-2.5}\times 10^{-15}$| and spectral index α = −0.5 ± 0.5, where the uncertainties represent 95 per cent credible regions, using information from the auto- and cross-correlation terms between the pulsars in the array. For a spectral index of α = −2/3, as expected from a population of inspiralling supermassive black hole binaries, the recovered amplitude is |$A = 2.8^{+1.2}_{-0.8}\times 10^{-15}$|⁠. None the less, no significant evidence of the Hellings–Downs correlations that would indicate a gravitational-wave origin was found. We also analysed the constituent data from the individual pulsar timing arrays in a consistent way, and clearly demonstrate that the combined international data set is more sensitive. Furthermore, we demonstrate that this combined data set produces comparable constraints to recent single-array data sets which have more data than the constituent parts of the combination. Future international data releases will deliver increased sensitivity to gravitational wave radiation, and significantly increase the detection probability. [ABSTRACT FROM AUTHOR]

Published
2022
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14. Multimessenger science opportunities with mHz gravitational waves

Author

Baker, J., Haiman, Z., Rossi, E.M., Berger, E., Brandt, N., Breedt, E., Breivik, K., Charisi, M., Derdzinski, A., D'Orazio, D.J., Ford, S., Greene, J.E., Hill, J.C., Holley-Bockelmann, K., Key, J.S., Kocsis, B., Kupfer, T., Madau, P., Marsh, T., McKernan, B., McWilliams, S.T., Natarajan, P., Nissanke, S., Noble, S., Phinney, E.S., Ramsay, G., Schnittman, J., Sesana, A., Shoemaker, D., Stone, N., Toonen, S., Trakhtenbrot, B., Vikhlinin, A., and Volonteri, M.

Published
2019

19. Rate of seizures in children with shigellosis.

Author

Galanakis, E, Tzoufi, M, Charisi, M, Levidiotou, S, and Papadopoulou, Z L

Subjects
SPASMS, SHIGELLOSIS, JUVENILE diseases
Abstract

Examines the rate of seizures in children with shigellosis. Duration of seizures; Association of Shigellae with convulsions; Medical history of children.

Published
2002
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20. The quest for dual and binary supermassive black holes: A multi-messenger view

Author

Rubén Herrero-Illana, Zoltan Haiman, Bernd Husemann, Pedro R. Capelo, Lisa Steinborn, Stefano Bianchi, Enrico Piconcelli, Margherita Giustini, Miguel A. Pérez-Torres, Alberto Sesana, Monica Colpi, S. Komossa, Kazushi Iwasawa, Sándor Frey, Davide Lena, Maria Charisi, Nora Loiseau, Zsolt Paragi, Elisabeta Lusso, Matteo Guainazzi, Cristian Vignali, Massimo Dotti, Jessie C. Runnoe, Tamara Bogdanovic, Krisztina É. Gabányi, Lucio Mayer, Noelia Herrera Ruiz, Marta Volonteri, Luciano del Valle, Alessandra De Rosa, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Lena, D. [0000-0003-4184-6152], Loiseau, N. [0000-0001-5471-3776], Haiman, Z. [0000-0003-3633-5403], De Rosa, A. [0000-0001-5668-6863], Husemann, B. [0000-0003-2901-6842], Agenzia Spaziale Italiana (ASI), Istituto Nazionale Astrofisica (INAF), National Aeronautics and Space Administration (NASA), Hungarian Scientific Research Fund (OTKA), Hungarian Academy of Sciences (MTA), Deutsche Forschungsgemeinschaft (DFG), European Union COFUND/Durham Junior Research Fellowship (EU), European Research Council (ERC), Swiss National Science Foundation (SNSF), Federal Ministry of Education & Research (BMBF), Ministerio de Economía y Competitividad (MINECO), Comunidad de Madrid, Agencia Estatal de Investigación (AEI), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Agenzia Spaziale Italiana, National Aeronautics and Space Administration (US), Hungarian Academy of Sciences, National Research, Development and Innovation Office (Hungary), German Research Foundation, European Commission, European Research Council, Ministerio de Economía y Competitividad (España), Swiss National Science Foundation, National Science Foundation (US), Hungarian National Research, New National Excellence Program of the Ministry for Innovation and Technology, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Coscmos de la Universidad de Barcelona, 'Programa de Atraccion de Talento' of the Comunidad de Madrid, 2018-T1/TIC-11733, De Rosa, A, Vignali, C, Bogdanovic, T, Capelo, P, Charisi, M, Dotti, M, Husemann, B, Lusso, E, Mayer, L, Paragi, Z, Runnoe, J, Sesana, A, Steinborn, L, Bianchi, S, Colpi, M, del Valle, L, Frey, S, Gabanyi, K, Giustini, M, Guainazzi, M, Haiman, Z, Herrera Ruiz, N, Herrero-Illana, R, Iwasawa, K, Komossa, S, Lena, D, Loiseau, N, Perez-Torres, M, Piconcelli, E, Volonteri, M, Rosa, Alessandra De, Vignali, Cristian, Bogdanović, Tamara, Capelo, Pedro R., Charisi, Maria, Dotti, Massimo, Husemann, Bernd, Lusso, Elisabeta, Mayer, Lucio, Paragi, Zsolt, Runnoe, Jessie, Sesana, Alberto, Steinborn, Lisa, Bianchi, Stefano, Colpi, Monica, Valle, Luciano Del, Frey, Sándor, Gabányi, Krisztina É., Giustini, Margherita, Guainazzi, Matteo, Haiman, Zoltan, Ruiz, Noelia Herrera, Herrero-Illana, Rubén, Iwasawa, Kazushi, Komossa, S., Lena, Davide, Loiseau, Nora, Perez-Torres, Miguel, Piconcelli, Enrico, Volonteri, Marta, De Rosa A., Vignali C., Bogdanovic T., Capelo P.R., Charisi M., Dotti M., Husemann B., Lusso E., Mayer L., Paragi Z., Runnoe J., Sesana A., Steinborn L., Bianchi S., Colpi M., del Valle L., Frey S., Gabanyi K.E., Giustini M., Guainazzi M., Haiman Z., Herrera Ruiz N., Herrero-Illana R., Iwasawa K., Komossa S., Lena D., Loiseau N., Perez-Torres M., Piconcelli E., and Volonteri M.

Subjects
Galaxies: active, Galaxies: interactions, Galaxies: nuclei, gravitational waves, Quasars: supermassive black holes, Active galactic nucleus, active [Galaxies], Electromagnetic spectrum, Astrophysics::High Energy Astrophysical Phenomena, Nuclear Theory, Binary number, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, interactions [Galaxies], 01 natural sciences, 7. Clean energy, Cosmology, Gravitational waves, General Relativity and Quantum Cosmology, 0103 physical sciences, 010303 astronomy & astrophysics, gravitational wave, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Supermassive black hole, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, 13. Climate action, Space and Planetary Science, Galaxies: interaction, Astrophysics of Galaxies (astro-ph.GA), nuclei [Galaxies], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], supermassive black holes [Quasars]
Abstract

69 pages, 21 figures. Accepted for publication in New Astronomy Reviews © 2020 Elsevier B.V., The quest for binary and dual supermassive black holes (SMBHs) at the dawn of the multi-messenger era is compelling. Detecting dual active galactic nuclei (AGN) -- active SMBHs at projected separations larger than several parsecs -- and binary AGN -- probing the scale where SMBHs are bound in a Keplerian binary -- is an observational challenge. The study of AGN pairs (either dual or binary) also represents an overarching theoretical problem in cosmology and astrophysics. The AGN triggering calls for detailed knowledge of the hydrodynamical conditions of gas in the imminent surroundings of the SMBHs and, at the same time, their duality calls for detailed knowledge on how galaxies assemble through major and minor mergers and grow fed by matter along the filaments of the cosmic web. This review describes the techniques used across the electromagnetic spectrum to detect dual and binary AGN candidates and proposes new avenues for their search. The current observational status is compared with the state-of-the-art numerical simulations and models for formation of dual and binary AGN. Binary SMBHs are among the loudest sources of gravitational waves (GWs) in the Universe. The search for a background of GWs at nHz frequencies from inspiralling SMBHs at low redshifts, and the direct detection of signals from their coalescence by the Laser Interferometer Space Antenna in the next decade, make this a theme of major interest for multi-messenger astrophysics. This review discusses the future facilities and observational strategies that are likely to significantly advance this fascinating field.© 2020 Elsevier B.V., All authors acknowledge the hospitality of the Lorentz Center for international workshops (Leiden, The Netherlands), where the idea of this work was born, and acknowledge the support of the International Space Science Institute (ISSI Bern, Switzerland), where the collaboration was originated. We thank the reviewers for having provided valuable and constructive comments that improved the clarity of the manuscript, and J.E. Barnes, L. Blecha, M. Eracleous, B.D. Farris, H. Fu, X. Liu, R. Pfeifle, L.C. Popovic, C. Ricci, S. Rodriguez, S. Tang, G. B. Taylor for their kind permission to reuse figures from their publications. ADR, CV and SB acknowledge financial support from ASI under grant ASI-INAF I/037/12/0 , and from the agreement ASI-INAF n. 2017-14-H.O . TB acknowledges support by the National Aeronautics and Space Administration under Grant No. NNX15AK84G and 80NSSC19K0319 issued through the Astrophysics Theory Program and by the Research Corporation for Science Advancement through a Cottrell Scholar Award. SF and KÉG thank the Hungarian National Research, Development, and Innovation Office ( OTKA NN110333 ) for support. KÉG was supported by the János Bolyai Research Scholarship of the Hungarian Academy of Sciences and by the ÚNKP-19-4 New National Excellence Program of the Ministry for Innovation and Technology. BH acknowledges financial support by the DFG grant GE625/17-1 . EL is supported by a European Union COFUND/Durham Junior Research Fellowship (under EU grant agreement no. 609412). DL acknowledges support from the European Research Council (ERC) under grant 647208 (PI Jonker). AS is supported by the ERC CoG grant 818691 (B Massive). MGi is supported by the “Programa de Atracción de Talento” of the Comunidad de Madrid grant 2018-T1/TIC-11733 for the project: “Unveiling Black Hole Winds from Space”, and by the Spanish State Research Agency (AEI) grant MDM-2017-0737 Unidad de Excelencia “María de Maeztu” - Centro de Astrobiología (INTA-CSIC). PRC and LM acknowledge support from the Swiss National Science Foundation under the Grant 200020_178949 . MC acknowledges support from the National Science Foundation (NSF) NANOGrav Physics Frontier Center, award number 1430284 . NHR acknowledges support from the BMBF Verbundforschung under FKZ: 05A17PC1 and FKZ: 05A17PC2. ZH acknowledges support from NASA grants NNX17AL82G and 80NSSC19K0149 and NSF grant 1715661 . KI acknowledges support by the Spanish MINECO under grant AYA2016-76012-C3-1-P and MDM-2014-0369 of ICCUB (Unidad de Excelencia ’María de Maeztu’). MPT acknowledges financial support from the Spanish MCIU through the “Center of Excellence Severo Ochoa” award for the Instituto de Astrofísica de Andalucía ( SEV-2017-0709 ) and through the MINECO grants AYA2012-38491-C02-02 and AYA2015-63939-C2-1-P .

Published
2019

21. Astrophysics with the Laser Interferometer Space Antenna

Author

Seoane, Pau Amaro, Andrews, Jeff, Sedda, Manuel Arca, Askar, Abbas, Baghi, Quentin, Balasov, Razvan, Bartos, Imre, Bavera, Simone S., Bellovary, Jillian, Berry, Christopher P. L., Berti, Emanuele, Bianchi, Stefano, Blecha, Laura, Blondin, Stephane, Bogdanović, Tamara, Boissier, Samuel, Bonetti, Matteo, Bonoli, Silvia, Bortolas, Elisa, Breivik, Katelyn, Capelo, Pedro R., Caramete, Laurentiu, Cattorini, Federico, Charisi, Maria, Chaty, Sylvain, Chen, Xian, Chruślińska, Martyna, Chua, Alvin J. K., Church, Ross, Colpi, Monica, D'Orazio, Daniel, Danielski, Camilla, Davies, Melvyn B., Dayal, Pratika, De Rosa, Alessandra, Derdzinski, Andrea, Destounis, Kyriakos, Dotti, Massimo, Duţan, Ioana, Dvorkin, Irina, Fabj, Gaia, Foglizzo, Thierry, Ford, Saavik, Fouvry, Jean-Baptiste, Franchini, Alessia, Fragos, Tassos, Fryer, Chris, Gaspari, Massimo, Gerosa, Davide, Graziani, Luca, Groot, Paul, Habouzit, Melanie, Haggard, Daryl, Haiman, Zoltan, Han, Wen-Biao, Istrate, Alina, Johansson, Peter H., Khan, Fazeel Mahmood, Kimpson, Tomas, Kokkotas, Kostas, Kong, Albert, Korol, Valeriya, Kremer, Kyle, Kupfer, Thomas, Lamberts, Astrid, Larson, Shane, Lau, Mike, Liu, Dongliang, Lloyd-Ronning, Nicole, Lodato, Giuseppe, Lupi, Alessandro, Ma, Chung-Pei, Maccarone, Tomas, Mandel, Ilya, Mangiagli, Alberto, Mapelli, Michela, Mathis, Steéphane, Mayer, Lucio, McGee, Sean, McKernan, Berry, Miller, M. Coleman, Mota, David F., Mumpower, Matthew, Nasim, Syeda S, Nelemans, Gijs, Noble, Scott, Pacucci, Fabio, Panessa, Francesca, Paschalidis, Vasileio, Pfister, Hugo, Porquet, Delphine, Quenby, John, Ricarte, Angelo, Röpke, Friedrich K., Regan, John, Rosswog, Stephan, Ruiter, Ashley, Ruiz, Milton, Runnoe, Jessie, Schneider, Raffaella, Schnittman, Jeremy, Secunda, Amy, Sesana, Alberto, Seto, Naoki, Shao, Lijing, Shapiro, Stuart, Sopuerta, Carlos, Stone, Nicholas C., Suvorov, Arthur, Tamanini, Nicola, Tamfal, Tomas, Tauris, Thomas, Temmink, Karel, Tomsick, John, Toonen, Silvia, Torres-Orjuela, Alejandro, Toscani, Martina, Tsokaros, Antonios, Unal, Caner, Vázquez-Aceves, Verónica, Valiante, Rosa, van Putten, Maurice, van Roestel, Jan, Vignali, Christian, Volonteri, Marta, Wu, Kinwah, Younsi, Ziri, Yu, Shenghua, Zane, Silvia, Zwick, Lorenz, Antonini, Fabio, Baibhav, Vishal, Barausse, Enrico, Rivera, Alexander Bonilla, Branchesi, Marica, Branduardi-Raymont, Graziella, Burdge, Kevin, Chakraborty, Srija, Cuadra, Jorge, Dage, Kristen, Davis, Benjamin, de Mink, Selma E., Decarli, Roberto, Doneva, Daniela, Escoffier, Stephanie, Fragione, Giacomo, Gandhi, Poshak, Haardt, Francesco, Lousto, Carlos O., Nissanke, Samaya, Nordhaus, Jason, O'Shaughnessy, Richard, Zwart, Simon Portegies, Pound, Adam, Schussler, Fabian, Sergijenko, Olga, Spallicci, Alessandro, Vernieri, Daniele, Vigna-Gómez, Alejandro, Amaro-Seoane, Pau, Andrews, Jeff, Arca Sedda, Manuel, Askar, Abba, Baghi, Quentin, Balasov, Razvan, Bartos, Imre, Bavera, Simone S., Bellovary, Jillian, Berry, Christopher P. L., Berti, Emanuele, Bianchi, Stefano, Blecha, Laura, Blondin, Stéphane, Bogdanović, Tamara, Boissier, Samuel, Bonetti, Matteo, Bonoli, Silvia, Bortolas, Elisa, Breivik, Katelyn, Capelo, Pedro R., Caramete, Laurentiu, Cattorini, Federico, Charisi, Maria, Chaty, Sylvain, Chen, Xian, Chruślińska, Martyna, Chua, Alvin J. K., Church, Ro, Colpi, Monica, D’Orazio, Daniel, Danielski, Camilla, Davies, Melvyn B., Dayal, Pratika, De Rosa, Alessandra, Derdzinski, Andrea, Destounis, Kyriako, Dotti, Massimo, Duţan, Ioana, Dvorkin, Irina, Fabj, Gaia, Foglizzo, Thierry, Ford, Saavik, Fouvry, Jean-Baptiste, Franchini, Alessia, Fragos, Tasso, Fryer, Chri, Gaspari, Massimo, Gerosa, Davide, Graziani, Luca, Groot, Paul, Habouzit, Melanie, Haggard, Daryl, Haiman, Zoltan, Han, Wen-Biao, Istrate, Alina, Johansson, Peter H., Khan, Fazeel Mahmood, Kimpson, Toma, Kokkotas, Kosta, Kong, Albert, Korol, Valeriya, Kremer, Kyle, Kupfer, Thoma, Lamberts, Astrid, Larson, Shane, Lau, Mike, Liu, Dongliang, Lloyd-Ronning, Nicole, Lodato, Giuseppe, Lupi, Alessandro, Ma, Chung-Pei, Maccarone, Toma, Mandel, Ilya, Mangiagli, Alberto, Mapelli, Michela, Mathis, Stéphane, Mayer, Lucio, Mcgee, Sean, Mckernan, Berry, Miller, M. Coleman, Mota, David F., Mumpower, Matthew, Nasim, Syeda S., Nelemans, Gij, Noble, Scott, Pacucci, Fabio, Panessa, Francesca, Paschalidis, Vasileio, Pfister, Hugo, Porquet, Delphine, Quenby, John, Ricarte, Angelo, Röpke, Friedrich K., Regan, John, Rosswog, Stephan, Ruiter, Ashley, Ruiz, Milton, Runnoe, Jessie, Schneider, Raffaella, Schnittman, Jeremy, Secunda, Amy, Sesana, Alberto, Seto, Naoki, Shao, Lijing, Shapiro, Stuart, Sopuerta, Carlo, Stone, Nicholas C., Suvorov, Arthur, Tamanini, Nicola, Tamfal, Toma, Tauris, Thoma, Temmink, Karel, Tomsick, John, Toonen, Silvia, Torres-Orjuela, Alejandro, Toscani, Martina, Tsokaros, Antonio, Unal, Caner, Vázquez-Aceves, Verónica, Valiante, Rosa, van Putten, Maurice, van Roestel, Jan, Vignali, Christian, Volonteri, Marta, Wu, Kinwah, Younsi, Ziri, Yu, Shenghua, Zane, Silvia, Zwick, Lorenz, Antonini, Fabio, Baibhav, Vishal, Barausse, Enrico, Bonilla Rivera, Alexander, Branchesi, Marica, Branduardi-Raymont, Graziella, Burdge, Kevin, Chakraborty, Srija, Cuadra, Jorge, Dage, Kristen, Davis, Benjamin, de Mink, Selma E., Decarli, Roberto, Doneva, Daniela, Escoffier, Stephanie, Gandhi, Poshak, Haardt, Francesco, Lousto, Carlos O., Nissanke, Samaya, Nordhaus, Jason, O’Shaughnessy, Richard, Portegies Zwart, Simon, Pound, Adam, Schussler, Fabian, Sergijenko, Olga, Spallicci, Alessandro, Vernieri, Daniele, Vigna-Gómez, Alejandro, Max Planck Institute for Gravitational Physics (Albert Einstein Institute) (AEI), Max-Planck-Gesellschaft, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics, Columbia University, Columbia University [New York], Department of Physics and Astronomy [Nashville], Vanderbilt University [Nashville], Fisk University, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des deux Infinis de Toulouse (L2IT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Amaro-Seoane, P, Andrews, J, Arca Sedda, M, Askar, A, Baghi, Q, Balasov, R, Bartos, I, Bavera, S, Bellovary, J, Berry, C, Berti, E, Bianchi, S, Blecha, L, Blondin, S, Bogdanović, T, Boissier, S, Bonetti, M, Bonoli, S, Bortolas, E, Breivik, K, Capelo, P, Caramete, L, Cattorini, F, Charisi, M, Chaty, S, Chen, X, Chruślińska, M, Chua, A, Church, R, Colpi, M, D’Orazio, D, Danielski, C, Davies, M, Dayal, P, De Rosa, A, Derdzinski, A, Destounis, K, Dotti, M, Duţan, I, Dvorkin, I, Fabj, G, Foglizzo, T, Ford, S, Fouvry, J, Franchini, A, Fragos, T, Fryer, C, Gaspari, M, Gerosa, D, Graziani, L, Groot, P, Habouzit, M, Haggard, D, Haiman, Z, Han, W, Istrate, A, Johansson, P, Khan, F, Kimpson, T, Kokkotas, K, Kong, A, Korol, V, Kremer, K, Kupfer, T, Lamberts, A, Larson, S, Lau, M, Liu, D, Lloyd-Ronning, N, Lodato, G, Lupi, A, Ma, C, Maccarone, T, Mandel, I, Mangiagli, A, Mapelli, M, Mathis, S, Mayer, L, Mcgee, S, Mckernan, B, Miller, M, Mota, D, Mumpower, M, Nasim, S, Nelemans, G, Noble, S, Pacucci, F, Panessa, F, Paschalidis, V, Pfister, H, Porquet, D, Quenby, J, Ricarte, A, Röpke, F, Regan, J, Rosswog, S, Ruiter, A, Ruiz, M, Runnoe, J, Schneider, R, Ministerio de Ciencia e Innovación (España), European Research Council, European Commission, Istituto Nazionale di Astrofisica, Agenzia Spaziale Italiana, and National Aeronautics and Space Administration (US)

Subjects
Astrofísica, ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), Black hole, Astronomy, Stellar remnant, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), TIDAL DISRUPTION EVENTS, General Relativity and Quantum Cosmology, Gravitational waves, MOCCA-SURVEY DATABASE, Settore FIS/05 - Astronomia e Astrofisica, Stellar remnants, Software Science, Multi-messenger, GRAVITATIONAL-WAVE SOURCES, Instrumentation and Methods for Astrophysics (astro-ph.IM), Extreme mass ratio in-spirals, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Black holes, Data Science, Astrophysics::Instrumentation and Methods for Astrophysics, Extreme mass ratio in-spiral, AM-CVN STARS, Astrophysics - Astrophysics of Galaxies, WHITE-DWARF BINARIES, DOUBLE NEUTRON-STARS, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astronomia, MASSIVE BLACK-HOLE, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, X-RAY BINARIES, COMMON-ENVELOPE EVOLUTION, Gravitational wave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Full list of authors: Amaro-Seoane, Pau; Andrews, Jeff; Sedda, Manuel Arca; Askar, Abbas.; Baghi, Quentin; Balasov, Razvan; Bartos, Imre; Bavera, Simone S.; Bellovary, Jillian; Berry, Christopher P. L.; Berti, Emanuele; Bianchi, Stefano; Blecha, Laura; Blondin, Stephane; Bogdanovic, Tamara; Boissier, Samuel; Bonetti, Matteo; Bonoli, Silvia; Bortolas, Elisa; Breivik, Katelyn; Capelo, Pedro R.; Caramete, Laurentiu; Cattorini, Federico; Charisi, Maria; Chaty, Sylvain; Chen, Xian; Chruslinska, Martyna; Chua, Alvin J. K.; Church, Ross; Colpi, Monica; D'Orazio, Daniel; Danielski, Camilla; Davies, Melvyn B.; Dayal, Pratika; De Rosa, Alessandra; Derdzinski, Andrea; Destounis, Kyriakos; Dotti, Massimo; Dutan, Ioana; Dvorkin, Irina; Fabj, Gaia; Foglizzo, Thierry; Ford, Saavik; Fouvry, Jean-Baptiste; Franchini, Alessia; Fragos, Tassos; Fryer, Chris; Gaspari, Massimo; Gerosa, Davide; Graziani, Luca; Groot, Paul; Habouzit, Melanie; Haggard, Daryl; Haiman, Zoltan; Han, Wen-Biao; Istrate, Alina; Johansson, Peter H.; Khan, Fazeel Mahmood; Kimpson, Tomas; Kokkotas, Kostas; Kong, Albert; Korol, Valeriya; Kremer, Kyle; Kupfer, Thomas; Lamberts, Astrid; Larson, Shane; Lau, Mike; Liu, Dongliang; Lloyd-Ronning, Nicole; Lodato, Giuseppe; Lupi, Alessandro; Ma, Chung-Pei; Maccarone, Tomas; Mandel, Ilya; Mangiagli, Alberto; Mapelli, Michela; Mathis, Stephane; Mayer, Lucio; McGee, Sean; McKernan, Berry; Miller, M. Coleman; Mota, David F.; Mumpower, Matthew; Nasim, Syeda S.; Nelemans, Gijs; Noble, Scott; Pacucci, Fabio; Panessa, Francesca; Paschalidis, Vasileios; Pfister, Hugo; Porquet, Delphine; Quenby, John; Ricarte, Angelo; Roepke, Friedrich K.; Regan, John; Rosswog, Stephan; Ruiter, Ashley; Ruiz, Milton; Runnoe, Jessie; Schneider, Raffaella; Schnittman, Jeremy; Secunda, Amy; Sesana, Alberto; Seto, Naoki; Shao, Lijing; Shapiro, Stuart; Sopuerta, Carlos; Stone, Nicholas C.; Suvorov, Arthur; Tamanini, Nicola; Tamfal, Tomas; Tauris, Thomas; Temmink, Karel; Tomsick, John; Toonen, Silvia; Torres-Orjuela, Alejandro; Toscani, Martina; Tsokaros, Antonios; Unal, Caner; Vazquez-Aceves, Veronica; Valiante, Rosa; van Putten, Maurice; van Roestel, Jan; Vignali, Christian; Volonteri, Marta; Wu, Kinwah; Younsi, Ziri; Yu, Shenghua; Zane, Silvia; Zwick, Lorenz; Antonini, Fabio; Baibhav, Vishal; Barausse, Enrico; Bonilla Rivera, Alexander; Branchesi, Marica; Branduardi-Raymont, Graziella; Burdge, Kevin; Chakraborty, Srija; Cuadra, Jorge; Dage, Kristen; Davis, Benjamin; de Mink, Selma E.; Decarli, Roberto; Doneva, Daniela; Escoffier, Stephanie; Gandhi, Poshak; Haardt, Francesco; Lousto, Carlos O.; Nissanke, Samaya; Nordhaus, Jason; O'Shaughnessy, Richard; Portegies Zwart, Simon; Pound, Adam; Schussler, Fabian; Sergijenko, Olga; Spallicci, Alessandro; Vernieri, Daniele; Vigna-Gomez, Alejandro.-- This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/., The Laser Interferometer Space Antenna (LISA) will be a transformative experiment for gravitational wave astronomy, and, as such, it will offer unique opportunities to address many key astrophysical questions in a completely novel way. The synergy with ground-based and space-born instruments in the electromagnetic domain, by enabling multi-messenger observations, will add further to the discovery potential of LISA. The next decade is crucial to prepare the astrophysical community for LISA’s first observations. This review outlines the extensive landscape of astrophysical theory, numerical simulations, and astronomical observations that are instrumental for modeling and interpreting the upcoming LISA datastream. To this aim, the current knowledge in three main source classes for LISA is reviewed; ultra-compact stellar-mass binaries, massive black hole binaries, and extreme or interme-diate mass ratio inspirals. The relevant astrophysical processes and the established modeling techniques are summarized. Likewise, open issues and gaps in our understanding of these sources are highlighted, along with an indication of how LISA could help making progress in the different areas. New research avenues that LISA itself, or its joint exploitation with upcoming studies in the electromagnetic domain, will enable, are also illustrated. Improvements in modeling and analysis approaches, such as the combination of numerical simulations and modern data science techniques, are discussed. This review is intended to be a starting point for using LISA as a new discovery tool for understanding our Universe. © The Author(s) 2023, corrected publication 2023., P. Dayal acknowledges support from the European Research council (ERC-717001) and from the Netherlands Research Council NWO (016.VIDI.189.162). P.H. Johansson acknowledges the support from the European Research Council (ERC-818930). S. Toonen acknowledges support from the Netherlands Research Council NWO (VENI 639.041.645 Grants) C. Unal is supported by European Structural and Investment Funds and the Czech Ministry of Education, Youth and Sports (Project CoGraDS - CZ.02.1.01/0.0/0.0/15_003/0000437). S. Chaty acknowledges the LabEx UnivEarthS for the funding of Interface project I10 “From binary evolution towards merging of compact objects”. A. De Rosa acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.O E. Berti is supported by NSF Grants No. PHY-1912550 and AST-2006538, NASA ATP Grants No. 17-ATP17-0225 and 19-ATP19-0051, NSF-XSEDE Grant No. PHY-090003, and NSF Grant PHY-20043. D. Gerosa is supported by European Union’s H2020 ERC Starting Grant No. 945155–GWmining, Leverhulme Trust Grant No. RPG-2019-350 and Royal Society Grant No. RGS-R2-202004. T. Bogdanovic acknowledges support by the NASA award No. 80NSSC19K0319 and by the NSF award AST-1908042. D. Porquet acknowledges funding support from CNES. C. Danielski acknowledges financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709) B.L. Davis acknowledges support from Tamkeen under the NYU Abu Dhabi Research Institute Grant CAP3. F. Pacucci acknowledges support from a Clay Fellowship by the SAO and from the Black Hole Initiative, which is funded by grants from the John Templeton Foundation and the Gordon and Betty Moore Foundation. A.J. Ruiter acknowledges support from the Australian Research Council Future Fellowship Grant FT170100243. V. Paschalidis is supported by NSF Grant PHY-1912619 and NASA Grant 80NSSC20K1542 to the University of Arizona, and NSF-XSEDE Grant TG-PHY190020. D. Haggard acknowledges support from the NSERC Discovery Grant and Canada Research Chairs programs, and the Bob Wares Science Innovation Prospectors Fund. M. Toscani acknowledges European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie Grant Agreement No. 823823 (RISE DUSTBUSTERS project) and COST Action CA16104 - Gravitational waves, black holes and fundamental physics, supported by COST (European Cooperation in Science and Technology). M. Chruslinska, A. Istrate and G. Nelemans acknowledge support from Netherlands Research Council NWO. T. Fragos and S. Bavera acknowledge support from a Swiss National Science Foundation Professorship Grant (project numbers PP00P2_176868 and PP00P2_211006)., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).

Published
2023

22. The International Pulsar Timing Array second data release: Search for an isotropic gravitational wave background

Author

J Antoniadis, Z Arzoumanian, S Babak, M Bailes, A-S Bak Nielsen, P T Baker, C G Bassa, B Bécsy, A Berthereau, M Bonetti, A Brazier, P R Brook, M Burgay, S Burke-Spolaor, R N Caballero, J A Casey-Clyde, A Chalumeau, D J Champion, M Charisi, S Chatterjee, S Chen, I Cognard, J M Cordes, N J Cornish, F Crawford, H T Cromartie, K Crowter, S Dai, M E DeCesar, P B Demorest, G Desvignes, T Dolch, B Drachler, M Falxa, E C Ferrara, W Fiore, E Fonseca, J R Gair, N Garver-Daniels, B Goncharov, D C Good, E Graikou, L Guillemot, Y J Guo, J S Hazboun, G Hobbs, H Hu, K Islo, G H Janssen, R J Jennings, A D Johnson, M L Jones, A R Kaiser, D L Kaplan, R Karuppusamy, M J Keith, L Z Kelley, M Kerr, J S Key, M Kramer, M T Lam, W G Lamb, T J W Lazio, K J Lee, L Lentati, K Liu, J Luo, R S Lynch, A G Lyne, D R Madison, R A Main, R N Manchester, A McEwen, J W McKee, M A McLaughlin, M B Mickaliger, C M F Mingarelli, C Ng, D J Nice, S Osłowski, A Parthasarathy, T T Pennucci, B B P Perera, D Perrodin, A Petiteau, N S Pol, N K Porayko, A Possenti, S M Ransom, P S Ray, D J Reardon, C J Russell, A Samajdar, L M Sampson, S Sanidas, J M Sarkissian, K Schmitz, L Schult, A Sesana, G Shaifullah, R M Shannon, B J Shapiro-Albert, X Siemens, J Simon, T L Smith, L Speri, R Spiewak, I H Stairs, B W Stappers, D R Stinebring, J K Swiggum, S R Taylor, G Theureau, C Tiburzi, M Vallisneri, E van der Wateren, A Vecchio, J P W Verbiest, S J Vigeland, H Wahl, J B Wang, J Wang, L Wang, C A Witt, S Zhang, X J Zhu, Antoniadis, J, Arzoumanian, Z, Babak, S, Bailes, M, Bak Nielsen, A, Baker, P, Bassa, C, Becsy, B, Berthereau, A, Bonetti, M, Brazier, A, Brook, P, Burgay, M, Burke-Spolaor, S, Caballero, R, Casey-Clyde, J, Chalumeau, A, Champion, D, Charisi, M, Chatterjee, S, Chen, S, Cognard, I, Cordes, J, Cornish, N, Crawford, F, Cromartie, H, Crowter, K, Dai, S, Decesar, M, Demorest, P, Desvignes, G, Dolch, T, Drachler, B, Falxa, M, Ferrara, E, Fiore, W, Fonseca, E, Gair, J, Garver-Daniels, N, Goncharov, B, Good, D, Graikou, E, Guillemot, L, Guo, Y, Hazboun, J, Hobbs, G, Hu, H, Islo, K, Janssen, G, Jennings, R, Johnson, A, Jones, M, Kaiser, A, Kaplan, D, Karuppusamy, R, Keith, M, Kelley, L, Kerr, M, Key, J, Kramer, M, Lam, M, Lamb, W, Lazio, T, Lee, K, Lentati, L, Liu, K, Luo, J, Lynch, R, Lyne, A, Madison, D, Main, R, Manchester, R, Mcewen, A, Mckee, J, Mclaughlin, M, Mickaliger, M, Mingarelli, C, Ng, C, Nice, D, Oslowski, S, Parthasarathy, A, Pennucci, T, Perera, B, Perrodin, D, Petiteau, A, Pol, N, Porayko, N, Possenti, A, Ransom, S, Ray, P, Reardon, D, Russell, C, Samajdar, A, Sampson, L, Sanidas, S, Sarkissian, J, Schmitz, K, Schult, L, Sesana, A, Shaifullah, G, Shannon, R, Shapiro-Albert, B, Siemens, X, Simon, J, Smith, T, Speri, L, Spiewak, R, Stairs, I, Stappers, B, Stinebring, D, Swiggum, J, Taylor, S, Theureau, G, Tiburzi, C, Vallisneri, M, Van Der Wateren, E, Vecchio, A, Verbiest, J, Vigeland, S, Wahl, H, Wang, J, Wang, L, Witt, C, Zhang, S, Zhu, X, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire Univers et Théories (LUTH (UMR_8102)), ANR-18-CE31-0015,PTA-France,Recherche d'ondes gravitationnelles avec un réseau de pulsars en France(2018), ITA, USA, GBR, FRA, DEU, AUS, CAN, GRC, NLD, CHN, RUS, CHE, and HUN

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, [PHYS]Physics [physics], Astrophysics and Astronomy, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, methods: Data analysi, pulsars: General, methods: data analysis, gravitational waves, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), gravitational wave, astro-ph.IM
Abstract

We searched for an isotropic stochastic gravitational wave background in the second data release of the International Pulsar Timing Array, a global collaboration synthesizing decadal-length pulsar-timing campaigns in North America, Europe, and Australia. In our reference search for a power law strain spectrum of the form $h_c = A(f/1\,\mathrm{yr}^{-1})^{\alpha}$, we found strong evidence for a spectrally-similar low-frequency stochastic process of amplitude $A = 3.8^{+6.3}_{-2.5}\times10^{-15}$ and spectral index $\alpha = -0.5 \pm 0.5$, where the uncertainties represent 95\% credible regions, using information from the auto- and cross-correlation terms between the pulsars in the array. For a spectral index of $\alpha = -2/3$, as expected from a population of inspiralling supermassive black hole binaries, the recovered amplitude is $A = 2.8^{+1.2}_{-0.8}\times10^{-15}$. Nonetheless, no significant evidence of the Hellings-Downs correlations that would indicate a gravitational-wave origin was found. We also analyzed the constituent data from the individual pulsar timing arrays in a consistent way, and clearly demonstrate that the combined international data set is more sensitive. Furthermore, we demonstrate that this combined data set produces comparable constraints to recent single-array data sets which have more data than the constituent parts of the combination. Future international data releases will deliver increased sensitivity to gravitational wave radiation, and significantly increase the detection probability., 17 pages, 12 figures, accepted in MNRAS

Published
2022

23. Efficient Large-Scale, Targeted Gravitational-Wave Probes of Supermassive Black-Hole Binaries.

Author

Charisi M, Taylor SR, Witt CA, and Runnoe J

Abstract

Binary systems of supermassive black holes are promising sources of low-frequency gravitational waves (GWs) and bright electromagnetic emission. Pulsar timing array GW searches for individual binaries have been limited to only a few candidate systems due to computational demands, which get worse as more pulsars are added. By modeling the GW signal using only components from when the GW passes Earth (rather than also each pulsar), we find constraints on the binary's total mass and GW frequency that are similar to a full signal analysis, yet ∼70 times more efficient.

Published
2024
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24. A multicenter study on the epidemiology of complicated parapneumonic effusion in the era of currently available pneumococcal conjugate vaccines.

Author

Papachristidou S, Lapea V, Charisi M, Kourkouni E, Kousi D, Xirogianni A, Dedousi O, Papaconstadopoulos I, Eleftheriou E, Krepis P, Pasparaki S, Pantalos G, Doudoulakakis A, Bozavoutoglou E, Daskalaki M, Kostaridou-Nikolopoulou S, Tzanakaki G, Spoulou V, and Tsolia M

Subjects
Child, Humans, Infant, Vaccines, Conjugate therapeutic use, Streptococcus pneumoniae, Pneumococcal Vaccines, Serogroup, Incidence, Pneumonia, Bacterial, Pleural Effusion epidemiology, Pneumococcal Infections prevention & control
Abstract

Background: Parapneumonic effusion (PPE) is a common complication of pneumonia. Streptococcus pneumoniae is the most common cause of bacterial pneumonia. A reduction in pneumonia hospitalizations has been observed since the introduction of the 7-valent pneumococcal conjugate vaccine (PCV7). Despite this apparent benefit, an increase in the incidence of PPE was recorded in some countries following PCV7 implementation. As the 13-valent pneumococcal conjugate vaccine (PCV13) was expected to provide a wider protection against PPE, the aim of the present study was to evaluate the impact of PCV13 introduction on the epidemiology of complicated parapneumonic effusion (c-PPE) among children in the Athens greater area., Methods: All cases of community-acquired pneumonia (CAP) with PPE requiring chest tube insertion (complicated PPE, c-PPE) hospitalized in the 3 public Children's hospitals in Athens between 01/01/2004 and 31/12/2019 were included in the study., Results: A total of 426 cases of c-PPE associated with pneumonia were recorded of which 198 were admitted during 2004-2010 (period A, prePCV13/PCV -7 introduction period) and 228 during 2011-2018 (period B, post - PCV13 period). A definite bacterial etiology was established in 44.4 % of all cases and of those 25.4 % were caused by S. pneumoniae. An increasing trend in c-PPE incidence was observed during period A; although, a significant decrease on c-PPE annual rates was observed during the period B (p = 0.011), a remarkable increase in serotype 3 cases was recorded., Conclusion: A decreasing time trend in c-PPE cases among children was shown after the introduction of PCV13 in our area. However, serotype 3 is nowadays a common cause of PPE. Hence, continuous surveillance is imperative in order to follow c-PPE epidemiology over time., Competing Interests: Declaration of Competing Interest The authors declare that they have no known competing financial interests or personal relationships that could have appeared to influence the work reported in this paper., (Copyright © 2023. Published by Elsevier Ltd.)

Published
2023
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25. Searching for Gravitational Waves from Cosmological Phase Transitions with the NANOGrav 12.5-Year Dataset.

Author

Arzoumanian Z, Baker PT, Blumer H, Bécsy B, Brazier A, Brook PR, Burke-Spolaor S, Charisi M, Chatterjee S, Chen S, Cordes JM, Cornish NJ, Crawford F, Cromartie HT, DeCesar ME, Demorest PB, Dolch T, Ellis JA, Ferrara EC, Fiore W, Fonseca E, Garver-Daniels N, Gentile PA, Good DC, Hazboun JS, Holgado AM, Islo K, Jennings RJ, Jones ML, Kaiser AR, Kaplan DL, Kelley LZ, Key JS, Laal N, Lam MT, Lazio TJW, Lee VSH, Lorimer DR, Luo J, Lynch RS, Madison DR, McLaughlin MA, Mingarelli CMF, Mitridate A, Ng C, Nice DJ, Pennucci TT, Pol NS, Ransom SM, Ray PS, Shapiro-Albert BJ, Siemens X, Simon J, Spiewak R, Stairs IH, Stinebring DR, Stovall K, Sun JP, Swiggum JK, Taylor SR, Turner JE, Vallisneri M, Vigeland SJ, Witt CA, and Zurek KM

Abstract

We search for a first-order phase transition gravitational wave signal in 45 pulsars from the NANOGrav 12.5-year dataset. We find that the data can be modeled in terms of a strong first order phase transition taking place at temperatures below the electroweak scale. However, we do not observe any strong preference for a phase-transition interpretation of the signal over the standard astrophysical interpretation in terms of supermassive black hole mergers; but we expect to gain additional discriminating power with future datasets, improving the signal to noise ratio and extending the sensitivity window to lower frequencies. An interesting open question is how well gravitational wave observatories could separate such signals.

Published
2021
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26. Factors associated with asthma symptoms in schoolchildren from Greece: the Physical Activity, Nutrition and Allergies in Children Examined in Athens (PANACEA) study.

Author

Priftis KN, Panagiotakos DB, Antonogeorgos G, Papadopoulos M, Charisi M, Lagona E, and Anthracopoulos MB

Subjects
Asthma physiopathology, Body Height, Body Mass Index, Body Weight, Child, Female, Greece epidemiology, Health Behavior, Humans, Hypersensitivity physiopathology, Life Style, Male, Prevalence, Asthma epidemiology, Diet, Hypersensitivity epidemiology, Physical Fitness
Abstract

To evaluate whether dietary habits and anthropometric and lifestyle characteristics are associated with the prevalence of asthma symptoms, a sample of 700 Greek schoolchildren were evaluated through a standardized questionnaire. Body height and weight were measured, and body mass index was calculated. Multiple logistic regression and multivariate techniques (principal components analysis) were performed. Overall lifetime prevalence for asthma symptoms was found to be 23.7%. Increased body weight, sedentary lifestyle, and consumption of sulphur-dioxide-enriched foods and beverages seem to promote asthma symptoms, while avoidance of this chemical preservative and physical activity was associated with reduced odds of reporting asthma symptoms.

Published
2007
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