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1. Electromagnetic probes of primordial black holes as dark matter

Author

Ali-Haimoud, Y., Clesse, S., Garcia-Bellido, J., Kashlinsky, A., Wyrzykowski, L., Achucarro, A., Amendola, L., Annis, J., Arbey, A., Arendt, R. G., Atrio-Barandela, F., Bellomo, N., Belotsky, K., Bernal, J-L., Bird, S., Bozza, V., Byrnes, C., Novati, S. Calchi, Calore, F., Carr, B. J., Chluba, J., Cholis, I., Cieplak, A., Cole, P., Dalianis, I., Davis, A-C., Davis, T., De Luca, V., Dvorkin, I., Emparan, R., Ezquiaga, J-M., Fleury, P., Franciolini, G., Gaggero, D., Georg, J., Germani, C., Giudice, G-F., Goobar, A., Hasinger, G., Hector, A., Hundertmark, M ., Hutsi, G., Jansen, R., Kamionkowski, M., Kawasaki, M., Kazanas, D., Kehagias, A., Khlopov, M., Knebe, A., Kohri, K., Koushiappas, S., Kovetz, E., Kuhnel, F., MacGibbon, J., Marzola, L., Mediavilla, E., Meszaros, P., Mroz, P., Munoz, J., Musco, I., Nesseris, S., Ozsoy, O., Pani, P., Poulin, V., Raccanelli, A., Racco, D., Raidal, M., Ranc, C., Rattenbury, N., Rhodes, J., Ricotti, M., Riotto, A., Rubin, S., Rubio, J., Ruiz-Morales, E., Sasaki, M., Schnittman, J., Shvartzvald, Y., Street, R., Takada, M., Takhistov, V., Tashiro, H., Tasinato, G., Tringas, G., Unal, C., Tada, Y., Tsapras, Y., Vaskonen, V., Veermae, H., Vidotto, F., Watson, S., Windhorst, R., Yokoyama, S., and Young, S.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The LIGO discoveries have rekindled suggestions that primordial black holes (BHs) may constitute part to all of the dark matter (DM) in the Universe. Such suggestions came from 1) the observed merger rate of the BHs, 2) their unusual masses, 3) their low/zero spins, and 4) also from the independently uncovered cosmic infrared background (CIB) fluctuations signal of high amplitude and coherence with unresolved cosmic X-ray background (CXB). Here we summarize the prospects to resolve this important issue with electromagnetic observations using the instruments and tools expected in the 2020's. These prospects appear promising to make significant, and potentially critical, advances. We demonstrate that in the next decade, new space- and ground-borne electromagnetic instruments, combined with concurrent theoretical efforts, should shed critical light on the long-considered link between primordial BHs and DM. Specifically the new data and methodologies under this program will involve: I) Probing with high precision the spatial spectrum of source-subtracted CIB with Euclid and WFIRST, and its coherence with unresolved cosmic X-ray background using eROSITA and Athena, II) Advanced searches for microlensing of Galactic stars by the intervening Galactic Halo BHs with OGLE, Gaia, LSST and WFIRST, III) Supernovae (SNe) lensing in the upcoming surveys with WFIRST, LSST and also potentially with Euclid and JWST, IV) Advanced theoretical work to understand the details of PBH accretion and evolution and their influence on cosmic microwave background (CMB) anisotropies in light of the next generation CMB experiments, V) Better new samples and theoretical understanding involving stability and properties of ultra faint dwarf galaxies, pulsar timing, and cosmological quasar lensing., Comment: Science whitepaper submitted to the Astro2020 Decadal Survey

Published
2019

2. Implications of the detection of primordial gravitational waves for the Standard Model

Author

Franciolini, G., Giudice, G. F., Racco, D., and Riotto, A.

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

The detection of primordial gravitational waves would not only have extraordinary implications for our understanding of early cosmology, but would also give non-trivial constraints on Standard Model parameters, under the assumption that no new physics enters below the Higgs instability scale. We study the resulting bounds on the top quark mass and the strong coupling constant, discussing their theoretical uncertainties and their robustness against changes in other parameters., Comment: 20 pages, 9 figures, matching published version

Published
2018
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3. Testing Primordial Black Holes as Dark Matter through LISA

Author

Bartolo, N., De Luca, V., Franciolini, G., Peloso, M., Racco, D., and Riotto, A.

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

The idea that primordial black holes (PBHs) can comprise most of the dark matter of the universe has recently reacquired a lot of momentum. Observational constraints, however, rule out this possibility for most of the PBH masses, with a notable exception around $10^{-12} M_\odot$. These light PBHs may be originated when a sizeable comoving curvature perturbation generated during inflation re-enters the horizon during the radiation phase. During such a stage, it is unavoidable that gravitational waves (GWs) are generated. Since their source is quadratic in the curvature perturbations, these GWs are generated fully non-Gaussian. Their frequency today is about the mHz, which is exactly the range where the LISA mission has the maximum of its sensitivity. This is certainly an impressive coincidence. We show that this scenario of PBHs as dark matter can be tested by LISA by measuring the GW two-point correlator. On the other hand, we show that the short observation time (as compared to the age of the universe) and propagation effects of the GWs across the perturbed universe from the production point to the LISA detector suppress the bispectrum to an unobservable level. This suppression is completely general and not specific to our model., Comment: 22 pages, 12 figures. v3: matching published version

Published
2018
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4. A Cosmological Signature of the Standard Model Higgs Vacuum Instability: Primordial Black Holes as Dark Matter

Author

Espinosa, J. R., Racco, D., and Riotto, A.

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

For the current central values of the Higgs and top masses, the Standard Model Higgs potential develops an instability at a scale of the order of $10^{11}$ GeV. We show that a cosmological signature of such instability could be dark matter in the form of primordial black holes seeded by Higgs fluctuations during inflation. The existence of dark matter might not require physics beyond the Standard Model., Comment: 6+1 pages, 3 figures; v2: updated to the published PRL version, and added an Appendix about Non-Gaussian effects

Published
2017
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5. Simplified models for dark matter searches at the LHC

Author

Abdallah, J, Araujo, H, Arbey, A, Ashkenazi, A, Belyaev, A, Berger, J, Boehm, C, Boveia, A, Brennan, A, Brooke, J, Buchmueller, O, Buckley, M, Busoni, G, Calibbi, L, Chauhan, S, Daci, N, Davies, G, De Bruyn, I, De Jong, P, De Roeck, A, de Vries, K, Del Re, D, De Simone, A, Di Simone, A, Doglioni, C, Dolan, M, Dreiner, HK, Ellis, J, Eno, S, Etzion, E, Fairbairn, M, Feldstein, B, Flaecher, H, Feng, E, Fox, P, Genest, MH, Gouskos, L, Gramling, J, Haisch, U, Harnik, R, Hibbs, A, Hoh, S, Hopkins, W, Ippolito, V, Jacques, T, Kahlhoefer, F, Khoze, VV, Kirk, R, Korn, A, Kotov, K, Kunori, S, Landsberg, G, Liem, S, Lin, T, Lowette, S, Lucas, R, Malgeri, L, Malik, S, McCabe, C, Mete, AS, Morgante, E, Mrenna, S, Nakahama, Y, Newbold, D, Nordstrom, K, Pani, P, Papucci, M, Pataraia, S, Penning, B, Pinna, D, Polesello, G, Racco, D, Re, E, Riotto, AW, Rizzo, T, Salek, D, Sarkar, S, Schramm, S, Skubic, P, Slone, O, Smirnov, J, Soreq, Y, Sumner, T, Tait, TMP, Thomas, M, Tomalin, I, Tunnell, C, Vichi, A, Volansky, T, Weiner, N, West, SM, Wielers, M, Worm, S, Yavin, I, Zaldivar, B, Zhou, N, and Zurek, K

Subjects
Dark matter, Direct detection, Collider search for dark matter, Simplified models, Effective field theory, hep-ph, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

This document a59Summary of the discussions and conclusions following from Dark Matter @ LHC 2014, held at Merton College, Oxford, on September 25-27, 2014. outlines a set of simplified models for dark matter and its interactions with Standard Model particles. It is intended to summarize the main characteristics that these simplified models have when applied to dark matter searches at the LHC, and to provide a number of useful expressions for reference. The list of models includes both s-channel and t-channel scenarios. For s-channel, spin-0 and spin-1 mediations are discussed, and also realizations where the Higgs particle provides a portal between the dark and visible sectors. The guiding principles underpinning the proposed simplified models are spelled out, and some suggestions for implementation are presented.

Published
2015

7. Precision cosmology with primordial GW backgrounds in presence of astrophysical foregrounds

Author

Racco, D, Poletti, D, D. Racco, D. Poletti, Racco, D, Poletti, D, D. Racco, and D. Poletti

Abstract

The era of Gravitational-Wave (GW) astronomy will grant the detection of the astrophysical GW background from unresolved mergers of binary black holes, and the prospect of probing the presence of primordial GW backgrounds. In particular, the low-frequency tail of the GW spectrum for causally-generated primordial signals (like a phase transition) offers an excellent opportunity to measure unambiguously cosmological parameters as the equation of state of the universe, or free-streaming particles at epochs well before recombination. We discuss whether this programme is jeopardised by the uncertainties on the astrophysical GW foregrounds that coexist with a primordial background. We detail the motivated assumptions under which the astrophysical foregrounds can be assumed to be known in shape, and only uncertain in their normalisation. In this case, the sensitivity to a primordial signal can be computed by a simple and numerically agile procedure, where the optimal filter function subtracts the components of the astrophysical foreground that are close in spectral shape to the signal. We show that the degradation of the sensitivity to the signal in presence of astrophysical foregrounds is limited to a factor of a few, and only around the frequencies where the signal is closer to the foregrounds. Our results highlight the importance of modelling the contributions of eccentric or intermediate-mass black hole binaries to the GW background, to consolidate the prospects to perform precision cosmology with primordial GW backgrounds.

Published
2023

10. Dark Matter benchmark models for early LHC Run-2 Searches: Report of the ATLAS/CMS Dark Matter Forum

Author

Abercrombie, D, Akchurin, N, Akilli, E, Maestre, J, Allen, B, Gonzalez, B, Andrea, J, Arbey, A, Azuelos, G, Azzi, P, Backovic, M, Bai, Y, Banerjee, S, Beacham, J, Belyaev, A, Boveia, A, Brennan, A, Buchmueller, O, Buckley, M, Busoni, G, Buttignol, M, Cacciapaglia, G, Caputo, R, Carpenter, L, Castro, N, Ceballos, G, Cheng, Y, Chou, J, Gonzalez, A, Cowden, C, D'Eramo, F, De Cosa, A, De Gruttola, M, De Roeck, A, De Simone, A, Deandrea, A, Demiragli, Z, Difranzo, A, Doglioni, C, du Pree, T, Erbacher, R, Erdmann, J, Fischer, C, Flaecher, H, Fox, P, Fuks, B, Genest, M, Gomber, B, Goudelis, A, Gramling, J, Gunion, J, Hahn, K, Haisch, U, Harnik, R, Harris, P, Hoepfner, K, Hoh, S, Hsu, D, Hsu, S, Iiyama, Y, Ippolito, V, Jacques, T, Ju, X, Kahlhoefer, F, Kalogeropoulos, A, Kaplan, L, Kashif, L, Khoze, V, Khurana, R, Kotov, K, Kovalskyi, D, Kulkarni, S, Kunori, S, Kutzner, V, Lee, H, Lee, S, Liew, S, Lin, T, Lowette, S, Madar, R, Malik, S, Maltoni, F, Perez, M, Mattelaer, O, Mawatari, K, Mccabe, C, Megy, T, Morgante, E, Mrenna, S, Moon, C, Narayanan, S, Nelson, A, Novaes, S, Padeken, K, Pani, P, Papucci, M, Paulini, M, Paus, C, Pazzini, J, Penning, B, Peskin, M, Pinna, D, Procura, M, Qazi, S, Racco, D, Re, E, Riotto, A, Rizzo, T, Roehrig, R, Salek, D, Pineda, A, Sarkar, S, Schmidt, A, Schramm, S, Shepherd, W, Singh, G, Soffi, L, Srimanobhas, N, Sung, K, Tait, T, Theveneaux-Pelzer, T, Thomas, M, Tosi, M, Trocino, D, Undleeb, S, Vichi, A, Wang, F, Wang, L, Wang, R, Whallon, N, Worm, S, Wu, M, Wu, S, Yang, H, Yang, Y, Yu, S, Zaldivar, B, Zanetti, M, Zhang, Z, Zucchetta, A, Abercrombie D., Akchurin N., Akilli E., Maestre J. A., Allen B., Gonzalez B. A., Andrea J., Arbey A., Azuelos G., Azzi P., Backovic M., Bai Y., Banerjee S., Beacham J., Belyaev A., Boveia A., Brennan A. J., Buchmueller O., Buckley M. R., Busoni G., Buttignol M., Cacciapaglia G., Caputo R., Carpenter L., Castro N. F., Ceballos G. G., Cheng Y., Chou J. P., Gonzalez A. C., Cowden C., D'Eramo F., De Cosa A., De Gruttola M., De Roeck A., De Simone A., Deandrea A., Demiragli Z., DiFranzo A., Doglioni C., du Pree T., Erbacher R., Erdmann J., Fischer C., Flaecher H., Fox P. J., Fuks B., Genest M. -H., Gomber B., Goudelis A., Gramling J., Gunion J., Hahn K., Haisch U., Harnik R., Harris P. C., Hoepfner K., Hoh S. Y., Hsu D. G., Hsu S. -C., Iiyama Y., Ippolito V., Jacques T., Ju X., Kahlhoefer F., Kalogeropoulos A., Kaplan L. S., Kashif L., Khoze V. V., Khurana R., Kotov K., Kovalskyi D., Kulkarni S., Kunori S., Kutzner V., Lee H. M., Lee S. -W., Liew S. P., Lin T., Lowette S., Madar R., Malik S., Maltoni F., Perez M. M., Mattelaer O., Mawatari K., McCabe C., Megy T., Morgante E., Mrenna S., Moon C. -S., Narayanan S. M., Nelson A., Novaes S. F., Padeken K. O., Pani P., Papucci M., Paulini M., Paus C., Pazzini J., Penning B., Peskin M. E., Pinna D., Procura M., Qazi S. F., Racco D., Re E., Riotto A., Rizzo T. G., Roehrig R., Salek D., Pineda A. S., Sarkar S., Schmidt A., Schramm S. R., Shepherd W., Singh G., Soffi L., Srimanobhas N., Sung K., Tait T. M. P., Theveneaux-Pelzer T., Thomas M., Tosi M., Trocino D., Undleeb S., Vichi A., Wang F., Wang L. -T., Wang R. -J., Whallon N., Worm S., Wu M., Wu S. L., Yang H., Yang Y., Yu S. -S., Zaldivar B., Zanetti M., Zhang Z., Zucchetta A., Abercrombie, D, Akchurin, N, Akilli, E, Maestre, J, Allen, B, Gonzalez, B, Andrea, J, Arbey, A, Azuelos, G, Azzi, P, Backovic, M, Bai, Y, Banerjee, S, Beacham, J, Belyaev, A, Boveia, A, Brennan, A, Buchmueller, O, Buckley, M, Busoni, G, Buttignol, M, Cacciapaglia, G, Caputo, R, Carpenter, L, Castro, N, Ceballos, G, Cheng, Y, Chou, J, Gonzalez, A, Cowden, C, D'Eramo, F, De Cosa, A, De Gruttola, M, De Roeck, A, De Simone, A, Deandrea, A, Demiragli, Z, Difranzo, A, Doglioni, C, du Pree, T, Erbacher, R, Erdmann, J, Fischer, C, Flaecher, H, Fox, P, Fuks, B, Genest, M, Gomber, B, Goudelis, A, Gramling, J, Gunion, J, Hahn, K, Haisch, U, Harnik, R, Harris, P, Hoepfner, K, Hoh, S, Hsu, D, Hsu, S, Iiyama, Y, Ippolito, V, Jacques, T, Ju, X, Kahlhoefer, F, Kalogeropoulos, A, Kaplan, L, Kashif, L, Khoze, V, Khurana, R, Kotov, K, Kovalskyi, D, Kulkarni, S, Kunori, S, Kutzner, V, Lee, H, Lee, S, Liew, S, Lin, T, Lowette, S, Madar, R, Malik, S, Maltoni, F, Perez, M, Mattelaer, O, Mawatari, K, Mccabe, C, Megy, T, Morgante, E, Mrenna, S, Moon, C, Narayanan, S, Nelson, A, Novaes, S, Padeken, K, Pani, P, Papucci, M, Paulini, M, Paus, C, Pazzini, J, Penning, B, Peskin, M, Pinna, D, Procura, M, Qazi, S, Racco, D, Re, E, Riotto, A, Rizzo, T, Roehrig, R, Salek, D, Pineda, A, Sarkar, S, Schmidt, A, Schramm, S, Shepherd, W, Singh, G, Soffi, L, Srimanobhas, N, Sung, K, Tait, T, Theveneaux-Pelzer, T, Thomas, M, Tosi, M, Trocino, D, Undleeb, S, Vichi, A, Wang, F, Wang, L, Wang, R, Whallon, N, Worm, S, Wu, M, Wu, S, Yang, H, Yang, Y, Yu, S, Zaldivar, B, Zanetti, M, Zhang, Z, Zucchetta, A, Abercrombie D., Akchurin N., Akilli E., Maestre J. A., Allen B., Gonzalez B. A., Andrea J., Arbey A., Azuelos G., Azzi P., Backovic M., Bai Y., Banerjee S., Beacham J., Belyaev A., Boveia A., Brennan A. J., Buchmueller O., Buckley M. R., Busoni G., Buttignol M., Cacciapaglia G., Caputo R., Carpenter L., Castro N. F., Ceballos G. G., Cheng Y., Chou J. P., Gonzalez A. C., Cowden C., D'Eramo F., De Cosa A., De Gruttola M., De Roeck A., De Simone A., Deandrea A., Demiragli Z., DiFranzo A., Doglioni C., du Pree T., Erbacher R., Erdmann J., Fischer C., Flaecher H., Fox P. J., Fuks B., Genest M. -H., Gomber B., Goudelis A., Gramling J., Gunion J., Hahn K., Haisch U., Harnik R., Harris P. C., Hoepfner K., Hoh S. Y., Hsu D. G., Hsu S. -C., Iiyama Y., Ippolito V., Jacques T., Ju X., Kahlhoefer F., Kalogeropoulos A., Kaplan L. S., Kashif L., Khoze V. V., Khurana R., Kotov K., Kovalskyi D., Kulkarni S., Kunori S., Kutzner V., Lee H. M., Lee S. -W., Liew S. P., Lin T., Lowette S., Madar R., Malik S., Maltoni F., Perez M. M., Mattelaer O., Mawatari K., McCabe C., Megy T., Morgante E., Mrenna S., Moon C. -S., Narayanan S. M., Nelson A., Novaes S. F., Padeken K. O., Pani P., Papucci M., Paulini M., Paus C., Pazzini J., Penning B., Peskin M. E., Pinna D., Procura M., Qazi S. F., Racco D., Re E., Riotto A., Rizzo T. G., Roehrig R., Salek D., Pineda A. S., Sarkar S., Schmidt A., Schramm S. R., Shepherd W., Singh G., Soffi L., Srimanobhas N., Sung K., Tait T. M. P., Theveneaux-Pelzer T., Thomas M., Tosi M., Trocino D., Undleeb S., Vichi A., Wang F., Wang L. -T., Wang R. -J., Whallon N., Worm S., Wu M., Wu S. L., Yang H., Yang Y., Yu S. -S., Zaldivar B., Zanetti M., Zhang Z., and Zucchetta A.

Abstract

This document is the final report of the ATLAS-CMS Dark Matter Forum, a forum organized by the ATLAS and CMS collaborations with the participation of experts on theories of Dark Matter, to select a minimal basis set of dark matter simplified models that should support the design of the early LHC Run-2 searches. A prioritized, compact set of benchmark models is proposed, accompanied by studies of the parameter space of these models and a repository of generator implementations. This report also addresses how to apply the Effective Field Theory formalism for collider searches and present the results of such interpretations.

Published
2020

11. Maximal axion misalignment from a minimal model

Author

Ministerio de Ciencia, Innovación y Universidades (España), Huang, J., Madden, A., Racco, D., Reig, Mario, Ministerio de Ciencia, Innovación y Universidades (España), Huang, J., Madden, A., Racco, D., and Reig, Mario

Abstract

The QCD axion is one of the best motivated dark matter candidates. The misalignment mechanism is well known to produce an abundance of the QCD axion consistent with dark matter for an axion decay constant of order 10 GeV. For a smaller decay constant, the QCD axion, with Peccei-Quinn symmetry broken during inflation, makes up only a fraction of dark matter unless the axion field starts oscillating very close to the top of its potential, in a scenario called “large-misalignment”. In this scenario, QCD axion dark matter with a small axion decay constant is partially comprised of very dense structures. We present a simple dynamical model realising the large-misalignment mechanism. During inflation, the axion classically rolls down its potential approaching its minimum. After inflation, the Universe reheats to a high temperature and a modulus (real scalar field) changes the sign of its minimum dynamically, which changes the sign of the mass of a vector-like fermion charged under QCD. As a result, the minimum of the axion potential during inflation becomes the maximum of the potential after the Universe has cooled through the QCD phase transition and the axion starts oscillating. In this model, we can produce QCD axion dark matter with a decay constant as low as 6 × 10 GeV and an axion mass up to 1 meV. We also summarise the phenomenological implications of this mechanism for dark matter experiments and colliders.

Published
2020

12. Electromagnetic probes of primordial black holes as dark matter

Author

Kashlinsky, A., Ali-Haimoud, Y., Clesse, S., Garcia-Bellido, J., Wyrzykowski, L., Achucarro, A., Amendola, L., Annis, J., Arbey, A., Arendt, R. G., Atriobarandela, F., Bellomo, N., Belotsky, K., Bernal, J-L, Bird, S., Bozza, V., Byrnes, C., Calchi Novati, S., Calore, F., Carr, B. J., Chluba, J., Cholis, I., Cieplak, A., Cole, P., Dalianis, I., Davis, A-C, Davis, T., Luca, V., Dvorkin, I., Emparan, R., Ezquiaga, J-M, Fleury, P., Franciolini, G., Gaggero, D., Georg, J., Germani, C., Giudice, G-F, Goobar, A., Hasinger, G., Hector, A., Hundertmark, M., Hutsi, G., Jansen, R., Kamionkowski, M., Kawasaki, M., Kazanas, D., Kehagias, A., Khlopov, M., Knebe, A., Kohri, K., Koushiappas, S., Kovetz, E., Kuhnel, F., Macgibbon, J., Marzola, L., Mediavilla, E., Meszaros, P., Mroz, P., Munoz, J., Musco, I., Nesseris, S., Ozsoy, O., Pani, P., Poulin, V., Raccanelli, A., Racco, D., Raidal, M., Ranc, C., Rattenbury, N., Rhodes, J., Ricotti, M., Riotto, A., Rubin, S., Rubio, J., Ruiz-Morales, E., Sasaki, M., Schnittman, J., Shvartzvald, Y., Street, R., Takada, M., Takhistov, V., Tashiro, H., Tasinato, G., Tringas, G., Caner Unal, Tada, Y., Tsapras, Y., Vaskonen, V., Veermae, H., Vidotto, F., Watson, S., Windhorst, R., Yokoyama, S., Young, S., Université Claude Bernard Lyon 1 (UCBL), Université de Lyon, Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), lens, Astrophysics::High Energy Astrophysical Phenomena, spin: 0, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, galaxy: halo, star, accretion, supernova, quasar, LIGO, Astrophysics::Galaxy Astrophysics, pulsar, fluctuation, Astrophysics::Instrumentation and Methods for Astrophysics, stability, coherence, electromagnetic, X-ray: background, infrared, astro-ph.CO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

The LIGO discoveries have rekindled suggestions that primordial black holes (BHs) may constitute part to all of the dark matter (DM) in the Universe. Such suggestions came from 1) the observed merger rate of the BHs, 2) their unusual masses, 3) their low/zero spins, and 4) also from the independently uncovered cosmic infrared background (CIB) fluctuations signal of high amplitude and coherence with unresolved cosmic X-ray background (CXB). Here we summarize the prospects to resolve this important issue with electromagnetic observations using the instruments and tools expected in the 2020's. These prospects appear promising to make significant, and potentially critical, advances. We demonstrate that in the next decade, new space- and ground-borne electromagnetic instruments, combined with concurrent theoretical efforts, should shed critical light on the long-considered link between primordial BHs and DM. Specifically the new data and methodologies under this program will involve: I) Probing with high precision the spatial spectrum of source-subtracted CIB with Euclid and WFIRST, and its coherence with unresolved cosmic X-ray background using eROSITA and Athena, II) Advanced searches for microlensing of Galactic stars by the intervening Galactic Halo BHs with OGLE, Gaia, LSST and WFIRST, III) Supernovae (SNe) lensing in the upcoming surveys with WFIRST, LSST and also potentially with Euclid and JWST, IV) Advanced theoretical work to understand the details of PBH accretion and evolution and their influence on cosmic microwave background (CMB) anisotropies in light of the next generation CMB experiments, V) Better new samples and theoretical understanding involving stability and properties of ultra faint dwarf galaxies, pulsar timing, and cosmological quasar lensing., Comment: Science whitepaper submitted to the Astro2020 Decadal Survey

Published
2019

17. Dark Matter Benchmark Models for Early LHC Run-2 Searches: Report of the ATLAS/CMS Dark Matter Forum

Author

Daniel Abercrombie, Nural Akchurin, Ece Akilli, Juan Alcaraz Maestre, Brandon Allen, Barbara Alvarez Gonzalez, Jeremy Andrea, Alexandre Arbey, Georges Azuelos, Patrizia Azzi, Mihailo Backović, Yang Bai, Swagato Banerjee, James Beacham, Alexander Belyaev, Antonio Boveia, Amelia Jean Brennan, Oliver Buchmueller, Matthew R. Buckley, Giorgio Busoni, Michael Buttignol, Giacomo Cacciapaglia, Regina Caputo, Linda Carpenter, Nuno Filipe Castro, Guillelmo Gomez Ceballos, Yangyang Cheng, John Paul Chou, Arely Cortes Gonzalez, Chris Cowden, Francesco D’Eramo, Annapaola De Cosa, Michele De Gruttola, Albert De Roeck, Andrea De Simone, Aldo Deandrea, Zeynep Demiragli, Anthony DiFranzo, Caterina Doglioni, Tristan du Pree, Robin Erbacher, Johannes Erdmann, Cora Fischer, Henning Flaecher, Patrick J. Fox, Benjamin Fuks, Marie-Helene Genest, Bhawna Gomber, Andreas Goudelis, Johanna Gramling, John Gunion, Kristian Hahn, Ulrich Haisch, Roni Harnik, Philip C. Harris, Kerstin Hoepfner, Siew Yan Hoh, Dylan George Hsu, Shih-Chieh Hsu, Yutaro Iiyama, Valerio Ippolito, Thomas Jacques, Xiangyang Ju, Felix Kahlhoefer, Alexis Kalogeropoulos, Laser Seymour Kaplan, Lashkar Kashif, Valentin V. Khoze, Raman Khurana, Khristian Kotov, Dmytro Kovalskyi, Suchita Kulkarni, Shuichi Kunori, Viktor Kutzner, Hyun Min Lee, Sung-Won Lee, Seng Pei Liew, Tongyan Lin, Steven Lowette, Romain Madar, Sarah Malik, Fabio Maltoni, Mario Martinez Perez, Olivier Mattelaer, Kentarou Mawatari, Christopher McCabe, Théo Megy, Enrico Morgante, Stephen Mrenna, Chang-Seong Moon, Siddharth M. Narayanan, Andy Nelson, Sérgio F. Novaes, Klaas Ole Padeken, Priscilla Pani, Michele Papucci, Manfred Paulini, Christoph Paus, Jacopo Pazzini, Björn Penning, Michael E. Peskin, Deborah Pinna, Massimiliano Procura, Shamona F. Qazi, Davide Racco, Emanuele Re, Antonio Riotto, Thomas G. Rizzo, Rainer Roehrig, David Salek, Arturo Sanchez Pineda, Subir Sarkar, Alexander Schmidt, Steven Randolph Schramm, William Shepherd, Gurpreet Singh, Livia Soffi, Norraphat Srimanobhas, Kevin Sung, Tim M.P. Tait, Timothee Theveneaux-Pelzer, Marc Thomas, Mia Tosi, Daniele Trocino, Sonaina Undleeb, Alessandro Vichi, Fuquan Wang, Lian-Tao Wang, Ren-Jie Wang, Nikola Whallon, Steven Worm, Mengqing Wu, Sau Lan Wu, Hongtao Yang, Yong Yang, Shin-Shan Yu, Bryan Zaldivar, Marco Zanetti, Zhiqing Zhang, Alberto Zucchetta, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Oviedo Univ, Louisville Univ, Duke Univ, CERN, Heidelberg Univ, Cornell Univ, INFN Padua, Boston Univ, Rutgers State Univ, NIKHEF, Paris LPTHE, Hyderabad Univ, UC Irvine, Munich MPI, MIT, INFN Rome, SISSA Trieste, LBL, Rhein Westfal TH Aachen, Princeton Univ, Delhi Univ, Florida Univ, Univ Maryland, Texas Tech Univ, Univ Geneva, CIEMAT, Univ Lyon, CNRS, Ecole Normale Super Lyon, Univ Montreal, TRIUMF, INFN Padova, Univ Wisconsin, Ohio State Univ, Rutherford Appleton Lab, Univ Southampton, Univ Melbourne, Imperial Coll London, SISSA, INFN, Univ Strasbourg, Univ Calif Santa Cruz, LIP Minho, Univ Porto, Univ Chicago, IFAE Barcelona, Univ Calif Berkeley, LBNL, Univ Zurich, Univ Lyon 1, Univ Calif Irvine, Dept Theoret Phys, Lund Univ, San Diego Univ, Louvain CP3, Osaka Univ, Kings Coll London, Freiburg Univ, DESY, Kyungpook Natl Univ, Vanderbilt Univ, Brandeis Univ, Perimeter, Annecy LAPTH, Mainz Univ, Univ Ghent, LPHE Lausanne, Univ Birmingham, Beijing IHEP, Shanghai Jiao Tong Univ, LAPTh, Zurich Univ, Univ Calif Davis, Tech Univ Dortmund, Univ Bristol, Fermilab Natl Accelerator Lab, Univ Grenoble Alpes, Austrian Acad Sci, Northwestern Univ, Univ Oxford, Univ Malaya, Harvard Univ, Univ Durham, Natl Cent Univ, Chung Ang Univ, Univ Tokyo, Vrije Univ Brussel IIHE, Lab Phys Corpusculaire, Catholic Univ Louvain, IPPP Durham, Vrije Univ Brussel, Int Solvay Inst, Univ Amsterdam, FNAL, Universidade Estadual Paulista (Unesp), Stockholm Univ, Carnegie Mellon Univ, Stanford Univ, Univ Wien, Quaid I Azam Univ, SLAC, Max Planck Inst Phys & Astrophys, Nikhef, GRAPPA, Univ Napoli, Niels Bohr Inst, Univ Hamburg, Santa Cruz Inst Particle Phys, Univ Copenhagen, Chulalongkorn Univ, Clermont Univ, Univ Blaise Pascal, Southampton Univ, Univ Padua, Northeastern Univ, Univ Washington, Univ Libre Bruxelles, Univ Paris Sud 11, Abercrombie D., Akchurin N., Akilli E., Maestre J.A., Allen B., Gonzalez B.A., Andrea J., Arbey A., Azuelos G., Azzi P., Backovic M., Bai Y., Banerjee S., Beacham J., Belyaev A., Boveia A., Brennan A.J., Buchmueller O., Buckley M.R., Busoni G., Buttignol M., Cacciapaglia G., Caputo R., Carpenter L., Castro N.F., Ceballos G.G., Cheng Y., Chou J.P., Gonzalez A.C., Cowden C., D'Eramo F., De Cosa A., De Gruttola M., De Roeck A., De Simone A., Deandrea A., Demiragli Z., DiFranzo A., Doglioni C., du Pree T., Erbacher R., Erdmann J., Fischer C., Flaecher H., Fox P.J., Fuks B., Genest M.-H., Gomber B., Goudelis A., Gramling J., Gunion J., Hahn K., Haisch U., Harnik R., Harris P.C., Hoepfner K., Hoh S.Y., Hsu D.G., Hsu S.-C., Iiyama Y., Ippolito V., Jacques T., Ju X., Kahlhoefer F., Kalogeropoulos A., Kaplan L.S., Kashif L., Khoze V.V., Khurana R., Kotov K., Kovalskyi D., Kulkarni S., Kunori S., Kutzner V., Lee H.M., Lee S.-W., Liew S.P., Lin T., Lowette S., Madar R., Malik S., Maltoni F., Perez M.M., Mattelaer O., Mawatari K., McCabe C., Megy T., Morgante E., Mrenna S., Moon C.-S., Narayanan S.M., Nelson A., Novaes S.F., Padeken K.O., Pani P., Papucci M., Paulini M., Paus C., Pazzini J., Penning B., Peskin M.E., Pinna D., Procura M., Qazi S.F., Racco D., Re E., Riotto A., Rizzo T.G., Roehrig R., Salek D., Pineda A.S., Sarkar S., Schmidt A., Schramm S.R., Shepherd W., Singh G., Soffi L., Srimanobhas N., Sung K., Tait T.M.P., Theveneaux-Pelzer T., Thomas M., Tosi M., Trocino D., Undleeb S., Vichi A., Wang F., Wang L.-T., Wang R.-J., Whallon N., Worm S., Wu M., Wu S.L., Yang H., Yang Y., Yu S.-S., Zaldivar B., Zanetti M., Zhang Z., Zucchetta A., Physics, Elementary Particle Physics, Universidade do Minho, GRAPPA (ITFA, IoP, FNWI), ATLAS (IHEF, IoP, FNWI), Daniel, A, Nural, A, Ece, A, Juan Alcaraz, M, Brandon, A, Barbara Alvarez, G, Jeremy, A, Alexandre, A, Georges, A, Patrizia, A, Mihailo, B, Yang, B, Swagato, B, James, B, Alexander, B, Antonio, B, Amelia Jean, B, Oliver, B, Matthew R., B, Giorgio, B, Michael, B, Giacomo, C, Regina, C, Linda, C, Nuno Filipe, C, Guillelmo Gomez, C, Yangyang, C, John Paul, C, Arely Cortes, G, Chris, C, Francesco, D, Annapaola De, C, Michele De, G, Albert De, R, Andrea De, S, Aldo, D, Zeynep, D, Anthony, D, Caterina, D, Tristan du PreeRobin, E, Johannes, E, Cora, F, Henning, F, Patrick J., F, Benjamin, F, Marie-Helene, G, Bhawna, G, Andreas, G, Johanna, G, John, G, Kristian, H, Ulrich, H, Roni, H, Philip C., H, Kerstin, H, Siew Yan, H, Dylan George, H, Shih-Chieh, H, Yutaro, I, Valerio, I, Thomas, J, Xiangyang, J, Felix, K, Alexis, K, Laser Seymour, K, Lashkar, K, Valentin V., K, Raman, K, Khristian, K, Dmytro, K, Suchita, K, Shuichi, K, Viktor, K, Hyun Min, L, Sung-Won, L, Seng Pei, L, Tongyan, L, Steven, L, Romain, M, Sarah, M, Fabio, M, Mario Martinez, P, Olivier, M, Kentarou, M, Christopher, M, Théo, M, Enrico, M, Stephen, M, Siddharth M., N, Andy, N, Sérgio F., N, Klaas Ole, P, Priscilla, P, Michele, P, Manfred, P, Christoph, P, Jacopo, P, Björn, P, Michael E., P, Deborah, P, Massimiliano, P, Shamona F., Q, Davide, R, Re, E, Antonio, R, Thomas G., R, Rainer, R, David, S, Arturo Sanchez, P, Subir, S, Alexander, S, Steven Randolph, S, William, S, Gurpreet, S, Livia, S, Norraphat, S, Kevin, S, Tim M. P., T, Timothee, T, Marc, T, Mia, T, Daniele, T, Sonaina, U, Alessandro, V, Fuquan, W, Lian-Tao, W, Ren-Jie, W, Nikola, W, Steven, W, Mengqing, W, Sau Lan, W, Hongtao, Y, Yong, Y, Shin-Shan, Y, Bryan, Z, Marco, Z, Zhiqing, Z, Alberto, Z, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
dark matter: interaction, Simplified model, Physics::Instrumentation and Detectors, mass [dark matter], Parameter space, 01 natural sciences, High Energy Physics - Experiment, dark matter: coupling, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), benchmark, effective field theory, search for [dark matter], scattering [p p], Effective field theory, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Dark Matter, Simplified models, 010303 astronomy & astrophysics, Physics, Large Hadron Collider, Atlas (topology), CMS, hep-ph, ATLAS, Settore FIS/02 - Fisica Teorica, Modelli e Metodi Matematici, High Energy Physics - Phenomenology, CERN LHC Coll, interpretation of experiments, LHC, colliding beams [p p], interaction [dark matter], EFT, Particle Physics - Experiment, Particle physics, p p: scattering, Ciências Naturais::Ciências Físicas, WIMP, dark matter: search for, Ciências Físicas [Ciências Naturais], Dark matter, FOS: Physical sciences, dark matter: production, coupling [dark matter], 0103 physical sciences, ddc:530, mediation, ComputingMethodologies_COMPUTERGRAPHICS, Particle Physics - Phenomenology, Science & Technology, 010308 nuclear & particles physics, hep-ex, dark matter: mass, Astronomy and Astrophysics, production [dark matter], Formalism (philosophy of mathematics), Space and Planetary Science, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], direct detection, p p: colliding beams
Abstract

This document is the final report of the ATLAS-CMS Dark Matter Forum, a forum organized by the ATLAS and CMS collaborations with the participation of experts on theories of Dark Matter, to select a minimal basis set of dark matter simplified models that should support the design of the early LHC Run-2 searches. A prioritized, compact set of benchmark models is proposed, accompanied by studies of the parameter space of these models and a repository of generator implementations. This report also addresses how to apply the Effective Field Theory formalism for collider searches and present the results of such interpretations., The authors would like to thank Daniel Whiteson for helping in the review of this document. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence "Origin and Structure of the Universe''. The authors would like to express a special thanks to the Mainz Institute for Theoretical Physics (MITP) for its hospitality and support. P. Pani wishes to thank the support of the Computing Infrastructure of Nikhef. In addition we thank CERN and acknowledge the support of: DOE and NSF (USA), including grant DE-SC0011726 for the preparation of this manuscript; SER, SNSF and Cantons of Bern and Geneva, Switzerland; MINECO, Spain; European Union, where the preparation of this manuscript is part of a project that has received funding from the European Research Council under the European Union's Horizon 2020 research and innovation program (grant agreement 679305); IN2P3-CNRS, CEA-DSM/IRFU, France; NSERC, NRC, and CFI, Canada; INFN, Italy; FNRS and FWO, Belgium; STFC, United Kingdom; ARC, Australia; GRICES and FCT, Portugal; SRC, Sweden; BMBF, DFG, HGF, MPG and AvH Foundation, Germany; Austrian Academy of Sciences, Austria; MOE and UM, Malaysia; National Research Foundation and Ministry of Education, Science and Technology, Korea; MEXT and JSPS, Japan; FOM and NWO, Netherlands; CNPq and FAPESP, Brazil; Atomic Energy Commission, Pakistan; DNRF, DNSRC and Lundbeck Foundation, Denmark; Thailand Center of Excellence in Physics, Institute for the Promotion of Teaching Science and Technology, Special Task Force for Activating Research and National Science and Technology Development Agency, Thailand; MOST, Taiwan., info:eu-repo/semantics/publishedVersion

Published
2015
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19. Footprints of the QCD Crossover on Cosmological Gravitational Waves at Pulsar Timing Arrays.

Author

Franciolini G, Racco D, and Rompineve F

Abstract

Pulsar timing arrays (PTAs) have reported evidence for a stochastic gravitational wave (GW) background at nanohertz frequencies, possibly originating in the early Universe. We show that the spectral shape of the low-frequency (causality) tail of GW signals sourced at temperatures around T≳1  GeV is distinctively affected by confinement of strong interactions (QCD), due to the corresponding sharp decrease in the number of relativistic species, and significantly deviates from ∼f^{3} commonly adopted in the literature. Bayesian analyses in the NANOGrav 15 years and the previous international PTA datasets reveal a significant improvement in the fit with respect to cubic power-law spectra, previously employed for the causality tail. While no conclusion on the nature of the signal can be drawn at the moment, our results show that the inclusion of standard model effects on cosmological GWs can have a decisive impact on model selection.

Published
2024
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