Line-like features in TeV γ-rays constitute a ''smoking gun'' for TeV-scale particle dark matter and new physics. Probing the Galactic Center region with ground-based Cherenkov telescopes enables the search for TeV spectral features in immediate association with a dense dark matter reservoir at a sensitivity out of reach for satellite γ-ray detectors, and direct detection and collider experiments. We report on 223 hours of observations of the Galactic Center region with the MAGIC stereoscopic telescope system reaching γ-ray energies up to 100 TeV. We improved the sensitivity to spectral lines at high energies using large-zenith-angle observations and a novel background modeling method within a maximum-likelihood analysis in the energy domain. No line-like spectral feature is found in our analysis. Therefore, we constrain the cross section for dark matter annihilation into two photons to ⟨σv⟩≲5×10−28cm3s−1 at 1 TeV and ⟨σv⟩≲1×10−25cm3s−1 at 100 TeV, achieving the best limits to date for a dark matter mass above 20 TeV and a cuspy dark matter profile at the Galactic Center. Finally, we use the derived limits for both cuspy and cored dark matter profiles to constrain supersymmetric wino models.

Search for gamma-ray spectral lines from dark matter annihilation up to 100 tev towards the galactic center with magic / Abe, H.; Abe, S.; Acciari, V. A.; Aniello, T.; Ansoldi, S.; 4, ; Antonelli, 5 L. A.; Arbet Engels, 3 A.; Arcaro, 6 C.; Artero, 7 M.; Asano, 8 K.; Baack, 1 D.; Babić, 9 A.; Baquero, 10 A.; Barres de Almeida, 11 U.; Barrio, 12 J. A.; Batković, 11 I.; Baxter, 7 J.; Becerra González, 1 J.; Bednarek, 2 W.; Bernardini, 13 E.; Bernardos, 7 M.; Berti, 14 A.; Besenrieder, 6 J.; Bhattacharyya, 6 W.; Bigongiari, 15 C.; Biland, 3 A.; Blanch, 16 O.; Bonnoli, 8 G.; Bošnjak, 3 Ž.; Burelli, 10 I.; Busetto, 4 G.; Carosi, 7 R.; Carretero-Castrillo, 17 M.; Ceribella, 18 G.; Chai, 1 Y.; Chilingarian, 6 A.; Cikota, 19 S.; Colombo, 10 E.; Contreras, 2 J. L.; Cortina, 11 J.; Covino, 20 S.; D’Amico, 3 G.; D’Elia, 21 V.; Da Vela, 3 P.; 17, ; Dazzi, 22 F.; De Angelis, 3 A.; De Lotto, 7 B.; Del Popolo, 4 A.; Delfino, 23 M.; 8, ; Delgado, 24 J.; 8, ; Delgado Mendez, 24 C.; Depaoli, 20 D.; Di Pierro, 25 F.; Di Venere, 25 L.; Do Souto Espiñeira, 26 E.; Dominis Prester, 8 D.; Donini, 27 A.; Dorner, 3 D.; Doro, 28 M.; Elsaesser, 7 D.; Emery, 9 G.; Fallah Ramazani, 29 V.; 30, ; Fariña, 31 L.; Fattorini, 8 A.; Font, 9 L.; Fruck, 32 C.; Fukami, 6 S.; Fukazawa, 16 Y.; García López, 33 R. J.; Garczarczyk, 2 M.; Gasparyan, 15 S.; Gaug, 34 M.; Giesbrecht Paiva, 32 J. G.; Giglietto, 12 N.; Giordano, 26 F.; Gliwny, 26 P.; Godinović, 13 N.; Green, 35 J. G.; Green, 6 D.; Hadasch, 6 D.; Hahn, 1 A.; Hassan, 6 T.; Heckmann, 20 L.; 6, ; Herrera, 36 J.; Hrupec, 2 D.; Hütten, 37 M.; 1, ; Imazawa, ∗ R.; Inada, 33 T.; 1, ; Iotov, ∗ R.; Ishio, 28 K.; Jiménez Martínez, 13 I.; Jormanainen, 20 J.; Kerszberg, 30 D.; 8, ; Kobayashi, ∗ Y.; Kubo, 1 H.; Kushida, 1 J.; Lamastra, 38 A.; Lelas, 3 D.; Leone, 35 F.; Lindfors, 3 E.; Linhoff, 30 L.; Lombardi, 9 S.; Longo, 3 F.; 4, ; López-Coto, 39 R.; López-Moya, 7 M.; López-Oramas, 11 A.; Loporchio, 2 S.; Lorini, 26 A.; Lyard, 40 E.; Machado de Oliveira Fraga, 29 B.; Majumdar, 12 P.; 41, ; Makariev, 42 M.; Maneva, 43 G.; Mang, 43 N.; Manganaro, 9 M.; Mangano, 27 S.; Mannheim, 20 K.; Mariotti, 28 M.; Martínez, 7 M.; Mas Aguilar, 8 A.; Mazin, 11 D.; 1, ; Menchiari, 6 S.; Mender, 40 S.; Mićanović, 9 S.; Miceli, 27 D.; Miener, 7 T.; Miranda, 11 J. M.; Mirzoyan, 40 R.; Molina, 6 E.; Mondal, 18 H. A.; Moralejo, 41 A.; Morcuende, 8 D.; Moreno, 11 V.; Nakamori, 32 T.; Nanci, 44 C.; Nava, 3 L.; Neustroev, 3 V.; Nievas Rosillo, 45 M.; Nigro, 2 C.; Nilsson, 8 K.; Nishijima, 30 K.; Njoh Ekoume, 38 T.; Noda, 2 K.; Nozaki, 1 S.; Ohtani, 6 Y.; Oka, 1 T.; Otero-Santos, 46 J.; Paiano, 2 S.; Palatiello, 3 M.; Paneque, 4 D.; Paoletti, 6 R.; Paredes, 40 J. M.; Pavletić, 18 L.; Persic, 27 M.; 4, ; Pihet, 47 M.; Podobnik, 6 F.; Prada Moroni, 40 P. G.; Prandini, 17 E.; Principe, 7 G.; Priyadarshi, 4 C.; Puljak, 8 I.; Rhode, 35 W.; Ribó, 9 M.; Rico, 18 J.; Righi, 8 C.; Rugliancich, 3 A.; Sahakyan, 17 N.; Saito, 34 T.; Sakurai, 1 S.; Satalecka, 1 K.; Saturni, 30 F. G.; Schleicher, 3 B.; Schmidt, 28 K.; Schmuckermaier, 9 F.; Schubert, 6 J. L.; Schweizer, 9 T.; Sitarek, 6 J.; Sliusar, 13 V.; Sobczynska, 29 D.; Spolon, 13 A.; Stamerra, 7 A.; Strišković, 3 J.; Strom, 37 D.; Strzys, 6 M.; Suda, 1 Y.; Surić, 33 T.; Takahashi, 48 M.; Takeishi, 49 R.; Tavecchio, 1 F.; Temnikov, 3 P.; Terauchi, 43 K.; Terzić, 46 T.; Teshima, 27 M.; 6, ; Tosti, 1 L.; Truzzi, 50 S.; Tutone, 40 A.; Ubach, 3 S.; van Scherpenberg, 32 J.; Vazquez Acosta, 6 M.; Ventura, 2 S.; Verguilov, 40 V.; Viale, 43 I.; Vigorito, 7 C. F.; Vitale, 25 V.; Vovk, 51 I.; Walter, 1 R.; Will, 29 M.; Wunderlich, 6 C.; Yamamoto, 40 T.; Zarić35, 52 and D.. - In: PHYSICAL REVIEW LETTERS. - ISSN 1092-0145. - (2022).

Search for gamma-ray spectral lines from dark matter annihilation up to 100 tev towards the galactic center with magic

T. Aniello;
2022

Abstract

Line-like features in TeV γ-rays constitute a ''smoking gun'' for TeV-scale particle dark matter and new physics. Probing the Galactic Center region with ground-based Cherenkov telescopes enables the search for TeV spectral features in immediate association with a dense dark matter reservoir at a sensitivity out of reach for satellite γ-ray detectors, and direct detection and collider experiments. We report on 223 hours of observations of the Galactic Center region with the MAGIC stereoscopic telescope system reaching γ-ray energies up to 100 TeV. We improved the sensitivity to spectral lines at high energies using large-zenith-angle observations and a novel background modeling method within a maximum-likelihood analysis in the energy domain. No line-like spectral feature is found in our analysis. Therefore, we constrain the cross section for dark matter annihilation into two photons to ⟨σv⟩≲5×10−28cm3s−1 at 1 TeV and ⟨σv⟩≲1×10−25cm3s−1 at 100 TeV, achieving the best limits to date for a dark matter mass above 20 TeV and a cuspy dark matter profile at the Galactic Center. Finally, we use the derived limits for both cuspy and cored dark matter profiles to constrain supersymmetric wino models.
2022
gamma-ray, dark matter, MAGIC
01 Pubblicazione su rivista::01a Articolo in rivista
Search for gamma-ray spectral lines from dark matter annihilation up to 100 tev towards the galactic center with magic / Abe, H.; Abe, S.; Acciari, V. A.; Aniello, T.; Ansoldi, S.; 4, ; Antonelli, 5 L. A.; Arbet Engels, 3 A.; Arcaro, 6 C.; Artero, 7 M.; Asano, 8 K.; Baack, 1 D.; Babić, 9 A.; Baquero, 10 A.; Barres de Almeida, 11 U.; Barrio, 12 J. A.; Batković, 11 I.; Baxter, 7 J.; Becerra González, 1 J.; Bednarek, 2 W.; Bernardini, 13 E.; Bernardos, 7 M.; Berti, 14 A.; Besenrieder, 6 J.; Bhattacharyya, 6 W.; Bigongiari, 15 C.; Biland, 3 A.; Blanch, 16 O.; Bonnoli, 8 G.; Bošnjak, 3 Ž.; Burelli, 10 I.; Busetto, 4 G.; Carosi, 7 R.; Carretero-Castrillo, 17 M.; Ceribella, 18 G.; Chai, 1 Y.; Chilingarian, 6 A.; Cikota, 19 S.; Colombo, 10 E.; Contreras, 2 J. L.; Cortina, 11 J.; Covino, 20 S.; D’Amico, 3 G.; D’Elia, 21 V.; Da Vela, 3 P.; 17, ; Dazzi, 22 F.; De Angelis, 3 A.; De Lotto, 7 B.; Del Popolo, 4 A.; Delfino, 23 M.; 8, ; Delgado, 24 J.; 8, ; Delgado Mendez, 24 C.; Depaoli, 20 D.; Di Pierro, 25 F.; Di Venere, 25 L.; Do Souto Espiñeira, 26 E.; Dominis Prester, 8 D.; Donini, 27 A.; Dorner, 3 D.; Doro, 28 M.; Elsaesser, 7 D.; Emery, 9 G.; Fallah Ramazani, 29 V.; 30, ; Fariña, 31 L.; Fattorini, 8 A.; Font, 9 L.; Fruck, 32 C.; Fukami, 6 S.; Fukazawa, 16 Y.; García López, 33 R. J.; Garczarczyk, 2 M.; Gasparyan, 15 S.; Gaug, 34 M.; Giesbrecht Paiva, 32 J. G.; Giglietto, 12 N.; Giordano, 26 F.; Gliwny, 26 P.; Godinović, 13 N.; Green, 35 J. G.; Green, 6 D.; Hadasch, 6 D.; Hahn, 1 A.; Hassan, 6 T.; Heckmann, 20 L.; 6, ; Herrera, 36 J.; Hrupec, 2 D.; Hütten, 37 M.; 1, ; Imazawa, ∗ R.; Inada, 33 T.; 1, ; Iotov, ∗ R.; Ishio, 28 K.; Jiménez Martínez, 13 I.; Jormanainen, 20 J.; Kerszberg, 30 D.; 8, ; Kobayashi, ∗ Y.; Kubo, 1 H.; Kushida, 1 J.; Lamastra, 38 A.; Lelas, 3 D.; Leone, 35 F.; Lindfors, 3 E.; Linhoff, 30 L.; Lombardi, 9 S.; Longo, 3 F.; 4, ; López-Coto, 39 R.; López-Moya, 7 M.; López-Oramas, 11 A.; Loporchio, 2 S.; Lorini, 26 A.; Lyard, 40 E.; Machado de Oliveira Fraga, 29 B.; Majumdar, 12 P.; 41, ; Makariev, 42 M.; Maneva, 43 G.; Mang, 43 N.; Manganaro, 9 M.; Mangano, 27 S.; Mannheim, 20 K.; Mariotti, 28 M.; Martínez, 7 M.; Mas Aguilar, 8 A.; Mazin, 11 D.; 1, ; Menchiari, 6 S.; Mender, 40 S.; Mićanović, 9 S.; Miceli, 27 D.; Miener, 7 T.; Miranda, 11 J. M.; Mirzoyan, 40 R.; Molina, 6 E.; Mondal, 18 H. A.; Moralejo, 41 A.; Morcuende, 8 D.; Moreno, 11 V.; Nakamori, 32 T.; Nanci, 44 C.; Nava, 3 L.; Neustroev, 3 V.; Nievas Rosillo, 45 M.; Nigro, 2 C.; Nilsson, 8 K.; Nishijima, 30 K.; Njoh Ekoume, 38 T.; Noda, 2 K.; Nozaki, 1 S.; Ohtani, 6 Y.; Oka, 1 T.; Otero-Santos, 46 J.; Paiano, 2 S.; Palatiello, 3 M.; Paneque, 4 D.; Paoletti, 6 R.; Paredes, 40 J. M.; Pavletić, 18 L.; Persic, 27 M.; 4, ; Pihet, 47 M.; Podobnik, 6 F.; Prada Moroni, 40 P. G.; Prandini, 17 E.; Principe, 7 G.; Priyadarshi, 4 C.; Puljak, 8 I.; Rhode, 35 W.; Ribó, 9 M.; Rico, 18 J.; Righi, 8 C.; Rugliancich, 3 A.; Sahakyan, 17 N.; Saito, 34 T.; Sakurai, 1 S.; Satalecka, 1 K.; Saturni, 30 F. G.; Schleicher, 3 B.; Schmidt, 28 K.; Schmuckermaier, 9 F.; Schubert, 6 J. L.; Schweizer, 9 T.; Sitarek, 6 J.; Sliusar, 13 V.; Sobczynska, 29 D.; Spolon, 13 A.; Stamerra, 7 A.; Strišković, 3 J.; Strom, 37 D.; Strzys, 6 M.; Suda, 1 Y.; Surić, 33 T.; Takahashi, 48 M.; Takeishi, 49 R.; Tavecchio, 1 F.; Temnikov, 3 P.; Terauchi, 43 K.; Terzić, 46 T.; Teshima, 27 M.; 6, ; Tosti, 1 L.; Truzzi, 50 S.; Tutone, 40 A.; Ubach, 3 S.; van Scherpenberg, 32 J.; Vazquez Acosta, 6 M.; Ventura, 2 S.; Verguilov, 40 V.; Viale, 43 I.; Vigorito, 7 C. F.; Vitale, 25 V.; Vovk, 51 I.; Walter, 1 R.; Will, 29 M.; Wunderlich, 6 C.; Yamamoto, 40 T.; Zarić35, 52 and D.. - In: PHYSICAL REVIEW LETTERS. - ISSN 1092-0145. - (2022).
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11573/1672886
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