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Testing the Molecular Cloud Paradigm for Ultra-High-Energy Gamma Ray Emission from the Direction of SNR G106.3+2.7

Fuente: arXiv

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Detalles Bibliográficos
Autores principales:	Alfaro, R., Alvarez, C., Arteaga-Velázquez, J. C., Rojas, D. Avila, Solares, H. A. Ayala, Babu, R., Belmont-Moreno, E., Bernal, A., Caballero-Mora, K. S., Capistrán, T., Carramiñana, A., Casanova, S., Cotti, U., Cotzomi, J., de León, S. Coutiño, De la Fuente, E., de León, C., Depaoli, D., Desiati, P., Di Lalla, N., Hernandez, R. Diaz, Dingus, B. L., DuVernois, M. A., Engel, K., Ergin, T., Espinoza, C., Fan, K. L., Fang, K., Fraija, N., Fraija, S., García-González, J. A., Garfias, F., González, M. M., Goodman, J. A., Groetsch, S., Harding, J. P., Hernández-Cadena, S., Herzog, I., Hinton, J., Huang, D., Hueyotl-Zahuantitla, F., Humensky, T. B., Hüntemeyer, P., Kaufmann, S., Kieda, D., Lee, W. H., Lee, J., Vargas, H. León, Linnemann, J. T., Longinotti, A. L., Luis-Raya, G., Malone, K., Martinez, O., Martínez-Castro, J., Matthews, J. A., Miranda-Romagnoli, P., Montes, J. A., Moreno, E., Mostafá, M., Nellen, L., Nisa, M. U., Olivera-Nieto, L., Omodei, N., Araujo, Y. Pérez, Pérez-Pérez, E. G., Rho, C. D., Rosa-González, D., Salazar, H., Salazar-Gallegos, D., Sandoval, A., Schneider, M., Serna-Franco, J., Smith, A. J., Son, Y., Springer, R. W., Tibolla, O., Tollefson, K., Torres, I., Torres-Escobedo, R., Turner, R., Ureña-Mena, F., Varela, E., Villaseñor, L., Wang, X., Wang, Z., Watson, I. J., Willox, E., Yu, S., Yun-Cárcamo, S., Zhou, H.
Formato:	Preprint
Publicado:	2024
Materias:	High Energy Astrophysical Phenomena
Acceso en línea:	Acceder al recurso
Etiquetas:	Agregar Etiqueta Sin Etiquetas, Sea el primero en etiquetar este registro!

_version_	1866916458893672448
author	Alfaro, R. Alvarez, C. Arteaga-Velázquez, J. C. Rojas, D. Avila Solares, H. A. Ayala Babu, R. Belmont-Moreno, E. Bernal, A. Caballero-Mora, K. S. Capistrán, T. Carramiñana, A. Casanova, S. Cotti, U. Cotzomi, J. de León, S. Coutiño De la Fuente, E. de León, C. Depaoli, D. Desiati, P. Di Lalla, N. Hernandez, R. Diaz Dingus, B. L. DuVernois, M. A. Engel, K. Ergin, T. Espinoza, C. Fan, K. L. Fang, K. Fraija, N. Fraija, S. García-González, J. A. Garfias, F. González, M. M. Goodman, J. A. Groetsch, S. Harding, J. P. Hernández-Cadena, S. Herzog, I. Hinton, J. Huang, D. Hueyotl-Zahuantitla, F. Humensky, T. B. Hüntemeyer, P. Kaufmann, S. Kieda, D. Lee, W. H. Lee, J. Vargas, H. León Linnemann, J. T. Longinotti, A. L. Luis-Raya, G. Malone, K. Martinez, O. Martínez-Castro, J. Matthews, J. A. Miranda-Romagnoli, P. Montes, J. A. Moreno, E. Mostafá, M. Nellen, L. Nisa, M. U. Olivera-Nieto, L. Omodei, N. Araujo, Y. Pérez Pérez-Pérez, E. G. Rho, C. D. Rosa-González, D. Salazar, H. Salazar-Gallegos, D. Sandoval, A. Schneider, M. Serna-Franco, J. Smith, A. J. Son, Y. Springer, R. W. Tibolla, O. Tollefson, K. Torres, I. Torres-Escobedo, R. Turner, R. Ureña-Mena, F. Varela, E. Villaseñor, L. Wang, X. Wang, Z. Watson, I. J. Willox, E. Yu, S. Yun-Cárcamo, S. Zhou, H.
author_facet	Alfaro, R. Alvarez, C. Arteaga-Velázquez, J. C. Rojas, D. Avila Solares, H. A. Ayala Babu, R. Belmont-Moreno, E. Bernal, A. Caballero-Mora, K. S. Capistrán, T. Carramiñana, A. Casanova, S. Cotti, U. Cotzomi, J. de León, S. Coutiño De la Fuente, E. de León, C. Depaoli, D. Desiati, P. Di Lalla, N. Hernandez, R. Diaz Dingus, B. L. DuVernois, M. A. Engel, K. Ergin, T. Espinoza, C. Fan, K. L. Fang, K. Fraija, N. Fraija, S. García-González, J. A. Garfias, F. González, M. M. Goodman, J. A. Groetsch, S. Harding, J. P. Hernández-Cadena, S. Herzog, I. Hinton, J. Huang, D. Hueyotl-Zahuantitla, F. Humensky, T. B. Hüntemeyer, P. Kaufmann, S. Kieda, D. Lee, W. H. Lee, J. Vargas, H. León Linnemann, J. T. Longinotti, A. L. Luis-Raya, G. Malone, K. Martinez, O. Martínez-Castro, J. Matthews, J. A. Miranda-Romagnoli, P. Montes, J. A. Moreno, E. Mostafá, M. Nellen, L. Nisa, M. U. Olivera-Nieto, L. Omodei, N. Araujo, Y. Pérez Pérez-Pérez, E. G. Rho, C. D. Rosa-González, D. Salazar, H. Salazar-Gallegos, D. Sandoval, A. Schneider, M. Serna-Franco, J. Smith, A. J. Son, Y. Springer, R. W. Tibolla, O. Tollefson, K. Torres, I. Torres-Escobedo, R. Turner, R. Ureña-Mena, F. Varela, E. Villaseñor, L. Wang, X. Wang, Z. Watson, I. J. Willox, E. Yu, S. Yun-Cárcamo, S. Zhou, H.
contents	Supernova remnants (SNRs) are believed to be capable of accelerating cosmic rays (CRs) to PeV energies. SNR G106.3+2.7 is a prime PeVatron candidate. It is formed by a head region, where the pulsar J2229+6114 and its boomerang-shaped pulsar wind nebula are located, and a tail region containing SN ejecta. The lack of observed gamma ray emission from the two regions of this SNR has made it difficult to assess which region would be responsible for the PeV CRs. We aim to characterize the very-high-energy (VHE, 0.1-100 TeV) gamma ray emission from SNR G106.3+2.7 by determining the morphology and spectral energy distribution of the region. This is accomplished using 2565 days of data and improved reconstruction algorithms from the HAWC Observatory. We also explore possible gamma ray production mechanisms for different energy ranges. Using a multi-source fitting procedure based on a maximum-likelihood estimation method, we evaluate the complex nature of this region. We determine the morphology, spectrum, and energy range for the source found in the region. Molecular cloud information is also used to create a template and evaluate the HAWC gamma ray spectral properties at ultra-high-energies (UHE, >56 TeV). This will help probe the hadronic nature of the highest-energy emission from the region. We resolve one extended source coincident with all other gamma ray observations of the region. The emission reaches above 100~TeV and its preferred log-parabola shape in the spectrum shows a flux peak in the TeV range. The molecular cloud template fit on the higher energy data reveals that the SNR's energy budget is fully capable of producing a purely hadronic source for UHE gamma rays.
format	Preprint
id	arxiv_https___arxiv_org_abs_2407_10729
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	Testing the Molecular Cloud Paradigm for Ultra-High-Energy Gamma Ray Emission from the Direction of SNR G106.3+2.7 Alfaro, R. Alvarez, C. Arteaga-Velázquez, J. C. Rojas, D. Avila Solares, H. A. Ayala Babu, R. Belmont-Moreno, E. Bernal, A. Caballero-Mora, K. S. Capistrán, T. Carramiñana, A. Casanova, S. Cotti, U. Cotzomi, J. de León, S. Coutiño De la Fuente, E. de León, C. Depaoli, D. Desiati, P. Di Lalla, N. Hernandez, R. Diaz Dingus, B. L. DuVernois, M. A. Engel, K. Ergin, T. Espinoza, C. Fan, K. L. Fang, K. Fraija, N. Fraija, S. García-González, J. A. Garfias, F. González, M. M. Goodman, J. A. Groetsch, S. Harding, J. P. Hernández-Cadena, S. Herzog, I. Hinton, J. Huang, D. Hueyotl-Zahuantitla, F. Humensky, T. B. Hüntemeyer, P. Kaufmann, S. Kieda, D. Lee, W. H. Lee, J. Vargas, H. León Linnemann, J. T. Longinotti, A. L. Luis-Raya, G. Malone, K. Martinez, O. Martínez-Castro, J. Matthews, J. A. Miranda-Romagnoli, P. Montes, J. A. Moreno, E. Mostafá, M. Nellen, L. Nisa, M. U. Olivera-Nieto, L. Omodei, N. Araujo, Y. Pérez Pérez-Pérez, E. G. Rho, C. D. Rosa-González, D. Salazar, H. Salazar-Gallegos, D. Sandoval, A. Schneider, M. Serna-Franco, J. Smith, A. J. Son, Y. Springer, R. W. Tibolla, O. Tollefson, K. Torres, I. Torres-Escobedo, R. Turner, R. Ureña-Mena, F. Varela, E. Villaseñor, L. Wang, X. Wang, Z. Watson, I. J. Willox, E. Yu, S. Yun-Cárcamo, S. Zhou, H. High Energy Astrophysical Phenomena Supernova remnants (SNRs) are believed to be capable of accelerating cosmic rays (CRs) to PeV energies. SNR G106.3+2.7 is a prime PeVatron candidate. It is formed by a head region, where the pulsar J2229+6114 and its boomerang-shaped pulsar wind nebula are located, and a tail region containing SN ejecta. The lack of observed gamma ray emission from the two regions of this SNR has made it difficult to assess which region would be responsible for the PeV CRs. We aim to characterize the very-high-energy (VHE, 0.1-100 TeV) gamma ray emission from SNR G106.3+2.7 by determining the morphology and spectral energy distribution of the region. This is accomplished using 2565 days of data and improved reconstruction algorithms from the HAWC Observatory. We also explore possible gamma ray production mechanisms for different energy ranges. Using a multi-source fitting procedure based on a maximum-likelihood estimation method, we evaluate the complex nature of this region. We determine the morphology, spectrum, and energy range for the source found in the region. Molecular cloud information is also used to create a template and evaluate the HAWC gamma ray spectral properties at ultra-high-energies (UHE, >56 TeV). This will help probe the hadronic nature of the highest-energy emission from the region. We resolve one extended source coincident with all other gamma ray observations of the region. The emission reaches above 100~TeV and its preferred log-parabola shape in the spectrum shows a flux peak in the TeV range. The molecular cloud template fit on the higher energy data reveals that the SNR's energy budget is fully capable of producing a purely hadronic source for UHE gamma rays.
title	Testing the Molecular Cloud Paradigm for Ultra-High-Energy Gamma Ray Emission from the Direction of SNR G106.3+2.7
topic	High Energy Astrophysical Phenomena
url	https://arxiv.org/abs/2407.10729