TeV Gamma-Ray Emission in the DA 495 Region from HAWC Observations of J1952+2924, J1954+2837, and J1958+2848

@misc{alfaro2026gammaray,
  title = {{TeV Gamma-Ray Emission in the DA 495 Region from HAWC Observations of J1952+2924, J1954+2837, and J1958+2848}},
  author = {R. Alfaro and C. Alvarez and E. Anita-Rangel and M. Araya and J. C. Arteaga-Velázquez and D. Avila Rojas and H. A. Ayala Solares and R. Babu and P. Bangale and A. Bernal and T. Capistrán and A. Carramiñana and S. Casanova and U. Cotti and J. Cotzomi and S. Coutiño de León and E. De la Fuente and N. Di Lalla and R. Diaz Hernandez and M. A. DuVernois and J. C. Díaz-Vélez and C. Espinoza and N. Fraija and S. Fraija and A. Galván-Gámez and J. A. García-González and F. Garfias and N. Ghosh and A. Gonzalez Muñoz and M. M. González and J. A. González and J. A. Goodman and J. Gyeong and J. P. Harding and I. Herzog and D. Huang and F. Hueyotl-Zahuantitla and P. Hüntemeyer and A. Iriarte and S. Kaufmann and D. Kieda and K. Leavitt and W. H. Lee and H. León Vargas and A. L. Longinotti and G. Luis-Raya and K. Malone and O. Martinez and J. Martínez-Castro and J. A. Matthews and P. Miranda-Romagnoli and P. E. Mirón-Enriquez and J. A. Morales-Soto and E. Moreno and M. Mostafá and M. Najafi and L. Nellen and M. U. Nisa and R. Noriega-Papaqui and M. Osorio-Archila},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.13771},
  eprint = {2610.13771},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.13771},
}

TY  - UNPB
TI  - TeV Gamma-Ray Emission in the DA 495 Region from HAWC Observations of J1952+2924, J1954+2837, and J1958+2848
AU  - R. Alfaro
AU  - C. Alvarez
AU  - E. Anita-Rangel
AU  - M. Araya
AU  - J. C. Arteaga-Velázquez
AU  - D. Avila Rojas
AU  - H. A. Ayala Solares
AU  - R. Babu
AU  - P. Bangale
AU  - A. Bernal
AU  - T. Capistrán
AU  - A. Carramiñana
AU  - S. Casanova
AU  - U. Cotti
AU  - J. Cotzomi
AU  - S. Coutiño de León
AU  - E. De la Fuente
AU  - N. Di Lalla
AU  - R. Diaz Hernandez
AU  - M. A. DuVernois
AU  - J. C. Díaz-Vélez
AU  - C. Espinoza
AU  - N. Fraija
AU  - S. Fraija
AU  - A. Galván-Gámez
AU  - J. A. García-González
AU  - F. Garfias
AU  - N. Ghosh
AU  - A. Gonzalez Muñoz
AU  - M. M. González
AU  - J. A. González
AU  - J. A. Goodman
AU  - J. Gyeong
AU  - J. P. Harding
AU  - I. Herzog
AU  - D. Huang
AU  - F. Hueyotl-Zahuantitla
AU  - P. Hüntemeyer
AU  - A. Iriarte
AU  - S. Kaufmann
AU  - D. Kieda
AU  - K. Leavitt
AU  - W. H. Lee
AU  - H. León Vargas
AU  - A. L. Longinotti
AU  - G. Luis-Raya
AU  - K. Malone
AU  - O. Martinez
AU  - J. Martínez-Castro
AU  - J. A. Matthews
AU  - P. Miranda-Romagnoli
AU  - P. E. Mirón-Enriquez
AU  - J. A. Morales-Soto
AU  - E. Moreno
AU  - M. Mostafá
AU  - M. Najafi
AU  - L. Nellen
AU  - M. U. Nisa
AU  - R. Noriega-Papaqui
AU  - M. Osorio-Archila
PY  - 2026
DA  - 2026/10/09
PB  - arXiv
DO  - 10.48550/arxiv.2610.13771
UR  - https://arxiv.org/abs/2610.13771
AB  - Previous observations of the DA 495 region, which contains the pulsar wind nebula (PWN) DA 495 and other very-high-energy (VHE; >100 GeV) gamma-ray emitters, showed inconsistent results across different VHE experiments, including differences in the measured flux of DA 495 and in the number of reported sources. Our new dedicated analysis using 3071 days of HAWC data resolves these discrepancies. We identify three extended sources, HAWC J1952+2924 (DA 495), HAWC J1954+2837, and HAWC J1958+2848, all with curved spectra, and find a hint of a fourth source. For DA 495, a multi-wavelength analysis, including our results, radio, X-ray, and other gamma-ray data, reveals that its extended emission is best described by leptonic interactions with an inferred magnetic field of B∼10 μG and that hadronic components are not required. On the other hand, we interpret the other two sources, which have no confirmed counterparts, as TeV halos associated with nearby pulsars, PSR J1954+2836 and PSR J1958+2846, respectively. These results reinforce the interpretation of DA 495 as a leptonic-dominated PWN and add two candidates to the growing population of TeV halos.
ER  -