% IMPORTANT: The following is UTF-8 encoded.  This means that in the presence
% of non-ASCII characters, it will not work with BibTeX 0.99 or older.
% Instead, you should use an up-to-date BibTeX implementation like “bibtex8” or
% “biber”.

@ARTICLE{Candn:627065,
      author       = {Candón, Francisco R. and Fiorillo, Damiano Francesco
                      Giuseppe and Lucente, Giuseppe and Vitagliano, Edoardo and
                      Vogel, Julia K.},
      title        = {{N}u{STAR} {B}ounds on {R}adiatively {D}ecaying {P}articles
                      from {M}82},
      journal      = {Physical review letters},
      volume       = {134},
      number       = {17},
      issn         = {0031-9007},
      address      = {College Park, Md.},
      publisher    = {APS},
      reportid     = {PUBDB-2025-01537, arXiv:2412.03660},
      pages        = {171004},
      year         = {2025},
      note         = {Phys. Rev. Lett. 134, 171004 (2025). 4 pages, 3 figures,
                      plus Supplemental Material},
      abstract     = {Axions and other putative feebly interacting particles
                      (FIPs) with a mass of tens to several hundreds of keVs can
                      be produced in stellar cores with a Lorentz boost factor
                      $E_a/m_a\lesssim 10$. Thus, starburst galaxies such as M82
                      are efficient factories of slow axions. Their decay
                      $a\rightarrow\gamma\gamma$ would produce a large flux of
                      X-ray photons, peaking around $100$ keV and spread around
                      the galaxy by an angle that can be relatively large. We use
                      observations of the Nuclear Spectroscopic Telescope Array
                      (NuSTAR) mission to show that the absence of these features
                      can constrain $30-500$ keV axion masses into uncharted
                      regions for axion-photon coupling of $g_{a\gamma}\sim
                      10^{-10}-10^{-12}\,\rm GeV^{-1}$. Our argument can be
                      applied to other heavy FIPs and astrophysical sources that
                      are hot enough to produce them, yet cold enough to avoid
                      large boost factors which slow down the decay.},
      cin          = {$Z_THAT$},
      ddc          = {530},
      cid          = {$I:(DE-H253)Z_THAT-20210408$},
      pnm          = {613 - Matter and Radiation from the Universe (POF4-613) /
                      INTERACTIONS - NBIA INTERACTIONS POSTDOCTORAL PROGRAMME
                      (847523) / HIDDeN - Hunting Invisibles: Dark sectors, Dark
                      matter and Neutrinos (860881)},
      pid          = {G:(DE-HGF)POF4-613 / G:(EU-Grant)847523 /
                      G:(EU-Grant)860881},
      experiment   = {EXP:(DE-MLZ)NOSPEC-20140101},
      typ          = {PUB:(DE-HGF)16},
      eprint       = {2412.03660},
      howpublished = {arXiv:2412.03660},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:2412.03660;\%\%$},
      doi          = {10.1103/PhysRevLett.134.171004},
      url          = {https://bib-pubdb1.desy.de/record/627065},
}