Neutrino mass bounds from neutrinoless double beta-decays and cosmological probes

详细信息    查看全文

• 作者：YONG-YEON KEUM
• 关键词：Neutrino masses ; neutrinoless double beta decay ; large ; scale structures ; interacting neutrino dark ; energy model ; 13.15.+g ; 14.60.Pq ; 14.60.St ; 95.36.+ x ; 95.75. ; z
• 刊名：Pramana
• 出版年：2016
• 出版时间：February 2016
• 年：2016
• 卷：86
• 期：2
• 页码：437-451
• 全文大小：448 KB
• 参考文献：[1]J Bonne et al, Nuch. Phys. B (Proc. Suppl.) 91, 273 (2001)CrossRef ADS
  [2]Ch Weinheimer, Nucl. Phys. B (Proc. Suppl.) 118, 279 (2003)CrossRef ADS
  [3]V A Rodin, A Faessler, F Simkovic and P Vogel, Phys. Rev. C 68, 044302 (2003)CrossRef ADS
  [4]Heidelberg-Moscow Collaboration: L Baudis et al, Phys. Rev. Lett. 83, 41 (1999)
  [5]IGEX Collaboration: C E Aalseth et al, Phys. Rev. D 65, 092007 (2002); Phys. Rev. D 70, 078302 (2004)
  [6]G Mangano et al, Nucl. Phys. B 729, 221 (2005)CrossRef ADS
  [7]J F Beacom, N F Bell and S Dodelson, Phys. Rev. Lett. 93, 121302 (2004)CrossRef ADS
  [8]S Dodelson, A Melchiorri and A Slasar, Phys. Rev. Lett. 97, 04031 (2006)
  [9]S Hannestad, J. Cosmol. Astropart. Phys. 05, 004 (2003)CrossRef ADS
  [10]E Pierpaoli, Mon. Not. R. Astron. Soc. 342, L63 (2003)CrossRef ADS
  [11]S Hannestad, J. Cosmol. Astropart. Phys. 0502, 011 (2005) arXiv:astro-ph/​0411475 CrossRef ADS
  [12]A Slosar, Phys. Rev. D 73, 123501 (2006)CrossRef ADS
  [13]M Fukugita, K Ichikawa, M Kawasaki and O Lahav, Phys. Rev. D 74, 027302 (2006)CrossRef ADS
  [14]O Elgaroy et al, Phys. Rev. Lett. 89, 061310 (2002) O Elgaroy and O Lahav, J. Cosmol. Astropart. Phys. 0304, 004 (2003)
  [15]A G Sanchez et al, Mon. Not. R. Astron. Soc. 366, 189 (2006)CrossRef ADS
  [16]S Hannestad, J. Cosmol. Astropart. Phys. 0305, 004 (2003)CrossRef ADS
  [17]V Barger, D Marfatia and A Tregre, Phys. Lett. B 595, 55 (2004)CrossRef ADS
  [18]WMAP Collaboration: D N Spergel et al, astro-ph/​ 0603449
  [19]A Goodbar, S Hannestad, E Mortsell and H Tu, J. Cosmol. Astropart. Phys. 06, 019 (2006)CrossRef ADS
  [20]U Seljak, A Slosar and P McDonald, J. Cosmol Astropart. Phys. 10, 014 (2006)CrossRef ADS
  [21]W Hu, D J Eisenstein and M Tegmark, Phys. Rev. Lett. 80, 5255 (1998) arXiv:astro-ph/​9712057 CrossRef ADS
  [22]J R Bond, G Efstathiou and J Silk, Phys. Rev. Lett. 45, 1980 (1980)CrossRef ADS
  [23]K Ichikawa, M Fukugita and M Kawasaki, Phys. Rev. D 71, 043001 (2005)CrossRef ADS
  [24]K Ichiki and Y-Y Keum, J. Cosmol. Astropart. Phys. 0806, 005 (2008)CrossRef ADS
  [25]Y-Y Keum, Mod. Phys. Lett. A22, 2131 (2007)CrossRef ADS
  [26]K Ichiki and Y-Y Keum, J. High Energy Phys. 0806, 058 (2008)CrossRef ADS
  [27]D B Kaplan, A E Nelson and N Weiner, Phys. Rev. Lett. 93, 091801 (2004) R D Peccei, Phys. Rev. D 71, 023527 (2005)
  [28]R Fardon, A E Nelson and N Weiner, J. Cosmol. Astropart. Phys. 0410, 005 (2004) arXiv:astro-ph/​0309800 CrossRef ADS
  [29]X J Bi, P h Gu, X l Wang and X M Zhang, Phys. Rev. D 69, 113007 (2004) arXiv:hep-ph/​0311022 CrossRef ADS
  [30]A W Brookfield, C van de Bruck, D F Mota, and D Tocchini-Valentini, Phys. Rev. Lett. 96, 061301 (2006); Phys. Rev. D 73, 083515 (2006)
  [31]G B Zhao, J Q Xia and X M Zhang, arXiv:astro-ph/​ 0611227
  [32]C P Ma and E Bertschinger, Astrophys. J. 455, 7 (1995)CrossRef ADS
  [33]WMAP Collaboration: G Hinshaw et al, arXiv: astro-ph/​0603451
  [34]WMAP Collaboration: L Page et al, arXiv:astro-ph/​ 0603450
  [35]The 2dFGRS Collaboration: S Cole et al, Mon. Not. R. Astron. Soc. 362, 505 (2005) arXiv:astro-ph/​0501174
  [36]P McDonald, J Miralda-Escude, M Rauch, W L W Sargent, T A Barlow, R Cen and J P Ostriker, Astrophys. J. 543, 1 (2000) arXiv:astro-ph/​9911196 CrossRef ADS
  [37]R A C Croft et al, Astrophys. J. 581, 20 (2002) arXiv:astro-ph/​0012324 CrossRef ADS
  [38]A Goobar, S Hannestad, E Mortsell and H Tu, J. Cosmol. Astropart. Phys. 0606, 019 (2006) arXiv:astro-ph/​0602155 CrossRef ADS
  [39]P McDonald, U Seljak, R Cen, P Bode and J P Ostriker, Mon. Not. R. Astron. Soc. 360, 1471 (2005), arXiv:astro-ph/​0407378 CrossRef ADS
  [40]A Lewis and S Bridle, Phys. Rev. D 66, 103511 (2002)CrossRef ADS
  [41]A W Brookfield, C van de Bruck, D F Mota and D Tocchini-Valentini, Phys. Rev. D 76, 049901 (2007)CrossRef ADS
  [42]N Afshordi, M Zaldarriaga and K Kohri, Phys. Rev. D 72, 065024 (2005)CrossRef ADS
  [43]R Bean, E E Flanagan and M Trodden, arXiv:0709.​ 1128 [astro-ph]
  [44]M Kaplinghat and A Rajaraman, Phys. Rev. D 75, 103504 (2007)CrossRef ADS
  [45]O E Bjaelde, A W Brookfield, C van de Bruck, S Hannestad, D F Mota, L Schrempp and D Tocchini-Valentini, arXiv:0705.​2018 [astro-ph]
  [46]R Takahashi and M Tanimoto, J. High Energy Phys. 0605, 021 (2006)CrossRef ADS
  [47]Y S Song and L Knox, Phys. Rev. D 70, 063510 (2004)CrossRef ADS
  [48]S Hannestad, H Tu and Y Y Y Wong, J. Cosmol. Astropart. Phys. 0606, 025 (2006)CrossRef ADS
  [49]J Lesgourgues and S Pastor, Phys. Rep. 429, 307 (2006)CrossRef ADS
  
• 作者单位：YONG-YEON KEUM (1)
  
  1. Institute of Basic Science, Seoul National University, 1 Kwan-Ak-Ro, Kwan-Ak-Gu, Seoul, Republic of Korea
  
• 刊物类别：Physics and Astronomy
• 刊物主题：Physics
  Physics
  Astronomy
  Astrophysics
  
• 出版者：Springer India
• ISSN：0973-7111

文摘

We investigate the way the total mass sum of neutrinos can be constrained from the neutrinoless double beta-decay and cosmological probes with cosmic microwave background (CMBR), large-scale structures including 2dFGRS and SDSS datasets. First we discuss, in brief, the current status of neutrino mass bounds from neutrino beta decays and cosmic constraint within the flat ΛCMD model. In addition, we explore the interacting neutrino dark-energy model, where the evolution of neutrino masses is determined by quintessence scalar field, which is responsible for cosmic acceleration. Assuming the flatness of the Universe, the constraint we can derive from the current observation is \(\sum m_{\nu } < 0.87\) eV at 95% confidence level, which is consistent with \(\sum m_{\nu } < 0.68\) eV in the flat ΛCDM model without Lyman alpha forest data. In the presence of Lyman- α forest data, interacting dark-energy models prefer a weaker bound \(\sum m_{\nu } < 0.43\) eV to \(\sum m_{\nu } < 0.17\) eV (Seljark et al). Finally, we discuss the future prospect of the neutrino mass bound with weak-lensing effects. Keywords Neutrino masses neutrinoless double beta decay large-scale structures interacting neutrino dark-energy model