Built on

P. J. E. Peebles, Astrophys. J. 146
1966
Earlier work this paper cites.
B. W. Lee and S. Weinberg, Phys. Rev. Lett. 39
1977
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P. Gondolo and G. Gelmini, Nucl. Phys. B360
1991
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A. Gelman and D. B. Rubin, Statist. Sci. 7
1992
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C.-P. Ma and E. Bertschinger, Astrophys. J. 455
1995
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T. Nakamura, M. Sasaki, T. Tanaka, and K. S. Thorne, Astrophys. J. 487
1997
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W. J. G. de Blok and S. S. McGaugh, Mon. Not. Roy. Astron. Soc. 290
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B. Moore, S. Ghigna, F. Governato, G. Lake, T. R. Quinn, J. Stadel, and P. Tozzi, Astrophys. J. 524
1999
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A. A. Klypin, A. V. Kravtsov, O. Valenzuela, and F. Prada, Astrophys. J. 522
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A. Lewis, A. Challinor, and A. Lasenby, Astrophys. J. 538
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A. R. Zentner and T. P. Walker, Phys. Rev. D65
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A. Lewis and S. Bridle, Phys. Rev. D66
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K. Ichiki, M. Oguri, and K. Takahashi, Phys. Rev. Lett. 93
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R. M. Neal, (2005), math/0502099 [math.ST]
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J. Lesgourgues and S. Pastor, Phys. Rept. 429
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J. B. Dent, S. Dutta, and R. J. Scherrer, Phys. Lett. B687
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J. Zavala, M. Vogelsberger, and S. D. M. White, Phys. Rev. D81
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J. L. Feng, M. Kaplinghat, and H.-B. Yu, Phys. Rev. D82
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F. Beutler, C. Blake, M. Colless, D. H. Jones, L. Staveley-Smith, L. Campbell, Q. Parker, W. Saunders, and F. Watson, Mon. Not. Roy. Astron. Soc. 416
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A. Loeb and N. Weiner, Phys. Rev. Lett. 106
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S.-H. Oh, W. J. G. de Blok, E. Brinks, F. Walter, and R. C. Kennicutt, Jr, Astron. J. 141
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M. G. Walker and J. Penarrubia, Astrophys. J. 742
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M. Boylan-Kolchin, J. S. Bullock, and M. Kaplinghat, Mon. Not. Roy. Astron. Soc. 415
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M. Cirelli, E. Moulin, P. Panci, P. D. Serpico, and A. Viana, Phys. Rev. D86
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2018

Converting non-relativistic dark matter to radiation

Bringmann, Torsten, Kahlhoefer, Felix, Schmidt-Hoberg, Kai et al.

Understand

Dark matter in the cosmological concordance model is parameterised by a single number, describing the covariantly conserved energy density of a non-relativistic fluid.

Here we test this assumption in a model-independent and conservative way by considering the possibility that, at any point during the cosmological evolution, dark matter may be converted into a non-interacting form of radiation.
This scenario encompasses, but is more general than, the cases where dark matter decays or annihilates into these states.
We show that observations of the cosmic microwave background allow to strongly constrain this scenario for any conversion time after big bang nucleosynthesis.

Built on

P. J. E. Peebles, Astrophys. J. 146
1966
Earlier work this paper cites.
B. W. Lee and S. Weinberg, Phys. Rev. Lett. 39
1977
Earlier work this paper cites.
P. Gondolo and G. Gelmini, Nucl. Phys. B360
1991
Earlier work this paper cites.
A. Gelman and D. B. Rubin, Statist. Sci. 7
1992
Earlier work this paper cites.
C.-P. Ma and E. Bertschinger, Astrophys. J. 455
1995
Earlier work this paper cites.
T. Nakamura, M. Sasaki, T. Tanaka, and K. S. Thorne, Astrophys. J. 487
1997
Earlier work this paper cites.
W. J. G. de Blok and S. S. McGaugh, Mon. Not. Roy. Astron. Soc. 290
1997
Earlier work this paper cites.
B. Moore, S. Ghigna, F. Governato, G. Lake, T. R. Quinn, J. Stadel, and P. Tozzi, Astrophys. J. 524
1999
Earlier work this paper cites.
A. A. Klypin, A. V. Kravtsov, O. Valenzuela, and F. Prada, Astrophys. J. 522
1999
Earlier work this paper cites.
A. Lewis, A. Challinor, and A. Lasenby, Astrophys. J. 538
2000
Earlier work this paper cites.
A. R. Zentner and T. P. Walker, Phys. Rev. D65
2002
Earlier work this paper cites.
A. Lewis and S. Bridle, Phys. Rev. D66
2002
Earlier work this paper cites.
K. Ichiki, M. Oguri, and K. Takahashi, Phys. Rev. Lett. 93
2004
Earlier work this paper cites.
S. Weinberg, Phys. Rev. D69
2004
Earlier work this paper cites.
R. M. Neal, (2005), math/0502099 [math.ST]
2005
Earlier work this paper cites.
J. Lesgourgues and S. Pastor, Phys. Rept. 429
2006
Earlier work this paper cites.
M. Lattanzi and J. W. F. Valle, Phys. Rev. Lett. 99
Original
2007
Earlier work this paper cites.
R. Iengo, JHEP 05
Original
2009
Earlier work this paper cites.
A. H. G. Peter, Phys. Rev. D81
Original
2010
Earlier work this paper cites.
M.-Y. Wang and A. R. Zentner, Phys. Rev. D82
Original
2010
Earlier work this paper cites.
J. B. Dent, S. Dutta, and R. J. Scherrer, Phys. Lett. B687
Original
2010
Earlier work this paper cites.
J. Zavala, M. Vogelsberger, and S. D. M. White, Phys. Rev. D81
Original
2010
Earlier work this paper cites.
J. L. Feng, M. Kaplinghat, and H.-B. Yu, Phys. Rev. D82
Original
2010
Earlier work this paper cites.
S. Cassel, J. Phys. G37
Original
2010
Earlier work this paper cites.
F. Beutler, C. Blake, M. Colless, D. H. Jones, L. Staveley-Smith, L. Campbell, Q. Parker, W. Saunders, and F. Watson, Mon. Not. Roy. Astron. Soc. 416
Original
2011
Earlier work this paper cites.
A. Loeb and N. Weiner, Phys. Rev. Lett. 106
Original
2011
Earlier work this paper cites.
S.-H. Oh, W. J. G. de Blok, E. Brinks, F. Walter, and R. C. Kennicutt, Jr, Astron. J. 141
Original
2011
Earlier work this paper cites.
M. G. Walker and J. Penarrubia, Astrophys. J. 742
Original
2011
Earlier work this paper cites.
M. Boylan-Kolchin, J. S. Bullock, and M. Kaplinghat, Mon. Not. Roy. Astron. Soc. 415
Original
2011
Earlier work this paper cites.
M. Cirelli, E. Moulin, P. Panci, P. D. Serpico, and A. Viana, Phys. Rev. D86
Original
2012
Earlier work this paper cites.