Linear Regime of Structure Formation with Scalar Field Dark Matter - - PowerPoint PPT Presentation
Linear Regime of Structure Formation with Scalar Field Dark Matter considering an Axion-like potential arXiv:1703.10180. Accepted for publication as a Rapid Communication in Physical Review D FRANCISCO XAVIER LINARES CEDEO ALMA XOCHITL
FRANCISCO XAVIER LINARES CEDEÑO ALMA XOCHITL GONZÁLEZ MORALES LUIS ARTURO UREÑA LÓPEZ
29th Indian-Summer School of Physics: Topics in Particle Cosmology September 2017, Prague - Czech Republic
DIVISIÓN DE CIENCIAS E INGENIERÍAS CAMPUS LEÓN - UNIVERSIDAD DE GUANAJUATO
arXiv:1703.10180. Accepted for publication as a Rapid Communication in Physical Review D
Thus, there is about ~25% of matter that we do not “observe”…
Planck collaboration, arXiv:1507.02702, (2016) .
SDSS collaboration, arXiv:0310723, (2004).
Hsi-Yu Schive, Tzihong Chiueh, Tom Broadhurst, arXiv:1406.6586, (2014)
* Free case * Non-relativitic
Strong CP problem in QCD:
Klein-Gordon equation (background)
Klein-Gordon equation (linear perturbations)
Klein-Gordon equation (background)
Klein-Gordon equation (linear perturbations)
Tachyonic Instability
Klein-Gordon equation (background)
Klein-Gordon equation (linear perturbations)
Tachyonic Instability
BOSS DR11 Lyman-alpha
PRELIMINARY RESULT!!! (by Alma González)
Axion-like particle is a compelling candidate to replace CDM: at large scales it behave just as CDM, and at smaller scales it solve the existing discrepancies between astrophysical observations and simulations based
The results were obtained based on: 1) transform the Klein-Gordon equation into a dynamical system, and 2) use an amended version of CLASS code to evolve the linear perturbations. We fully computed the MPS for the axion potential and showed that its features do change significantly in the case when an Axion-like potential is considered, for which linear perturbations in a certain range of wavenumbers suffer a tachyonic instability. This causes the appearance of a bump in the MPS which is close to the cut-off scale, which in turn is also displaced towards smaller scales in comparison to the free case. It will be interesting to know whether future surveys as DESI and LSST, in case a bump and a cut-off in the MPS, or the 1D-MPS are detected, will be able to spot the differences between the free case and the full axion one and in turn put constraints on the decay parameter. Some statistical analysis will be made to constraint the parameters of our model (MCMC, Bayesian Inference).