[1] A. G. Riess, et al., “Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant”, Astron. J. 116, 1009 (1998).
[2] S. Perlmutter, et al., “Measurements of Ω and Λ from 42 High-Redshift Supernovae”, Astron. J. 517, 565 (1999).
[3] P. Bernardis et al., “A Flat Universe from High-Resolution Maps of the Cosmic Microwave Background Radiation”, Nature 404, 955 (2000).
[4] R. A. Knop et al., “New Constraints on ΩM , ΩΛ, and w from an Independent Set of 11 High-Redshift Supernovae Observed with the Hubble Space Telescope”, Astrophys. J. 598, 102 (2003).
[5] M. Colless, et al., “The 2dF Galaxy Redshift Survey: spectra and redshifts”, Mon. Not. R. Astron. Soc. 328, 1039 (2001).
[6] M. Tegmark et al., “Cosmological parameters from SDSS and WMAP”, Phys. Rev. D 69, 103501 (2004).
[7] S. Cole et al., “The 2dF Galaxy Redshift survey : power-spectrum analysis of the final data set and cosmological implications”, Mon. Not. R. Astron. Soc. 362, 505534 (2005).
[8] V. Springel, C. S. Frenk and S. M. D. White, “The large-scale structure of the Universe”, Nature 440, 1137 (2006).
[9] S. Hanany et al., “MAXIMA-1: A Measurement of the Cosmic Microwave Background Anisotropy on angular scales of 10 arcminutes to 5 degrees”, Astrophys. J., 545, L5L9 (2000).
[10] C. B. Netterfield et al., “A measurement by BOOMERANG of multiple peaks in the angular power spectrum of the cosmic microwave background”, Astrophys. J. 571, 604614 (2002).
[11] D. N. Spergel et al., “FIRST-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP)”, Astrophys. J. Suppl. 148, 175 (2003).
[12] U. Alam, V. Sahni and A. A. Starobinsky, “The case for dynamical dark energy revisited”, J. Cosmol. Astropart. Phys. 0406, 008 (2004).
[13] A. Sen, “Tachyon Matter”, J. High Energy Phys. 065, 0207 (2002).
[14] M. Malekjani, T. Naderi, and F. Pace, “Effects of ghost dark energy perturbations on the evolution of spherical overdensities”, Mon. Not. R. Astron. Soc. 453, 41484158 (2015).
[15] T. Chiba, T. Okabe, and M.Yamaguchi, “Kinetically driven quintessence”, Phys. Rev. D 62, 023511 (2000).
[16] R. Myrzakulov, “Fermionic K-essence”, arXiv:1011.4337.
[17] S. Maity and U.Debnath, “Correspondence between fermionic field and other dark energies”, Astrophys. Space Sci. 345, 399-403 (2013).
[18] S. Maity and U. Debnath, “Correspondence of F-essence with Chaplygin gas cosmology”, Eur. Phys. J. Plus 129, 14 (2014).
[19] S. Nojiri and S. D.Odintsov, “Quantum de Sitter cosmology and phantom matter”, Phys. Lett. B 562, 147152 (2003).
[20] A. Yu. Kamenshchik, U. Moschella, V. Pasquier, “An alternative to quintessence”, Phys. Lett. B 511, 265268 (2001).
[21] S. Weinberg, “The Cosmological Constant Problem”, Rev. Mod. Phys. 61, 120 (1998).
[22] E. J. Copeland, M. Sami and S. Tsujikawa, “Dynamics of dark energy”, Int. J. Mod. Phys. D 15, 17531935 (2006).
[23] T. Padmanabhan, “Cosmological constantthe weight ofthe vacuum”, Phys. Rep. 380, 235320 (2003).