Measuring the velocity bulk flow in presence of chameleon fields | ||
| Iranian Journal of Astronomy and Astrophysics | ||
| مقاله 5، دوره 4، شماره 2، دی 2017، صفحه 121-137 اصل مقاله (6.96 M) | ||
| شناسه دیجیتال (DOI): 10.22128/ijaa.2017.112 | ||
| نویسندگان | ||
| Amin Salehi؛ Muhammad yarahmadi؛ Shahriar Fathi | ||
| Department of Physics, Lorestan University of Lorestan, Lorestan, Iran | ||
| چکیده | ||
| cluster are responsible for the peculiar motion; however the exact source of the peculiar motion is still uncertain and it seems that this motion and other types of anisotropies in large scales have a common source. The chameleon fields can be a good candid to explain both types of anisotropy, namely the bulk flow in small scales and other types of anisotropies in large scales. In this paper, we study the bulk in the presence of chameleon fields flow in different scales. While in the past , this has been studied mostly using galaxies as distance indicators, the weight of type Ia supernovae (SNe Ia) has increased recently. We use Union2 catalogue containing 557 type Ia supernovae (SNe Ia) in redshift range, ٠٫ ١۵ < z < ١٫ ۴. The results indicate that for distances smaller than 150 Mpc, the bulk flow is moving in the (l, b) = (٢٨۶, ١۶) direction with amplitude of ٢٧٣kms−١. This result is consistence with the direction of CMB dipole in (١- σ) confidence level. In large scales (٣٠٠h−١Mpc), the convergence between direction of the bulk flow and CMB dipole decreases while the bulk flow tends to the direction of dark energy dipole; thus it seems that chameleon field can be a common source for bulk flow and dark energy dipole. Moreover, we have estimated the chameleon parameter using peculiar velocity of Type Ia supernovae. | ||
| کلیدواژهها | ||
| Camelon: bulk flow؛ supernova؛ distance modulus | ||
| مراجع | ||
|
[1] Conklin, E.K. 1969, Nature, 222, 971
[2] Henry, P.S. 1971, Nature, 231, 516
[3] Smoot, G.F., Gorenstein, M.V., & Muller, R. A. 1977, Phys. Rev. Lett., 39,898
[4] Villumsen, J., & Strauss, M. 1987, ApJ, 322, 37
[5] Shaya,E.1984,ApJ280,470
[6] Tammann,G.andSandage,A.1985,ApJ294,81
[7] Aaronson, M., Bothun, G., Mould, J., Huchra, J., Schommer, R., & Cornell, M. 1986, ApJ, 302, 536
[8] Dressier, A., Faber, S., Burstein, D., Davies, R., Lynden-Bell, D., Terlevich, R., & Wegner, G. 1987, ApJ, 313, L37
[9] Lynden Bell, D., Faber, S.M., Burstein,D., Davies,R.L., Dressler, A., Terlevich, R.J.andWegner, G.1988, ApJ326, 19
[10] Bothun, G. D., Harris, H. C., & Hesser, J. E. 1992, PASP, 104, 1220
[11] A. Kogut et al., 1993, ApJ, 419, 1
[12] HoffmanY., Eldar A., Zaroubi S., Dekel A., 2001, preprint (astro-ph/ 0102190)
[13] Kocevski, D. D. & Ebeling, H. 2006, ApJ, 645, 1043
[14] A. Kashlinsky; F. Atrio-Barandela, D. Kocevski, and H. Ebeling, Astrophys. J. 686, L49 (2008).
[15] Kashlinsky, A., Atrio-Barandela,F., Ko cevski, D., & Eb eling, H. 2009, ApJ, 691, 1479
[16] A. Kashlinsky;F. Atrio-Barandela, H. Ebeling, A. Edge, and D. Kocevski, Astrophys. J. 712, L81 (2010).
[17] Atrio-Barandela,F.; Kashlinsky, A.; Ebeling, H.; Fixsen, D. J.; Kocevski, D. (2015. Astrophys. J. 810 (2):143.
[18] Colin, J., Mohayaee, R., Sarkar, S., Shafieloo, A. 2011, MNRAS, 414, 264
[19] Dai, D.-C., Kinney, W. H., & Sto jkovic, D. 2011, J. Cosmol. Astropart. Phys., JCAP04(2011)015
[20] Turnbull, S. J., Hudson, M. J., Feldman, H. A., et al. 2012, MNRAS, 420, 447
[21] U. Feindt et.al 2013,arXiv:1310.4184v3
[22] Hudson, M. J., Smith, R. J., Lucey, J. R., & Branchini, E. 2004, MNRAS, 352,61
[23] Watkins, R., Feldman, H. A., & Hudson, M. J. 2009, MNRAS, 392, 743
[24] Lavaux, G., Tully, R. B., Mohayaee, R., & Colombi, S. 2010, ApJ, 709, 483
[25] Nusser, A. & Davis, M. 2011, ApJ, 736, 93
[26] Branchini, E., Davis, M., & Nusser, A. 2012, MNRAS, 424, 472
[27] Ma, Y.-Z. & Scott, D. 2013, MNRAS, 428, 2017
[28] Planck Collaboration. 2013, ArXiv e-prints, arxiv:1303.5090
[29] Camille Bonvin, Ruth Durrer, and Martin Kunz Phys. Rev. Lett. 96, 191302 – Published 17 May 2006
[30] Lam Hui and Patrick B. Greene, Phys.Rev.D73:123526,2006
[31] J. Khoury and A. Weltman, astro-ph/0309300 and astro-ph/0309411
[32]P. G. Ferreira and M. Joyce, Phys. Rev. Lett. 79, 4740 (1997); Phys. Rev D 58, 023503 (1998).
[33] C. Wetterich, Nucl. Phys. B302, 668 (1988).
[34] H.Farajollahi, A. Salehi, Physical Review D 85, 083514 (2012)
[35] Amanullah R. et al., 2010, ApJ, 716, 712.
[36] Feldman H. A., Watkins R., Hudson M. J., 2010, MNRAS, 407,2328
[37] De-Chang Dai1, William H. Kinney2 and Dejan Stojkovic,arXiv: 1102.0800v2
[38] Antoniou I., Perivolaropoulos L., 2010, JCAP, 12, 12
[39] R.-G. Cai, Y.-Z. Ma, B. Tang and Z.-L. Tuo, Phys. Rev. D 87, 123522 (2013).
[40] Mariano A., Perivolaropoulos L., 2012, Phys. Rev. D, 86, 083517
[41] C. Armendariz-Picon, JCAP 0407, 007 (2004).
[42] W. Zhao andY. Zhang, Class. Quant. Grav. 23, 3405 (2006).
[43] W. Zhao andY. Zhang, Phys. Lett. B 640, 69 (2006).
[44]Y. Zhang, T. Y. Xia, W. Zhao, Class. Quant. Grav. 24, 3309 (2007).
[45] A. Salehi and S. Aftabi, JHEP, 09(2016)140
[46] A. Salehi and S. Aftabi, Int. J. Mod. Phys. D 25, 1650042 (2016)
[47] T. S. Koivisto and D.F. Mota, JCAP 0808, 021 (2008).
[48] Yang X.F., WangF. Y., Chu Z., 2014, MNRAS, 437, 1840 | ||
|
آمار تعداد مشاهده مقاله: 740 تعداد دریافت فایل اصل مقاله: 485 |
||