Can baryonic halos form early in cosmic history?

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Observational evidence points to the formation of super-massive black holes and galactic halos much earlier in cosmic history than expected (1). However, if photon scattering cross sections were less, it becomes possible for baryonic halos to form at earlier times, and relax tensions that exist with Lambda Cold Dark Matter (LCDM) theory. Furthermore, recent quantum calculations (2-5) have shown that photon-baryon interaction cross sections in deep gravity wells can indeed be significantly less than those theoretically calculated for traditional localized particles. If reduced baryon-photon interaction cross sections are combined with Carr’s prediction (6) of the formation of black holes by direct collapse of over-density regions during phase transitions in the primordial universe, it becomes possible to formulate a scenario in which baryonic halos form very early in cosmic history. Carr’s primordial black hole mass spectrum formulation, calculated for the last phase transition (t = 1 s), leads to an order-of-magnitude, supermassive primordial black hole (SMPBH) number density consistent with that of present day galaxy number densities, suggesting these as the origin of galactic centre black holes. Such early formed SMPBHs, combined with reduced baryon-photon oscillation, provide wells of sufficient depth to enable baryonic halos (and ultimately their descendent galaxies) to form much earlier in cosmic history, yet potentially maintain consistency with cosmic microwave background observations and primordial nucleosynthesis. In addition, this scenario enables an understanding of the black hole-bulge/black hole-dark halo relations, provides a unified model relating globular clusters, dwarf spheroidal galaxies and bulges, and enables prediction of the dark to visible matter ratio based on the physical parameters of a halo. The physics of reduced cross sections in deep gravity wells and the scenario of early halo formation will be presented and discussed. (1) Xue- Bing Wu et al, (2015). Nature, 518,512-515 doi: 10.1038/nature14241 (2) Ernest, A. D., 2006, in Proceedings of the EPS-13 Conference, Eds: A.M. Cruise, L. Ouwehand. ESA-SP 637 (3) Ernest A. D., 2009, J. Phys. A: Math. Theor. 42 115207, 115208 (4) Ernest A. D, 2012, in Advances in Quantum Theory, Ion I. Cotaescu, Ed. ISBN: 978-953-51-0087-4, InTech, Rijeka., 221-248 (5) Ernest A. D., and Collins, M.P., 2015, Proceedings of the International Astronomical Union, 11, pp 298-299. doi:10.1017/S1743921315006894 (6) Carr B. J., 1975. ApJ., 201, pp. 1-19. doi: 10.1086/153853
Original languageEnglish
Number of pages1
Publication statusPublished - 2017
EventOn the Origin (and Evolution) of Baryonic Galaxy Halos - Centro de Informacion de Energia Renovable (CIER), Puerto Ayora, Santa Cruz, Galapagos Islands, Ecuador
Duration: 13 Mar 201717 Mar 2017 (Conference website)


ConferenceOn the Origin (and Evolution) of Baryonic Galaxy Halos
CityPuerto Ayora, Santa Cruz, Galapagos Islands
OtherThis meeting will focus on the baryonic content of galaxy halos -- their properties, origin and evolution with cosmic time. The halos of our own Milky Way galaxy and close neighbour M31 have been studied in some detail. Deep, wide and detailed observations of galaxy halos beyond the Local Group are becoming more ubiquitous. Simulations, that incorporate realistic baryonic physics in a cosmological context have also made significant progress in recent years in modelling galaxy halos. These simulations predict outer halo regions that differ strongly in their formation processes and properties from the well-studied inner regions of galaxies. Halos have long dynamical times and as such preserve the unique signatures of galaxy assembly. This meeting bring together observers and simulators of the baryonic halos of galaxies, focusing on extragalactic halos.
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