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tokens: and mid-IR emission by Li Draine ( 2001b ). Figure 8. Schematic of allowable parameters for silicate nanoparticles for which the rotational emission and polarization do not violate observational constraints (white area). The orange shaded region represents the parameter space where the polarization violates the observed AME polarization, and the blue shaded area depicts the space where rotational emission violates the AME and the polarization by nanosilicate violates the UV polarization of starlight for the ISM. 6.4. Comparison with Previous Spinning Dust Studies Previous spinning dust models ( DL98 ; Ali-Haïmoud et al. 2009 ; Silsbee et al. 2011 ; HDL10 ; HLD11 ) dealt with spinning PAHs, because they are a well-established dust population in the ISM (see Tielens 2008 ). The last spinning dust model ( HDL10 ; HLD11 ) treats all known important physical effects, including grain wobbling due to thermal fluctuations within the grain, transient spin-up by single-ion collisions. In particular, the model can be applied to spinning dust grains of arbitrary shape and arbitrary temperature ( HLD11 ). Since the physics of spinning silicate (iron) is essentially analogous to that of spinning PAHs, it is natural to use our advanced spinning dust model for modeling emission from spinning non-PAHs. Finally, the spinning dust model developed in HDL 10 and HLD11 is the unique model that can predict self-consistently the polarization level of spinning dust emission (see also Hoang et al. 2013 , 2014 ); the spinning models from other groups only provide rotational emissivity. Therefore, our spinning dust model can be used to constrain the dipole moment and magnetic properties of nanoparticles using the AME polarization data. 7. SUMMARY In this paper, we have obtained the principal results as follows: 1. We have quantified rotational emission from spinning ultra-small silicate grains for different grain size distribution parameters, various fractions of total Si abundance contained in ultra-small grains , and a wide range of the dipole moment per atom β . 2. The polarization fraction of spinning silicate emission is found to increase with decreasing value of β . The polarization fraction is below for the dipole moments , but it can reach for assuming K. 3. We have identified that the presence of silicate nanoparticles with and the dipole moment does not violate the UV polarization of starlight and the observed polarization of the AME. With this realization (), rotational emission from spinning nanosilicate can adequately reproduce the observed AME from the ISM. 4. Our quantitative results suggest that rotational emission from spinning silicate nanoparticles may be an important source of AME. Future observations searching for signatures of nanosilicates from the regions with prominent AME would be valuable in understanding the carrier of AME. There are several outstanding questions on the problem of spinning nanosilicates, including the dipole moment and