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Additional file 1: Table S1. Histopathological score criteria for heart, liver, spleen, lung, and kidneys.

Additional file 4: Table S4. Tumour volume, weight, and tumour inhibition rate (M ± SD).

Additional file 3: Table S3. Anti-TPD52 antiserum titre detection (OD450).

Additional file 2: Table S2. Information on seven antigenic genes obtained by screening.

A modified de Broglie?Bohm approach is generalized to the Schwarzschild black hole. By using this method, the quantum potential and the quantum trajectories of the black hole are investigated. And we find that the linear combination of two particular solutions of the black hole wavefunction is not physical although each of them is physical, if we think that the quantum gravity should reduce into its corresponding classical counterpart in which the gravity vanishes. It seems to confirm the argument, given by Alwis and MacIntire, that a possible resolution on the quantum gravity is to give up the superposition principle.

In this paper the entropy of a toroidal black hole due to a scalar field is investigated by using the DLM scheme. The entropy is renormalized to the standard Bekenstein-Hawking formula with a one-loop correction arising from the higher curvature terms of the gravitational action. For the scalar field, the renormalized Newton constant and two renormalized coupling constants in the toroidal black hole are the same as those in the Reissner-Nordstrom black hole except for other one.

From the partition function of canonical ensemble we derive the entropy of the de Sitter space by anti-Wick rotation. And then from the one-loop bubble $S^2\times S^2$ created from vacuum fluctuation in de Sitter background space, we obtain the one-loop quantum correction to the entropy of de Sitter space., 10 pages, 0 figures

The entropies of quantum fields on event horizon of a toroidal black hole are given using the improved brick-wall model. According to the view of the improved brick-wall model, these entropies are nothing but the entropy of the black hole. So the entropy of the toroidal black hole is proportional to the area of event horizon, which satisfies the Bekenstein-Hawking formula.