We investigate the effects of chameleon scalar field to the effective density and pressure of a dark matter (DM) halo. The pressure is generated from the chameleonic fifth force on the matter. We demonstrate that the thick-shell nonsingular boundary condition which forbids singular point, leads to extremely stringent constraint on the matter-chameleon coupling when applied to galaxy. We argue that chameleon profile with central singularity is more likely to develop in general physical situation. The chameleonic fifth force from the chameleon profile with central singularity experienced by DM could significantly modify the rotation curve of galaxies. The chameleonic fifth force could generate steeper cusp to the rotation curves in any DM profiles starting from the NavarroFrenkWhite (NFW) to the pseudo-isothermal (ISO) profile. Upper limits on the coupling constant between the chameleon and DM are estimated from observational data of the late-type low surface brightness galaxies (LSB). It is in the order of β < 10 -3.
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