We present an analysis of the mass distribution in the core of A 383 ( z = 0.188 ) , one of twelve X-ray luminous galaxy clusters at z \sim 0.2 selected for a comprehensive and unbiased study of the mass distribution in massive galaxy clusters .
Deep optical imaging performed by the Hubble Space Telescope ( HST ) reveals a wide variety of gravitationally lensed features in the core of A 383 , including a giant arc formed from the strongly-lensed images of two background galaxies , two radial arcs in the halo of the central cluster galaxy , several multiply-imaged arcs and numerous arclets .
Based upon the constraints from the various lensed features , as well as from color information from ground-based observations , we construct a detailed model of the mass distribution in the central regions of the cluster , taking into account both the cluster-scale potential and perturbations from individual cluster galaxies .
Keck spectroscopy of one component of the giant arc identifies it as an image of a star-forming galaxy at z = 1.01 and provides an accurate measurement of the mass of the cluster within the projected radius of the giant arc ( 65 kpc ) of ( 3.5 \pm 0.1 ) \times 10 ^ { 13 } M _ { \odot } .
Using the weak shear measured from our HST observations we extend our mass model to larger scales and determine a mass of ( 1.8 \pm 0.2 ) \times 10 ^ { 14 } M _ { \odot } within a radius of 250 kpc .
On smaller scales we employ the radial arcs as probes of the shape of the mass distribution in the cluster core ( r \mathrel { \raise 1.505 pt \hbox { $ \scriptstyle < $ } \kern - 6.0 pt \lower 1.72 pt \hbox { { $% \scriptstyle \sim$ } } } 20 kpc ) , find that the mass profile is more peaked than a single Navarro , Frenk & White ( NFW , 1997 ) profile .
Our findings therefore support the proposal that massive cluster cores contain more mass than can be explained by a single cluster-scale NFW profile .
The optical and X-ray properties of A 383 indicate the presence of a central cooling flow , for which we derive a mass deposition rate of \mathrel { \raise 1.505 pt \hbox { $ \scriptstyle > $ } \kern - 6.0 pt \lower 1.72 pt \hbox { { $% \scriptstyle \sim$ } } } 200 M _ { \odot } yr ^ { -1 } .
We also use the X-ray emission from A 383 to obtain independent estimates of the total mass within projected radii of 65 and 250 kpc : ( 4.0 ^ { +1.1 } _ { -1.7 } ) \times 10 ^ { 13 } M _ { \odot } and ( 1.2 \pm 0.5 ) \times 10 ^ { 14 } M _ { \odot } , which are consistent with the lensing measurements .