Context : Despite their carbon-rich photospheres , silicate carbon stars show evidence of oxygen-rich circumstellar material , which is considered to exist in disks .
Silicate carbon stars represent interesting cases that allow us to study the possible effects of binarity on stellar evolution and the mass loss accompanied by the formation of disks .

Aims : We present a small survey of the 22 GHz H _ { 2 } O masers toward 10 silicate carbon stars with much better sensitivity than the previous observations .

Methods : We observed our sample with the Karl G. Jansky Very Large Array ( VLA ) using the most expanded configuration ( A-configuration ) with a maximum baseline of 36 km .
For some of our program stars with noisy IRAS Low Resolution Spectra ( LRS ) , we present new mid-IR spectra obtained with the Very Large Telescope Interferometer and the Spitzer Space Telescope .

Results : We detected the H _ { 2 } O masers toward 5 out of 10 silicate carbon stars ( EU And , V778 Cyg , IRAS06017+1011 , V1415 Cyg , and NC83=V1945 Cyg ) , with NC83 being new detection .
No H _ { 2 } O masers were detected toward BM Gem , IRAS07221-0431 , IRAS08002-3803 , IRAS18006-3213 , and HD189605 .
The velocity separation between the most blue- and red-shifted maser features is 10–14 km s ^ { -1 } .
If we assume that the masers originate in circum-companion disks , the measured velocity separations translate into a lower limit of the rotational velocity of 5–7 km s ^ { -1 } , and the upper limit of the radius of the maser emitting region is estimated to be 10–68 AU for a companion mass of 0.5–1.7 M _ { \sun } .
The new mid-IR spectra of NC83 , IRAS06017+1011 , and HD189605 confirm the 10 \mu m silicate emission .
The latter two stars show a bump at \sim 11.5 \mu m , which is presumably due to SiC originating in the ongoing mass loss from the carbon-rich primary star , not due to crystalline silicate .
We also report on the detection of the UV flux at 2271 Å toward HD189605 .

Conclusions :