Context : The young systems PZ Tel and HD 1160 , hosting known low-mass companions , were observed during the commissioning of the new planet finder of the Very Large Telescope ( VLT ) SPHERE with several imaging and spectroscopic modes .

Aims : We aim to refine the physical properties and architecture of both systems .

Methods : We use SPHERE commissioning data and dedicated Rapid Eye Mount ( REM ) observations , as well as literature and unpublished data from VLT/SINFONI , VLT/NaCo , Gemini/NICI , and Keck/NIRC2 .

Results : We derive new photometry and confirm the short-term ( P = 0.92 d ) photometric variability of the star PZ Tel A with values of 0.06 and 0.14 mag at optical and near-infrared wavelengths , respectively .
We note from the comparison to literature data spanning 38 yr that the star also exhibits a long-term variability trend with a brightening of \sim 0.25 mag .
The 0.63–3.8 \muup m spectral energy distribution of PZ Tel B ( separation \sim 25 AU ) allows us to revise its physical characteristics : spectral type M7 \pm 1 , T _ { eff } = 2700 \pm 100 K , log ( g ) < 4.5 dex , luminosity log ( L / L _ { \odot } ) = - 2.51 \pm 0.10 dex , and mass 38–72 M _ { J } from “ hot-start ” evolutionary models combining the ranges of the temperature and luminosity estimates .
The 1–3.8 \muup m SED of HD 1160 B ( \sim 85 au ) suggests a massive brown dwarf or a low-mass star with spectral type M6.0 ^ { +1.0 } _ { -0.5 } , T _ { eff } = 3000 \pm 100 K , subsolar metallicity [ M/H ] = - 0.5–0.0 dex , luminosity log ( L / L _ { \odot } ) = - 2.81 \pm 0.10 dex , and mass 39–168 M _ { J } .
The physical properties derived for HD 1160 C ( \sim 560 au ) from K _ { s } L ^ { \prime } -band photometry are consistent with the discovery study .
The orbital study of PZ Tel B confirms its deceleration and the high eccentricity of its orbit ( e > 0.66 ) .
For eccentricities below 0.9 , the inclination , longitude of the ascending node , and time of periastron passage are well constrained .
In particular , both star and companion inclinations are compatible with a system seen edge-on .
Based on “ hot-start ” evolutionary models , we reject other brown dwarf candidates outside 0.25 ^ { \prime \prime } for both systems , and giant planet companions outside 0.5 ^ { \prime \prime } that are more massive than 3 M _ { J } for the PZ Tel system .
We also show that K 1 - K 2 color can be used along with YJH low-resolution spectra to identify young L-type companions , provided high photometric accuracy ( \leq 0.05 mag ) is achieved .

Conclusions : SPHERE opens new horizons in the study of young brown dwarfs and giant exoplanets using direct imaging thanks to high-contrast imaging capabilities at optical ( 0.5–0.9 \muup m ) and near-infrared ( 0.95–2.3 \muup m ) wavelengths , as well as high signal-to-noise spectroscopy in the near-infrared domain ( 0.95–2.3 \muup m ) from low resolutions ( R \sim 30–50 ) to medium resolutions ( R \sim 350 ) .