Context : In this work we present data from observations with the MAGIC telescopes of SN 2014J detected in January 21 2014 , the closest Type Ia supernova since Imaging Air Cherenkov Telescopes started to operate .

Aims : We probe the possibility of very-high-energy ( VHE ; E \geq 100 GeV ) gamma rays produced in the early stages of Type Ia supernova explosions .

Methods : We performed follow-up observations after this supernova explosion for 5 days , between January 27 and February 2 in 2014 .
We search for gamma-ray signal in the energy range between 100 GeV and several TeV from the location of SN 2014J using data from a total of \sim 5.5 hours of observations .
Prospects for observing gamma-rays of hadronic origin from SN 2014J in the near future are also being addressed .

Results : No significant excess was detected from the direction of SN 2014J .
Upper limits at 95 \% confidence level on the integral flux , assuming a power-law spectrum , d F / d E \propto E ^ { - \Gamma } , with a spectral index of \Gamma = 2.6 , for energies higher than 300 GeV and 700 GeV , are established at 1.3 \times 10 ^ { -12 } and 4.1 \times 10 ^ { -13 } photons cm ^ { -2 } s ^ { -1 } , respectively .

Conclusions : For the first time , upper limits on the VHE emission of a Type Ia supernova are established .
The energy fraction isotropically emitted into TeV gamma rays during the first \sim 10 days after the supernova explosion for energies greater than 300 GeV is limited to 10 ^ { -6 } of the total available energy budget ( \sim 10 ^ { 51 } erg ) .
Within the assumed theoretical scenario , the MAGIC upper limits on the VHE emission suggest that SN 2014J will not be detectable in the future by any current or planned generation of Imaging Atmospheric Cherenkov Telescopes .