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Low-ionization transitions such as the MgII 2796/2803 doublet trace cold gasin the vicinity of galaxies. It is not clear whether this gas is part of theinterstellar medium of large proto-disks, part of dwarfs, or part of entrainedmaterial in supernovae-driven outflows. Studies based on MgII statistics, e.g.stacked images and clustering analysis, have invoked starburst-driven outflowswhere MgII absorbers are tracing the denser and colder gas of the outflow. Aconsequence of the outflow scenario is that the strongest absorbers ought to beassociated with starbursts. We use the near-IR integral field spectrographSINFONI to test whether starbursts are found around z~1 MgII absorbers. For 67%(14 out of 21) of the absorbers with rest-frame equivalent width larger than 2AA, we do detect Ha in emission within 200 km/s of the predicted wavelengthbased on the \MgII redshift.  The star-formation rate (SFR) inferred from Halpha ranges from 1 to 20Msun/yr, i.e. showing a level of star-formation larger than in M82 by a factorof >4 on average. Our flux limit (3-sigma) corresponds to a SFR of 0.5 Msun/yr.We find evidence (at >95% confidence) for a correlation between SFR andequivalent width, indicating a physical connection between starburst phenomenaand gas seen in absorption. In the cases where we can extract the velocityfield, the host-galaxies reside in halos with mean mass <log M_h>=11.2 in goodagreement with clustering measurements.

The SINFONI MgII Program for Line Emitters (SIMPLE): Discovering starbursts near QSO sight-lines