Cosmic dichotomy in the hosts of rapidly star-forming systems at low and
  high redshifts
  This paper presents a compilation of clustering results taken from the
literature for galaxies with highly enhanced (SFR [30-10^3] Msun/yr) star
formation activity observed in the redshift range z=[0-3]. We show that,
irrespective of the selection technique and only very mildly depending on the
star forming rate, the clustering lengths of these objects present a sharp
increase of about a factor 3 between z~1 and z~2, going from values of ~5 Mpc
to about 15 Mpc and higher. This behaviour is reflected in the trend of the
masses of the dark matter hosts of star-forming galaxies which increase from
~10^11.5 Msun to ~10^13.5 Msun between z~1 and z~2. Our analysis shows that
galaxies which actively form stars at high redshifts are not the same
population of sources we observe in the more local universe. In fact, vigorous
star formation in the early universe is hosted by very massive structures,
while for z~1 a comparable activity is encountered in much smaller systems,
consistent with the down-sizing scenario. The available clustering data can
hardly be reconciled with merging as the main trigger for intense star
formation activity at high redshifts.
  We further argue that, after a characteristic time-scale of ~1 Gyr, massive
star-forming galaxies at z>~2 evolve into z<~1.5 passive galaxies with large
(Mstellar=[10^11 - 10^12] Msun) stellar masses.
