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We present Star Formation Histories (SFHs) for a sample of 104 massive(stellar mass M > 10$^{10}$ M$_{\odot}$) quiescent galaxies (MQGs) at$z$=1.0-1.5 from the analysis of spectro-photometric data from the SHARDS andHST/WFC3 G102 and G141 surveys of the GOODS-N field, jointly with broad-bandobservations from ultraviolet (UV) to far-infrared (Far-IR). The sample isconstructed on the basis of rest-frame UVJ colours and specific star formationrates (sSFR=SFR/Mass). The Spectral Energy Distributions (SEDs) of each galaxyare compared to models assuming a delayed exponentially declining SFH. A MonteCarlo algorithm characterizes the degeneracies, which we are able to breaktaking advantage of the SHARDS data resolution, by measuring indices such asMgUV and D4000. The population of MQGs shows a duality in their properties. Thesample is dominated (85%) by galaxies with young mass-weighted ages, tM $<$ 2Gyr, short star formation timescales, $\langle \tau \rangle$ $\sim$ 60-200 Myr,and masses log(M/M$_{\odot}$) $\sim$ 10.5. There is an older population (15%)with tM$=$2 - 4 Gyr, longer star formation timescales, $\langle \tau\rangle$$\sim$ 400 Myr, and larger masses, log(M/M$_{\odot}$) $\sim$ 10.7. TheSFHs of our MQGs are consistent with the slope and the location of the MainSequence (MS) of star-forming galaxies at $z$ $>$ 1.0, when our galaxies were0.5-1.0 Gyr old. According to these SFHs, all the MQGs experienced a LuminousInfrared Galaxy (LIRG) phase that lasts for $\sim$ 500 Myr, and half of them anUltra Luminous Infrared Galaxy (ULIRG) phase for $\sim$ 100 Myr. We find thatthe MQG population is almost assembled at $z$ $\sim$ 1, and continues evolvingpassively with few additions to the population.

Pathways to quiescence: SHARDS view on the Star Formation Histories of massive quiescent galaxies at 1.0 < z < 1.5