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We present preliminary results froma survey of cold gas in an intermediate-redshift cluster, Zw Cl0024.1+1652 at z = 0.395, using the EMIR instrument at the IRAM-30m telescope, Pico Veleta observatory,Sierra Nevada, Spain. We observed the CO 2-1and 1-0 transitions in a sample of seven star-forming galaxies drawn out of the GLACE catalogue of H-alpha+[NII] emission-line galaxies. These galaxies have been chosen to be bright in far-IR and to span a wide range of local densities/cluster-centric distances. We have derived the L'_CO luminosity (tracing the amount of cold gas available for star formation) and combined these data with the L_TIR data (tracing the SFR)derived by our team, and with additional CO and FIR data from literature to study how the amount of cold gas in an intermediate-redshift cluster relates to the SFR and cluster-centric distance. The results suggest that, at a given SFR, the reservoir of cold gas is smaller in cluster galaxies. Furthermore, there are also hints that the amount of cold gas increases with the cluster-centric distance, hence pointing to an environmental dependency.

OTELO is an ultradeep, 2D-spectroscopic (resolution R∼700) blind survey, de- fined on a window of 210 Å, centred at 9175 Å, targeting a region of the Extended Groth Field that is embedded in the Deep field 3 of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS). Is the deepest pointing of GALEX in imag- ing and spectroscopy. Such spectra (more properly speaking Pseudo-Spectra or PS) were obtained using the red Tunable Filter (RTF) of the OSIRIS instrument at GTC. OTELO detects emission lines with a limiting flux of 5x10−19 erg/s/cm2 and observed equivalent widths (EW)≥5Å. Besides, OTELO is targeting low mass galaxies, down to M∗ ∼ 106M0. As reference, the MUSE Hubble Ultra Deep Field barely reach down to M∗ ∼ 108M0in few cases, and only at redshifts below 0.4, and none at redshifts above ∼ 0.7. However, OTELO detects the bulk of emitters around 108 − 109M0 even at redshifts as high as 1.4, reaching down to 107M0 at redshift 0.4. Then, OTELO reaches stellar masses one order of magnitude lower than MUSE Hubble Ultra Deep Field. From OTELO database, we were able to generate a catalogue of 60[OII], emitters at < z >= 1.43. Approximately 93% of those emitters have masses in the range of 108 < M∗/M0 < 109 (inside the low-mass regime) and all of them are classified as late-type galaxies. From these [OII] emitters we generated the Luminosity Function, sampling it down to ∼ 1 dex lower than in previous works. Taking into account the results obtained for the lines Hα, Hβ and [OII], we were able to study the star formation rate, star formation rate density, and number density and the evolution of those parameters between redshift z ∼ 0.4 and 1.43. We obtained a robust estimate of the specific star formation rate stellar mass relation based on the lowest mass sample published so far. We also determine a flat trend of the star formation rate density and number density with redshift. Our results suggest a scenario of no evolution of the number density of galaxies, regardless of their masses, up to redshift z ∼ 1.4. This implies agradual change of the relative importance of the star forming processes, fromhigh-mass galaxies to low-mass galaxies, with decreasing redshift. We also found little or no variation of the star formation rate density in the redshift range of0.4 < z < 1.43.&nbsp

OTELO is an ultradeep, 2D-spectroscopic (resolution R∼700) blind survey, de- fined on a window of 210 Å, centred at 9175 Å, targeting a region of the ExtendedGroth Field that is embedded in the Deep field 3 of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS). Is the deepest pointing of GALEX in imag- ing and spectroscopy. Such spectra (more properly speaking Pseudo-Spectra or PS) were obtained using the red Tunable Filter (RTF) of the OSIRIS instrument at GTC. OTELO detects emission lines with a limiting flux of 5x10−19 erg/s/cm2 and observed equivalent widths (EW) ≥ 5Å. Besides, OTELO is targeting low mass galaxies, down to M∗ ∼ 106M0. As reference, the MUSE Hubble Ultra Deep Field barely reach down to M∗ ∼ 108M0in few cases, and only at redshifts below 0.4, and none at redshifts above ∼ 0.7. However, OTELO detects the bulk of emitters around 108 − 109M0 even at redshifts as high as 1.4, reaching down to 107M0 at redshift 0.4. Then, OTELO reaches stellar masses one order of magnitude lower than MUSE Hubble Ultra Deep Field. From OTELO database, we were able to generate a catalogue of 60[OII], emitters at < z >= 1.43. Approximately 93% of those emitters have masses in the range of 108 < M∗/M0 < 109 (inside the low-mass regime) and all of them are classified as late-type galaxies. From these [OII] emitters we generated the Luminosity Function, sampling it down to ∼ 1 dex lower than in previous works. Taking into account the results obtained for the lines Hα, Hβ and [OII], we were able to study the star formation rate, star formation rate density, and number density and the evolution of those parameters between redshift z ∼ 0.4 and 1.43. We obtained a robust estimate of the specific star formation rate stellar mass relation based on the lowest mass sample published so far. We also determine a flat trend of the star formation rate density and number density with redshift. Our results suggest a scenario of no evolution of the number density of galaxies, regardless of their masses, up to redshift z ∼ 1.4. This implies agradual change of the relative importance of the star forming processes, fromhigh-mass galaxies to low-mass galaxies, with decreasing redshift. We also found little or no variation of the star formation rate density in the redshift range of0.4 < z < 1.43.&nbsp