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Stellar Populations at intermediate redshifts Survey (StePS)


Team Lead: Angela Iovino

Survey Working Group members: Amata Mercurio & Angela Iovino

Quality Assurance Group members: Marcella Longhetti, Stefano Zibetti & Francesco La Barbera

One of the major goals of extragalactic astrophysics is to understand the physical processes that cause the formation and evolution of luminous structures.

Recent surveys such as SDSS and GAMA have made ground-breaking progress in the low-redshift Universe in describing how the main galaxy properties vary with both galaxy mass and host halo mass. However, detailed observations of the evolutionary changes of galaxy properties as a function of look-back time are needed to establish which mechanisms dominate galaxy evolution, what drives the star formation history of galaxies and their mass assembly (Fig. 1).

Fig.1 The evolution of the star formation rate–stellar mass relation with redshift. The origin of a such relation and its evolution are among the fundamental questions addressed by StePS. Credits: Lee et al. (2015)

Scientific aims

Shallow spectroscopic observations can provide galaxy redshifts, rough measurements of emission lines and a reliable estimate of the D4000 break, but detailed information on the stellar and gas content of galaxies can only be achieved through deep spectroscopy providing reliable measurements of the absorption features in the stellar continuum.

None of the existing large surveys of distant galaxies have the adequate resolution and spectral quality/range to derive the stellar population properties in sufficient detail for statistically large samples of galaxies in different environmental conditions (Fig.2).

Fig 2. Comparison of a typical absorption-line spectrum from StePS (magenta) and BOSS (black) at z=0.55. The shaded areas identify the main absorption features (red Balmer lines, blue metal lines). The superior quality of the StePS spectra provide a reliable measurement of both Balmer and metallic lines that is unattainable in BOSS.

StePS aims to perform a full spectral analysis for a large sample of galaxies at intermediate redshifts, similar to what the SDSS has done in the local Universe.

StePS will derive galaxy stellar ages, star-formation timescales, stellar and gas metallicities, and dust attenuation, and will infer the past evolution of galaxies at different masses and redshift, relating their star formation histories to their intrinsic (e.g., stellar mass, galaxy morphology) and environmental properties. These spectra will also provide gas kinematics and stellar velocity dispersions, which will allow us to perform a dynamical classification of our galaxies and make a link between star formation history, mass assembly history and dynamics.

Fig 3. Galaxy bimodality in a colour–stellar mass diagram: StePS will study how the bimodality evolves with redshift and how galaxies move with time in this diagram. Credits: Schawinski et al. (2014)


The goal of StePS is to address the following questions:

  • What physical mechanisms drive the star formation histories of galaxies and its quenching over two thirds of the life of the Universe?
  • What is the role of environment vs. intrinsic galaxy properties in this evolution?
  • How do galaxies assemble their mass during the last 7 Gyr?

Fig 4. Galaxy properties strongly depend on the environment where they reside. The average star formation activity decreases going from the least dense regions of the Universe (voids/field) to denser environments (groups and clusters of galaxies).

Top left: the galaxy cluster A370; top right: the galaxy group known as the Stephan’s Quintet; bottom: a void spiral galaxy (MCG+01-02-015). Credits: NASA/HST

Observational strategy

StePS will carry out a MOS survey of ~30,000 galaxies at 0.3<z<0.7 over four areas on the sky for a total of ~25 square degrees. Targets are drawn from a magnitude-limited sample with IAB<20.5 and pre-selected from high quality photometric redshifts to be at z>0.3, except for the COSMOS field where no photo-z pre-selection is applied. This magnitude limit corresponds to a logarithmic stellar mass limit of 10.2 at z=0.3, 11.0 at z=0.5 and 11.3 at z=0.7, for a Chabrier IMF.

This large sample will enable us to explore galaxy evolution in a sufficient number of bins of different galaxy masses, galaxy morphologies/colours, environments and cosmic epochs.

Using WEAVE’s LR mode (R~5000) we will obtain spectra with high enough signal-to-noise per resolution element (S/N>15) over a broad wavelength range to undertake a detailed analysis of the underlying stellar  populations and of the emission line properties of these faint galaxies. This requires exposure times of between 7 and 14 hours.

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