Description
In this talk, I will explore the promising synergy between WEAVE/StePS and Euclid for studying dust attenuation in the COSMOS field. The well-constrained ratios of intrinsic hydrogen emission lines provide a robust method for measuring wavelength-dependent dust attenuation, which is crucial for accurate flux corrections and reducing biases in the estimation of physical parameters of galaxies (e.g., Star Formation rates). By combining high-resolution WEAVE spectra (0.36 to 0.96 μm, R > 5000) with Euclid's low-resolution near-infrared spectra (R > 380) from its blue (0.92–1.30 μm) and red (1.25–1.86 μm) grisms, we achieve comprehensive spectral coverage, capturing Balmer and Paschen hydrogen emission lines (Hβ, Hα, Paschen β, and Paschen γ) in star-forming galaxies at 0.3 < z < 0.7. I will discuss the powerful possible cross-calibration between the two spectrographs, highlighting the challenges of integrating data from different instruments, particularly when one is slitless and the other fiber-based. Additionally, I will present how these efforst led me to work on the first Euclid emission line maps and will present some of them in the talk. These maps are essential for ensuring consistency between WEAVE and Euclid measurements.
