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In this paper we investigate the impact of lensing magnification on theanalysis of Euclid's spectroscopic survey, using the multipoles of the 2-pointcorrelation function for galaxy clustering. We determine the impact of lensingmagnification on cosmological constraints, and the expected shift in thebest-fit parameters if magnification is ignored. We consider two cosmologicalanalyses: i) a full-shape analysis based on the $\Lambda$CDM model and itsextension $w_0w_a$CDM and ii) a model-independent analysis that measures thegrowth rate of structure in each redshift bin. We adopt two complementaryapproaches in our forecast: the Fisher matrix formalism and the Markov chainMonte Carlo method. The fiducial values of the local count slope (ormagnification bias), which regulates the amplitude of the lensingmagnification, have been estimated from the Euclid Flagship simulations. We uselinear perturbation theory and model the 2-point correlation function with thepublic code coffe. For a $\Lambda$CDM model, we find that the estimation ofcosmological parameters is biased at the level of 0.4-0.7 standard deviations,while for a $w_0w_a$CDM dynamical dark energy model, lensing magnification hasa somewhat smaller impact, with shifts below 0.5 standard deviations. In amodel-independent analysis aiming to measure the growth rate of structure, wefind that the estimation of the growth rate is biased by up to $1.2$ standarddeviations in the highest redshift bin. As a result, lensing magnificationcannot be neglected in the spectroscopic survey, especially if we want todetermine the growth factor, one of the most promising ways to test generalrelativity with Euclid. We also find that, by including lensing magnificationwith a simple template, this shift can be almost entirely eliminated withminimal computational overhead.

Euclid Preparation. TBD. Impact of magnification on spectroscopic galaxy clustering