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Consistent Dynamical and Stellar Masses with Potential Light IMF in Massive Quiescent Galaxies at 3 < z < 4 Using Velocity Dispersions Measurements with MOSFIRE

• Authors: James Esdaile, Karl Glazebrook, Ivo Labbé, Edward Taylor, Corentin Schreiber, Themiya Nanayakkara, Glenn G. Kacprzak, Pascal A. Oesch, Kim-Vy H. Tran, Casey Papovich, Lee Spitler, and Caroline M. S. Straatman

2021 The Astrophysical Journal Letters 908 L35.

• Provider: AAS Journals

Caption: Figure 3.

IMF parameter: α vs. σe. Sample and marker layout are the same as in Figure 2, but instead using the mass-follows-light models for the z ∼2 sample from Mendel et al. (2020), which have a tighter ασ relation. Error ellipse in the bottom right represents the correlated errors for the 3.2 < z < 3.7 sample. Dotted lines are for a Chabrier and Salpeter IMF normalization. Blue solid line is the IMF–σe relation for the ATLAS3D+SLACS sample derived in Posacki et al. (2015), with blue shaded area representing the 1σ scatter.