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The Spitzer Survey of Stellar Structure in Galaxies (S$^{4}$G) is a detailedstudy of over 2300 nearby galaxies in the near-infrared (NIR), which has beencritical to our understanding of the detailed structures of nearby galaxies.Because the sample galaxies were selected only using radio-derived velocities,however, the survey favored late-type disk galaxies over lenticulars andellipticals. A follow-up Spitzer survey was conducted to rectify this bias,adding 465 early-type galaxies (ETGs) to the original sample, to be analyzed ina manner consistent with the initial survey. We present the data release ofthis ETG extension, up to the third data processing pipeline (P3): surfacephotometry. We produce curves of growth and radial surface brightness profiles(with and without inclination corrections) using reduced and masked SpitzerIRAC 3.6$\mu$m and 4.5$\mu$m images produced through Pipelines 1 and 2,respectively. From these profiles, we derive the following integratedquantities: total magnitudes, stellar masses, concentration parameters, andgalaxy size metrics. We showcase NIR scaling relations for ETGs among thesequantities. We examine general trends across the whole S$^{4}$G and ETGextension among our derived parameters, highlighting differences between ETGsand late-type galaxies (LTGs). ETGs are, on average, more massive and moreconcentrated than LTGs, and also show subtle distinctions among ETGmorphological sub-types. We also derive the following scaling relations andcompare with previous results in visible light: mass--size (both half-light andisophotal), mass--concentration, mass--surface brightness (central, effective,and within 1 kpc), and mass--color. We find good agreement with previous works,though some relations (e.g., mass--central surface brightness) will requiremore careful multi-component decompositions to be fully understood.

astronomy and astrophysics

Stellar masses, sizes, and radial profiles for 465 nearby early-type  galaxies: an extension to the Spitzer Survey of Stellar Structure in Galaxies  (S$^{4}$G)