The stellar mass assembly of low-redshift, massive, central galaxies in SDSS and the TNG300 simulation

Journal Article · Fri Aug 07 00:00:00 EDT 2020 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/staa2306· OSTI ID:1648593

Jackson, Thomas M. ^[1]; Pasquali, A.  ^[1]; Pacifici, C. ^[2]; Engler, C.  ^[3]; Pillepich, A. ^[4]; Grebel, E. K. ^[1]

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1. Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr 12–14, D-69120 Heidelberg, Germany
2. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
3. Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr 12–14, D-69120 Heidelberg, Germany, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
4. Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany

ABSTRACT The stellar mass assembly of galaxies can be affected by both secular and environmental processes. In this study, for the first time, we investigate the stellar mass assembly of $$\sim 90\, 000$$ low-redshift, central galaxies selected from SDSS group catalogues ($$M_{\rm Stellar}\gtrsim 10^{9.5}\, \mathrm{M}_{\odot }$$, $$M_{\rm Halo}\gtrsim 10^{12}\, \mathrm{M}_{\odot }$$) as a function of both stellar mass and halo mass. We use estimates of the times at which 10, 50, and 90 per cent of the stellar mass were assembled from photometric spectral energy distribution fitting, allowing a more complete investigation than single stellar ages alone. We consider trends in both stellar mass and halo mass simultaneously, finding dependences of all assembly times on both. We find that galaxies with higher stellar masses (at constant halo mass) have on average older lookback times, similar to previous studies of galaxy assembly. We also find that galaxies at higher halo mass (at constant stellar mass) have younger lookback times, possibly due to a larger reservoir of gas for star formation. An exception to this is a subsample with high stellar-to-halo mass ratios, which are likely massive, field spirals. We compare these observed trends to those predicted by the TNG300 simulation, finding good agreement overall as a function of either stellar mass or halo mass. However, some differences in the assembly times (of up to ∼3 Gyr) appear when considering both stellar mass and halo mass simultaneously, noticeably at intermediate stellar masses (MStellar ∼ 1011 M⊙). These discrepancies are possibly linked to the quenched fraction of galaxies and the kinetic mode active galactic nucleus feedback implemented in TNG300.

• Sponsoring Organization: USDOE
• OSTI ID: 1648593
• Journal Information: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Vol. 497 Journal Issue: 4; ISSN 0035-8711
• Publisher: Oxford University Press
• Country of Publication: United Kingdom
• Language: English