The Black Hole Mass–Color Relations for Early- and Late-type Galaxies: Red and Blue Sequences
| Autor: | Alexandre Y. K. Bouquin, Javier Gorgas, Johan H. Knapen, Bililign T. Dullo, Armando Gil de Paz |
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| Rok vydání: | 2020 |
| Předmět: |
Physics
Astrofísica Supermassive black hole Spiral galaxy Cosmology and Nongalactic Astrophysics (astro-ph.CO) 010504 meteorology & atmospheric sciences Star formation FOS: Physical sciences Astronomy and Astrophysics Astrophysics 01 natural sciences Astrophysics - Astrophysics of Galaxies Galaxy Black hole Astronomía Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) 0103 physical sciences Elliptical galaxy 010303 astronomy & astrophysics Lenticular galaxy Stellar evolution 0105 earth and related environmental sciences Astrophysics - Cosmology and Nongalactic Astrophysics |
| Zdroj: | The Astrophysical Journal E-Prints Complutense. Archivo Institucional de la UCM instname E-Prints Complutense: Archivo Institucional de la UCM Universidad Complutense de Madrid |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/ab9dff |
| Popis: | [Abridged] Tight correlations between supermassive black hole (SMBH) mass ($M_{\rm BH}$) and the properties of the host galaxy have useful implications for our understanding of the growth of SMBHs and evolution of galaxies. Here, we present newly observed correlations between $M_{\rm BH}$ and the host galaxy total UV$-$ [3.6] color ($\mathcal{C_{\rm UV,tot}}$, Pearson's r = $0.6-0.7$) for a sample of 67 galaxies (20 early-type galaxies and 47 late-type galaxies) with directly measured $M_{\rm BH}$ in the GALEX/S$^{4}$G survey. The colors are carefully measured in a homogeneous manner using the galaxies' FUV, NUV and 3.6 $\micron$ magnitudes and their multi-component structural decompositions in the literature. We find that more massive SMBHs are hosted by (early- and late-type) galaxies with redder colors, but the $M_{\rm BH}- \mathcal{C_{\rm UV,tot}}$ relations for the two morphological types have slopes that differ at $\sim 2 \sigma$ level. Early-type galaxies define a red sequence in the $M_{\rm BH}- \mathcal{C_{\rm UV,tot}}$ diagrams, while late-type galaxies trace a blue sequence. Within the assumption that the specific star formation rate of a galaxy (sSFR) is well traced by $L_{\rm UV}/L_{\rm 3.6}$, it follows that the SMBH masses for late-type galaxies exhibit a steeper dependence on sSFR than those for early-type galaxies. The $M_{\rm BH}- \mathcal{C_{\rm UV,tot}}$ and $M_{\rm BH}-L_{\rm 3.6,tot}$ relations for the sample galaxies reveal a comparable level of vertical scatter in the log $M_{\rm BH}$ direction, roughly $5\%-27\%$ more than the vertical scatter of the $M_{\rm BH}-\sigma$ relation. Our $M_{\rm BH}- \mathcal{C_{\rm UV,tot}}$ relations suggest different channels of SMBH growth for early- and late-type galaxies, consistent with their distinct formation and evolution scenarios. Comment: 27 pages, 8 figures, 6 tables, accepted for publication in ApJ |
| Databáze: | OpenAIRE |
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