METALLICITY AND AGE OF THE STELLAR STREAM AROUND THE DISK GALAXY NGC 5907
ABSTRACT Stellar streams have become central to studies of the interaction histories of nearby galaxies. To characterize the most prominent parts of the stellar stream around the well-known nearby (d = 17 Mpc) edge-on disk galaxy NGC 5907, we have obtained and analyzed new, deep gri Subaru/Suprime-C...
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| Veröffentlicht in: | The Astronomical journal 2016-09, Vol.152 (3), p.72 |
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| creator | Laine, Seppo Grillmair, Carl J. Capak, Peter Arendt, Richard G. Romanowsky, Aaron J. Martínez-Delgado, David Ashby, Matthew L. N. Davies, James E. Majewski, Stephen R. Brodie, Jean P. GaBany, R. Jay Arnold, Jacob A. |
| description | ABSTRACT Stellar streams have become central to studies of the interaction histories of nearby galaxies. To characterize the most prominent parts of the stellar stream around the well-known nearby (d = 17 Mpc) edge-on disk galaxy NGC 5907, we have obtained and analyzed new, deep gri Subaru/Suprime-Cam and 3.6 m Spitzer/Infrared Array Camera observations. Combining the near-infrared 3.6 m data with visible-light images allows us to use a long wavelength baseline to estimate the metallicity and age of the stellar population along an ∼60 kpc long segment of the stream. We have fitted the stellar spectral energy distribution with a single-burst stellar population synthesis model and we use it to distinguish between the proposed satellite accretion and minor/major merger formation models of the stellar stream around this galaxy. We conclude that a massive minor merger (stellar mass ratio of at least 1:8) can best account for the metallicity of −0.3 inferred along the brightest parts of the stream. |
| doi_str_mv | 10.3847/0004-6256/152/3/72 |
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We have fitted the stellar spectral energy distribution with a single-burst stellar population synthesis model and we use it to distinguish between the proposed satellite accretion and minor/major merger formation models of the stellar stream around this galaxy. We conclude that a massive minor merger (stellar mass ratio of at least 1:8) can best account for the metallicity of −0.3 inferred along the brightest parts of the stream.</description><identifier>ISSN: 0004-6256</identifier><identifier>ISSN: 1538-3881</identifier><identifier>EISSN: 1538-3881</identifier><identifier>DOI: 10.3847/0004-6256/152/3/72</identifier><language>eng</language><publisher>United States: The American Astronomical Society</publisher><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; CAMERAS ; ENERGY SPECTRA ; GALAXIES ; galaxies: evolution ; galaxies: interactions ; galaxies: structure ; MASS ; METALLICITY ; SATELLITES ; STAR CLUSTERS ; STARS ; STREAMS ; SYNTHESIS ; VISIBLE RADIATION</subject><ispartof>The Astronomical journal, 2016-09, Vol.152 (3), p.72</ispartof><rights>2016. The American Astronomical Society. 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Combining the near-infrared 3.6 m data with visible-light images allows us to use a long wavelength baseline to estimate the metallicity and age of the stellar population along an ∼60 kpc long segment of the stream. We have fitted the stellar spectral energy distribution with a single-burst stellar population synthesis model and we use it to distinguish between the proposed satellite accretion and minor/major merger formation models of the stellar stream around this galaxy. 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| subjects | ASTROPHYSICS, COSMOLOGY AND ASTRONOMY CAMERAS ENERGY SPECTRA GALAXIES galaxies: evolution galaxies: interactions galaxies: structure MASS METALLICITY SATELLITES STAR CLUSTERS STARS STREAMS SYNTHESIS VISIBLE RADIATION |
| title | METALLICITY AND AGE OF THE STELLAR STREAM AROUND THE DISK GALAXY NGC 5907 |
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