Generalizations of the Tully-Fisher Relation for Early- and Late-Type Galaxies
Generalizations of the Tully-Fisher Relation for Early- and Late-Type Galaxies
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早型和晚型星系塔利-费舍尔关系的推广
DOI：
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发表时间：
2007
期刊：
影响因子：
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通讯作者：
H. Dejonghe
中科院分区：
文献类型：
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作者：
S. De Rijcke;W. Zeilinger;G. Hau;P. Prugniel;H. Dejonghe
我们根据塔利-费舍尔关系（TFR）、恒星质量塔利-费舍尔关系（sTFR）和所谓的重子或 H I 气体+恒星质量塔利-费舍尔关系（gsTFR）研究矮星系和巨型早型和晚型星系的轨迹。我们表明，早型和晚型星系，从矮星系到巨星系，都遵循不同但近似平行的 TFR。令人惊讶的是，早型和晚型星系在恒星质量的 3.5 个数量级范围内追踪到单一但弯曲的 sTFR。此外，所有星系都追踪单一的线性 gsTFR，在 H I 气体+恒星质量中超过 3.5 个数量级。然而，矮椭圆略低于 gsTFR。这可能表明，与晚期类型相反，早期类型的矮星已经失去了气体，例如通过银河风或冲压压力剥离。总体而言，环境在塑造这些关系中只发挥次要作用，使它们成为一个相当“干净”的宇宙学工具。 ΛCDM 模拟大致预测了这些关系的正确斜率。
We study the locus of dwarf and giant early- and late-type galaxies on the Tully-Fisher relation (TFR), the stellar mass Tully-Fisher relation (sTFR), and the so-called baryonic or H I gas+stellar mass Tully-Fisher relation (gsTFR). We show that early-type and late-type galaxies, from dwarfs to giants, trace different yet approximately parallel TFRs. Surprisingly, early-type and late-type galaxies trace a single yet curved sTFR over a range of 3.5 orders of magnitude in stellar mass. Moreover, all galaxies trace a single, linear gsTFR, over 3.5 orders of magnitude in H I gas+stellar mass. Dwarf ellipticals, however, lie slightly below the gsTFR. This may indicate that early-type dwarfs, contrary to the late types, have lost their gas, e.g., by galactic winds or ram pressure stripping. Overall, environment only plays a secondary role in shaping these relations, making them a rather "clean" cosmological tool. ΛCDM simulations predict roughly the correct slopes for these relations.