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arXiv · 1004.4365

The slope of the Baryonic Tully-Fisher relation

Sebastián Gurovich·Kenneth Freeman·Helmut Jerjen·Lister Staveley-Smith·Ivânio Puerari
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Abstract

We present the results of a baryonic Tully-Fisher relation (BTFR) study for a local sample of relatively isolated disk galaxies. We derive a BTFR with a slope near 3 measured over about 4 dex in baryon mass for our combined \textrm{H\,\scriptsize{I}} and bright spiral disk samples. This BTFR is significantly flatter and has less scatter than the TFR (stellar mass only) with its slope near 4 reported for other samples and studies. A BTFR slope near 3 is in better agreement with the expected slope from simple $\Lambda$CDM cosmological simulations that include both stellar and gas baryons. The scatter in the TFR/BTFR appears to depend on $W_{20}$: galaxies that rotate slower have more scatter. The atomic gas--to--stars ratio shows a break near $W_{20} = 250$ \kms\, probably associated with a change in star formation efficiency. In contrast the absence of such a break in the BTFR suggests that this relation was probably set at the main epoch of baryon dissipation rather than as a product of later galactic evolution.

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Sebastián Gurovich, Kenneth Freeman, Helmut Jerjen, Lister Staveley-Smith, Ivânio Puerari. 2010-04-25. The slope of the Baryonic Tully-Fisher relation. https://doi.org/10.1088/0004-6256/140/3/663

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