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The baryonic tully-fisher relationship for S4G galaxies and the "condensed" baryon fraction of galaxies



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Gil de Paz, Armando (2014) The baryonic tully-fisher relationship for S4G galaxies and the "condensed" baryon fraction of galaxies. The Astronomical Journal, 147 (6). ISSN 0004-6256


Official URL: http://dx.doi.org/10.1088/0004-6256/147/6/134



We combine data from the Spitzer Survey for Stellar Structure in Galaxies, a recently calibrated empirical stellar mass estimator from Eskew et al., and an extensive database of H i spectral line profiles to examine the baryonic Tully–Fisher (BTF) relation. We find (1) that the BTF has lower scatter than the classic Tully–Fisher (TF) relation and is better described as a linear relationship, confirming similar previous results, (2) that the inclusion of a radial scale in the BTF decreases the scatter but only modestly, as seen previously for the TF relation, and (3) that the slope of the BTF, which we find to be 3.5 ± 0.2 (Δ log Mbaryon/Δ log v_c), implies that on average a nearly constant fraction (∼0.4) of all baryons expected to be in a alo are “condensed” onto the central region of rotationally supported galaxies. The condensed baryon fraction, M_baryon/M_total, is, to our measurement precision, nearly independent of galaxy circular velocity (our sample spans circular velocities, v_c, between 60 and 250 km s^−1, but is extended to v_c ∼ 10 km s^−1 using data from the literature). The observed galaxy-to-galaxy scatter in this fraction is generally ≤a factor of 2 despite fairly liberal selection criteria. These results imply that cooling and heating processes, such as cold versus hot accretion, mass loss due to stellar winds, and active galactic nucleus driven feedback, to the degree that they affect the global galactic properties involved in the BTF, are independent of halo mass for galaxies with 10 < vc < 250 km s^−1 and typically introduce no more than a factor of two range in the resulting M_baryon/M_total. Recent simulations by Aumer et al. of a small sample of disk galaxies are in excellent agreement with our data, suggesting that current simulations are capable of reproducing the global properties of individual disk galaxies. More detailed comparison to models using the BTF holds great promise, but awaits improved determinations of the stellar masses.

Item Type:Article
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© 2014 The American Astronomical Society.
D.Z. acknowledges financial support from NASA ADAP NX12AE27G and NSF AST-1311326, and thanks NYU CCPP for its hospitality during long-term visits. The authors thank Michael Aumer for sending us the baryonic masses and circular velocities of simulated galaxies that we incorporated into Figure 8, and Marc Verheijen and R. Brent Tully for comments on the manuscript. We also gratefully acknowledge discussions with Stacy McGaugh, which led both to improvements of the current manuscript and to related ideas to pursue in subsequent work. H.C. and J.S. acknowledge support from the Lyon Institute of Origins under grant ANR-10-LABX-66. The authors acknowledge the support from the FP7 Marie Curie Actions
of the European Commission, via the Initial Training Network DAGAL under REA grant agreement PITN-GA-2011-289313. The authors thank the entire S4G team for the efforts in making this program possible. K.S., J-C.M-M, and T.K acknowledge support from the National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the NASA/IPAC Extragalactic atabase (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.

Uncontrolled Keywords:Galaxies: evolution; Galaxies: formation; Galaxies: fundamental parameters; Galaxies: stellar content; Galaxies: structure
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:29206
Deposited On:13 Mar 2015 13:16
Last Modified:10 Dec 2018 15:05

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