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The Baryonic Tully–Fisher Relation

Published online by Cambridge University Press:  05 March 2013

Sebastián Gurovich ,
Stacy S. McGaugh ,
Ken C. Freeman ,
Helmut Jerjen ,
Lister Staveley-Smith  and
W. J. G. De Blok
Sebastián Gurovich*
Affiliation:
Mount Stromlo Observatory, Australian National University, Weston Creek ACT 2611, Australia Australia Telescope National Facility, Marsfield NSW 2122, Australia
Stacy S. McGaugh
Affiliation:
Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
Ken C. Freeman*
Affiliation:
Mount Stromlo Observatory, Australian National University, Weston Creek ACT 2611, Australia
Helmut Jerjen
Affiliation:
Mount Stromlo Observatory, Australian National University, Weston Creek ACT 2611, Australia
Lister Staveley-Smith
Affiliation:
Australia Telescope National Facility, Marsfield NSW 2122, Australia
W. J. G. De Blok
Affiliation:
Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, UK
*
ECorresponding author. Email: [email protected]; [email protected]
ECorresponding author. Email: [email protected]; [email protected]
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Abstract

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We validate the baryonic Tully–Fisher (TF) relation by exploring the Tully–Fisher (TF) and BTF properties of optically and Hi-selected disk galaxies. The data includes galaxies from Sakai et al. (2000) calibrator sample, McGaugh et al. (2000: M2000) I-band sample, and 18 newly acquired Hi-selected field dwarf galaxies observed with the ANU 2.3-m telescope and the ATNF Parkes telescope (Gurovich 2005a).

As in M2000, we re-cast the TF and BTF relations as relationships between baryon mass and W20. First we report some numerical errors in M2000. Then, we calculate weighted bi-variate linear fits to the data, and finally we compare the fits of the intrinsically fainter dwarfs with the brighter galaxies of Sakai et al. (2000). With regards to the local calibrator disk galaxies of Sakai et al. (2000), our results suggest that the BTF relation is indeed tighter than the TF relation and that the slopes of the BTF relations are statistically flatter than the equivalent TF relations. Further, for the fainter galaxies which include the I-band M2000 and Hi-selected galaxies of Gurovich's sample, we calculate a break from a simple power law model because of what appears to be real cosmic scatter. Not withstanding this point, the BTF models are marginally better models than the equivalent TF ones with slightly smaller Χred2 values.

Keywords

dark mattergalaxies: baryonic Tully–Fishergas-rich dwarf galaxiesnear-field cosmology
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 21 , Special Issue 4: Structure and Dynamics in the Local Universe , 2004 , pp. 412 - 414
Copyright
Copyright © Astronomical Society of Australia 2004

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