Wise TF: A mid-infrared, 3.4 μm extension of the tully-fisher relation using wise photometry

David J. Lagattuta, Jeremy R. Mould, Lister Staveley-Smith, Tao Hong, Christopher M. Springob, Karen L. Masters, Bärbel S. Koribalski, D. Heath Jones

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We present a mid-infrared Tully-Fisher (TF) relation using photometry from the 3.4 μm W1 band of the Wide-field Infrared Survey Explorer (WISE) satellite. The WISE TF relation is formed from 568 galaxies taken from the all-sky 2MASS Tully-Fisher (2MTF) galaxy catalog, spanning a range of environments including field, group, and cluster galaxies. This constitutes the largest mid-infrared TF relation constructed to date. After applying a number of corrections to galaxy magnitudes and line widths, we measure a master TF relation given by M corr = -22.24-10.05[log (W corr)-2.5], with an average dispersion of σWISE = 0.686 mag. There is some tension between WISE TF and a preliminary 3.6 μm relation, which has a shallower slope and almost no intrinsic dispersion. However, our results agree well with a more recent relation constructed from a large sample of cluster galaxies. We additionally compare WISE TF to the near-infrared 2MTF template relations, finding a good agreement between the TF parameters and total dispersions of WISE TF and the 2MTF K-band template. This fact, coupled with typical galaxy colors of (K-W1) ∼ 0, suggests that these two bands are tracing similar stellar populations, including the older, centrally-located stars in the galactic bulge which can (for galaxies with a prominent bulge) dominate the light profile.

Original languageEnglish
Article number88
Pages (from-to)1-12
Number of pages12
JournalAstrophysical Journal
Issue number2
Publication statusPublished - 10 Jul 2013
Externally publishedYes

Bibliographical note

Copyright 2013 The American Astronomical Society. First published in the Astrophysical Journal, 771(2), 88, 2013. The original publication is available at http://doi.org/10.1088/0004-637X/771/2/88, published by IOP Publishing. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.


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