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CO Tully–Fisher relation of star-forming galaxies at = 0.05–0.3

Topal, Selçuk; Bureau, Martin; Tiley, Alfred L.; Davis, Timothy A.; Torii, Kazufumi

CO Tully–Fisher relation of star-forming galaxies at = 0.05–0.3 Thumbnail


Authors

Selçuk Topal

Martin Bureau

Alfred L. Tiley

Timothy A. Davis

Kazufumi Torii



Abstract

The Tully–Fisher relation (TFR) is an empirical relation between galaxy luminosity and rotation velocity. We present here the first TFR of galaxies beyond the local Universe that uses carbon monoxide (CO) as the kinematic tracer. Our final sample includes 25 isolated, non-interacting star-forming galaxies with double-horned or boxy CO integrated line profiles located at redshifts z ≤ 0.3, drawn from a larger ensemble of 67 detected objects. The best reverse Ks-band, stellar mass and baryonic mass CO TFRs are, respectively, MKs = (−8.4 ± 2.9)[log ( W50/km s−1 sin i ) − 2.5] + (−23.5 ± 0.5), log (M/M) = (5.2 ± 3.0)[log ( W50/km s−1 sin i ) − 2.5] + (10.1 ± 0.5) and log (Mb/M) = (4.9 ± 2.8)[log ( W50/km s−1 sin i ) − 2.5] + (10.2 ± 0.5), where MKs is the total absolute Ks-band magnitude of the objects, M and Mb their total stellar and baryonic masses, and W50 the width of their line profile at 50 per cent of the maximum. Dividing the sample into different redshift bins and comparing to the TFRs of a sample of local (z = 0) star-forming galaxies from the literature, we find no significant evolution in the slopes and zero-points of the TFRs since z ≈ 0.3, this in either luminosity or mass. In agreement with a growing number of CO TFR studies of nearby galaxies, we more generally find that CO is a suitable and attractive alternative to neutral hydrogen (HI). Our work thus provides an important benchmark for future higher redshift CO TFR studies.

Citation

Topal, S., Bureau, M., Tiley, A. L., Davis, T. A., & Torii, K. (2018). CO Tully–Fisher relation of star-forming galaxies at = 0.05–0.3. Monthly Notices of the Royal Astronomical Society, 479(3), 3319-3334. https://doi.org/10.1093/mnras/sty1617

Journal Article Type Article
Acceptance Date Jun 15, 2018
Online Publication Date Jun 19, 2018
Publication Date Sep 21, 2018
Deposit Date Aug 23, 2018
Publicly Available Date Mar 29, 2024
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Royal Astronomical Society
Peer Reviewed Peer Reviewed
Volume 479
Issue 3
Pages 3319-3334
DOI https://doi.org/10.1093/mnras/sty1617

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Copyright Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.





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