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

Topal, Selçuk and Bureau, Martin and Tiley, Alfred L. and Davis, Timothy A. and Torii, Kazufumi (2018) 'CO Tully–Fisher relation of star-forming galaxies at = 0.05–0.3.', Monthly notices of the Royal Astronomical Society., 479 (3). pp. 3319-3334.

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.

Item Type:Article
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Status:Peer-reviewed
Publisher Web site:https://doi.org/10.1093/mnras/sty1617
Publisher 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.
Date accepted:15 June 2018
Date deposited:23 August 2018
Date of first online publication:19 June 2018
Date first made open access:23 August 2018

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