2016A&A...593A..39P


C.D.S. - SIMBAD4 rel 1.7 - 2020.06.04CEST12:35:13

2016A&A...593A..39P - Astronomy and Astrophysics, volume 593A, 39-39 (2016/9-1)

An accurate measurement of the baryonic Tully-Fisher relation with heavily gas-dominated ALFALFA galaxies.

PAPASTERGIS E., ADAMS E.A.K. and VAN DER HULST J.M.

Abstract (from CDS):

We use a sample of 97 galaxies selected from the Arecibo legacy fast ALFA (ALFALFA) 21cm survey to make an accurate measurement of the baryonic Tully-Fisher relation (BTFR). These galaxies are specifically selected to be heavily gas-dominated (Mgas/M*≥2.7) and to be oriented edge-on. The former property ensures that the error on the galactic baryonic mass is small, despite the large systematic uncertainty involved in galactic stellar mass estimates. The latter property means that rotational velocities can be derived directly from the width of the 21cm emission line, without any need for inclination corrections. We measure a slope for the linewidth-based BTFR of α=3.75±0.11, a value that is somewhat steeper than (but in broad agreement with) previous literature results. The relation is remarkably tight, with almost all galaxies being located within a perpendicular distance of±0.1dex from the best fit line. The low observational error budget for our sample enables us to establish that, despite its tightness, the measured linewidth-based BTFR has some small (i.e., non-zero) intrinsic scatter. We furthermore find a systematic difference in the BTFR of galaxies with "double-horned" 21cm line profiles - suggestive of flat outer galactic rotation curves - and those with "peaked" profiles - suggestive of rising rotation curves. When we restrict our sample of galaxies to objects in the former category, we measure a slightly steeper slope of α=4.13±0.15. Overall, the high-accuracy measurement of the BTFR presented in this article is intended as a reliable observational benchmark against which to test theoretical expectations. Here we consider a representative set of semi-analytic models and hydrodynamic simulations in the lambda cold dark matter (ΛCDM) context, as well as modified Newtonian dynamics (MOND). In the near future, interferometric follow-up observations of several sample members will enable us to further refine the BTFR measurement, and make sharper comparisons with theoretical models.

Abstract Copyright: © ESO, 2016

Journal keyword(s): galaxies: fundamental parameters - galaxies: kinematics and dynamics - galaxies: formation - radio lines: galaxies

Status at CDS:  

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 AGC 122217 G 02 33 32.202 +27 01 13.87           ~ 4 0
2 AGC 188761 G 08 21 59.040 +13 02 22.72           ~ 3 0
3 LEDA 1764097 G 09 39 20.369 +26 08 13.24           ~ 4 0
4 LEDA 90938 G 09 43 45.737 +14 40 47.97           ~ 8 0
5 LEDA 1712509 G 11 50 20.181 +24 38 37.29           ~ 7 0
6 IC 3105 G 12 17 33.750 +12 23 17.15   15.0       ~ 75 0
7 LEDA 1766890 EmG 12 52 05.527 +26 11 54.85           ~ 7 0
8 UGC 8575 GiG 13 35 45.619 +08 58 09.56   15.5       ~ 42 0
9 2MASX J15080557+0651483 G 15 08 05.562 +06 51 48.47   15.4       ~ 10 0
10 NAME Local Group GrG ~ ~           ~ 6926 0

    Equat.    Gal    SGal    Ecl

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2020.06.04-12:35:13

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