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20 April 2024
 
  » arxiv » 1602.2757

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A Slippery Slope: Systematic Uncertainties in the Baryonic Tully-Fisher Relation
Jeremy D. Bradford ; Marla C. Geha ; Frank C. van den Bosch ;
Date 8 Feb 2016
AbstractThe baryonic Tully-Fisher relation (BTFR) is both a valuable observational tool and a critical test of galaxy formation theory. We explore the systematic uncertainty in the slope and the scatter of the observed BTFR utilizing a homogeneously measured dataset of 930 isolated galaxies. We measure a fiducial relation of log_10 M_baryon = 3.24 log_10 V_rot + 3.21 with a scatter of 0.25 dex over the baryonic mass range of 10^7.4 to 10^11.3 M_sun. We then conservatively vary the definitions of M_baryon and V_rot, the sample definition and the linear fitting algorithm used to fit the BTFR. We obtain slopes ranging from 2.64 to 3.46 and scatter measurements ranging from 0.16 to 0.41 dex. We next compare our fiducial slope to literature measurements, where reported slopes range from 3.0 to 4.3 and scatter is either unmeasured, unmeasurable or as large as 0.4 dex. Measurements derived from unresolved HI line-widths tend to produce slopes of 3.2, while measurements derived strictly from resolved asymptotic rotation velocities produce slopes of 4.0. The largest factor affecting the BTFR slope is the definition of rotation velocity. Sample definition, mass range and linear fitting algorithm also significantly affect the measured BTFR. Galaxies with V_rot < 100 km/s are consistent with the BTFR of more massive galaxies, but these galaxies drive most of the scatter in the BTFR. This is most likely due to the diversity in rotation curve shapes of low-mass galaxies and underestimated systematic uncertainties. It is critical when comparing predictions to an observed BTFR that the rotation velocity definition, the sample selection and the fitting algorithm are similarly defined. Fitting a power-law model to the BTFR is an oversimplification and we recommend direct statistical comparisons between datasets with commensurable properties.
Source arXiv, 1602.2757
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