We measure the Tully-Fisher relations of 14 lenticular galaxies (S0s) and 14 spirals. We use two measures of rotational velocity. One is derived directly from observed spatially-resolved stellar kinematics and the other from the circular velocities of mass models that include a dark halo and whose parameters are constrained by detailed kinematic modelling. Contrary to the naive expectations of theories of S0 formation, we find no significant difference between the Tully-Fisher relations of the two samples when plotted as functions of both brightness and stellar mass.
The space density distribution of galaxies in the absolute magnitude - rotation velocity plane: a volume-complete Tully-Fisher relation from CALIFA stellar kinematics
We explore the Baryonic Tully-Fisher Relation in the Local Group. Rotationally supported Local Group galaxies adhere precisely to the relation defined by more distant galaxies. For pressure supported dwarf galaxies, we determine the scaling factor $β_c$ that relates their observed velocity dispersion to the equivalent circular velocity of rotationally supported galaxies of the same mass such that $V_o = β_c σ_*$. For a typical mass-to-light ratio $Υ_* = 2\;\mathrm{M}_{\odot}/\mathrm{L}_{\odot}$ in the $V$-band, we find that $β_c = 2$. More generally, $\log β_c = 0.25 \log Υ_* +0.226$. This pro…
We present a novel 2D flux density model for observed HI emission lines combined with a Bayesian stacking technique to measure the baryonic Tully-Fisher relation below the nominal detection threshold. We simulate a galaxy catalogue, which includes HI lines described either with Gaussian or busy function profiles, and HI data cubes with a range of noise and survey areas similar to the MeerKAT International Giga-Hertz Tiered Extragalactic Exploration (MIGHTEE) survey. With prior knowledge of redshifts, stellar masses and inclinations of spiral galaxies, we find that our model can reconstruct the…
The scatter, residual correlations and curvature of the SPARC baryonic Tully-Fisher relation
在最近的工作中，Lelli et al.（2016）认为，LCDM星系样本的重子Tully-Fisher关系（BTFR）的紧密性，以及其残差与有效半径的相关性的弱点，对LCDM宇宙学提出了挑战。在这封信中，我们计算的统计意义，这些结果的框架中的晕丰度匹配，这强加了一个典型的星系晕连接。考虑到样本方差之间的类SPARC实现的父晕人口，我们发现在预测的BTFR的分散是3.6西格玛太高，但其残差与星系大小的相关性是自然弱。此外，我们发现丰度匹配产生BTFR曲率在3.0西格玛不同意的数据，和一小部分的星系与非平坦的旋转曲线略大于观察。
The Baryonic Tully-Fisher Relation (BTFR) links baryonic mass of rotationally supported galaxies to their flat disk velocities. A popular form of the BTFR linked to MOND is based on an empirically determined characteristic acceleration, a0 that serves as the constant of proportionality. In this work, we propose an alternative, parametric form of the BTFR employing individual galactic properties from the SPARC galaxy database. Based on this data we find that a precise mass-velocity correlation is possible taking into account galactic disk radius and two dynamical related properties; mass discre…
A Transition Mass in the Local Tully-Fisher Relation
本文研究了红移为0.1 $<$ z $<$ 0.375的发射线星系的形态盲选的恒星质量Tully-Fisher关系（TFR，恒星质量与自转速度）。Kinetics（$σ_g$，V $_{rot}$）是从凯克/DEIMOS光谱中的发射线测量的，定量形态是从V和I波段哈勃图像测量的。我们在TFR中发现了一个过渡恒星质量，$\log$ M $_*$ = 9.5 M $_{\odot}$ .在这个质量以上，几乎所有的星系都是旋转主导的，根据定量形态学，平均来说更像是盘状的，并且位于相对较紧的TFR上。低于这个质量，TFR有显着的分散到低旋转速度和星系可以是旋转为主的磁盘上的TFR或不对称或紧凑的星系散射。我们把这个过渡质量称为“盘形成质量”，M $_{\mathrm{df}}$，因为在它上面所有的恒星形成星系都形成盘（除了少数主要合并和高度恒星形成系统），而在它下面的星系可能会或可能不会形成盘。
We present SAMI-HI, a survey of the atomic hydrogen content of 296 galaxies with integral field spectroscopy available from the SAMI Galaxy Survey. The sample spans nearly 4 dex in stellar mass ($M_\star = 10^{7.4}-10^{11.1}~ \rm M_\odot$), redshift $z<0.06$, and includes new Arecibo observations of 153 galaxies, for which we release catalogues and HI spectra. We use these data to compare the rotational velocities obtained from optical and radio observations and to show how systematic differences affect the slope and scatter of the stellar-mass and baryonic Tully-Fisher relations. Specifically…
We present stellar population models to calculate the mass-to-light ratio ($Υ_*$) based on galaxy's colors ranging from $GALEX$ FUV to Spitzer IRAC1 at 3.6$μ$m. We present a new composite bulge+disk $Υ_*$ model that considers the varying contribution from bulges and disks based on their optical and near-IR colors. Using these colors, we build plausible star formation histories and chemical enrichment scenarios based on the star formation rate-stellar mass and mass-metallicity correlations for star-forming galaxies. The most accurate prescription is to use the actual colors for the bulge and di…
We investigate the Baryonic Tully-Fisher Relation (BTFR) in the $(100\,h^{-1}{\rm Mpc})^3$ Simba hydrodynamical galaxy formation simulation together with a higher-resolution $(25\,h^{-1}{\rm Mpc})^3$ Simba run, for over $10,000$ disk-dominated, HI-rich galaxies. We generate simulated galaxy rotation curves from the mass distribution, which we show yields similar results to using the gas rotational velocities. From this we measure the galaxy rotation velocity $V_{\rm circ}$ using four metrics: $V_{\rm max}, V_{\rm flat}, V_{2R_e},$ and $V_{\rm polyex}$. We compare the predicted BTFR to the SPAR…
We present Tully-Fisher distances for 24 AGN host galaxies with black hole mass ($M_\textrm{BH}$) measurements from reverberation mapping, as well as the first calibration of the $V-$band Tully-Fisher relation. Combining our measurements of HI 21cm emission with $HST$ and ground-based optical and near-infrared images allows multiple distance measurements for 19 galaxies and single measurements for the remaining 5. Separation of the nucleus from its host galaxy via surface brightness decomposition yields galaxy-only luminosities, thus allowing measurements of the distance moduli free of contami…
We explore the use of the baryonic Tully-Fisher relation (bTFR) as a new distance indicator. Advances in near-IR imaging and stellar population models, plus precise rotation curves, have reduced the scatter in the bTFR such that distance is the dominant source of uncertainty. Using 50 galaxies with accurate distances from Cepheids or tip magnitude of the red giant branch, we calibrate the bTFR on a scale independent of $H_o$. We then apply this calibrated bTFR to 95 independent galaxies from the SPARC sample, using CosmicFlows-3 velocities, to deduce the local value of $H_o$. We find $H_o$ = 7…
We compare an observed Baryonic Tully-Fisher Relation (BTFR) from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) and HI-MaNGA surveys to a simulated BTFR from the cosmological magnetohydrodynamical simulation IllustrisTNG. To do so, we calibrate the BTFR of the local universe using 377 galaxies from the MaNGA and HI-MaNGA surveys, and perform mock 21 cm observations of matching galaxies from IllustrisTNG. The mock observations are used to ensure that the comparison with the observed galaxies is fair since it has identical measurement algorithms, observational limitations, bias…
A break in the high-redshift stellar mass Tully-Fisher relation
本文研究了恒星质量与气体速度色散积分之间的Tully-Fisher关系（TFR），该关系由运动学估计量S_0.5量化，由星系光谱中0<z<5的强发射线测量。我们将光度选择的星系（“高光度样本”）与以其他方式选择的星系（“低光度样本"）结合起来，以覆盖几乎跨越五个数量级的恒星质量范围：7.0 < log M* < 11.5。我们发现，对数幂律斜率和归一化的TFR是独立的红移到z~3。TFR的离散度为<0.5 dex such that the gas velocity dispersion can be used as a proxy for the stellar mass of a galaxy independently of its redshift. At z>3，离散度增大，相关性不明显。在z<3时，高光度样品的斜率为1.5 $\pm$ 0.2，而低光度样品的斜率为2.9 $\pm$ 0.3，这表明TFR发生了转换。合并后的样本与TFR在M*~10 $^{10}$ M $_{\odot}$的特征恒星质量标度处的突变很好地拟合，没有显著的演化到z~3。我们证明，TFR在低质量端出现斜率更陡的突变是具有质量依赖性恒星与晕质量比的星系模型的自然结果。
The WALLABY pilot survey has been conducted using the Australian SKA Pathfinder (ASKAP). The integrated 21-cm HI line spectra are formed in a very different manner compared to usual single-dish spectra Tully-Fisher measurements. It is thus extremely important to ensure that slight differences (e.g. biases due to missing flux) are quantified and understood in order to maximise the use of the large amount of data becoming available soon. This article is based on four fields for which the data are scientifically interesting by themselves. The pilot data discussed here consist of 614 galaxy spectr…
A recent work (arXiv:2104.14481) has found a statistically significant transition in the Baryonic Tully-Fisher relation (BTFR) using low redshift data ($z<0.1$), with the transitions occurring at about 9 and 17 Mpc. Motivated by this finding, we carry out a variant of this analysis by fitting the data to an augmented BTFR, where both the exponent as well as normalization constant vary as a function of distance. We find that both the exponent and normalization constant show only a marginal variation with distance, and are consistent with a constant value, to within $2σ$. We also checked to see …
2MTF - VII. 2MASS Tully-Fisher survey final data release: distances for 2,062 nearby spiral galaxies
我们提出了2 MASS塔利-费舍尔（2 MTF）调查的最终距离测量。最终的2 MTF目录包含2，062个邻近的旋涡星系，其宇宙微波背景的标架速度范围为600 km s $^{-1}$ $< cz < 10,000$ km s $^{-1}$，平均速度为4，805 km s $^{-1}$。本版本的主要更新是用较新的ALCARFA数据替换了一些存档HI数据。利用2 MTF模板关系，我们计算了所有2 MTF星系的距离和特有速度。在所有三个红外波段的线性距离测量的平均不确定度约为22%。2 MTF测量值与Cosmicflows-3汇编的距离吻合得很好，其中包含1，117个常见星系，包括28个SNIa距离测量值。使用从“3波段组合”2 MTF样本和$χ^2$最小化方法估计的距离，我们分别在$R_I = $ 20、30和40 $h^{-1}{\rm Mpc}$的深度处找到了$308 \pm 26$ km s $^{-1}$、$318 \pm 29$ km s $^{-1}$和$286 \pm 25$ km s $^{-1}$的最佳拟合整体流振幅，这与$Λ$ CDM模型和先前使用不同估计技术和初步目录的2 MTF结果一致。
