MIGHTEE-HI: The baryonic Tully-Fisher relation over the last billion years
Anastasia A. Ponomareva, Wanga Mulaudzi, Natasha Maddox, Bradley S. Frank, Matt J. Jarvis, Enrico M. Di Teodoro, Marcin Glowacki, Renée C. Kraan-Korteweg, Tom A… 展开作者
Anastasia A. Ponomareva, Wanga Mulaudzi, Natasha Maddox, Bradley S. Frank, Matt J. Jarvis, Enrico M. Di Teodoro, Marcin Glowacki, Renée C. Kraan-Korteweg, Tom A. Oosterloo, Elizabeth A. K. Adams, Hengxing Pan, Isabella Prandoni, Sambatriniaina H. A. Rajohnson, Francesco Sinigaglia, Nathan J. Adams, Ian Heywood, Rebecca A. A. Bowler, Peter W. Hatfield, Jordan D. Collier, Srikrishna Sekhar
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11 pages, 6 figures, accepted for publication in MNRAS
Using a sample of 67 galaxies from the MIGHTEE Survey Early Science data we study the HI-based baryonic Tully-Fisher relation (bTFr), covering a period of $\sim$one billion years ($0 \leq z \leq 0.081 $). We consider the bTFr based on two different rotational velocity measures: the width of the global HI profile and $\rm V_{out}$, measured as the outermost rotational velocity from the resolved HI rotation curves. Both relations exhibit very low intrinsic scatter orthogonal to the best-fit relation ($σ_{\perp}=0.07\pm0.01$), comparable to the SPARC sample at $z \simeq 0$. The slopes of the relations are similar and consistent with the $ z \simeq 0$ studies ($3.66^{+0.35}_{-0.29}$ for $\rm W_{50}$ and $3.47^{+0.37}_{-0.30}$ for $\rm V_{out}$). We find no evidence that the bTFr has evolved over the last billion years, and all galaxies in our sample are consistent with the same relation independent of redshift and the rotational velocity measure. Our results set up a reference for all future studies of the HI-based bTFr as a function of redshift that will be conducted with the ongoing deep SKA pathfinders surveys.
Most rotationally-supported galaxies strictly follow the Baryonic Tully-Fisher Relation (BFTR) linking circular velocity with baryon content. This firmly established empirical relationship is currently thought to have origins in either modified gravity or dark matter halo effects. In this work, we construct a physically-based version of the BFTR founded on known scaling relations, disk dynamics (acceleration, jerk and snap) that also reveals the foundational elements responsible for this phenomenology. We employ the Milky Way galaxy as an exemplar to quantitatively compare the two leading theo…
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…
Galaxies covering several orders of magnitude in stellar mass and a variety of Hubble types have been shown to follow the "Radial Acceleration Relation" (RAR), a relationship between $g_{\rm obs}$, the observed circular acceleration of the galaxy, and $g_{\rm bar}$, the acceleration due to the total baryonic mass of the galaxy. For accelerations above $10^{10}~{\rm m \, s}^{-2}$, $g_{\rm obs}$ traces $g_{\rm bar}$, asymptoting to the 1:1 line. Below this scale, there is a break in the relation such that $\rm g_{\rm obs} \sim g_{\rm bar}^{1/2}$. We show that the RAR slope, scatter and the accel…
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…
In this paper we investigate the statistical properties of the Baryonic Tully-Fisher relation (BTFr) for a sample of 32 galaxies with accurate distances based on Cepheids and/or TRGB stars. We make use of homogeneously analysed photometry in 18 bands ranging from the FUV to 160 $μ$m, allowing us to investigate the effect of the inferred stellar mass-to-light ratio $Υ_{*}$ on the statistical properties of the BTFr. Stellar masses of our sample galaxies are derived with four different methods based on full SED-fitting, studies of stellar dynamics, near-infrared colours, and the assumption of the…
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 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 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…
MIGHTEE HI observations of low surface brightness and ultra-diffuse galaxies in the XMM-LSS field
ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire（赫特福德大学物理、天文与数学学院天体物理研究中心）；Astrophysics, Department of Physics, University of Oxford（牛津大学物理系天体物理学）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；STFC UK Astronomy Technology Centre, Royal Observatory, Edinburgh（爱丁堡皇家望远镜标准设备中心）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）
The interstellar gas in spiral galaxies can constitute a significant fraction of the baryon mass and it has been demonstrated that the sum of stellar and gas components correlates well with the kinematic signature of the total mass content, the widths of HI line profiles. The correlation of baryonic mass with HI line widths is used here to obtain distances for 9984 galaxies extending to ~0.05c. The sample is HI flux limited and a correction is required to account for an HI selection bias. The absolute scale is established by 64 galaxies with known distances from studies of Cepheid variables an…
The ratio of baryonic-to-dark matter in present-day galaxies constrains galaxy formation theories and can be determined empirically via the baryonic Tully-Fisher relation (BTFR), which compares a galaxy's baryonic mass (Mbary) to its maximum rotation velocity (Vmax). The BTFR is well-determined at Mbary >10^8 Msun, but poorly constrained at lower masses due to small samples and the challenges of measuring rotation velocities in this regime. For 25 galaxies with high-quality data and Mbary <~10^8 Msun, we estimate Mbary from infrared and HI observations and Vmax from the HI gas rotation. Many o…
The baryonic Tully-Fisher relation (BTFR) is an important tool for constraining galaxy evolution models. As 21-cm HI emission studies have been largely restricted to low redshifts, the redshift evolution of the BTFR is less studied. The upcoming LADUMA survey (Looking At the Distant Universe with the MeerKAT Array) will address this. As preparation for LADUMA, we use the Simba hydrodynamical galaxy formation simulation from the Simba-hires (25 h$^{-1}$ Mpc)$^{3}$ run to generate rotational velocity measures from galaxy rotation curves ($V_{\rm flat}$) and HI spectral line profile widths ($W_{\…
We present HI-based B- and R-band Tully-Fisher relations (TFRs) and the Baryonic TFR (BTFR) at z=0.2 using direct HI detections from the Blind Ultra-Deep HI Environmental Survey (BUDHIES). Deep photometry from the Isaac Newton Telescope was used for 36 out of 166 HI sources, matching the quality criteria required for a robust TFR analysis. Two velocity definitions at 20% and 50% of the peak flux were measured from the global HI profiles and adopted as proxies for the circular velocities. We compare our results with an identically constructed z=0 TFR from the Ursa Major (UMa) association of gal…
A recent work (arXiv:2104.14481) has found a statistically significant transition in the Baryonic Tully-Fisher relation (BTFR) using low redshift data ($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 …
We study the gas kinematics traced by the 21-cm emission of a sample of six HI$-$rich low surface brightness galaxies classified as ultra-diffuse galaxies (UDGs). Using the 3D kinematic modelling code $\mathrm{^{3D}}$Barolo we derive robust circular velocities, revealing a startling feature: HI$-$rich UDGs are clear outliers from the baryonic Tully-Fisher relation, with circular velocities much lower than galaxies with similar baryonic mass. Notably, the baryon fraction of our UDG sample is consistent with the cosmological value: these UDGs are compatible with having no "missing baryons" withi…
MIGHTEE-HI: Mass Models and Dark Matter properties
University of Hertfordshire（赫特福德大学）；University of Oxford（牛津大学）；Leiden University（莱顿大学）；University of Edinburgh（爱丁堡大学）；University of Cape Town（开普敦大学）；University of Portsmouth（朴茨茅斯大学）；University of the Western Cape（西开普大学）
MIGHTEE-HI / LADUMA: Investigating the link between baryons and dynamics with 130 resolved HI-selected galaxies
University of Oxford（牛津大学）；University of the Western Cape（西开普大学）；University of Portsmouth（朴茨茅斯大学）；University of Hertfordshire（赫特福德大学）；University of Bristol（布里斯托大学）
FAST Ultra-Deep Survey: the baryonic Tully-Fisher relation in FUDS0 field
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；International Centre for Radio Astronomy Research (ICRAR), University of Western Australia（西澳大利亚大学国际射电天文学研究中心）；Department of Astronomy and Institute of Interdisciplinary Studies, Hunan Normal University（湖南师范大学天文学系及交叉科学研究院）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）
本研究基于 FAST 极深巡天先导天区 FUDS0 的星系，探究红移至 0.42 的重子 Tully-Fisher 关系，识别出两个成分，分析离群点起源，发现低红移区间无显著演化，完整巡天将提供更大样本以约束其演化。
We study the baryonic Tully-Fisher relation (BTFR) at z=0 using 153 galaxies from the SPARC sample. We consider different definitions of the characteristic velocity from HI and H-alpha rotation curves, as well as HI line-widths from single-dish observations. We reach the following results: (1) The tightest BTFR is given by the mean velocity along the flat part of the rotation curve. The orthogonal intrinsic scatter is extremely small (6%) and the best-fit slope is 3.85+/-0.09, but systematic uncertainties may drive the slope from 3.5 to 4.0. Other velocity definitions lead to BTFRs with system…
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 M_Ks = (-8.4+/-2.9) [log(W_50/sini)-2.5]+(-23.5 +/- 0.5), log (Mstar/Msu…
MIGHTEE-HI: The direct detection of neutral hydrogen in galaxies at $z>0.25$
University of Oxford（牛津大学）；University of the Western Cape（西开普敦大学）；Rhodes University（罗兹大学）；South African Radio Astronomy Observatory（南非射电天文观测台）；University of Hertfordshire（赫特福德大学）；Universiteit Gent（根特大学）；University of Bristol（布里斯托大学）；Queen’s University（女王大学）
