A Bayesian Approach to Locating the Red Giant Branch Tip Magnitude (Part II); Distances to the Satellites of M31
Anthony R. Conn, Rodrigo A. Ibata, Geraint F. Lewis, Quentin A. Parker, Daniel B. Zucker, Nicolas F. Martin, Alan W. McConnachie, Mike J. Irwin, Nial Tanvir, Ma… 展开作者
Anthony R. Conn, Rodrigo A. Ibata, Geraint F. Lewis, Quentin A. Parker, Daniel B. Zucker, Nicolas F. Martin, Alan W. McConnachie, Mike J. Irwin, Nial Tanvir, Mark A. Fardal, Annette M. N. Ferguson, Scott C. Chapman, David Valls-Gabaud
In `A Bayesian Approach to Locating the Red Giant Branch Tip Magnitude (PART I),' a new technique was introduced for obtaining distances using the TRGB standard candle. Here we describe a useful complement to the technique with the potential to further reduce the uncertainty in our distance measurements by incorporating a matched-filter weighting scheme into the model likelihood calculations. In this scheme, stars are weighted according to their probability of being true object members. We then re-test our modified algorithm using random-realization artificial data to verify the validity of the generated posterior probability distributions (PPDs) and proceed to apply the algorithm to the satellite system of M31, culminating in a 3D view of the system. Further to the distributions thus obtained, we apply a satellite-specific prior on the satellite distances to weight the resulting distance posterior distributions, based on the halo density profile. Thus in a single publication, using a single method, a comprehensive coverage of the distances to the companion galaxies of M31 is presented, encompassing the dwarf spheroidals Andromedas I - III, V, IX-XXVII and XXX along with NGC147, NGC 185, M33 and M31 itself. Of these, the distances to Andromeda XXIV - XXVII and Andromeda XXX have never before been derived using the TRGB. Object distances are determined from high-resolution tip magnitude posterior distributions generated using the Markov Chain Monte Carlo (MCMC) technique and associated sampling of these distributions to take into account uncertainties in foreground extinction and the absolute magnitude of the TRGB as well as photometric errors. The distance PPDs obtained for each object both with, and without the aforementioned prior are made available to the reader in tabular form...
Astrophysical Distance Scale VII: A Self-Consistent, Multi-Wavelength Calibration of the Slopes and Relative Zero Points for the Run of Luminosity with Color of Stars Defining the Tip of the Red Giant Branch
Comparing Tip of the Red Giant Branch Distance Scales: An Independent Reduction of the Carnegie-Chicago Hubble Program and the Value of the Hubble Constant
The Parallax of Omega Centauri Measured from Gaia EDR3 and a Direct, Geometric Calibration of the Tip of the Red Giant Branch and the Hubble Constant
我们使用来自欧空局盖亚任务早期数据发布3（EDR3）的数据来测量$ω$ Cen的三角视差，这是银河系中最大的球状星团的第一个高精度视差测量。我们使用来自EDR3的位置和高质量自行数据的组合来识别超过100，000个集群成员，其中67，000个在EDR3视差最佳校准的幅度和颜色范围内。我们发现估计视差是强大的，表现出良好的控制系统内的颜色星等图的集群。我们发现一个视差的集群$0.191\pm0.001$（统计）$\pm0.004$（系统）mas（2.2\%的总不确定性）对应的距离为$5.24\pm0.11$千秒差距。$ω$ Cen的视差提供了一个独特的机会，可以直接和几何校准红巨星分支尖端（TRGB）的光度，因为它是唯一一个具有足够质量的星团，可以提供足够的红巨星，比尖端低100个一等，以精确，无模型测量尖端。结合预先存在的和最广泛使用的尖端和前景银河系消光的测量，我们发现$M_{I,TRGB}=-3.97\pm0.06$的蓝色边缘的$I$带光度的mag。使用从$ω$ Cen的盖亚EDR3视差校准的TRGB光度来校准SNIa的光度，得到哈勃常数的值为$H_0=72.1\pm2.0$ km s $^{-1}$ Mpc $^{-1}$。我们使数据的恒星在$ω$岑可电子和鼓励独立分析的结果在这里。
The Carnegie-Chicago Hubble Program. II. The Distance to IC 1613: The Tip of the Red Giant Branch and RR Lyrae Period-Luminosity Relations
IC 1613是本星系群中一个孤立的矮星系。低前景和内部消光，低金属丰度和低拥挤使其成为校准局部距离阶梯的宝贵测试平台。我们提出了新的，高保真的距离估计IC 1613通过其尖端的红巨星分支（TRGB）和它的RR天琴座（RRL）变量的一部分，芝加哥哈勃计划，寻求一个替代的本地路线\ho使用第二星族恒星。我们已经测量了TRGB星等I=20.35+/-0.01（统计）+/-0.01（系统）使用麦哲伦巴德望远镜上的IMACS相机获得的宽视场观测。我们进一步构建了光学和近红外RRL光变曲线使用档案BI和新的H波段观测ACS/WFC和WFC 3/IR仪器搭载哈勃太空望远镜（HST）。在未来的盖亚数据发布之前，我们通过大麦云云和银河系RRL零点通过HST视差设置TRGB光度的临时值。我们发现对应的真实距离模量μ（TRGB）=24.30+/-0.03（统计）+/-0.05（系统）和μ（RRL）=24.28+/-0.04（统计+系统）。我们比较了我们的结果，最近发表的IC 1613的身体，并发现没有统计学上的显着差异，从恒星的人口I和II之间的距离。
A Maximum Likelihood Calibration of the Tip of the Red Giant Branch Luminosity from High Latitude Field Giants using Gaia Early Data Release 3 Parallaxes
在$I$波段对红巨星分支（TRGB）尖端的校准在确定哈勃常数中有着直接的作用，由于直接和间接估计值之间的差异，哈勃常数是最近引起人们兴趣的一个课题。我们提出了一个极大似然（ML）的方法，旨在获得一个独立的校准TRGB的亮度使用$Gaia$从早期的数据发布3（EDR3）银河系场巨人在高银河系纬度。我们采用简单的参数化的银河系恒星的光度函数和密度法和优化的可能性，观察到的样本作为这些参数的函数。使用参数来部分地约束从其他星系类似的银河系的高质量TRGB数据的光度函数，我们发现值的TRGB幅度的$ M_I^{TRGB} = -3.91 \pm 0.05 $（统计）$ \pm 0.09 $（系统）马格，其中系统的不确定性涵盖了我们的银河系样本和参考星系中发现的形状参数的范围。虽然APASS Data Release 9全天空测光不足以对银河系光度函数的形状提供可靠的约束，但我们估计$Gaia$ Data Release 3（2022年中期）的测光将允许对形状进行更好的约束，并将尖端的统计不确定性降低3倍。随着$Gaia$改进视差测量的预期发布，从Giants现场校准TRGB光度的方法预计将达到$\sim$ 0.01等的不确定性，这是朝着基于TRGB精确确定哈勃常数迈出的重要一步。
Consistent Calibration of the Tip of the Red Giant Branch in the Large Magellanic Cloud on the Hubble Space Telescope Photometric System and a Re-determination of the Hubble Constant
The Astrophysical Distance Scale III: Distance to the Local Group Galaxy WLM using Multi-Wavelength Observations of the Tip of the Red Giant Branch, Cepheids, and JAGB Stars
A Uniform Type Ia Supernova Distance Ladder with the Zwicky Transient Facility: Absolute Calibration Based on the Tip of the Red Giant Branch (TRGB) Method
Tip of the Red Giant Branch Distances to NGC 1316, NGC 1380, NGC 1404, & NGC 4457: A Pilot Study of a Parallel Distance Ladder Using Type Ia Supernovae in Early-Type Host Galaxies
本研究利用红巨星支尖距离校准大质量宁静早型星系中的Ia型超新星，构建平行距离阶梯，测得哈勃常数为75.3±2.9 km s⁻¹ Mpc⁻¹，验证了属性匹配子样本在宇宙学研究中的应用潜力。
