A Generalist, Automated ALFALFA Baryonic Tully–Fisher Relation
A Generalist, Automated ALFALFA Baryonic Tully–Fisher Relation
复制标题
DOI：
10.3847/1538-4357/accb53
复制
发表时间：
2022-12
期刊：
影响因子：
--
通讯作者：
C. Ball;M. Haynes;Michael G. Jones;Bo Peng;A. Durbala;R. Koopmann;J. Ribaudo;A. O’Donoghue
中科院分区：
文献类型：
--
作者：
C. Ball;M. Haynes;Michael G. Jones;Bo Peng;A. Durbala;R. Koopmann;J. Ribaudo;A. O’Donoghue
重子Tully-Fisher关系（BTFR）在星系演化中作为星系晕连接的测试床，在观测宇宙学中作为与红移无关的次级距离指标。这项分析利用了31，000多个星系Arecibo Legacy Fast ALFA（Arecibo L-band Feed Array）Survey（ALCAFA）样本，该样本提供了本地宇宙中大量含气星系的红移，速度宽度和H i含量，以拟合和测试广泛的本地宇宙BTFR。的基准关系是适合使用3000个星系的子样本的ALCAFA，并显示出与完整的样本是一致的。该BTFR旨在尽可能包括ALP4FA和可比样品。通过自动化方法测量的速度宽度和从调查数据中提取的M B代理可以均匀有效地测量其他样品，使这种分析具有广泛的适用性。我们还研究了样本人口统计学在确定最佳拟合关系中的作用。我们发现，最佳拟合关系的变化显着的样品质量范围和二阶的质量采样，气体分数，不同的恒星质量和速度宽度测量的变化。我们使用了一个具有人口统计学特征的ALCAFA子集，反映了完整样本，以测量3.30 ± 0.06的稳健BTFR斜率。我们应用这种关系和估计源距离，发现一般协议与流模型的距离以及平均距离的不确定性为0.17 dex的完整的ALCARFA样本。我们证明了这些距离估计的实用性，将它们应用到室女座附近的源样本，恢复与以前的工作一致的下降签名。
The baryonic Tully–Fisher relation (BTFR) has applications in galaxy evolution as a test bed for the galaxy–halo connection and in observational cosmology as a redshift-independent secondary distance indicator. This analysis leverages the 31,000+ galaxy Arecibo Legacy Fast ALFA (Arecibo L-band Feed Array) Survey (ALFALFA) sample—which provides redshifts, velocity widths, and H i content for a large number of gas-bearing galaxies in the local universe—to fit and test an extensive local universe BTFR. The fiducial relation is fit using a 3000-galaxy subsample of ALFALFA, and is shown to be consistent with the full sample. This BTFR is designed to be as inclusive of ALFALFA and comparable samples as possible. Velocity widths measured via an automated method and M b proxies extracted from survey data can be uniformly and efficiently measured for other samples, giving this analysis broad applicability. We also investigate the role of sample demographics in determining the best-fit relation. We find that the best-fit relations are changed significantly by changes to the sample mass range and to second order by changes to mass sampling, gas fraction, different stellar mass and velocity width measurements. We use a subset of ALFALFA with demographics that reflect the full sample to measure a robust BTFR slope of 3.30 ± 0.06. We apply this relation and estimate source distances, finding general agreement with flow-model distances as well as average distance uncertainties of ∼0.17 dex for the full ALFALFA sample. We demonstrate the utility of these distance estimates by applying them to a sample of sources in the Virgo vicinity, recovering signatures of infall consistent with previous work.