论文标题
天体物理距离II。 JAGB方法的应用：附近的星系样本
Astrophysical Distance Scale II. Application of the JAGB Method: A Nearby Galaxy Sample
论文作者
论文摘要
我们应用了Madore \＆Freedman（2020）最近引入的近红外J区渐近分支（JAGB）方法，以测量到附近14个星系的距离至4 MPC。我们将到LMC和SMC的几何脱落（DEB）距离用作独立的零点校准器。 We find excellent agreement with previously published distances based on the Tip of the Red Giant Branch (TRGB): the JAGB distance determinations (including the LMC and SMC) agree in the mean to within Delta(JAGB-TRGB) = +0.025 +/- 0.013 mag, just over 1%, where the TRGB I-band zero point is M_I = ~-4.05 mag.通过进一步的开发和测试，JAGB方法具有对IA型超新星的独立校准，尤其是JWST。可以比较弱的trgb恒星检测到JAGB恒星（具有M_J = -6.20 mag），从而使校准星系数量更多以确定HO。与TRGB和CEPHEID一起，JAGB恒星可以理论理解并进一步完善经验校准。初步测试几乎没有对jagb幅度的依赖性，而父级的金属性。这些早期的结果表明，JAGB方法在为当地宇宙中的星系提供高精度距离具有巨大的希望，这些距离独立于Leavitt Law和/或TRGB方法中的距离。与可能使用MIRA变量相比，它具有许多可证明的优势。
We apply the near-infrared J-region Asymptotic Giant Branch (JAGB) method, recently introduced by Madore \& Freedman (2020), to measure the distances to 14 nearby galaxies out to 4 Mpc. We use the geometric detached eclipsing binary (DEB) distances to the LMC and SMC as independent zero-point calibrators. We find excellent agreement with previously published distances based on the Tip of the Red Giant Branch (TRGB): the JAGB distance determinations (including the LMC and SMC) agree in the mean to within Delta(JAGB-TRGB) = +0.025 +/- 0.013 mag, just over 1%, where the TRGB I-band zero point is M_I = ~-4.05 mag. With further development and testing, the JAGB method has the potential to provide an independent calibration of Type Ia supernovae, especially with JWST. The JAGB stars (with M_J = -6.20 mag) can be detected farther than the fainter TRGB stars, allowing greater numbers of calibrating galaxies for the determination of Ho. Along with the TRGB and Cepheids, JAGB stars are amenable to theoretical understanding and further refined empirical calibration. A preliminary test shows little dependence, if any, of the JAGB magnitude with metallicity of the parent galaxy. These early results suggest that the JAGB method has considerable promise for providing high-precision distances to galaxies in the local universe that are independent of distances derived from the Leavitt Law and/or the TRGB method; and it has numerous and demonstrable advantages over the possible use of Mira variables.
