The Sonora Substellar Atmosphere Models VI. Red Diamondback: Extending Diamondback with SPHINX for Brown Dwarf Early Evolution

OVERVIEW V2 UPDATE: The evolution code's atmospheric boundary condition now has a "weighted transition region" across Teff 2000 - 2400 K (where both the original Sonora Diamondback and new SPHINX grids have modeled atmospheres). This differs from V1, where the atmospheric boundary condition used Sonora Diamondback atmospheres at Teff < 2400 K, and SPHINX atmospheres at Teff >= 2400 K. The V2 atmospheric boundary condition and the regions where one or both of the atmosphere grids are used can be seen in Fig. 2 of the arXiv pre-print, and are described further in Section 2.2. ----- Presented here are models for non-irradiated, substellar mass objects spanning ages from 1 Myr to 15 Gyr, which belong to the Sonora model series. The models are described in Davis et al. 2025. The files inlcuded here are thermal evolution tracks ("evolution") and synthetic photometry ("photometry"). This particular set of evolution tracks and photometry, which we name Sonora "Red Diamondback", supersedes the original Sonora Diamondback (Morley et al. 2024) evolution tracks due to the inclusion of high Teff atmospheric boundary conditions from the SPHINX M dwarf Spectral Grid. This addition to the atmospheric boundary condition allows for an accurate treatment of evolution at early ages. The evolution models presented here are computed for objects with 3.0 ≤ log g (cgs) ≤ 5.5 and 900 ≤ Teff ≤ 4000K (steps in Teff are 100 K and steps in log g are 0.25.) Models are provided for [M/H] = -0.5, 0.0, and +0.5 and "rainout" chemical equilibrium. For the convenience of having a rectangular table in (Teff, gravity) space, the atmospheric models used as boundary conditions in the evolution models presented here were calculated in regimes that are not reached by the evolution, such as very high gravity and very low Teff. Refer to the evolution tables to identify combinations of Teff and log g outside the bounds covered by the evolution. For other Sonora models that cover different temperature, gravities, metallicities, and disequilibrium chemistry, see Sonora Bobcat, Sonora Cholla, and Sonora Elf Owl. EVOLUTION Evolution tables include each of the three metallicities (+0.5, +0.0, -0.5) and span ages from 1 Myr to 15 Gyr for objects greater than the hydrogen burning minimum mass down to half a Jupiter mass. PHOTOMETRY We include tables of absolute magnitudes in a number of photometric systems commonly used in brown dwarf and exoplanet research (MKO, WISE, Spitzer IRAC, etc). Magnitudes are computed on the Vega system. CREDITS If you use these tables in your research, please cite Davis et al. submitted. ([LINK HERE])OVERVIEW V2版本更新：演化代码的大气边界条件现在在有效温度(Teff) 2000~2400 K区间增设了加权过渡区，该区间内原始索诺拉菱纹背(Sonora Diamondback)与新型SPHINX网格均已完成大气建模。这与V1版本不同：V1版本的大气边界条件在Teff < 2400 K时采用索诺拉菱纹背大气，在Teff ≥2400 K时采用SPHINX大气。V2版本的大气边界条件以及单/双大气网格的使用区域可参阅arXiv预印本的图2，相关细节将在2.2节进一步阐述。 ----- 本次发布的模型属于索诺拉(Sonora)模型系列，涵盖年龄从1 Myr（百万年）至15 Gyr（十亿年）的非辐照亚恒星质量天体，相关模型已在Davis等人2025年的研究中详细描述。本次提供的文件包含热演化轨迹（"evolution"）与合成测光（"photometry"）两类数据。 本套演化轨迹与合成测光数据集被命名为索诺拉“红菱纹背”(Sonora "Red Diamondback")，由于纳入了SPHINX M矮星光谱网格的高Teff大气边界条件，因此替代了原始的索诺拉菱纹背（Sonora Diamondback，Morley等人2024年）演化轨迹。这一大气边界条件的新增内容可实现对早期天体演化的精确处理。本次发布的演化模型针对满足3.0 ≤ 表面重力对数(log g, 厘米克秒制) ≤5.5、900 ≤ Teff ≤4000 K的天体计算得到，其中Teff步长为100 K，log g步长为0.25。模型的金属丰度[M/H]取-0.5、0.0与+0.5，并采用“雨落”化学平衡假设。为了在Teff-引力空间中构建规整的表格，本演化模型所使用的大气边界条件，其计算参数范围超出了演化模型本身覆盖的区间，例如极高引力与极低Teff的情况。请参考演化表格以识别超出演化覆盖范围的Teff与log g组合。如需其他覆盖不同温度、引力、金属丰度与非平衡化学的索诺拉模型，请参阅Sonora Bobcat、Sonora Cholla与Sonora Elf Owl。 EVOLUTION 演化表格包含全部三种金属丰度（+0.5、+0.0、-0.5），覆盖质量介于氢燃烧最小质量至0.5倍木星质量的天体，年龄跨度为1 Myr至15 Gyr。 PHOTOMETRY 本次提供了棕矮星与系外行星研究中常用的多款测光系统的绝对星等表格，包括MKO、WISE、斯皮策(Spitzer) IRAC等。星等计算基于Vega系统。 CREDITS 若您在研究中使用本数据集表格，请引用Davis等人已投稿的研究（[链接待填]）。