We present angular diameters for 42 luminosity class I stars and 32 luminosity class II stars that have been interferometrically determined with the Palomar Testbed Interferometer. Derived values of radius and effective temperature are established for these objects, and an empirical calibration of these parameters for supergiants will be presented as a functions of spectral type and colors. For the effective temperature versus $(V-K)_0$ color, we find an empirical calibration with a median deviation of $ΔT = 70$K in the range of $0.7 < (V-K)_0 < 5.1$ for LC I stars; for LC II, the median deviation is $ΔT = 120$K from $0.4 < (V-K)_0 < 4.3$. Effective temperature as a function of spectral type is also calibrated from these data, but shows significantly more scatter than the $T_{\rm EFF}$ versus $(V-K)_0$ relationship. No deviation of $T_{\rm EFF}$ versus spectral type is seen for these high luminosity objects relative to luminosity class II giants. Directly determined diameters range up to $400 R_\odot$, though are limited by poor distance determinations, which dominate the error estimates. These temperature and radii measures reflect a direct calibration of these parameters for supergiants from empirical means.
Atmospheric dynamics of red supergiant stars and Interferometry
我们开发了一个3D纯LTE辐射转移程序，从用CO5 BOLD进行的红超巨星（RSG）辐射流体动力学（RHD）模拟中推导出RSG的观测值，重点是小尺度结构（Freytag et al. 2002）。我们表明，对流相关的表面结构与今天的干涉仪是可观察的。此外，RHD模拟是一个很大的改进参数模型的干涉观测的解释。
The vicinity of the galactic supergiant B[e] star CPD -57 2874 from near- and mid-IR long baseline spectro-interferometry with the VLTI (AMBER and MIDI)
Bispectrum speckle interferometry observations and radiative transfer modelling of the red supergiant NML Cyg: Multiple dust-shell structures evidencing previous superwind phases
UV Observations of the Powering Source of the Supergiant Shell in IC2574
对附近矮不规则星系IC 2574中包含超巨星HI壳的区域的多波段分析提供了中央星团、周围膨胀的HI壳和HI壳边缘的次级恒星形成点之间存在因果关系的证据。远紫外（FUV，1521 A），光学宽带，H-α，X射线和HI形态的比较表明，该地区是在一个吉祥的时刻，恒星形成的中央星团触发。HI壳层、中央星团和边缘恒星形成区的衍生性质支持这一假设：HI壳层的运动学年龄<1400万年，与FUV观测得出的中央星团的年龄一致（近似1100万年）。根据FUV测光和由此导出的星团年龄，估算了SN和中央星团星风输入的机械能为4.1 x 10^52尔格，大约是HI壳层动能的几倍。根据HI观测结果（使用Chevalier的数值模型）以"标准"方式得出的生成HI壳层所需的能量输入为2.6 x 10^53 erg，这几乎比根据FUV数据得出的估计能量输入高出一个数量级。鉴于压倒性的观测证据表明，中央集群是负责扩大HI壳，这种差异表明，所需的能量输入是高估了使用“标准”的方法。这也许可以解释为什么到目前为止，在巨大的HI黑洞中寻找残余星团的其他一些搜索都没有成功。我们的观测还表明，星团确实能够创造超巨星HI壳，即使在大的银河系中心半径，一个方案，最近受到质疑的一些作者。
Quantitative Spectroscopy of 24 A supergiants in the Sculptor galaxy NGC 300: Flux weighted gravity luminosity relationship, metallicity and metallicity gradient
First VLTI infrared spectro-interferometry on GCIRS 7 - Characterizing the prime reference source for Galactic center observations at highest angular resolution
