3.8-μm photometry during the secondary eclipse of the extrasolar planet HD 209458b

We report infrared photometry of the extrasolar planet HD 209458b during the time of secondary eclipse (planet passing behind the star). Observations were acquired during two secondary eclipses at the NASA Infrared Telescope Facility (IRTF) in 2003 September. We used a circular variable filter (1.5 per cent bandpass) centred at 3.8 μm to isolate the predicted flux peak of the planet at this wavelength. Residual telluric absorption and instrument variations were removed by offsetting the telescope to nearby bright comparison stars at a high temporal cadence. Our results give a secondary eclipse depth of 0.0013 ± 0.0011, not yet sufficient precision to detect the eclipse, whose expected depth is  ∼0.002 –0.003  . We here elucidate the current observational limitations to this technique, and discuss the approach needed to achieve detections of hot Jupiter secondary eclipses at 3.8 μm from the ground.     

中、强震前川滇块体遥感红外辐射异常分析——以宁蒗M5.7地震和鲁甸M6.5地震为例

许多研究表明中强地震前出现了红外辐射异常。近年来,川滇块体中、强地震频发,利用遥感数据对其红外辐射异常变化开展深入分析十分必要。结合13年MODIS/Terra遥感红外数据,采用空间距平分析法、辐射增强阈值面积指数法及辐射亮温均值低频时间序列法,对2004年4月—2017年6月红外亮温数据进行深入分析,研究川滇块体及周边构造断裂M≥5.5地震的震前异常信息。结果表明:(1)M≥6.0地震在震前3～6个月川滇块体会出现较为明显的红外辐射增强异常现象;(2)震前红外异常并非随机分布,而可能是受到相关块体的控制;(3)以宁蒗M5.7地震和鲁甸M6.5地震为例研究发现,震前辐射增强较高的小范围区域与震中位置存在一定关联。     

Lunar photometric properties at wavelengths 0.5-1.6 μm acquired by SELENE Spectral Profiler and their dependency on local albedo and latitudinal zones

The lunar photometric function, which describes the dependency of the observed radiance on the observation geometry, is used for photometric correction of lunar visible/near-infrared data. A precise photometric correction parameter set is crucial for many applications including mineral identification and reflectance map mosaics. We present, for the first time, spectrally continuous photometric correction parameters for both sides of the Moon for wavelengths in the range 0.5-1.6 μm and solar phase angles between 5° and 85°, derived from Kaguya (SELENE) Spectral Profiler (SP) data. Since the measured radiance also depends on the surface albedo, we developed a statistical method for selecting areas with relatively uniform albedos from a nearly 7000-orbit SP data set. Using the selected data set, we obtained empirical photometric correction parameter sets for three albedo groups (high, medium, and low). We did this because the photometric function depends on the albedo, especially at phase angles below about 20° for which the shadow hiding opposition effect is appreciable. We determined the parameters in 160 bands and discovered a small variation in the opposition effect due to the albedo variation of mafic mineral absorption. The consistency of the photometric correction was checked by comparing observations made at different times of the same area on the lunar surface. Variations in the spectra obtained were lower than 2%, except for the large phase angle data in mare. Lastly, we developed a correction method for low solar elevation data, which is required for high latitude regions. By investigating low solar elevation data, we introduced an additional correction method. We used the new photometric correction to generate a 1° mesh global lunar reflectance map cube in a wavelength range of 0.5-1.6 μm. Surprisingly, these maps reveal that high latitude (?75°) regions in both the north and south have much lower spectral continuum slopes (color ratio r_1547.7nm/r_752.8nm ? 1.8) than the low and medium latitude regions, which implies lower degrees of space weathering.     

The stellar populations within theρ Oph cloud cores

We have obtained infrared colors and limiting magnitudes from 1.25–4.8µm for a sample of 26 of the cm continuum radio sources located in the core of the Oph molecular cloud. Their colors demonstrate that the majority of the sources appear to be heavily reddened objects surrounded by circumstellar accretion disks. In these cases the radio emission most likely diagnoses accretion driven energetic outflow phenomena: either ionized winds or possibly synchrotron emission from shocked gas associated with stellar jets.     

卫星红外云图上台风中心定位技术研究和应用

利用红外卫星云图的灰度分布和对应亮温特征,系统地研究、归纳了基于红外卫星云图的台风中心定位方法和技术.对结构特征不同的台风云系,拟订了不同的定位方法.对各定位方法的算法和实现步骤进行优化和拓展后,将其转化成实际业务工作中可操作的一整套（共计7种）台风中心定位的业务系统.整套方法以人机交互为主,部分实现了全自动化.实践证明,无论是何种结构特征的台风云系,选择其中某种方法,都能较准确地定出台风中心.     

地物反射光谱对MODIS近红外波段水汽反演影响的模拟分析

在近红外辐射传输方程的基础上,利用近红外波段水汽的不同吸收属性,在MODTRAN的模拟下,深入分析了基于MODIS近红外数据的可降水汽反演算法,并着重讨论了地物反射光谱非线性在可降水汽反演中的影响。研究结果显示,当波段间反射率之比不等于1时,MODIS近红外波段反演水汽将存在较大偏差。同时,在地物光谱库基础上,计算了不同地物反射率比值,其分布表明,大部分地物波段反射率比值不等于1。研究表明,应用现有MODIS近红外波段水汽反演算法,如果不考虑地表反射率光谱变化的影响,由地表反射光谱造成的误差最大约为反射率比值与1偏差的15倍,同时,这一误差还与大气波段透过率之比有关。     

震前云下增温异常及其时段特征

利用卫星热红外图像资料做地震短临预报, 主要依据的是地表大气增温异常在卫星图像上的亮温反映。 但在阴云密布的天气条件下, 这种预报方法却受到了限制, 因为卫星无法探测到地面或水面是否有增温异常。 通过气象资料分析, 得知云层或其他气象条件引起的降温并不能改变震前地表温度增加的趋势。 某些地震之前虽然震中及其附近地区天空阴云密布, 地面增温幅度却可高达十几度。 云下增温曲线可划分为3个时段(即A、 B、 C段), 其中A段与C段分别为增温前与震后的温度变化曲线, 多与日照时间呈正相关关系, 特别是A段的这种关系更具普遍性。 然而, 反映震前地面增温特征的B段却与日照时间没有明显的相关性, 可见这种持续增温、 与云量无关的波状增温等都主要不是由日照或气象条件引起的, 而是一种与地下应力作用、 气体释放、 瞬变电场等有关的震兆现象。 因此, 提高对云下增温的系统观测能力, 是改善热红外地震预报的有效途径。