Ammonia observations of the nearby molecular cloud MBM 12

We present NH₃(1,1) and (2,2) observations of MBM 12, the closest known molecular cloud (65-pc distance), aimed at finding evidence for on-going star formation processes. No local temperature (with a T _rot upper limit of 12 K) or linewidth enhancement is found, which suggests that the area of the cloud that we have mapped (15-arcmin size) is not currently forming stars. Therefore this nearby 'starless' molecular gas region is an ideal laboratory to study the physical conditions preceding new star formation.
A radio continuum source has been found in Very Large Array archive data, close to but outside the NH₃ emission. This source is likely to be a background object.     

Infrared emission from 6.7-GHz methanol maser sources

Near-infrared photometry was performed on 56 southern 6.7-GHz methanol maser sources. A simple spherically symmetric model of the radiative transfer through a dust shell was developed and used to study the conditions in the dust cloud in which the masers are produced. The parameters investigated were the size of the cloud, the spectral type of the embedded star, the optical depth of the dust cloud and the dust density distribution. It was found that the infrared colours of the models have a complex dependence on the parameters and that no unique combination of parameter values explains the spectral energy distribution of any particular source. The model effectively reproduces the far-infrared ( IRAS ) colours but cannot simultaneously explain the near-infrared colours for any of the observed sources.     

A source of extended HCO+ emission in young stellar objects

Anomalous molecular line profile shapes are the strongest indicators of the presence of the infall of gas that is associated with star formation. Such profiles are seen for well-known tracers, such as HCO⁺, CS and H₂CO. In certain cases, optically thick emission lines with appropriate excitation criteria may possess the asymmetric double-peaked profiles that are characteristic of infall. However, recent interpretations of the HCO⁺ infall profile observed towards the protostellar infall candidate B335 have revealed a significant discrepancy between the inferred overall column density of the molecule and that which is predicted by standard dark cloud chemical modelling.
This paper presents a model for the source of the HCO⁺ emission excess. Observations have shown that, in low-mass star-forming regions, the collapse process is invariably accompanied by the presence of collimated outflows; we therefore propose the presence of an interface region around the outflow in which the chemistry is enriched by the action of jets. This hypothesis suggests that the line profiles of HCO⁺, as well as other molecular species, may require a more complex interpretation than can be provided by simple, chemically quiescent, spherically symmetric infall models.
The enhancement of HCO⁺ depends primarily on the presence of a shock-generated radiation field in the interface. Plausible estimates of the radiation intensity imply molecular abundances that are consistent with those observed. Further, high-resolution observations of an infall-outflow source show HCO⁺ emission morphology that is consistent with that predicted by this model.     

Rotational contours of CH2X chain species compared with several diffuse interstellar bands

We have calculated synthetic spectra of perpendicular and parallel rovibronic bands of cumulene carbene molecules of the form C _n H₂. The perpendicular bands are consistent with a regularly spaced group of diffuse interstellar bands (DIBs) near 6850 Å. Parallel bands calculated for these molecular structures are consistent with the intrinsic profile of the associated 6614-Å DIB. Both types of bands are expected for an electronic transition that these species should have at those energies. We could not determine if the molecule was charged or if an atom other than carbon terminated the chain-end. Constraints due to molecular geometry and temperature place the chain length at 7–15 carbons to fit the 6850-Å group and 9–13 carbons to fit the 6614-Å DIB.     

Filling factors and scale heights of the diffuse ionized gas in the Milky Way

The combination of dispersion measures of pulsars, distances from the model of Cordes & Lazio (2002) and emission measures from the WHAM survey enabled a statistical study of electron densities and filling factors of the diffuse ionized gas (DIG) in the Milky Way. The emission measures were corrected for absorption and contributions from beyond the pulsar distance. For a sample of 157 pulsars at |b | > 5. and 60° < ℓ < 360°, located in mainly interarm regions within about 3 kpc from the Sun, we find that: (1) The average volume filling factor along the line of sight and the mean density in ionized clouds are inversely correlated: ( ) = (0.0184 ± 0.0011) ^{–1.07 ± 0.03} for the ranges 0.03 < < 2 cm^–3 and 0.8 > > 0.01. This relationship is very tight. The inverse correlation of and causes the well‐known constancy of the average electron density along the line of sight. As (z ) increases with distance from the Galactic plane |z |, the average size of the ionized clouds increases with |z |. (2) For |z| < 0.9 kpc the local density in clouds n _c(z ) and local filling factor f (z ) are inversely correlated because the local electron density n _e(z ) = f (z )n _c(z ) is constant. We suggest that f (z ) reaches a maximum value of >0.3 near |z | = 0.9 kpc, whereas n _c(z ) continues to decrease to higher |z |, thus causing the observed flattening in the distribution of dispersion measures perpendicular to the Galactic plane above this height. (3) For |z | < 0.9 kpc the local distributions n _c(z ), f (z ) and (z ) have the same scale height which is in the range 250 < h ≲ 500 pc. (4) The average degree of ionization of the warm atomic gas (z ) increases towards higher |z | similarly to (z ). Towards |z | = 1 kpc, (z ) = 0.24 ± 0.05 and (z ) = 0.24 ± 0.02. Near |z | = 1 kpc most of the warm, atomic hydrogen is ionized. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Observational characteristics of dense cores with deeply embedded young protostars

Class 0 objects, which are thought to be the youngest protostars, are identified in terms of NIR or radio emission and/or the presence of molecular outflows. We present combined hydrodynamic and radiative transfer simulations of the collapse of a star‐forming molecular core, which suggest two criteria for identifying dense cores with deeply embedded very young protostars that may not be observable in the NIR or radio with current telescopes. We find that cores with protostars are relatively warm (T > 15 K) with their SEDs peaking at wavelengths <170 µm, and they tend to appear circular. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

基于LiDAR点云的建筑物分割深度学习模型研究

本文针对深度神经网络算法应用于机载激光点云进行大规模建筑物提取的问题,分别选取PointNet++和PointCNN两个网络模型进行了改进和对比。对于PointCNN,通过参数调整,使其更适合大场景信息提取。对于PointNet++,为了增加更多特征,加快大场景下网络模型的训练效率,在网络体系结构中添加了一种新的特征提取层——K-means层。另外,通过在测试数据集上的训练和验证发现,本文基于深度学习方法的分类较好地克服了点云的无序特性,能够更好地利用点之间的空间相关性,改进后两种模型的精度均达96%以上,在建筑物提取的时间效率和效果上优于原始模型。     

一个长生命期准静止中尺度对流系统的观测特征及其持续的环境条件

2010年5月31日至6月1日华南特大暴雨过程经历了三次集中降水期,共有4次MCS（Mesoscale Convective Systems）演变过程,其中一个TL/AS MCS（Training Line/Adjoining Stratiform Mesoscale Convective System,邻接层状单向发展的中尺度对流系统）在广西壮族自治区中部准静止地维持了10多个小时,导致了多个观测站出现极端强降水。用观测资料和数值模拟结果重点探讨了该TL/AS MCS的观测特征及其发展持续的环境条件。结果表明,准静止TL/AS MCS发展在一个高空强辐散、低空气旋性汇合环流的天气尺度环境中,TL/AS MCS维持期间热力环境特征表现为对流层中低层持续高湿近饱和态、偏中性层结、合适的对流有效位能和极小的对流抑制能量。在对流层中低层,低空急流的加强发展维持与对流层中层相对弱的环境风形成了风垂直切变随高度呈现强逆转,近地层风垂直切变垂直于对流线的分量大,而在中层风垂直切变平行于对流线的分量占绝对优势,风切变特征可能是TL/AS MCS 准静止的原因;低空急流和中层环流的相互作用、对流层动力和热力条件有利于强上升运动的长时间维持与发展,不断触发新对流从而组织成一个长生命期准静止的TL/AS MCS     

基于地面LiDAR技术的异形建筑竣工测量方法研究

在分析地面LiDAR技术特点基础上,以广州市会展中心某异形建筑为工程实例,提出一种基于地面LiDAR技术的城市异形建筑竣工测量方法。首先对工程概况及其作业流程进行阐述,继而分别对地面三维竣工测量数据采集和处理过程中的关键技术进行详细介绍,最后对工程结果进行分析。研究和分析结果表明,地面LiDAR技术在结构复杂的异形建筑物测量中具有较好的应用前景。     

利用RANSAC算法对建筑物立面进行点云分割

建筑物立面点云分割是车载激光扫描数据特征提取与建模的基础.本文将随机抽样一致性算法( Random Sampling Consensus)方法引入对点云的分割中,并在判断准则中引入了点云的r半径密度,消除了噪声的影响,同时建立角度和距离两个约束条件对平面分割结果进行优化,提取出了最终的建筑物立面特征平面.