分类： 天文学 >> 天文学 提交时间： 2023-02-19
Lixia Yuan
Ji Yang
Fujun Du
Yang Su
Xunchuan Liu
Shaobo Zhang
Yan Sun
Xin Zhou
Qing-Zeng Yan
Yuehui Ma
摘要： After the morphological classification of the 18,190 $^{12}$CO molecular clouds, we further investigate the properties of their internal molecular gas structures traced by the $^{13}$CO($J=$ 1$-$0) line emissions. Using three different methods to extract the $^{13}$CO gas structures within each $^{12}$CO cloud, we find that $\sim$ 15$\%$ of $^{12}$CO clouds (2851) have $^{13}$CO gas structures and these $^{12}$CO clouds contribute about 93$\%$ of the total integrated flux of $^{12}$CO emission. In each of 2851 $^{12}$CO clouds with $^{13}$CO gas structures, the $^{13}$CO emission area generally does not exceed 70$\%$ of the $^{12}$CO emission area, and the $^{13}$CO integrated flux does not exceed 20$\%$ of the $^{12}$CO integrated flux. We reveal a strong correlation between the velocity-integrated intensities of $^{12}$CO lines and those of $^{13}$CO lines in both $^{12}$CO and $^{13}$CO emission regions. This indicates the H$_{2}$ column densities of molecular clouds are crucial for the $^{13}$CO lines emission. After linking the $^{13}$CO structure detection rates of the 18,190 $^{12}$CO molecular clouds to their morphologies, i.e. nonfilaments and filaments, we find that the $^{13}$CO gas structures are primarily detected in the $^{12}$CO clouds with filamentary morphologies. Moreover, these filaments tend to harbor more than one $^{13}$CO structure. That demonstrates filaments not only have larger spatial scales, but also have more molecular gas structures traced by $^{13}$CO lines, i.e. the local gas density enhancements. Our results favor the turbulent compression scenario for filament formation, in which dynamical compression of turbulent flows induces the local density enhancements. The nonfilaments tend to be in the low-pressure and quiescent turbulent environments of the diffuse interstellar medium.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
摘要： In this work, we investigate the observational and algorithmic effects on molecular cloud samples identified from position-position-velocity (PPV) space. By smoothing and cutting off the high quality data of the Milky Way Imaging Scroll Painting (MWISP) survey, we extract various molecular cloud samples from those altered data with the DBSCAN (density-based spatial clustering of applications with noise) algorithm. Those molecular cloud samples are subsequently used to gauge the significance of sensitivity, angular/velocity resolution, and DBSCAN parameters. Two additional surveys, the FCRAO Outer Galaxy Survey (OGS) and the CfA-Chile 1.2 m complete CO (CfA-Chile) survey, are used to verify the MWISP results. We found that molecular cloud catalogs are not unique and the boundary and therefore the number shows strong variation with angular resolution and sensitivity. At low angular resolution (large beam sizes), molecular clouds merge together in PPV space, while low sensitivity (high cutoffs) misses small faint molecular clouds and takes bright parts of large molecular clouds as single ones. At high angular resolution and sensitivity, giant molecular clouds (GMCs) are resolved into individual clouds, and their diffuse components are also revealed. Consequently, GMCs are more appropriately interpreted as clusters or aggregates of molecular clouds, i.e., GMCs represent molecular cloud samples themselves.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Dang Yao
Yuan-Wei Wu
Bo Zhang
Jing Sun
Yan Sun
Shuang-Jing Xu
Jia Liu
Lang-Ming Ma
Jian-Jun Gong
Ying Yang
Xu-Hai Yang
摘要： In order to measure the Universal Time (UT1) in real time, National Time Service Center (NTSC) has built a VGOS-like (VLBI Global Observing System) broadband VLBI network, which includes three 13-m radio telescopes located in Jilin, Sanya and Kashi, and a data analysis center in Xi'an. Each station is equipped with a highly stable hydrogen atomic clock and a self-developed VLBI backend, and is co-located with two GPS receivers. This VGOS-like VLBI network may play an important role in improving the Chinese broadband VLBI technology and making valuable contributions to domestic VLBI measurements of UT1. In this paper, we introduce the specifications of this VLBI network, and present the UT1 measurements at C-band conducted in 2018 using the Jilin-Kashi baseline of this network. The comparisons between our UT1 estimates and those provided by IERS suggest that the NTSC VLBI network is capable to determine UT1 accurate at the level of 58.8 microseconds.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Dang Yao
Yuan-Wei Wu
Bo Zhang
Jing Sun
Yan Sun
Shuang-Jing Xu
Jia Liu
Lang-Ming Ma
Jian-Jun Gong
Ying Yang
Xu-Hai Yang
摘要： In order to measure the Universal Time (UT1) in real time, National Time Service Center (NTSC) has built a VGOS-like (VLBI Global Observing System) broadband VLBI network, which includes three 13-m radio telescopes located in Jilin, Sanya and Kashi, and a data analysis center in Xi'an. Each station is equipped with a highly stable hydrogen atomic clock and a self-developed VLBI backend, and is co-located with two GPS receivers. This VGOS-like VLBI network may play an important role in improving the Chinese broadband VLBI technology and making valuable contributions to domestic VLBI measurements of UT1. In this paper, we introduce the specifications of this VLBI network, and present the UT1 measurements at C-band conducted in 2018 using the Jilin-Kashi baseline of this network. The comparisons between our UT1 estimates and those provided by IERS suggest that the NTSC VLBI network is capable to determine UT1 accurate at the level of 58.8 microseconds.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Lixia Yuan
Ji Yang
Fujun Du
Xunchuan Liu
Yang Su
Qing-Zeng Yan
Xuepeng Chen
Yan Sun
Shaobo Zhang
Xin Zhou
Yuehui Ma
摘要： We look into the 2851 $^{12}$CO molecular clouds harboring $^{13}$CO structures to reveal the distribution of the projected angular separations and radial velocity separations between their internal $^{13}$CO structures. The projected angular separations are determined using the minimal spanning tree algorithm. We find that $\sim$ 50$\%$ of the angular separations fall in a narrow range of $\sim$ 3 - 7 arcmin with a median of $\sim$ 5 arcmin, and the corresponding radial velocity separations mainly range from $\sim$ 0.3 km s$^{-1}$ to 2.5 km s$^{-1}$. The mean and standard deviation of the angular separations of the internal $^{13}$CO structures within $^{12}$CO clouds appear to be universal, independent of the $^{12}$CO cloud angular areas and the counts of their internal $^{13}$CO structures. We also reveal a scaling relation between the $^{12}$CO cloud angular area and its harbored $^{13}$CO structure count. These results suggest there is a preferred angular separation between $^{13}$CO structures in these $^{12}$CO clouds, considering the distance effects. According to that, we propose an alternative picture for the assembly and destruction of molecular clouds: there is a fundamental separation for the internal structures of molecular clouds, the build-up and destruction of molecular clouds proceeds under this fundamental unit.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
摘要： We report VLBA observations of 22 GHz H$_{2}$O and 43 GHz SiO masers toward the Mira variable RR Aql. By fitting the SiO maser emission to a circular ring, we estimate the absolute stellar position of RR Aql and find agreement with Gaia astrometry to within the joint uncertainty of $\approx1$ mas. Using the maser astrometry we measure a stellar parallax of 2.44 $\pm$ 0.07 mas, corresponding to a distance of 410$^{+12}_{-11}$ pc. The maser parallax deviates significantly from the Gaia EDR3 parallax of 1.95 $\pm$ 0.11 mas, indicating a $3.8\sigma$ tension between radio and optical measurements. This tension is most likely caused by optical photo-center variations limiting the Gaia astrometric accuracy for this Mira variable. Combining infrared magnitudes with parallaxes for RR Aql and other Miras, we fit a period-luminosity relation using a Bayesian approach with MCMC sampling and a strong prior for the slope of -3.60 $\pm$ 0.30 from the LMC. We find a $K$-band zero-point (defined at logP(days) = 2.30) of -6.79 $\pm$ 0.15 mag using VLBI parallaxes and -7.08 $\pm$ 0.29 mag using Gaia parallaxes. The Gaia zero-point is statistically consistent with the more accurate VLBI value.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Yang Su
Shiyu Zhang
Ji Yang
Qing-Zeng Yan
Yan Sun
Hongchi Wang
Shaobo Zhang
Xuepeng Chen
Zhiwei Chen
Xin Zhou
Lixia Yuan
摘要： Based on the MWISP survey, we study high-z CO emission toward the tangent points, in which the distances of the molecular clouds (MCs) are well determined. In the region of l=12-26 deg and |b| 110 pc are identified, of which nearly 30 extreme high-z MCs (EHMCs at |z|> 260 pc) are concentrated in a narrow region of R_GC=2.6-3.1 kpc. The EHMC concentrations, together with other high-z MCs at R_GC=2.3-2.6 kpc, constitute molecular crater-wall structures surrounding the edges of the HI voids that are physically associated with the Fermi bubbles. Intriguingly, some large high-z MCs, which lie in the crater walls above and below the Galactic plane, show cometary structures with the head toward the plane, favouring the scenario that the entrained molecular gas moves with the multi-phase flows from the plane to the high-z regions. We suggest that the Milky Way nuclear wind has a significant impact on the Galactic gaseous disk. The powerful nuclear wind at ~3-6 Myr ago is likely responsible for the observational features, (1) the enhanced CO gas lying in the edges of the HI voids, (2) the deficiency of atomic and molecular gas within R_GC<3 kpc, (3) the possible connection between the EHMC concentrations and the 3-kpc arm, and (4) the elongated high-z MCs with the tail pointing away from the Galactic plane.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Lixia Yuan
Ji Yang
Fujun Du
Xunchuan Liu
Yang Su
Qing-Zeng Yan
Xuepeng Chen
Yan Sun
Shaobo Zhang
Xin Zhou
Yuehui Ma
摘要： We look into the 2851 $^{12}$CO molecular clouds harboring $^{13}$CO structures to reveal the distribution of the projected angular separations and radial velocity separations between their internal $^{13}$CO structures. The projected angular separations are determined using the minimal spanning tree algorithm. We find that $\sim$ 50$\%$ of the angular separations fall in a narrow range of $\sim$ 3 - 7 arcmin with a median of $\sim$ 5 arcmin, and the corresponding radial velocity separations mainly range from $\sim$ 0.3 km s$^{-1}$ to 2.5 km s$^{-1}$. The mean and standard deviation of the angular separations of the internal $^{13}$CO structures within $^{12}$CO clouds appear to be universal, independent of the $^{12}$CO cloud angular areas and the counts of their internal $^{13}$CO structures. We also reveal a scaling relation between the $^{12}$CO cloud angular area and its harbored $^{13}$CO structure count. These results suggest there is a preferred angular separation between $^{13}$CO structures in these $^{12}$CO clouds, considering the distance effects. According to that, we propose an alternative picture for the assembly and destruction of molecular clouds: there is a fundamental separation for the internal structures of molecular clouds, the build-up and destruction of molecular clouds proceeds under this fundamental unit.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
摘要： The principle of the background-eliminated extinction-parallax (BEEP) method is examining the extinction difference between on- and off-cloud regions to reveal the extinction jump caused by molecular clouds, thereby revealing the distance in complex dust environments. The BEEP method requires high-quality images of molecular clouds and high-precision stellar parallaxes and extinction data, which can be provided by the Milky Way Imaging Scroll Painting (MWISP) CO survey and the Gaia DR2 catalog, as well as supplementary AV extinction data. In this work, the BEEP method is further improved (BEEP-II) to measure molecular cloud distances in a global search manner. Applying the BEEP-II method to three regions mapped by the MWISP CO survey, we collectively measured 238 distances for 234 molecular clouds. Compared with previous BEEP results, the BEEP-II method measures distances efficiently, particularly for those molecular clouds with large angular size or in complicated environments, making it suitable for distance measurements of molecular clouds in large samples.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Weihua Guo
Xuepeng Chen
Jiancheng Feng
Li Sun
Chen Wang
Yang Su
Yan Sun
Yiping Ao
Shaobo Zhang
Xin Zhou
Lixia Yuan
Ji Yang
摘要： We present the survey of $^{12}$CO/$^{13}$CO/C$^{18}$O (J=1-0) toward the California Molecular Cloud (CMC) within the region of 161.75$^{\circ} \leqslant l \leqslant$ 167.75$^{\circ}$,-9.5$^{\circ} \leqslant b \leqslant $-7.5$^{\circ}$, using the Purple Mountain Observatory (PMO) 13.7 m millimeter telescope. Adopting a distance of 470 pc, the mass of the observed molecular cloud estimated from $^{12}$CO, $^{13}$CO, and C$^{18}$O is about 2.59$\times$10$^{4}$ M$_\odot$, 0.85$\times$10$^{4}$ M$_\odot$, and 0.09$\times$10$^{4}$ M$_\odot$, respectively. A large-scale continuous filament extending about 72 pc is revealed from the $^{13}$CO images. A systematic velocity gradient perpendicular to the major axis appears and is measured to be $\sim$ 0.82 km s$^{-1}$ pc$^{-1}$. The kinematics along the filament shows an oscillation pattern with a fragmentation wavelength of $\sim$ 2.3 pc and velocity amplitude of $\sim$ 0.92 km s$^{-1}$, which may be related with core-forming flows. Furthermore, assuming an inclination angle to the plane of the sky of 45$^{\circ}$, the estimated average accretion rate is $\sim$ 101 M$_\odot$ Myr$^{-1}$ for the cluster LkH$\alpha$ 101 and $\sim$ 21 M$_\odot$ Myr$^{-1}$ for the other regions. In the C$^{18}$O observations, the large-scale filament could be resolved into multiple substructures and their dynamics are consistent with the scenario of filament formation from converging flows. Approximately 225 C$^{18}$O cores are extracted, of which 181 are starless cores. Roughly 37$\%$ (67/181) of the starless cores have $\alpha_{\text{vir}}$ less than 1. Twenty outflow candidates are identified along the filament. Our results indicate active early-phase star formation along the large-scale filament in the CMC region.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Yang Su
Ji Yang
Qing-Zeng Yan
Shaobo Zhang
Hongchi Wang
Yan Sun
Zhiwei Chen
Chen Wang
Xin Zhou
Xuepeng Chen
Zhibo Jiang
Min Wang
摘要： We use the ~370 square degrees data from the MWISP CO survey to study the vertical distribution of the molecular clouds (MCs) toward the tangent points in the region of l=[16,52]deg and |b|100pc from the Galactic plane. However, only a few samples (i.e., 32 MCs) are located in the |z|>360pc region. Typically, the discrete MCs of the thick disk population have a median peak temperature of 2.1 K, a median velocity dispersion of 0.8km/s, and a median effective radius of 2.5pc. The median surface density of these MCs is 6.8 Msun/pc^2, indicating very faint CO emission for these high-z MCs. The cloud-cloud velocity dispersion is 4.9+-1.3 km/s and a linear variation with a slope of -0.4 km/s/kpc is obtained in the region of R_GC=2.2-6.4kpc. Assuming that these clouds are supported by their turbulent motions against the gravitational pull of the disk, a model of rho0(R) = 1.28exp(-R/3.2kpc) Msun/pc^3 can be used to describe the distribution of the total mass density in the Galactic midplane.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Xuepeng Chen
Weihua Guo
Li Sun
Jiancheng Feng
Yang Su
Yan Sun
Shaobo Zhang
Xin Zhou
Qing-Zeng Yan
Min Fang
Ji Yang
摘要： We present wide-field multi-wavelength observations of $\gamma$ Cassiopeiae (or $\gamma$~Cas for short) in order to study its feedback toward the interstellar environment. A large expanding cavity is discovered toward $\gamma$~Cas in the neutral hydrogen (HI) images at a systemic velocity of about -10 km/s. The measured dimension of the cavity is roughly 2.0 deg $\times$ 1.4 deg (or 6.0 pc $\times$ 4.2 pc at a distance of 168 pc), while the expansion velocity is about 5.0$\pm$0.5 km/s. The CO observations reveal systematic velocity gradients in IC63 (about 20 km/s/pc) and IC59 (about 30 km/s/pc), two cometary globules illuminated by $\gamma$~Cas, proving fast acceleration of the globules under stellar radiation pressure. The gas kinematics indicate that the cavity is opened by strong stellar wind, which has high potential to lead to the peculiar X-ray emission observed in $\gamma$~Cas. Our result favors a recent new scenario that emphasizes the roles of stellar wind and binarity in the X-ray emission of the $\gamma$~Cas stars.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Yan Sun
Ji Yang
Qing-Zeng Yan
Zehao Lin
Shaobo Zhang
Yang Su
Ye Xu
Xuepeng Chen
Hongchi Wang
Xin Zhou
摘要： We report the global properties recovered by an ongoing CO survey of the Milky Way Imaging Scroll Painting (MWISP) toward the Galactic outskirts. %To better understand the observational biases, Our results are also compared to those extracted by a uniform decomposition method from the CfA 1.2 m CO survey and the FCRAO 14 m outer Galaxy survey (OGS). We find that more extended and unseen structures are present in the MWISP data. The total flux across the disk recovered by the MWISP survey is 1.6 times larger than those recovered by the CfA and OGS surveys in the case of the same resolution. The discrepancies are scaling with distance. For example, in the outermost OSC arm, the flux ratios for MWISP-to-CfA and MWISP-to-OGS increase up to 43.8 and 7.4, respectively. Nonetheless, the census of molecular gas in our Galaxy is still far from complete by the MWISP, with flux completeness of $<$58%. The total mass ratios of the tabulated molecular clouds between different surveys are similar to the CO flux ratio. The application of these ratios to the total H$_{\rm 2}$ mass of our Galaxy yields a correction factor of at least 1.4, meaning that the H$_{\rm 2}$ mass of our Galaxy should be at least 40% more massive than previously determined. Including the completeness correction, an even more significant fraction of the matter should be contributed by baryonic matter. The mass spectrum in the outer Galactic plane is better described by a non-truncating power-law with $\gamma$=$-$1.83$\pm$0.05, and an upper mass of $M_0$=(1.3$\pm$0.5)$\times$10$^{\rm 6}$ $M_\odot$.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Xuepeng Chen
Li Sun
Jiancheng Feng
Shiyu Zhang
Weihua Guo
Xiaoyun Xu
Yang Su
Yan Sun
Shaobo Zhang
Xin Zhou
Zhiwei Chen
Qing-Zeng Yan
Miaomiao Zhang
Min Fang
Ji Yang
摘要： We present wide-field and high-sensitivity CO(1-0) molecular line observations toward the Cassiopeia region, using the 13.7m millimeter telescope of the Purple Mountain Observatory (PMO). The CO observations reveal a large-scale highly filamentary molecular cloud within the Galactic region of 132\fdg0\,$\geq$\,$l$\,$\geq$\,122\fdg0 and -1\fdg0\,$\leq$\,$b$\,$\leq$\,3\fdg0 and the velocity range from approximately +1 to +4 km/s. The measured length of the large-scale filament, referred to as the Cassiopeia Filament, is about 390 pc. The observed properties of the Cassiopeia Filament, such as length, column density, and velocity gradient, are consistent with those synthetic large-scale filaments in the inter-arm regions. Based on its observed properties and location on the Galactic plane, we suggest that the Cassiopeia Filament is a spur of the Local arm, which is formed due to the galactic shear. The western end of the Cassiopeia Filament shows a giant arc-like molecular gas shell, which is extending in the velocity range from roughly -1 to +7 km/s. Finger-like structures, with systematic velocity gradients, are detected in the shell. The CO kinematics suggest that the large shell is expanding at a velocity of ~6.5 km/s. Both the shell and finger-like structures outline a giant bubble with a radius of ~16 pc, which is likely produced by stellar wind from the progenitor star of a supernova remnant. The observed spectral linewidths suggest that the whole Cassiopeia Filament was quiescent initially until its west part was blown by stellar wind and became supersonically turbulent.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Lixia Yuan
Ji Yang
Fujun Du
Xunchuan Liu
Shaobo Zhang
Zehao Lin
Jingfei Sun
Qing-Zeng Yan
Yuehui Ma
Yang Su
Yan Sun
Xin Zhou
摘要： We attempt to visually classify the morphologies of 18190 molecular clouds, which are identified in the $^{12}$CO(1-0) spectral line data over $\sim$ 450 deg$^{2}$ of the second Galactic quadrant from the Milky Way Imaging Scroll Painting project (MWISP). Using the velocity-integrated intensity maps of the $^{12}$CO(1-0) emission, molecular clouds are first divided into unresolved and resolved ones. The resolved clouds are further classified as non-filaments or filaments. Among the 18190 molecular clouds, $\sim$ 25 $\%$ are unresolved, $\sim$ 64$\%$ are non-filaments, and $\sim$ 11$\%$ are filaments. In the terms of the integrated flux of $^{12}$CO(1-0) spectra of the whole 18190 molecular clouds, $\sim$ 90$\%$ are from filaments, $\sim$ 9$\%$ are from non-filaments, and the rest $\sim$ 1$\%$ are from unresolved sources. Although non-filaments are dominant in the number of the discrete molecular clouds, filaments are the main contributor of $^{12}$CO emission flux. We also present the number distributions of physical parameters of the molecular clouds in our catalog, including their angular sizes, velocity spans, peak intensities of $^{12}$CO(1-0) emission, and $^{12}$CO(1-0) total fluxes. We find that there is a systematic difference between the angular sizes of the non-filaments and filaments, with the filaments tending to have larger angular scales. The H$_{2}$ column densities of them are not significantly different. We also discuss the observational effects, such as those induced by the finite spatial resolution, beam dilution and line-of-sight projection, on the morphological classification of molecular clouds in our sample.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Shuangjing Xu
Hiroshi Imai
Youngjoo Yun
Bo Zhang
Maria J. Rioja
Richard Dodson
Se-Hyung Cho
Jaeheon Kim
Lang Cui
Andrey M. Sobolev
James O. Chibueze
Dong-Jin Kim
Kei Amada
Jun-ichi Nakashima
Gabor Orosz
Miyako Oyadomari
Sejin Oh
Yoshinori Yonekura
Yan Sun
Xiaofeng Mai
摘要： We report VLBI monitoring observations of the 22 GHz water (H$_{2}$O) masers around the Mira variable BX Cam, which were carried out as a part of the EAVN Synthesis of Stellar Maser Animations (ESTEMA) project. Data of 37 epochs in total were obtained from 2018 May to 2021 June with a time interval of 3-4 weeks, spanning approximately three stellar pulsation periods ($P= \sim$440 d). In particular, the dual-beam system equipped on the VERA stations was used to measure the kinematics and parallaxes of the H$_{2}$O maser features. The measured parallax, $\pi=1.79\pm 0.08$ mas, is consistent with $Gaia$ EDR3 and previously measured VLBI parallaxes within a 1-$\sigma$ error level. The position of the central star was estimated, based on both the $Gaia$ EDR3 data and the center position of the ring-like 43 GHz silicon-monoxide (SiO) maser distribution imaged with the KVN. The three-dimensional H$_{2}$O maser kinematics indicates that the circumstellar envelope is expanding at a velocity of $13\pm4$ km s$^{-1}$, while there are asymmetries in both the spatial and velocity distributions of the maser features. Furthermore, the H$_{2}$O maser animation achieved by our dense monitoring program manifests the propagation of shock waves in the circumstellar envelope of BX Cam.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Xuepeng Chen
Li Sun
Jiancheng Feng
Shiyu Zhang
Weihua Guo
Xiaoyun Xu
Yang Su
Yan Sun
Shaobo Zhang
Xin Zhou
Zhiwei Chen
Qing-Zeng Yan
Miaomiao Zhang
Min Fang
Ji Yang
摘要： We present wide-field and high-sensitivity CO(1-0) molecular line observations toward the Cassiopeia region, using the 13.7m millimeter telescope of the Purple Mountain Observatory (PMO). The CO observations reveal a large-scale highly filamentary molecular cloud within the Galactic region of 132\fdg0\,$\geq$\,$l$\,$\geq$\,122\fdg0 and -1\fdg0\,$\leq$\,$b$\,$\leq$\,3\fdg0 and the velocity range from approximately +1 to +4 km/s. The measured length of the large-scale filament, referred to as the Cassiopeia Filament, is about 390 pc. The observed properties of the Cassiopeia Filament, such as length, column density, and velocity gradient, are consistent with those synthetic large-scale filaments in the inter-arm regions. Based on its observed properties and location on the Galactic plane, we suggest that the Cassiopeia Filament is a spur of the Local arm, which is formed due to the galactic shear. The western end of the Cassiopeia Filament shows a giant arc-like molecular gas shell, which is extending in the velocity range from roughly -1 to +7 km/s. Finger-like structures, with systematic velocity gradients, are detected in the shell. The CO kinematics suggest that the large shell is expanding at a velocity of ~6.5 km/s. Both the shell and finger-like structures outline a giant bubble with a radius of ~16 pc, which is likely produced by stellar wind from the progenitor star of a supernova remnant. The observed spectral linewidths suggest that the whole Cassiopeia Filament was quiescent initially until its west part was blown by stellar wind and became supersonically turbulent.
分类： 农、林、牧、渔 >> 土壤学 提交时间： 2021-03-17
摘要： Purpose Soil structures are the main course of the formation and development of collapsing gullies, which are the most severe type of erosion in south China. However, few studies have focused on the relationship between soil macropores, soil erosion, and local topography. This study aimed to quantify and compare soil properties and macropore characteristics in the collapsing gully region, and explore their influences on the formation and development of the associated erosion. Materials and methods Soil core columns at different positions of a typical collapsing gully were excavated, and then scanned to analyze soil macropores. Moreover, soil properties and saturated hydraulic conductivity were investigated in the laboratory and in the field, respectively. Results and discussion The results indicated that the sand content increased from the ridge to the slope and the valley, while silt and clay contents decreased for the same catena. The mean weight diameter of aggregates was largest at the ridge and lowest at the valley. The infiltrate rates were highest at the valley and lowest at the slope. The valley had the greatest macroporosity (1.09±0.33%), and the highest number (5919±703), volumes (24.7±7.5 cm3) and surface (10.4±2.6 m2) of macropores, as well as the highest conectivity (42.3), while the slope had the smallest macroporosity (0.15±0.14%), and the smallest number (1189±747), volumes (3.4±3.2 cm3) and surface (1.7±1.4 m2) of macropores. The mean pore volume of macropores larger than 1 mm3 was largest at the ridge (16.8±7.4), and smallest at the slope (10.6±2.9). The number of macropores and their macroporosity mainly decreased with increasing depth, but were influenced by the soil macrofauna as well as the erosion and sediment processes. Macropores were mainly vertical, which is affected by the roots of plants and is conducive to the vertical infiltration of water. But, there wer many horizontal macropores at the valley because of the sediment process. The equivalent pore diameter of macropores was mainly smaller than 2 mm (accouting for more than 76.3%), and the macropores larger than 5 mm were less than 1%. Conclusions The macropore characteristics at different sites of the collapsing gullies affected the soil water infiltration and hydraulic conductivity, and further affected the processes of water erosion and mass ersion. The highest macroposities at the valley would result strong subsurface flow erosion and the loss of the base of collapsing wall. Macropores at the ridge would increase rain infiltration and promote soil collapsing. Few macropores and low infiltration abilities at the slope would strengthen the overland flow erosion. Thus, macropore characteristics had significant effects on both the formation and development of collapsing gullies.
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