scholarly journals Error analyses of a multistatic meteor radar system to obtain a 3-dimensional spatial resolution distribution

2020 ◽  
Author(s):  
Wei Zhong ◽  
Xianghui Xue ◽  
Wen Yi ◽  
Iain M. Reid ◽  
Tingdi Chen ◽  
...  
Keyword(s):  
Spatial Resolution ◽  
Measurement Errors ◽  
Dimensional Space ◽  
Lower Thermosphere ◽  
Radar System ◽  
Meteor Radar ◽  
3 Dimensional ◽  
Radar Systems ◽  
Good Spatial Resolution ◽  
First Time

Abstract. In recent years, the concept of multistatic meteor radar systems has attracted the attention of the atmospheric radar community, focusing on the mesosphere and lower thermosphere (MLT). Recently, there have been some notable experiments using multistatic meteor radar systems (Chau et al., 2019; Spargo et al., 2019; Stober and Chau, 2015; Stober et al., 2018). Good spatial resolution is vital for meteor radars because nearly all parameter inversion processes rely on the accurate location of the meteor trail reflecting points. It is timely then for a careful discussion focussed on the error distribution of multistatic meteor radar systems. In this study, we discuss the measurement errors that affect the spatial resolution and obtain the resolution distribution in 3-dimensional space for the first time. The spatial resolution distribution can both help design a multistatic meteor radar system and improve the performance of existing radar systems. Moreover, the spatial resolution distribution allows the accuracy of retrieved parameters such as the wind field to be determined.

scholarly journals Error analyses of a multistatic meteor radar system to obtain a three-dimensional spatial-resolution distribution

2021 ◽  
Vol 14 (5) ◽  
pp. 3973-3988
Author(s):  
Wei Zhong ◽  
Xianghui Xue ◽  
Wen Yi ◽  
Iain M. Reid ◽  
Tingdi Chen ◽  
...  
Keyword(s):  
Spatial Resolution ◽  
Measurement Errors ◽  
Dimensional Space ◽  
Lower Thermosphere ◽  
Three Dimensional ◽  
Radar System ◽  
Meteor Radar ◽  
Radar Systems ◽  
Good Spatial Resolution ◽  
First Time

Abstract. In recent years, the concept of multistatic meteor radar systems has attracted the attention of the atmospheric radar community, focusing on the mesosphere and lower thermosphere (MLT) region. Recently, there have been some notable experiments using such multistatic meteor radar systems. Good spatial resolution is vital for meteor radars because nearly all parameter inversion processes rely on the accurate location of the meteor trail specular point. It is timely then for a careful discussion focused on the error distribution of multistatic meteor radar systems. In this study, we discuss the measurement errors that affect the spatial resolution and obtain the spatial-resolution distribution in three-dimensional space for the first time. The spatial-resolution distribution can both help design a multistatic meteor radar system and improve the performance of existing radar systems. Moreover, the spatial-resolution distribution allows the accuracy of retrieved parameters such as the wind field to be determined.

3D ionization structure and kinematics of NGC 2392

2011 ◽  
Vol 7 (S283) ◽  
pp. 348-349
Author(s):  
Reginald J. Dufour ◽  
Jonathan N. Sick ◽  
Patrick M. Hartigan ◽  
Richard B. C. Henry ◽  
Karen B. Kwitter ◽  
...  
Keyword(s):  
Spatial Resolution ◽  
Velocity Structure ◽  
High Spatial Resolution ◽  
Emission Lines ◽  
3 Dimensional ◽  
3D Morphology ◽  
Ionization Structure ◽  
First Time ◽  
Echelle Spectroscopy

AbstractWe discuss the 3D morphology, ionization structure, and kinematics of NGC 2392, the “Eskimo,” based on new and archival HST imagery and new long-slit echelle spectroscopy. High spatial resolution ionization maps of the nebula were made from HST WFPC2 imagery and compared with their velocity structure in various emission lines from echelle spectra taken with the 4m telescope at Kitt Peak. The imagery and spectra were then compared to map the kinematics of the nebula in several emission lines and decode the 3-dimensional morphology and ionization structure of the nebula, including that of C+2 from C III] 1909 Å for the first time.

scholarly journals CO, HI, recent Spitzer SAGE results in the Large Magellanic Cloud

2006 ◽  
Vol 2 (S237) ◽  
pp. 31-39
Author(s):  
Yasuo Fukui
Keyword(s):  
Galaxy Evolution ◽  
Time Scale ◽  
Dimensional Space ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
3 Dimensional ◽  
Physical Connection ◽  
First Time

AbstractFormation of GMCs is one of the most crucial issues in galaxy evolution. I will compare CO and HI in the LMC in 3 dimensional space for the first time aiming at revealing the physical connection between GMCs and associated HI gas at a ~40 pc scale. The present major findings are 1) [total CO intensity] ∝ [total HI intensity]0.8 for the 110 GMCs, and 2) the HI intensity tends to increase with the evolution of GMCs. I argue that these findings are consistent with the growth of GMCs via HI accretion over a time scale of a few × 10 Myrs. I will also discuss the role of the background stellar gravity and the dynamical compression by supershells in formation of GMCs.

scholarly journals Real-Time Tsunami Detection with Oceanographic Radar Based on Virtual Tsunami Observation Experiments

2018 ◽  
Vol 10 (7) ◽  
pp. 1126 ◽  
Author(s):  
Kohei Ogata ◽  
Shuji Seto ◽  
Ryotaro Fuji ◽  
Tomoyuki Takahashi ◽  
Hirofumi Hinata
Keyword(s):  
Real Time ◽  
Detection Probability ◽  
Cross Correlation ◽  
Temporal Change ◽  
Detection Method ◽  
Radar System ◽  
Hf Radar ◽  
Tsunami Detection ◽  
Radar Systems ◽  
First Time

The tsunami generated by the 2011 Tohoku-Oki earthquake was the first time that the velocity fields of a tsunami were measured by using high-frequency oceanographic radar (HF radar) and since then, the development of HF radar systems for tsunami detection has progressed. Here, a real-time tsunami detection method was developed, based on virtual tsunami observation experiments proposed by Fuji et al. In the experiments, we used actual signals received in February 2014 by the Nagano Japan Radio Co., Ltd. radar system installed on the Mihama coast and simulated tsunami velocities induced by the Nankai Trough earthquake. The tsunami was detected based on the temporal change in the cross-correlation of radial velocities between two observation points. Performance of the method was statistically evaluated referring to Fuji and Hinata. Statistical analysis of the detection probability was performed using 590 scenarios. The maximum detection probability was 15% at 4 min after tsunami occurrence and increased to 80% at 7 min, which corresponds to 9 min before tsunami arrival at the coast. The 80% detection probability line located 3 km behind the tsunami wavefront proceeded to the coast as the tsunami propagated to the coast. To obtain a comprehensive understanding of the tsunami detection probability of the radar system, virtual tsunami observation experiments are required for other seasons in 2014, when the sea surface state was different from that in February, and for other earthquakes.

scholarly journals Line observations of the 30-Dor complex and N159A5 with the MPE imaging NIR spectrometer FAST

1991 ◽  
Vol 148 ◽  
pp. 205-206 ◽  
Author(s):  
A. Krabbe ◽  
J. Storey ◽  
V. Rotaciuc ◽  
S. Drapatz ◽  
R. Genzel
Keyword(s):  
Spatial Resolution ◽  
Molecular Hydrogen ◽  
Near Infrared ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Emission Lines ◽  
Resolving Power ◽  
Max Planck ◽  
First Time ◽  
Infrared Array

Images with subarcsec spatial resolution in the light of near-infrared atomic (Bry) and molecular hydrogen H2 (S(1) v=1-0) emission lines were obtained for some extended, pointlike objects in the Large Magellanic Cloud (LMC) for the first time. We used the Max-Planck-Institut für extraterrestrische Physik (MPE) near-infrared array spectrometer FAST (image scale 0.8”/pix, spectral resolving power 950) at the ESO/MPI 2.2m telescope, La Silla. We present some results on the 30-Dor complex and N159A5.

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