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 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.

scholarly journals Morphology of z ~ 1 galaxies from deep K-band AO imaging

2006 ◽  
Vol 2 (S235) ◽  
pp. 405-405
Author(s):  
Marc Huertas-Company ◽  
Daniel Rouan ◽  
Geneviève Soucail ◽  
Olivier Le Fèvre ◽  
Lidia Tasca
Keyword(s):  
Adaptive Optics ◽  
Spatial Resolution ◽  
Near Infrared ◽  
High Spatial Resolution ◽  
Integration Time ◽  
Early Type ◽  
Distant Galaxies ◽  
First Time ◽  
Concentration Asymmetry ◽  
Adaptive Optics System

AbstractWe present the results of observations of distant galaxies (z ~ 0.8) at high spatial resolution (~0.1"). We observed 7 fields of 1' × 1' with the NACO Adaptive Optics system (VLT) in Ks (2.2μm) band with typical V ~ 14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area. We analyze the morphologies by means of B/D (Bulge/Disk) decomposition with GIM2D and CAS (Concentration-Asymmetry) estimators for 79 galaxies with magnitudes between Ks = 17 − 23 and classify them in three main morphological types (Late Type, Early Type and Irregulars). We obtain for the first time an estimate of the distribution of galaxy types at redshift z ~ 1 as measured from the near infrared at high spatial resolution.

scholarly journals High-Spatial Resolution Observations of Planetary Nebulae

1983 ◽  
Vol 103 ◽  
pp. 507-508
Author(s):  
C. T. Hua ◽  
R. Louise
Keyword(s):  
Spatial Resolution ◽  
Morphological Study ◽  
High Spatial Resolution ◽  
Planetary Nebulae ◽  
Emission Lines ◽  
Interference Filters

Monochromatic images in Hα, Hβ, (NII) λ 6584, (SII) λ 6717 and (OIII) λ 5007 lines are presented for morphological study of planetary nebulae. Narrow bandpass (Δλ = 5 to 10 Å) interference filters are generally used in order to discriminate peculiar structures existing in different emission lines. However, large bandwidths (Δλ = 50 Å) along with long exposures, are also necessary in searching for faint nebulosities associated with planetaries.

scholarly journals The kinematically decoupled core of MCG–6-30-15

2013 ◽  
Vol 9 (S304) ◽  
pp. 270-273
Author(s):  
Sandra I. Raimundo
Keyword(s):  
Spatial Resolution ◽  
High Spatial Resolution ◽  
Seyfert Galaxy ◽  
Very High Spatial Resolution ◽  
The Galaxy ◽  
First Time ◽  
Very High

AbstractThe Seyfert galaxy MCG–6-30-15 has recently been observed in the infrared using SINFONI on the VLT, reaching a very high spatial resolution of 0.1 arcsec. This allowed us for the first time to detect a stellar kinematically decoupled core in the inner r < 125 pc of the galaxy. Here we summarise the main theories for the formation of the decoupled core and the implications on the study of this galaxy.

scholarly journals High-mass star formation at sub-50 au scales

2019 ◽  
Vol 621 ◽  
pp. A122 ◽  
Author(s):  
H. Beuther ◽  
A. Ahmadi ◽  
J. C. Mottram ◽  
H. Linz ◽  
L. T. Maud ◽  
...  
Keyword(s):  
Star Formation ◽  
Optical Depth ◽  
Spatial Resolution ◽  
Velocity Structure ◽  
Spatial Scales ◽  
Spectral Lines ◽  
Emission Lines ◽  
High Mass ◽  
Mass Star ◽  
Small Scales

Context. The hierarchical process of star formation has so far mostly been studied on scales from thousands of au to parsecs, but the smaller sub-1000 au scales of high-mass star formation are still largely unexplored in the submillimeter regime. Aims. We aim to resolve the dust and gas emission at the highest spatial resolution to study the physical properties of the densest structures during high-mass star formation. Methods. We observed the high-mass hot core region G351.77-0.54 with the Atacama Large Millimeter Array with baselines extending out to more than 16 km. This allowed us to dissect the region at sub-50 au spatial scales. Results. At a spatial resolution of 18/40 au (depending on the distance), we identify twelve sub-structures within the inner few thousand au of the region. The brightness temperatures are high, reaching values greater 1000 K, signposting high optical depth toward the peak positions. Core separations vary between sub-100 au to several 100 and 1000 au. The core separations and approximate masses are largely consistent with thermal Jeans fragmentation of a dense gas core. Due to the high continuum optical depth, most spectral lines are seen in absorption. However, a few exceptional emission lines are found that most likely stem from transitions with excitation conditions above 1000 K. Toward the main continuum source, these emission lines exhibit a velocity gradient across scales of 100–200 au aligned with the molecular outflow and perpendicular to the previously inferred disk orientation. While we cannot exclude that these observational features stem from an inner hot accretion disk, the alignment with the outflow rather suggests that it stems from the inner jet and outflow region. The highest-velocity features are found toward the peak position, and no Hubble-like velocity structure can be identified. Therefore, these data are consistent with steady-state turbulent entrainment of the hot molecular gas via Kelvin–Helmholtz instabilities at the interface between the jet and the outflow. Conclusions. Resolving this high-mass star-forming region at sub-50 au scales indicates that the hierarchical fragmentation process in the framework of thermal Jeans fragmentation can continue down to the smallest accessible spatial scales. Velocity gradients on these small scales have to be treated cautiously and do not necessarily stem from disks, but may be better explained with outflow emission. Studying these small scales is very powerful, but covering all spatial scales and deriving a global picture from large to small scales are the next steps to investigate.

scholarly journals 4.4. The Sagittarius C region mapped in CS(2→1) and (3→2) by the IRAM 30m telescope

1998 ◽  
Vol 184 ◽  
pp. 173-174
Author(s):  
C. Kramer ◽  
J. Staguhn ◽  
H. Ungerechts ◽  
A. Sievers
Keyword(s):  
Spatial Resolution ◽  
Radio Telescope ◽  
Molecular Cloud ◽  
High Spatial Resolution ◽  
Ionized Gas ◽  
Hii Region ◽  
Molecular Material ◽  
Giant Molecular Cloud ◽  
First Time

We study the interaction of a dense giant molecular cloud with the HII region Sagittarius C, and a prominent nonthermal filament (NTF). For this purpose, we mapped the CS(2→1) and (3→2) transitions simultaneously with the IRAM 30m radio telescope, using the on-the-fly observing mode, and covering a 20pc×37pc (8′ × 15′) region. The high spatial resolution, 0.7pc (16″) at 147 GHz, allows for the first time to analyze in detail the morphology and kinematics of the molecular material and its relation to the ionized gas.

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 ALMA detects a radial disk wind in DG Tauri

2018 ◽  
Vol 620 ◽  
pp. L1 ◽  
Author(s):  
M. Güdel ◽  
C. Eibensteiner ◽  
O. Dionatos ◽  
M. Audard ◽  
J. Forbrich ◽  
...  
Keyword(s):  
Flow Pattern ◽  
Spatial Resolution ◽  
Velocity Structure ◽  
High Spatial Resolution ◽  
Disk Surface ◽  
Molecular Gas ◽  
Wind Component ◽  
Disk Wind ◽  
Molecular Outflow ◽  
Jet Axis

Aims. We aim to use the high spatial resolution of the Atacama Large Millimeter/submillimeter Array (ALMA) to map the flow pattern of molecular gas near DG Tauri and its disk, a young stellar object driving a jet and a molecular outflow. Methods. We use observations from ALMA in the J = 2 − 1 transition of 12CO, 13CO, and C18O to study the Keplerian disk of DG Tauri and outflows that may be related to the disk and the jet. Results. We find a new wind component flowing radially at a steep angle (≈25° from the vertical) above the disk with a velocity of ≈3.1 km s−1. It continues the trend of decreasing velocity for increasing distance from the jet axis (“onion-like velocity structure”). Conclusions. The new component is located close to the protostellar disk surface and may be related to photoevaporative winds.

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