scholarly journals The Environmental Effect of the CMF in the Galactic Center 50 km s−1 Molecular Cloud

2012 ◽  
Vol 8 (S292) ◽  
pp. 114-114
Author(s):  
Masato Tsuboi ◽  
Atsushi Miyazaki
Keyword(s):  
Emission Line ◽  
Molecular Cloud ◽  
Environmental Effect ◽  
Galactic Center ◽  
Power Laws ◽  
Statistical Properties ◽  
The Other ◽  
Size Spectrum ◽  
Other Hand ◽  
Sgr A

AbstractWe present the statistical properties of molecular clumps in the Galactic center 50 km s−1 molecular cloud based on observations of the CS J = 1 − 0 emission line with the Nobeyama Millimeter Array. The CMF and size spectrum for the whole cloud can be described by power laws of dN/dM ∝ M−2.6 ± 0.1 and dN/dR ∝ R−5.9±0.3, respectively. The CMF observed in the interacting part with the Sgr A East steepens to dN/dM ∝ M−4.0±0.2. On the other hand, the interaction presumably truncates the size spectrum on the larger side of R ∼ 0.4 pc.

scholarly journals CO and OH in the Galactic Center Region

1980 ◽  
Vol 87 ◽  
pp. 111-112
Author(s):  
Junji Inatani ◽  
Nobuharu Ukita
Keyword(s):  
Emission Line ◽  
Intensity Ratio ◽  
Molecular Clouds ◽  
Galactic Center ◽  
Point Of View ◽  
The Other ◽  
Kinetic Temperature ◽  
Two Dimensional ◽  
Center Region ◽  
Dimensional Distribution

The two-dimensional distribution of molecular clouds in the galactic center region has been investigated in the CO 115 GHz line and in the OH 1665 and 1667 MHz lines. As the former is an emission line, we can find molecular clouds without the unavoidable bias to continuum sources which is inherent in a survey of OH absorption lines. Because the CO line is usually optically thick, the brightness temperature of the line is directly related to the kinetic temperature of the cloud. On the other hand, the real optical depth of the OH line can be obtained from the intensity ratio between 1665 and 1667 MHz lines (assuming LTE). From this point of view we have compared the CO and OH observational results.

scholarly journals Chemical Analysis of B stars within 9–11 kpc from the Galactic Center

2009 ◽  
Vol 5 (S265) ◽  
pp. 362-363
Author(s):  
Maria Isela Zevallos Herencia ◽  
Simone Daflon
Keyword(s):  
Chemical Analysis ◽  
Galactic Center ◽  
Thin Disk ◽  
Open Clusters ◽  
The Other ◽  
Galactocentric Distance ◽  
B Stars ◽  
Ob Stars ◽  
Other Hand ◽  
Chemical Distribution

AbstractRadial gradients of metallicity are supported by observations of different young objects in the Galactic thin disk. The shape of the abundance distributions, however, is not completely constrained. Some works describe the abundance distributions as a function of the Galactocentric distance RG by linear fits with a single slope. On the other hand some analyses of open clusters, cepheids and OB stars suggest a discontinuity in the abundance distributions around RG=10 kpc. In this work we analyse a sample of 13 B stars members of four open clusters located within RG=9-11 kpc in order to better constrain the chemical distribution in this region of the disk.

scholarly journals Tidally-disrupted Molecular Clouds falling to the Galactic Center

2016 ◽  
Vol 11 (S322) ◽  
pp. 115-118 ◽  
Author(s):  
Masato Tsuboi ◽  
Yoshimi Kitamura ◽  
Kenta Uehara ◽  
Ryosuke Miyawaki ◽  
Atsushi Miyazaki
Keyword(s):  
Molecular Cloud ◽  
Molecular Clouds ◽  
Galactic Center ◽  
Outer Region ◽  
Recombination Line ◽  
Ionized Gas ◽  
Boundary Area ◽  
Gas Streams ◽  
Uv Emission ◽  
Sgr A

AbstractWe found a molecular cloud connecting from the outer region to the “Galactic Center Mini-spiral (GCMS)” which is a bundle of the ionized gas streams adjacent to Sgr A*. The molecular cloud has a filamentary appearance which is prominent in the CSJ=2-1 emission line and is continuously connected with the GCMS. The velocity of the molecular cloud is also continuously connected with that of the ionized gas in the GCMS observed in the H42α recombination line. The morphological and kinematic relations suggest that the molecular cloud is falling from the outer region to the vicinity of Sgr A*, being disrupted by the tidal shear of Sgr A* and ionized by UV emission from the Central Cluster. We also found the SiOJ=2-1 emission in the boundary area between the filamentary molecular cloud and the GCMS. There seems to exist shocked gas in the boundary area.

scholarly journals The Deuterium Abundance In The Galactic Center 50 km/s Molecular Cloud: Evidence For A Cosmological Origin Of D

2000 ◽  
Vol 198 ◽  
pp. 167-175
Author(s):  
D. A. Lubowich ◽  
Jay M. Pasachoff ◽  
Robert P. Galloway ◽  
Thomas J. Balonek ◽  
Christy Tremonti ◽  
...  
Keyword(s):  
Molecular Cloud ◽  
Galactic Center ◽  
Reaction Model ◽  
Baryon Density ◽  
The Galaxy ◽  
Chemical Reaction Model ◽  
Sgr A ◽  
Galactic Sources ◽  
Continuous Injection ◽  
The Universe

We confirm that deuterium exists in the Galactic Center (GC) and estimate that D/H = 3 × 10−6 using a new 5192-chemical reaction model. This is the lowest D/H ratio observed in the Galaxy, five times lower than the local ISM D/H = 1.5 × 10−5 but 106 × larger than D/H predicted by GC models. We detected DCN in the GC Sgr A 50 km/s molecular cloud located 10 pc from the GC with the NRAO 12m telescope and obtained T*R = 0.061 ± 0.007 K and 0.04 ± 0.02 K for the J = 1-0 and 2-1 lines. The most likely source of the GC D is continuous injection from the infall of primordial matter with D/H = 5 × 10−5 with the D/H determined by astration and mixing. Thus there are no significant Galactic sources of D and no recent quasar or AGN activity in the GC. This primordial D/H implies that the baryon density is less than the density necessary to close the Universe; most of the baryons are in dark matter; and there are fewer than four ν families.

scholarly journals 158μm [CII] Mapping of the Galactic Center Molecular Clouds

1989 ◽  
Vol 136 ◽  
pp. 151-155
Author(s):  
R. Genzel ◽  
G. J. Stacey ◽  
C. H. Townes ◽  
A. Poglitsch ◽  
N. Geis
Keyword(s):  
Emission Line ◽  
Molecular Clouds ◽  
Galactic Center ◽  
Hii Regions ◽  
Radio Continuum ◽  
Large Intensity ◽  
Sgr A

We have made 55″ resolution maps of the 158 μm [CII] emission line in the region of the curved, thermal filaments and the +20 / +50 kms−1 molecular clouds in Sgr A. The [CII] emission is spatially well correlated with the radio continuum in the filaments. The large intensity of the [CII] radiation excludes shocks as the origin of the ionization and we conclude that the curved filaments are most likely photo-ionized HII regions at the surface of dense molecular clouds. Our [CII] maps of the +20 / +50 kms−1 clouds indicate that the +50 kms−1 cloud is close to (<10pc) Sgr A west while the more massive +20 kms−1 cloud is at a greater distance from the center (>30pc).

scholarly journals HARD X-RAY MORPHOLOGICAL AND SPECTRAL STUDIES OF THE GALACTIC CENTER MOLECULAR CLOUD SGR B2: CONSTRAINING PAST SGR A⋆ FLARING ACTIVITY

2015 ◽  
Vol 815 (2) ◽  
pp. 132 ◽  
Author(s):  
Shuo Zhang ◽  
Charles J. Hailey ◽  
Kaya Mori ◽  
Maïca Clavel ◽  
Régis Terrier ◽  
...  
Keyword(s):  
Molecular Cloud ◽  
Galactic Center ◽  
Spectral Studies ◽  
X Ray ◽  
Sgr A

scholarly journals Effects of Antimodularity and Multiscale Influence in Random Boolean Networks

Complexity ◽  
2019 ◽  
Vol 2019 ◽  
pp. 1-14
Author(s):  
Luis A. Escobar ◽  
Hyobin Kim ◽  
Carlos Gershenson
Keyword(s):  
Complex Dynamics ◽  
Boolean Networks ◽  
Downward Causation ◽  
Statistical Properties ◽  
The Other ◽  
Random Boolean Networks ◽  
Dynamical Behaviors ◽  
Modular Networks ◽  
Other Hand ◽  
The One

We investigate the effects of modularity, antimodularity, and multiscale influence on random Boolean networks (RBNs). On the one hand, we produced modular, antimodular, and standard RBNs and compared them to identify how antimodularity affects the dynamical behaviors of RBNs. We found that the antimodular networks showed similar dynamics to the standard networks. Confirming previous results, modular networks had more complex dynamics. On the other hand, we generated multilayer RBNs where there are different RBNs in the nodes of a higher scale RBN. We observed the dynamics of micro- and macronetworks by adjusting parameters at each scale to reveal how the behavior of lower layers affects the behavior of higher layers and vice versa. We found that the statistical properties of macro-RBNs were changed by the parameters of micro-RBNs, but not the other way around. However, the precise patterns of networks were dominated by the macro-RBNs. In other words, for statistical properties only upward causation was relevant, while for the detailed dynamics downward causation was prevalent.

scholarly journals ALMA view of the Galactic Center 50km/s molecular cloud

2016 ◽  
Vol 11 (S322) ◽  
pp. 162-163
Author(s):  
Kenta Uehara ◽  
Masato Tsuboi ◽  
Yoshimi Kitamura ◽  
Ryosuke Miyawaki ◽  
Atsushi Miyazaki
Keyword(s):  
Emission Line ◽  
Molecular Cloud ◽  
Molecular Clouds ◽  
Galactic Center ◽  
Center Region

AbstractWe have observed the Galactic Center 50km/s molecular cloud (50MC) with ALMA to search for filamentary structures. In the CS J=2-1 emission line channel maps, we succeeded in identifying 27 molecular cloud filaments using the DisPerSE algorithm. This is the first attempt of filament-finding in the Galactic Center Region. These molecular cloud filaments strongly suggest that the molecular cloud filaments are also ubiquitous in the molecular clouds of the Galactic Center Region.

scholarly journals Further evidence that the Worst Performance Rule is a special case of the Correlation of Sorted Scores Rule

2020 ◽  
Author(s):  
Kimmo Sorjonen ◽  
Guy Madison ◽  
Tomas Hemmingsson ◽  
Bo Melin ◽  
Fredrik Ullén
Keyword(s):  
Standard Deviation ◽  
Reaction Time ◽  
Large Range ◽  
Rank Order ◽  
Statistical Properties ◽  
The Other ◽  
Other Hand ◽  
Test Rank ◽  
Higher Rank ◽  
Special Case

According to the worst performance rule (WPR), the correlations between intelligence and sorted performances, for example on reaction time tasks, should strengthen from the best to the worst performance. A commonly proposed explanation for the WPR is that poor performances reflect lapses of attention that are particularly strongly related to intelligence. The correlation of sorted scores rule (CSSR), on the other hand, claims that the WPR arises due to certain statistical properties of the data. Specifically, the magnitude of intelligence-performance correlations will change with the rank order of the test when intelligence is correlated with the within-individual standard deviation (WISD) of the tests. If the latter correlation is negative, a WPR is seen, i.e. intelligence-performance correlations will be lower for tests with higher rank order. If the intelligence-WISD correlation is positive, however, intelligence-performance correlations instead increase with test rank order. In the present study, through strategic slicing of two full samples (N = 5467 and N = 43,987, respectively), we created subsamples with a large range of intelligence-WISD correlations. In accordance with the CSSR, but not the WPR, the association between intelligence-performance correlations and test rank order was found to reflect the intelligence-WISD correlation of the subsample. This indicates that the WPR might be a special case of the more general CSSR and that the WPR is crucially dependent on intelligence-WISD correlations. The findings also indicate that the predictions made by the CSSR generalize to other predictors besides intelligence and to other outcomes besides reaction time.

scholarly journals 2.1. ISOCAM CVF observations of the Quintuplet and Object#17 clusters near the galactic center. diffuse components

1998 ◽  
Vol 184 ◽  
pp. 59-60
Author(s):  
T. Nagata ◽  
K. Kawara ◽  
T. Onaka ◽  
Y. Kitamura ◽  
H. Okuda
Keyword(s):  
Emission Line ◽  
Galactic Center ◽  
Star Clusters ◽  
The Other ◽  
Spectral Features ◽  
Diffuse Emission ◽  
Central Parsec ◽  
Absorption Features

There are two star clusters near the Galactic Center which might be similar to the central parsec cluster. One is the Quintuplet cluster at (l = 0.16°, b = −0.06°), and the other is the Object #17 cluster at (l = 0.12°, b = 0.02°). The Quintuplet, first found in a polarimetric survey by Kobayashi et al. (1983), includes five very bright stars whose color temperatures are in the range of 600-900K (Okuda et al. 1990; Nagata et al. 1990). Object #17 is a cluster of emission line stars (Nagata et al. 1993, 1995; Cotera et al. 1996; Morris & Serabyn 1996). Spectral features of these two objects observed with the ISOCAM (Kessler et al. 1996; Cesarsky et al. 1996) have been reported (Nagata et al., 1996); absorption features due to O-H (2.8μm) CO2(4.3μm), and CO (4.7μm) are present. In this paper, we report diffuse emission components detected in these two fields.

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