Dust and Molecular Gas in the Barred Spiral Galaxy NGC 1530

1995 ◽  
Vol 449 ◽  
pp. 576 ◽  
Author(s):  
Michael W. Regan ◽  
Stuart N. Vogel ◽  
Peter J. Teuben
Keyword(s):  
Spiral Galaxy ◽  
Molecular Gas ◽  
Barred Spiral Galaxy

scholarly journals Dense Molecular Gas Associated with the Circumnuclear Star‐forming Ring in the Barred Spiral Galaxy NGC 6951

1999 ◽  
Vol 511 (1) ◽  
pp. 157-177 ◽  
Author(s):  
Kotaro Kohno ◽  
Ryohei Kawabe ◽  
Baltasar Vila‐Vilaro
Keyword(s):  
Spiral Galaxy ◽  
Molecular Gas ◽  
Star Forming ◽  
Barred Spiral Galaxy

scholarly journals CO Multi-line Imaging of Nearby Galaxies (COMING). I. Physical properties of molecular gas in the barred spiral galaxy NGC 2903

2016 ◽  
Vol 68 (5) ◽  
pp. 89 ◽  
Author(s):  
Kazuyuki Muraoka ◽  
Kazuo Sorai ◽  
Nario Kuno ◽  
Naomasa Nakai ◽  
Hiroyuki Nakanishi ◽  
...  
Keyword(s):  
Physical Properties ◽  
Spiral Galaxy ◽  
Molecular Gas ◽  
Nearby Galaxies ◽  
Barred Spiral Galaxy ◽  
Line Imaging

scholarly journals 3.26. Molecular gas in the nuclear region and the bar of NGC 253

1998 ◽  
Vol 184 ◽  
pp. 141-142
Author(s):  
K. Sorai ◽  
N. Nakai ◽  
N. Kuno ◽  
K. Nishiyama
Keyword(s):  
Radio Telescope ◽  
Inclination Angle ◽  
Spiral Galaxy ◽  
Early Stage ◽  
Emission Lines ◽  
Molecular Gas ◽  
Nuclear Region ◽  
Star Forming ◽  
Barred Spiral Galaxy

In order to study relationship between molecular gas and star-forming activities, we have made observations of the barred spiral galaxy NGC 253 in 12CO(J = 1–0), 13CO(J = 1–0), and HCN(J = 1–0) emission lines with the Nobeyama 45-m radio telescope. NGC 253 is located in a distance of 2.5 M pc(Mauersbergeretal.(1996)) and has an inclination angle of 78°.5 (Pence 1980). This galaxy has a starburst nuclear region and is suggested in an early stage of a starburst (Rieke, Lebofsky, & Walker (1988)).

scholarly journals A High-Resolution CO Mapping of the Nucleus of the Barred-Spiral Galaxy, M83

1994 ◽  
Vol 140 ◽  
pp. 341-342 ◽  
Author(s):  
Toshihiro Handa ◽  
Sumio Ishizuki ◽  
Ryohei Kawabe
Keyword(s):  
High Resolution ◽  
Spiral Galaxy ◽  
Central Region ◽  
Molecular Gas ◽  
Nuclear Region ◽  
Circular Rotation ◽  
Frequency Coverage ◽  
Barred Spiral Galaxy ◽  
Gas Response ◽  
Co Emission

M83 is the best sample to investigate gas response to bar potential because it is one of the nearest galaxy with a pronounced bar structure (distance=3.7 Mpc). Handa et al. (1990) observed it with the Nobeyama 45-m telescope in CO(J=1-0) and found concentration of the CO emission to the dust lanes along the bar and non-circular rotation. However we need better spatial resolution in order to investigate kinematics and distribution of molecular gas in the nuclear region. So we observe the central region of M83 using the Nobeyama Millimeter Array. The synthesized beamsize was 12″ × 6″ and frequency coverage was 325 km s-1.

scholarly journals CO Multi-line Imaging of Nearby Galaxies (COMING). III. Dynamical effect on molecular gas density and star formation in the barred spiral galaxy NGC 4303

2019 ◽  
Vol 71 (Supplement_1) ◽  
Author(s):  
Yoshiyuki Yajima ◽  
Kazuo Sorai ◽  
Nario Kuno ◽  
Kazuyuki Muraoka ◽  
Yusuke Miyamoto ◽  
...  
Keyword(s):  
Star Formation ◽  
Spiral Galaxy ◽  
Galactic Disk ◽  
Molecular Gas ◽  
Kinetic Temperature ◽  
Spiral Arms ◽  
Nearby Galaxies ◽  
Barred Spiral Galaxy ◽  
Barred Spiral Galaxies ◽  
Line Imaging

AbstractWe present the results of $^{12}\textrm{C}$$\textrm{O}$(J = 1–0) and $^{13}\textrm{C}$$\textrm{O}$(J = 1–0) simultaneous mappings toward the nearby barred spiral galaxy NGC 4303 as part of the CO Multi-line Imaging of Nearby Galaxies (COMING) project. Barred spiral galaxies often show lower star-formation efficiency (SFE) in their bar region compared to the spiral arms. In this paper, we examine the relation between the SFEs and the volume densities of molecular gas n(H2) in the eight different regions within the galactic disk with $\textrm{C}$$\textrm{O}$ data combined with archival far-ultraviolet and 24 μm data. We confirmed that SFE in the bar region is lower by 39% than that in the spiral arms. Moreover, velocity-alignment stacking analysis was performed for the spectra in the individual regions. Integrated intensity ratios of $^{12}\textrm{C}$$\textrm{O}$ to $^{13}\textrm{C}$$\textrm{O}$ (R12/13) ranging from 10 to 17 were the results of this stacking. Fixing a kinetic temperature of molecular gas, $n(\rm {H_2})$ was derived from R12/13 via non-local thermodynamic equilibrium (non-LTE) analysis. The density n(H2) in the bar is lower by 31%–37% than that in the arms and there is a rather tight positive correlation between SFEs and n(H2), with a correlation coefficient of ∼0.8. Furthermore, we found a dependence of $n(\rm {H}_2)$ on the velocity dispersion of inter-molecular clouds (ΔV/sin i). Specifically, n(H2) increases as ΔV/sin i increases when ΔV/sin i < 100 km s−1. On the other hand, n(H2) decreases as ΔV/sin i increases when ΔV/sin i > 100 km s−1. These relations indicate that the variations of SFE could be caused by the volume densities of molecular gas, and the volume densities could be governed by the dynamical influence such as cloud–cloud collisions, shear, and enhanced inner-cloud turbulence.

scholarly journals 5.18. Molecular gas in the poststarburst galaxy NGC7331

1998 ◽  
Vol 184 ◽  
pp. 247-248
Author(s):  
T. Tosaki ◽  
Y. Shioya
Keyword(s):  
High Resolution ◽  
Spiral Galaxy ◽  
Stellar Populations ◽  
Optical Spectra ◽  
Molecular Gas ◽  
Early Type ◽  
Origin And Evolution ◽  
Co Observations

To understand the origin and evolution of starburst activity, we must study the full evolution of starburst; i.e., pre-, on-going, and post-starburst phases. It seems reasonable to suppose the numerous A-type stars indicate past starburst and they show strong Balmer absorption. NGC7331, nearby early-type spiral galaxy, is one of the poststarburst galaxies which show strong Balmer absorption. The optical spectra of NGC7331 were dominated by component of intermediate-age (5 × 109 years) stellar populations (Ohyama & Taniguchi 1996). We present the result of the high resolution CO observations of NGC7331 using Nobeyama Milimeter Array.

scholarly journals Study of the Gas Kinematics in the Center of the Barred Spiral Galaxy NGC 4258.

1996 ◽  
Vol 157 ◽  
pp. 164-167
Author(s):  
S. N. Dodonov
Keyword(s):  
Spiral Galaxy ◽  
Spatial Sampling ◽  
Kinematic Structure ◽  
Gas Kinematics ◽  
Barred Spiral Galaxy ◽  
Integral Field Spectrograph ◽  
Integral Field

AbstractIntegral Field Spectrograph observations of southeast (SE) gas outflow in the center (11×13 arcsec) of NGC 4258 with spatial sampling 0.6 and 1.2 arcsec were made with the 6-m Telescope. Reconstructed spatial and kinematic structure of the SE outflow from 20-30 pc to 200-220 pc are presented.

scholarly journals Supplying Gas for Nuclear Star Formation: The Central Molecular Spiral of IC 342

1994 ◽  
Vol 140 ◽  
pp. 339-340 ◽  
Author(s):  
D. A. Levine ◽  
J. L. Turner ◽  
R. L. Hurt
Keyword(s):  
Star Formation ◽  
Spiral Galaxy ◽  
Density Wave ◽  
Wave Pattern ◽  
Molecular Gas ◽  
Spiral Arms

IC 342 is a large nearby (1.8Mpc) spiral galaxy undergoing a moderate nuclear starburst. Previous maps of the inner arc minute in 13CO (1→0) show that the nuclear molecular gas forms spiral arms approximately 500 pc in extent in a density wave pattern (Turner & Hurt, 1992).

scholarly journals Molecular Gas in the Edge-On Galaxy NGC 4013

2004 ◽  
Vol 217 ◽  
pp. 166-167
Author(s):  
E. Schinnerer ◽  
R. J. Rand ◽  
N. Z. Scoville
Keyword(s):  
Spiral Galaxy ◽  
Molecular Gas ◽  
Sensitivity Limit ◽  
Gas Kinematics

Our OVRO observations at 300 pc resolution of the molecular gas disk in the edge-on spiral galaxy NGC 4013 show no evidence for extraplanar material at our sensitivity limit. The observed molecular gas kinematics are in agreement with gas motion in a barred potential.

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