Emission line velocity field in the central region of M82

1986 ◽  
Vol 119 (1) ◽  
pp. 181-184
Author(s):  
Minoru Sasaki ◽  
Mamoru Saito
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Central Region

scholarly journals Complex distribution and velocity field of molecular gas in NGC 1316 as revealed by the Morita Array of ALMA

2019 ◽  
Vol 71 (4) ◽  
Author(s):  
Kana Morokuma-Matsui ◽  
Paolo Serra ◽  
Filippo M Maccagni ◽  
Bi-Qing For ◽  
Jing Wang ◽  
...  
Keyword(s):  
Velocity Field ◽  
Central Region ◽  
Milky Way ◽  
Conversion Factor ◽  
Rotating Disk ◽  
Molecular Gas ◽  
Dust Formation ◽  
Low Mass ◽  
First Time ◽  
Complex Distribution

Abstract We present the results of 12CO(J = 1–0) mosaicing observations of the cD galaxy NGC 1316 at kiloparsec resolution performed with the Morita Array of the Atacama Large Millimeter/submillimeter Array (ALMA). We reveal the detailed distribution of the molecular gas in the central region for the first time: a shell structure in the northwest, a barely resolved blob in the southeast of the center, and some clumps between them. The total molecular gas mass obtained with a standard Milky Way CO-to-H2 conversion factor is $(5.62 \pm 0.53) \times 10^{8}\, M_{\odot }$, which is consistent with previous studies. The disturbed velocity field of the molecular gas suggests that the molecular gas was injected very recently (<1 Gyr) if it has an external origin, and is in the process of settling into a rotating disk. Assuming that a low-mass gas-rich galaxy has accreted, the gas-to-dust ratio and H2-to-H i ratio are unusually low (∼28) and high (∼5.6), respectively. To explain these ratios additional processes should be taken into account, such as effective dust formation and conversion from atomic to molecular gas during the interaction. We also discuss the interaction between the nuclear jet and the molecular gas.

scholarly journals Observational Constraints on the Internal Velocity Field of Quasar Emission‐Line Clouds

2000 ◽  
Vol 542 (2) ◽  
pp. 644-654 ◽  
Author(s):  
Mark Bottorff ◽  
Gary Ferland ◽  
Jack Baldwin ◽  
Kirk Korista
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Observational Constraints ◽  
Internal Velocity

scholarly journals γ2 Velorum, photon loss and the velocity field

1999 ◽  
Vol 193 ◽  
pp. 229-230
Author(s):  
Orsola De Marco ◽  
Werner Schmutz ◽  
Alex de Koter
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Loss Model ◽  
Ionization Structure ◽  
Classical Models ◽  
Photon Loss

The interception of 0.01% of photons (termed photon loss) from the He II Lyα line by Fe VI and Ca V line-opacity can alter substantially the ionization structure of the wind. This is shown to increase the stellar luminosity and hence the wind driving efficiency. Our classical models for WR11 (the WR component in the γ2 Vel binary) underestimate the stellar luminosity as compared to the luminosity derived from the mass-luminosity relation. Here we present a model for WR11 where photon-loss is included. This model succeeds in that it has a higher luminosity for the same spectral appearance and V brightness. Line-blanketing has not yet been added, so that the force-factors and the velocity-law cannot yet be calculated. However, a hydro-dynamical velocity-law derived from a photon-loss model of a WN5 star improves considerably the fit to the narrow He II λ4686 emission line over the use of a β-law.

scholarly journals Taurus Observations of the Emission-Line Velocity Field of Centaurus A (NGC 5128)

1983 ◽  
Vol 100 ◽  
pp. 331-334
Author(s):  
Keith Taylor ◽  
Paul D. Atherton
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Spatial Resolution ◽  
Line Material ◽  
Fabry Perot ◽  
Dark Lane ◽  
Centaurus A

Using TAURUS – an Imaging Fabry Perot system in conjunction with the IPCS on the AAT, we have studied the velocity field of the Ha emission line at a spatial resolution of 1.7″ over the dark lane structure of Centaurus A. The derived velocity field is quite symmetrical and strongly suggests that the emission line material is orbiting the elliptical component, as a warped disc.

scholarly journals High-Velocity Outflow in the Extended Emission-Line Region of the Seyfert Galaxy NGC 7319

1997 ◽  
Vol 159 ◽  
pp. 357-358
Author(s):  
Kentaro Aoki
Keyword(s):  
Velocity Field ◽  
Compact Group ◽  
Emission Line ◽  
High Velocity ◽  
Seyfert Galaxy ◽  
Line Region ◽  
Systemic Velocity ◽  
Extended Emission

NGC 7319 is a member of the compact group of galaxies known as Stephan’s Quintet. The systemic velocity 6740 km s−1 gives a distance of 90Mpc (H0= 75 kms−1 Mpc−1) for NGC 7319. This galaxy has a tail and/or ring which suggests interaction with a neighboring pair of galaxies, NGC 7318A and B (e.g., Arp 1973). Durret & Warrin (1990) and Durret (1994) performed optical long-slit spectroscopy and found an extended emission-line region (EELR) in NGC 7319. They detected highly excited gas over along PA = 61° and 10″ along PA – 151°. Apart from these works, there have not been any studies on the velocity field and excitation of the gas in the EELR of NGC 7319. More details were published by Aoki et al. (1996).

The gas distribution and kinematics in the central region of the Seyfert 2 galaxy NGC 1125

2019 ◽  
Vol 15 (S359) ◽  
pp. 448-449
Author(s):  
Johan M. Marques ◽  
Rogemar A. Riffel ◽  
Thaisa Storchi-Bergmann ◽  
Rogério Riffel ◽  
Marlon R. Diniz
Keyword(s):  
Emission Line ◽  
Central Region ◽  
Near Infrared ◽  
Line Profiles ◽  
Gas Distribution ◽  
Bipolar Outflow ◽  
Broad Component ◽  
Integral Field Spectrograph ◽  
Integral Field

AbstractWe present Gemini Near-Infrared Integral-Field Spectrograph (NIFS) observations of the inner 660 × 660 pc2 of the Seyfert 2 galaxy NGC 1125, which reveals that the emission-line profiles present two kinematic components: a narrow one (σ < 150 km s−1) due to emission of the gas in the disk and a broad component (σ > 150 km s−1) produced by a bipolar outflow, perpendicular to the galaxy’s disk.

scholarly journals Hα KINEMATICS OF THE ISOLATED INTERACTING GALAXY PAIR KPG 486 (NGC 6090)

2020 ◽  
Vol 56 (1) ◽  
pp. 71-83
Author(s):  
M. M. Sardaneta ◽  
M. Rosado ◽  
M. Sánchez-Cruces
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Kinematic Analysis ◽  
Rotation Curve ◽  
Dynamic Behaviour ◽  
Hydrogen Gas ◽  
Kinematic Parameters ◽  
Optical Images ◽  
Fabry Perot ◽  
Hα Emission

In optical images, the barely studied isolated interacting galaxy pair KPG 486 (NGC 6090) displays similar features to the Antennae (NGC 4038/39) galaxy pair. To compare the distribution of ionized hydrogen gas, morphology and kinematic and dynamic behaviour of both galaxy pairs, we present observations in the Hα emission line of NGC 6090 acquired with the scanning Fabry-Perot interferometer, PUMA. For each galaxy in NGC 6090 we obtained several kinematic parameters, its velocity field and its rotation curve. We also analysed some of the perturbations induced by their encounter. We verified the consistency of our results by comparing them with kinematic results from the literature. The comparison of our results on NGC 6090 with those obtained in a previous similar kinematic analysis of the Antennae highlighted great differences between these galaxy pairs.

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