RECORD
The flaring HI disk of the nearby spiral galaxy NGC 2683
Astrophysics of Galaxies · Submitted 22 Dec 2015
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We propose a scenario where this external accretion leads to turbulent adiabatic compression that enhances the turbulent velocity dispersion and might quench star formation in the outer gas disk of NGC 2683.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
New deep VLA D array HI observations of the highly inclined nearby spiral galaxy NGC 2683 are presented. Archival C array data were processed and added to the new observations. To investigate the 3D structure of the atomic gas disk, we made different 3D models for which we produced model HI data cubes. The main ingredients of our best-fit model are (i) a thin disk inclined by 80 degrees; (ii) a crude approximation of a spiral and/or bar structure by an elliptical surface density distribution of the gas disk; (iii) a slight warp in inclination; (iv) an exponential flare; and (v) a low surface-density gas ring. The slope of NGC 2683's flare is comparable, but somewhat steeper than those of other spiral galaxies. NGC 2683's maximum height of the flare is also comparable to those of other galaxies. On the other hand, a saturation of the flare is only observed in NGC 2683. Based on the comparison between the high resolution model and observations, we exclude the existence of an extended atomic gas halo around the optical and thin gas disk. Under the assumption of vertical hydrostatic equilibrium we derive the vertical velocity dispersion of the gas. The high turbulent velocity dispersion in the flare can be explained by energy injection by (i) supernovae, (ii) magneto-rotational instabilities, (iii) ISM stirring by dark matter substructure, or (iv) external gas accretion. The existence of the complex large-scale warping and asymmetries favors external gas accretion as one of the major energy sources that drives turbulence in the outer gas disk. We propose a scenario where this external accretion leads to turbulent adiabatic compression that enhances the turbulent velocity dispersion and might quench star formation in the outer gas disk of NGC 2683.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | New deep VLA D array HI observations of the highly inclined nearby spiral galaxy NGC 2683 are presented. | contribution 0.73 | 0.95 | 0.02 | asserted 0.99 |
| s1 | Archival C array data were processed and added to the new observations. | method 1.00 | 0.86 | 0.01 | asserted 1.00 |
| s2 | To investigate the 3D structure of the atomic gas disk, we made different 3D models for which we produced model HI data cubes. | method 0.98 | 0.97 | 0.03 | asserted 0.97 |
| s3 | The main ingredients of our best-fit model are (i) a thin disk inclined by 80 degrees; (ii) a crude approximation of a spiral and/or bar structure by an elliptical surface density distribution of the gas disk; (iii) a slight warp in inclination; (iv) an exponential flare; and (v) a low surface-density gas ring. | method 0.70 | 0.93 | 0.10 | asserted 1.00 |
| s4 | The slope of NGC 2683's flare is comparable, but somewhat steeper than those of other spiral galaxies. | result 0.98 | 0.85 | 0.07 | asserted 1.00 |
| s5 | NGC 2683's maximum height of the flare is also comparable to those of other galaxies. | result 0.99 | 0.85 | 0.04 | asserted 1.00 |
| s6 | On the other hand, a saturation of the flare is only observed in NGC 2683. | result 1.00 | 0.90 | 0.09 | asserted 1.00 |
| s7 | Based on the comparison between the high resolution model and observations, we exclude the existence of an extended atomic gas halo around the optical and thin gas disk. | result 0.99 | 0.95 | 0.24 | asserted 1.00 |
| s8 | Under the assumption of vertical hydrostatic equilibrium we derive the vertical velocity dispersion of the gas. | method 0.73 | 0.96 | 0.03 | asserted 1.00 |
| s9 | The high turbulent velocity dispersion in the flare can be explained by energy injection by (i) supernovae, (ii) magneto-rotational instabilities, (iii) ISM stirring by dark matter substructure, or (iv) external gas accretion. | interpretation 0.98 | 0.68 | 0.08 | hedged possibility 0.68 |
| s10 | The existence of the complex large-scale warping and asymmetries favors external gas accretion as one of the major energy sources that drives turbulence in the outer gas disk. | interpretation 0.98 | 0.78 | 0.29 | hedged possibility 0.64 |
| s11 | We propose a scenario where this external accretion leads to turbulent adiabatic compression that enhances the turbulent velocity dispersion and might quench star formation in the outer gas disk of NGC 2683. | interpretation 1.00 | 0.66 | 0.47 | speculative 0.86 |
What was examined, and what was not
- arXiv listing abstract v1
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
New deep VLA D array HI observations of the highly inclined nearby spiral galaxy NGC 2683 are presented. Archival C array data were processed and added to the new observations. To investigate the 3D structure of the atomic gas disk, we made different 3D models for which we produced model HI data cubes. The main ingredients of our best-fit model are (i) a thin disk inclined by 80 degrees; (ii) a crude approximation of a spiral and/or bar structure by an elliptical surface density distribution of the gas disk; (iii) a slight warp in inclination; (iv) an exponential flare; and (v) a low surface-density gas ring. The slope of NGC 2683's flare is comparable, but somewhat steeper than those of other spiral galaxies. NGC 2683's maximum height of the flare is also comparable to those of other galaxies. On the other hand, a saturation of the flare is only observed in NGC 2683. Based on the comparison between the high resolution model and observations, we exclude the existence of an extended atomic gas halo around the optical and thin gas disk. Under the assumption of vertical hydrostatic equilibrium we derive the vertical velocity dispersion of the gas. The high turbulent velocity dispersion in the flare can be explained by energy injection by (i) supernovae, (ii) magneto-rotational instabilities, (iii) ISM stirring by dark matter substructure, or (iv) external gas accretion. The existence of the complex large-scale warping and asymmetries favors external gas accretion as one of the major energy sources that drives turbulence in the outer gas disk. We propose a scenario where this external accretion leads to turbulent adiabatic compression that enhances the turbulent velocity dispersion and might quench star formation in the outer gas disk of NGC 2683.
Human review
How the literature uses it
2 arXiv papers cite this in 2 sentences
Papers citing it · 1 sentence without a confident label
Uses its data or values 1 paper
-
The Hubble type and distance $d$ are taken from the https://ned.ipac.caltech.edu/NASA Extragalactic Database. a: [ref] , b: [ref] , c: [ref] , d: [ref] 1: [ref] , 2: [ref] , 3: [ref] , 4: [ref] , 5: [ref] , 6: [ref] , 7: [ref] , 8: [ref] , 9: [ref] , 10: [ref] , 11: [ref] , 12: [ref] , 13: [ref] , 15: [ref] , 16: [ref] , 17: [ref] , 18: [ref] , 19: [ref] , 20: [ref] , 21: [ref] , 22: [ref] , 23: [ref] , 24: [ref] , 25: [ref] , 26: [ref] , 27: [ref] . deluxetable
Radio Continuum Emission from Evolving Star-Forming Galaxies -- I. Correlations Involving the Total Synchrotron Luminosity · Adjustable parameters of the model · 0.96
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.