Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · astro-ph/9301009

Extended Co(7-6) Emission from Warm Gas in Orion

J. E. Howe·D. T. Jaffe·E. N. Grossman·W. F. Wall·J. G. Mangum·G. J. Stacey
View original source ↗Read source document ↗Export metadata ↓

Abstract

We mapped quiescent 807 GHz CO(7-6) emission from Orion along a strip in RA extending from 0.7 pc west to 1.2 pc east of Ori theta 1C. The lines arise in warm gas with T > 40 K. The line brightness temperature is > 160 K in the di- rection of theta 1C, more than twice the dust temperature, and still exceeds 35 K more than a parsec east of theta 1C. The lines are narrow, with a max- imum velocity width of 7 km s^-1 near theta 1C and decreasing to 1.5-3 km s^-1 at the map boundaries. The density of the emitting gas is > 10^4 cm^-3 and the column density exceeds 10^21 cm^-2. The correlation of the bright, narrow CO(7-6) lines with 158 micron [C II] emission suggests that over the entire region mapped, the narrow CO lines arise in warm photo-dissociation regions ex- cited by UV photons from the Trapezium cluster. Although the Trapezium stars lie in front of the Orion A molecular cloud, not all of the warm gas is at the cloud surface. To the east of theta 1C the CO(7-6) lines split into two velo- city components (also seen in 13CO(2-1) emission) which persist over several arcminutes. Since only one of these components can be on the surface, the other must arise from a dense, UV-illuminated clump or filament within the molecular cloud. Comparison of the quiescent CO(7-6) emission to CO(7-6) ob- served in a cross-map of the energetic Orion KL outflow shows that the lumino- sity of shock-excited CO(7-6) emission in Orion is only a few percent of the luminosity of the widespread quiescent CO(7-6) emission.

Explore related subjects

astro-ph

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

J. E. Howe, D. T. Jaffe, E. N. Grossman, W. F. Wall, J. G. Mangum, G. J. Stacey. 1993-01-18. Extended Co(7-6) Emission from Warm Gas in Orion. https://doi.org/10.1086/172736

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Frame covariance of CMBR lensing in the exact 1+3 covariant radiation hierarchy

The exact $1+3$ covariant Boltzmann hierarchy for the cosmic microwave background contains acceleration, shear and vorticity couplings whose coefficients grow linearly in $\ell$. We show that all are the multipole form of the aberration operator in the photon Liouville equation. Under a change of threading, this operator shifts by the along-ray generator of a Lorentz boost. The acceleration coupling of $\ell$ to $\ell\pm1$ and the shear coupling of $\ell$ to $\ell\pm2$ are therefore frame-covariant descriptions of the same operator, related by an algebraic, pointwise relabelling of direction. With emitter and observer frames fixed, the observed sky is independent of the intermediate threading at every $\ell$. We derive this in $1+3$ covariant and gauge-invariant variables without constructing second-order gauge-invariant variables. The $O(ε^2\ell)$ content is gravitational lensing, as known in metric variables. Linearisation about a Friedmann--Lemaître--Robertson--Walker background removes these couplings, requiring lensing to be reinstated from the geodesic equation. Keeping the threading arbitrary makes frame covariance explicit and places observer aberration in the same operator. In the Newtonian threading we compute both halves of the deflection: the equivalence-principle contribution enters through aberration, while the spatial-curvature contribution arises from free streaming on perturbed spatial sections and reduces to the same operator. The lensing efficiency follows from the direction derivative. The angular-power-spectrum contribution is quartic in the potential: for a deflection statistically independent of the source, the two fourth-order terms carrying $\ell^2$ cancel where the spectrum is smooth on the deflection scale, and lensing redistributes power without adding ensemble variance.

astro-ph↗
arXiv2026

Cosmic Conundrums with Quantum Corrections

Darh energy was discovered over 25 years ago and we do not have an explanation of it. Dark matter comprises 95% of matter in the universe and we still don't know what it is. The Webb telescope has been finding fully formed galaxies with massive black holes millions of times the mass of the sun in the early universe and we don't have any explanation. A quantum density limitation will be used to solve these and other outstanding problems.

astro-ph↗
arXiv2026

On binary pulsars and the force of gravity

The energy-momentum budget of the astrophysical systems can be studied by the exact local conservation equation derived by Landau and Lifshitz. We show that a similar equation is valid for the Einstein-Cartan gravity. We reanalyze a binary pulsar system using the Landau-Lifshitz conservation equation and show that the orbital period change rate can be completely understood as a curvature backreaction process. Taking into account the detailed theoretical and observational research of relativistic binary pulsar systems, especially the system of Hulse and Taylor, we conclude that general relativity and astrophysical observations rule out the existence of gravitational radiation. We comment upon the LIGO GW events and their alternative explanation, as well as the recent pulsar timing arrays data.

astro-ph↗