Velocity-resolved Fabry-Perot imaging of molecular hydrogen emission in OMC-1

Chrysostomou, A.; Burton, M. G.; Axon, D. J.; Brand, P. W. J. L.; Bland-Hawthorn, Joss; Geballe, T. R.

doi:10.1093/mnras/289.3.605

Cited by 38 publications

(65 citation statements)

References 33 publications

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“…In this regard atmospheric absorption in these lines must be considered. Data obtained (Dec. 2000) on the Canada-France-Hawaii Telescope, using a combination of the PUEO adaptive optics system and Fabry-Perot interferometry ("GriF"; Clénet et al 2002), as well as extensive data in Chrysostomou et al (1997), reveal that OMC1 as a whole contains H 2 emission which shows velocity shifts, relative to Earth, of between +60 to −10 km s −1 . Using the atmospheric absorption line atlas of Livingston & Wallace (1991), we find that there is negligible absorption for the v = 1−0 line in all cases, save over a very narrow range of velocities around +30 kms −1 for which an absorption of ∼7% is found.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

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H₂excitation imaging of the Orion Molecular Cloud

Kristensen

Gustafsson

Field

et al. 2003

A&A

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Abstract.Observations are reported of IR emission in H 2 , around 2 µm in the K-band, obtained with the ESO 3.6 m telescope using the ADONIS adaptive optics system. Data cover a region of the Orion Molecular Cloud north of the Trapezium stars and SW of the Becklin-Neugebauer object. Excellent seeing yielded diffraction limited images in the v = 2−1 S(1) line at 2.247 µm. Excitation temperature images were created by combining these data with similar data for H 2 emission in the v = 1−0 S(1) line reported earlier ). Shock models are used to estimate densities in emitting clumps of material. In local zones with high excitation temperatures, post-shock densities are found to be as high as several times 10 8 cm −3 , an order of magnitude denser than our previous estimates. We propose that the nature of these zones is dictated by the combined activity of shocks, which create dense structures, and the powerful radiation field of θ 1 C Ori which photoevaporates the boundaries of these structures.

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Section: Observations and Data Reductionmentioning

confidence: 99%

“…2, would yield data which provide a useful test of the model proposed. Existing data in Chrysostomou et al (1997) or Salas et al (1999) is of sufficient spectral resolution but has a spatial resolution of no better than ∼1. 6.…”

Section: The Influence Of θ 1 C Orimentioning

confidence: 99%

H₂excitation imaging of the Orion Molecular Cloud

Kristensen

Gustafsson

Field

et al. 2003

A&A

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“…Bullets have also been observed in CO (2-1) emission and are correlated spatially with H 2 O maser emission in this region (Rodriguez-Franco et al 1999;Gaume et al 1998;Genzel & Downes 1977). The favored description of the bullets is that they arise in situ in the outflowing material through hydrodynamic instabilities (Stone et al 1995), with densities of 2 to 3 10 5 cm −3 and masses of a few times 10 −3 solar masses (Chrysostomou et al 1997), moving with speeds relative to the background gas of ∼200 km s −1 (Lee & Burton 1999).…”

Section: Introductionmentioning

confidence: 96%

“…These features, which are essentially Herbig-Haro (HH) objects, have been very thoroughly studied with respect to velocity profiles, morphology and most recently proper motions (e.g. Lee & Burton 1999;Tedds et al 1999;Chrysostomou et al 1997). Bullets have also been observed in CO (2-1) emission and are correlated spatially with H 2 O maser emission in this region (Rodriguez-Franco et al 1999;Gaume et al 1998;Genzel & Downes 1977).…”

Section: Introductionmentioning

confidence: 99%

“…A great deal of theoretical work has been performed concerning the nature of shocks in OMC1 (e.g. Smith et al 1991), for example in conjunction with velocity-resolved imaging of H 2 emission (Chrysostomou et al 1997). Models have tended to explore fast shocks, for example of 200 km s −1 , in order to explain the very broad profiles of H 2 emission lines, which have a total extent of up to 150 km s −1 .…”

Section: Introductionmentioning

confidence: 99%

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H₂infrared emission and the formation of dense structures in the Orion molecular cloud

Vannier

Lemaire

Field

et al. 2001

A&A

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Abstract.Observations are reported of IR emission of H2 from a region of the Orion molecular cloud (OMC1) between the Becklin-Neugebauer object and IRc2 to the north and the Trapezium stars to the south. Data were obtained using the ESO 3.6 m telescope in the K-band around 2 µm with the ADONIS adaptive optics system. Images of H2 v = 1−0 S(1) show a spatial resolution of ∼0.15 . Detailed investigations of the distribution of sizes of structures in our images have been performed by area-perimeter analysis, Fourier analysis and brightness distribution studies. These demonstrate that structure is not fractal but shows a preferred scales of between 3 10 −3 and 4 10 −3 pc. In an attempt to estimate the density in observed structures, predictions of both shock models and photodissociation region models have been compared with measured emission brightness in the H2 v = 1−0 S(1) line. Magnetic (C-type) shocks with velocities of 30 km s −1 and pre-shock densities of 10 6 cm −3 yield the best representation of our data, notwithstanding significant discrepancies for the brightness ratio between v = 2−1 S(1) and v = 1−0 S(1) lines. Our results show that post-shock densities are several times 10 7 cm −3 . This is sufficiently high that the passage of C-type shocks in Orion yields gravitational instability which may in turn trigger star formation in the post-shock gas.

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The High-Resolution Frontier in Infrared Spectroscopy

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High Resolution Infrared Spectroscopy in Astronomy

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High-resolution astronomical spectroscopy in the infrared from large groundbased telescopes will lead to outstanding developments in many areas of astrophysics. A few examples are discussed, including isotope abundances in rapidly evolving stars, absorption spectroscopy of interstellar clouds, and terrestrial remote sensing with astronomical facilities. A picture may be worth a thousand words, but a spectrum is worth a thousand pictures-J. S. Miller. There is no such thing as too much resolution-J. J. Charfman.

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Velocity-resolved Fabry-Perot imaging of molecular hydrogen emission in OMC-1

Cited by 38 publications

References 33 publications

H₂excitation imaging of the Orion Molecular Cloud

H₂excitation imaging of the Orion Molecular Cloud

H₂infrared emission and the formation of dense structures in the Orion molecular cloud

The High-Resolution Frontier in Infrared Spectroscopy

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Velocity-resolved Fabry-Perot imaging of molecular hydrogen emission in OMC-1

Cited by 38 publications

References 33 publications

H2excitation imaging of the Orion Molecular Cloud

H2excitation imaging of the Orion Molecular Cloud

H2infrared emission and the formation of dense structures in the Orion molecular cloud

The High-Resolution Frontier in Infrared Spectroscopy

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Product

Resources

About

H₂excitation imaging of the Orion Molecular Cloud

H₂excitation imaging of the Orion Molecular Cloud

H₂infrared emission and the formation of dense structures in the Orion molecular cloud