[Fe<scp>ii</scp>] 1.257 μm and He<scp>i</scp>1.083 μm Emission in the Central Region of the Orion Nebula: H<scp>ii</scp>Region, HH Flows, Jets, and Proplyds

Takami, M.; Usuda, Tomonori; Sugai, Hajime; Shimada, Hiroshi; Pyo, Tae‐Soo; Takeyama, Norihide; Aoki, Tetsuo; Mizutani, K.; Tanaka, Masuo

doi:10.1086/338245

Cited by 20 publications

(27 citation statements)

References 57 publications

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“…28). Our measurements are more closely comparable to the velocities measured in the near-infrared by Takami et al (2002, with Since our data are of lower spectral resolution than some other studies, we should be sensitive only to high-velocity features in the primary component of each emission line. Since strong bipolarities as reported by e.g., Doi et al (2004) around some proplyds are only detectable in fainter components -which in our data are blended with the main line profile -we cannot detect such features.…”

Section: Derived Velocitiessupporting

confidence: 83%

A MUSE map of the central Orion Nebula (M 42)

Weilbacher

Monreal-Ibero

Kollatschny

et al. 2015

A&A

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We present a new integral field spectroscopic dataset of the central part of the Orion Nebula (M 42), observed with the MUSE instrument at the ESO VLT. We reduced the data with the public MUSE pipeline. The output products are two FITS cubes with a spatial size of ∼5. 9 × 4. 9 (corresponding to ∼0.76 × 0.63 pc 2 ) and a contiguous wavelength coverage of 4595 . . . 9366 Å, spatially sampled at 0. 2. We provide two versions with a sampling of 1.25 Å and 0.85 Å in dispersion direction. Together with variance cubes these files have a size of 75 and 110 GiB on disk. They are the largest integral field mosaics to date in terms of information content. We make them available for use in the community. To validate this dataset, we compare world coordinates, reconstructed magnitudes, velocities, and absolute and relative emission line fluxes to the literature values and find excellent agreement. We derive a 2D map of extinction and present de-reddened flux maps of several individual emission lines and of diagnostic line ratios. We estimate physical properties of the Orion Nebula, using the emission line ratios [ (for the electron density N e ), and show 2D images of the velocity measured from several bright emission lines.

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Section: Derived Velocitiessupporting

confidence: 83%

A MUSE map of the central Orion Nebula (M 42)

Weilbacher

Monreal-Ibero

Kollatschny

et al. 2015

A&A

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“…Following Wen & O'Dell (1995), the main wall of the HII region lies 0.15 to 0.2 pc beyond the region observed. This is corroborated, for example, by recent data in Takami et al (2002), who describe the morphology of the HII zone around the Trapezium stars, using [FeII], HeI and Paβ lines as diagnostic of the presence of the HII region. These data show that the present region is overrun by the HII zone and thus that the clumps observed are dense fragments, surviving in the HII region around the Trapezium stars (O'Dell 2001).…”

Section: The Influence Of θ 1 C Orisupporting

confidence: 72%

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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“…For the object we examine here, no [FeII] emission has been observed (Takami et al 2002). Therefore it is likely that the shock observed is not dissociative (Kristensen et al 2007, in preparation , in preparation) which is above the noise limit of Takami et al (2002). In a C-type shock very little [FeII] emission is predicted (i.e.…”

Section: C-versus J-type Shockmentioning

confidence: 89%

Observational 2D model of H₂emission from a bow shock in the Orion Molecular Cloud

Kristensen¹,

Ravkilde

Forêts

et al. 2007

A&A

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Aims. We present a new method for reproducing high spatial resolution observations of bow shocks by using 1D plane parallel shock models. As an example we analyse one bow shock located in the Orion Molecular Cloud (OMC1). Methods. We use high spatial resolution near-infrared observations of H 2 rovibrational emission to constrain shock models. These observations have been made at the ESO-VLT using a combination of the NACO adaptive optics system and infrared camera array and the Fabry-Perot interferometer. Three rovibrational H 2 lines have been observed: v = 1−0 S(1) at 2.12 µm, v = 1−0 S(0) at 2.23 µm and v = 2−1 S(1) at 2.25 µm. The spatial resolution is 0. 15 ∼ 70 AU. We analyse a single bow shock located in our field, featuring a very well defined morphology and high brightness. Results. One dimensional shock models are combined to estimate the physical properties of pre-shock density, shock velocity and transverse magnetic field strength along the bow shock. We find that the pre-shock density is constant at ∼5 × 10 5 cm −3 and shock velocities lie between ∼35 km s −1 in the wings of the shock and ∼50 km s −1 at the apex. We also find that the transverse magnetic field is stronger at the apex and weaker further down the wings varying between ∼2 and 4 mGauss. Predictions of shock velocity and magnetic field strength agree with previous independent observations.

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[Feii] 1.257 μm and Hei1.083 μm Emission in the Central Region of the Orion Nebula: HiiRegion, HH Flows, Jets, and Proplyds

Cited by 20 publications

References 57 publications

A MUSE map of the central Orion Nebula (M 42)

A MUSE map of the central Orion Nebula (M 42)

H₂excitation imaging of the Orion Molecular Cloud

Observational 2D model of H₂emission from a bow shock in the Orion Molecular Cloud

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[Feii] 1.257 μm and Hei1.083 μm Emission in the Central Region of the Orion Nebula: HiiRegion, HH Flows, Jets, and Proplyds

Cited by 20 publications

References 57 publications

A MUSE map of the central Orion Nebula (M 42)

A MUSE map of the central Orion Nebula (M 42)

H2excitation imaging of the Orion Molecular Cloud

Observational 2D model of H2emission from a bow shock in the Orion Molecular Cloud

Contact Info

Product

Resources

About

H₂excitation imaging of the Orion Molecular Cloud

Observational 2D model of H₂emission from a bow shock in the Orion Molecular Cloud