Integral field spectroscopy of selected areas of the Bright bar and Orion-S cloud in the Orion nebula★

Mesa‐Delgado, A.; Núñez-Díaz, M.; Esteban, C.; López‐Martín, L.; García‐Rojas, J.

doi:10.1111/j.1365-2966.2011.19278.x

Cited by 23 publications

(28 citation statements)

References 59 publications

(134 reference statements)

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“…The fact that the abundances are not constant across the nebula but show a certain degree of structure has already been discussed in (Mesa-Delgado et al 2011, henceforth referred to as MD11) and Núñez-Díaz et al (2012). Specifically, MD11 find that for the BB their mean value of 8.49 ± 0.03 for the O/H ratio agrees with previous estimates of 8.50 (e.g.…”

Section: Ionic and Total Abundancessupporting

confidence: 57%

“…Peimbert & Torres-Peimbert 1977;Baldwin et al 1991;Rubin, Dufour & Walter 1993;Esteban et al 1998;Sánchez et al 2007;Mesa-Delgado et al 2011), and it serves as the comparison ground for abundances in other extra-and Galactic H II regions. One of the major problems in determining abundances is the dependence of line emissivity on the electron temperature T e : the emissivity of recombination lines (RLs) decreases with increasing T e , while the emissivity of collisionally excited lines (CELs) increases with T e in an exponential manner (O'Dell 2001).…”

Section: Ionic and Total Abundancesmentioning

confidence: 99%

“…In the era of integral field spectroscopy, new studies have emerged that exploit the combination of simultaneous imaging and spectroscopy on large spatial and spectral scales (e.g. Sánchez et al 2007;Mesa-Delgado et al 2011). A common analysis in the study of H II regions is given by line ratios of nebular emission lines which are used as abundance tracers (e.g (Vilchez & Esteban 1996), which is commonly used to determine star formation histories and evolutionary scenarios, as this parameter is found to vary as a function of position within a galaxy.…”

Section: Introductionmentioning

confidence: 99%

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A nebular analysis of the central Orion nebula with MUSE

Leod

Weilbacher

Ginsburg

et al. 2015

Mon. Not. R. Astron. Soc.

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A nebular analysis of the central Orion nebula and its main structures is presented. We exploit observations from the integral field spectrograph Multi Unit Spectroscopic Explorer (MUSE) in the wavelength range 4595-9366 Å to produce the first O, S and N ionic and total abundance maps of a region spanning 6 arcmin × 5 arcmin with a spatial resolution of 0.2 arcsec. We use theas an indicator of the degree of ionization, to distinguish between the various small-scale structures. The only Orion bullet covered by MUSE is HH 201, which shows a double component in the [Fe II] λ8617 line throughout indicating an expansion, and we discuss a scenario in which this object is undergoing a disruptive event. We separate the proplyds located south of the Bright Bar into four categories depending on their S 23 values, propose the utility of the S 23 parameter as an indicator of the shock contribution to the excitation of line-emitting atoms, and show that the MUSE data are able to identify the proplyds associated with discs and microjets. We compute the second-order structure function for the Hα, [O III] λ5007, [S II] λ6731 and [O I] λ6300 emission lines to analyse the turbulent velocity field of the region covered with MUSE. We find that the spectral and spatial resolution of MUSE are not able to faithfully reproduce the structure functions of previous works.

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Section: Ionic and Total Abundancessupporting

confidence: 57%

Section: Ionic and Total Abundancesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A nebular analysis of the central Orion nebula with MUSE

Leod

Weilbacher

Ginsburg

et al. 2015

Mon. Not. R. Astron. Soc.

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“…At the moment, however, this improved dataset is not publicly available in reduced form. Additionally, there are several studies with very good data quality in terms of depth, spectral, and spatial resolution devoted to the study of invidiual targets within the Orion Nebula that observed the interplay of gas and stars in proplyds and Herbig-Haro objects (e.g., Vasconcelos et al 2005;Mesa-Delgado et al 2011Tsamis & Walsh 2011;Tsamis et al 2013;Núñez-Díaz et al 2012). Therefore, they only mapped very small (∼10 ) rectangular areas.…”

Section: Introductionmentioning

confidence: 99%

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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“…), making the O + + H 2 channel a likely source of OH + at low depths. Detailed comparison of the optical and near-IR (forbidden and/or permitted) lines of O and O + would be a stronger test of this scenario (Walmsley et al 2000;Mesa-Delgado et al 2011). In addition, simulations of the full molecular + atomic + ionized gas in the Orion PDR with the Cloudy program (Ferland et al 2013) would be useful to constrain the role of possible ion sources in the Orion Bar.…”

Section: Possible Ion Sourcesmentioning

confidence: 99%

Spatially extended OH⁺emission from the Orion Bar and Ridge

Tak

Nagy

Ossenkopf

et al. 2013

A&A

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ContextWe analyze these HIFI data with non-local thermodynamic equilibrium radiative transfer and PDR chemical models, using newly calculated inelastic collision data for the e-OH + system. Results. Line emission is detected over ∼1 (0.12 pc), tracing the Bar itself as well as a perpendicular feature identified as the southern tip of the Orion Ridge, which borders the Orion Nebula on its western side. The line width of ≈4 km s −1 suggests an origin of the OH + emission close to the PDR surface, at a depth of A V ∼ 0.3-0.5 into the cloud where most hydrogen is in atomic form. Steadystate collisional and radiative excitation models for OH + require unrealistically high column densities to match the observed line intensity, indicating that the formation of OH + in the Bar is rapid enough to influence its excitation. Our best-fit OH + column density of ∼1.0 × 10 14 cm −2 is similar to that in previous absorption line studies, while our limits on the ratios of OH + /H 2 O + ( > ∼ 40) and OH + /H 3 O + ( > ∼ 15) are somewhat higher than seen before. Conclusions. The column density of OH + is consistent with estimates from a thermo-chemical model for parameters applicable to the Orion Bar, given the current uncertainties in the local gas pressure and the spectral shape of the ionizing radiation field. The unusually high OH + /H 2 O + and OH + /H 3 O + ratios are probably due to the high UV radiation field and electron density in this object. In the Bar, photodissociation and electron recombination are more effective destroyers of OH + than the reaction with H 2 , which limits the production of H 2 O + . The appearance of the OH + lines in emission is the result of the high density of electrons and H atoms in the Orion Bar, since for these species, inelastic collisions with OH + are faster than reactive ones. In addition, chemical pumping, far-infrared pumping by local dust, and near-UV pumping by Trapezium starlight contribute to the OH + excitation. Similar conditions may apply to extragalactic nuclei where H n O + lines are seen in emission.

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Integral field spectroscopy of selected areas of the Bright bar and Orion-S cloud in the Orion nebula★

Cited by 23 publications

References 59 publications

A nebular analysis of the central Orion nebula with MUSE

A nebular analysis of the central Orion nebula with MUSE

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

Spatially extended OH⁺emission from the Orion Bar and Ridge

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Integral field spectroscopy of selected areas of the Bright bar and Orion-S cloud in the Orion nebula★

Cited by 23 publications

References 59 publications

A nebular analysis of the central Orion nebula with MUSE

A nebular analysis of the central Orion nebula with MUSE

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

Spatially extended OH+emission from the Orion Bar and Ridge

Contact Info

Product

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Spatially extended OH⁺emission from the Orion Bar and Ridge