The Orion Nebula (M42)
This dramatic image from the Hubble Space Telescope offers a detailed view inside the vast Orion Nebula (M42) — a nearby turbulent
Orions Messier 42 (M42) region
visible light (HST) near-infrared (ESO) mid-infrared (SOFIA). Trapezium Stars. BNKL Region. BNKL Region. Orion's Messier 42 (M42) region. Orion “Bright Bar”
90 GHz AND 150 GHz OBSERVATIONS OF THE ORION M42
Oct 9 2009 90 GHz AND 150 GHz OBSERVATIONS OF THE ORION M42 REGION. A SUBMILLIMETER TO RADIO. ANALYSIS. S. R. DICkER1
The Central Orion Nebula (M42) as seen by MUSE
mosaic of the central Orion Nebula. (M42) known as the Huygens region. During the past year
The Orion Nebula (M42)
This dramatic image from the Hubble Space Telescope offers a detailed view inside the vast Orion Nebula (M42) — a nearby turbulent
The Eighty Six H? Spectra from the Orion Nebula (M42 Sh2-281
Nov 27 2017 HII regions—ISM individual (Orion Nebula NGC1976
Messier 42 - M42 - Orion Nebula
Messier 42 - M42 - Orion Nebula freestarcharts.com. Right Ascension. Declina tion. 0. 0. 6h. 5h. 5h. 6h. 0. 0. 10. 0. 10. 0. 4h 30m. 4h 30m. 5h 30m.
La Nebulosa de Orión (M42)
Esta imagen espectacular del Telescopio Espacial Hubble nos brinda una vista detallada de la gran Nebulosa de Orión (M42) una región cercana y turbulenta
tearing the veil: interaction of the orion nebula with its neutral
Dec 20 2012 M42 is located in front of the parent molecular cloud OMC-1
A MUSE map of the central Orion Nebula (M 42) ???
dataset of the central part of the Orion Nebula (M42) observed with the MUSE ... characterized Orion's emission spectrum (e.g.
The Messenger 162 - December 2015
1 2 3 3 4 1 1,5 1 6 1Potsdam, Germany
2Research University, CNRS, Université
Paris Diderot, Sorbonne Paris Cité,
Meudon, France
3 ESO 4 54MHUDQRHSS/NSRC@L&DQL@MX6
CRAL, Observatoire de Lyon, Saint-
Genis Laval, France
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(Bacon et al., 2012) was commissioned NE (SBNUDQR@jDKCNEUHDVNE@ANTS1 by 1 arcminute on the sky at a sampling
of 0.2 arcseconds per spatial element and has a nominal wavelength range of480 to 930 nm. An extended mode with-
which allows a contiguous data coverage the instrument will be enhanced with an adaptive optics module and a narrow- spatial sampling. A summary of the com- ities was presented in Bacon et al. (2014) and these activities have already amply demonstrated the instrument"s capabili- this article we highlight the Orion Nebula dataset taken during commissioning, which we have reduced and now make available as science-ready cubes 1The Orion Nebula
we can study the interplay between the recently born (massive) stars and the surrounding interstellar medium. One of the best-known and closest examples, at a distance of about 440 pc, is theOrion Nebula (M42; a review is given in
O"Dell [2001]). As such, it is one of the
favourite targets when a new instrument needs to be validated, on account of its high surface brightness, richness in terms of structures and wealth of previous ob - servations. The nebula was observed during the commissioning of MUSE with the main technical goals of testing offsets stress test for the data reduction system.The collected data: i) mapped the com-
plete bright core (called the Huygens ii) achieved a depth similar to previous studies with only 5 seconds exposure time; iii) offered a large spectral coverage ranging from approximately 460 nm to935 nm; and iv) had reasonably good spa-
tial and spectral resolution. Since none of the previous datasets obtained using long- sessed all these properties simultane- ously, it was decided to release the MUSEOrion Nebula data to the community, as
a fully reduced and science-ready cube.Data processing
Basic data processing of each individual
pointing was done using the dedicatedMUSE pipeline (Weilbacher et al. [2012],
and publicly available for download 2 ) and and throughput correction, wavelength calibration, geometric characterisation, application of an astrometric solution, cor-rection for atmospheric refraction, appli- cation of the barycentric velocity offset to remove the sky background or the telluric absorption. The 2-Micron All SkySurvey (2MASS) positions of the stars
present in each pointing were used to establish the relative positioning between the individual pointings, and all the cubes3GDC@S@RDSBNMRSHSTSDRNMDNESGDjQRS
observations with the MUSE extended %KTW: lDQFRBL
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The red end of one Orion spectrum illus-
trating the contamination of the data by the broad second order. Broad bumps caused by second order contamination of H and H are indicated.Astronomical Science
38The Messenger 162 - December 2015
Extinction structure
offered by this set of data is presented map derived from the observed H/H emission line ratio and standard assump- tions for the assumed intrinsic H/H ratio. The Dark Bay and the southwest cloud show the strongest extinction, while regions like the Bright Bar exhibit moderate reddening. This map is quali- tatively similar to the reddening map who use a different technique (i.e., radio- to-optical surface brightness compari- higher by a factor of 1.5 in extinction c(H) with respect to the one found with the MUSE data. This difference can be understood in terms of the differing capacity of both tracers to penetrate the dust, which is higher for the one involving radio emission.Digging up proplyds by means of line
ratio mappingAlthough lacking the high angular resolu-
tion of Hubble Space Telescope (HST) opportunities to evaluate the effects of second-order overlap. The central OrionNebula shows very strong emission lines
that are easy to identify, while the second order is unfocused and offset from the expected wavelength calibration. Figure 1 illustrates its appearance in the spectral direction: strong emission lines in the blue create broad bumps in the red region spectrum, two bumps caused by the second order spectrum of H and H are modelled and subtracted as background, thereby minimising their effect in the esti- part of the spectra.Data release
The released data products have a spa-
tial size of 5.9 by 4.9 arcminutes (0.76 by 0.63 pc) at a 0.2 by 0.2 arcsecond sampling and a contiguous spectral cov- erage of 459.5 to 936.6 nm. They are sions, including cubes for the data and the statistical variance, and reconstructed vide two versions of the cube, with spec- tral samplings of 0.125 nm and 0.085 nm, tively. We also provide an online facility that offers the possibility of extracting only a subsection of the cubes, since by current standards these are rather large 1The combined scope of the spatial and
spectral directions is illustrated by the cover page and in Figure 2, which show several of the many possible three-colour composite images that can be extracted from these data. The cover page shows an image constructed from three emis- sion lines of hydrogen: H, H and from all three ionisation stages of oxygen :.p(([PDF] m=p/g
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