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J/A+A/604/A32 Orion BN-KL ALMA view (Pagani+, 2017)
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Beginning of ReadMe :J/A+A/604/A32 Orion BN-KL ALMA view (Pagani+, 2017)
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The complexity of Orion: an ALMA view. I. Data and first results.
Pagani L., Favre C., Goldsmith P.F., Bergin E.A., Snell R., Melnick G.
<Astron. Astrophys. 604, A32 (2017)>
=2017A&A...604A..32P (SIMBAD/NED BibCode)
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ADC_Keywords: Molecular clouds ; Interstellar medium
Keywords: ISM: clouds - ISM: structure -
ISM: individual objects : Orion-KL (except planetary nebulae) -
astrochemistry - molecular processes
Abstract:
We wish to improve our understanding of the Orion central star
formation region (Orion-KL) and disentangle its complexity.
We collected data with ALMA during cycle 2 in 16GHz of total
bandwidth spread between 215.1 and 252.0GHz with a typical
sensitivity of 5mJy/beam (2.3mJy/beam from 233.4 to 234.4GHz) and a
typical beam size of 1.7"x1.0" (average position angle of 89). We
produced a continuum map and studied the emission lines in nine
remarkable infrared spots in the region including the Hot Core and the
Compact Ridge, plus the recently discovered Ethylene Glycol Peak.
We present the data, and report the detection of several species not
previously seen in Orion, including n- and i-propyl cyanide
(C_3_H_7_CN), and the tentative detection of a number of other species
including glycolaldehyde (CH_2_(OH)CHO). The first detections of gGg'
ethylene glycol (gGg' (CH_2_OH)_2_) and of acetic acid (CH_3_COOH) in
Orion are presented in a companion paper. We also report the possible
detection of several vibrationally excited states of cyanoacetylene
(HC_3_N), and of its ^13^C isotopologues. We were not able to detect
the ^16^O^18^O line predicted by our detection of O_2_ with Herschel,
due to blending with a nearby line of vibrationally excited ethyl
cyanide. We do not confirm the tentative detection of hexatriynyl
(C_6_H) and cyanohexatriyne (HC_7_N) reported previously, or of
hydrogen peroxide (H_2_O_2_) emission.
We report a complex velocity structure only partially revealed before.
Components as extreme as -7 and +19km/s are detected inside the hot
region. Thanks to different opacities of various velocity components,
in some cases we can position these components along the line of
sight. We propose that the systematically redshifted and blueshifted
wings of several species observed in the northern part of the region
are linked to the explosion that occurred 500 years ago. The compact
ridge, noticeably farther south displays extremely narrow lines
( 1km/s) revealing a quiescent region that has not been acted by this
explosion. This probably indicates that the compact ridge is either
over 10,000 au in front of or behind the rest of the region.
Many lines remain unidentified, and only a detailed modeling of all
known species, including vibrational states of isotopologues combined
with the detailed spatial analysis offered by ALMA enriched with
zero-spacing data, will allow new species to be detected.
Description:
The observations were performed on 29 December 2014 with 37 antennas
for the first four scheduling blocks and on 30 December 2014 for the
last block with 39 antennas
Objects:
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RA (2000) DE Designation(s)
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05 35 14.16 -05 22 21.5 Orion BN-KL = NAME Orion BN/KL
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