Aortic Intramural Hematoma Associated with Primary Aldosteronism

Chung, Jin Ook; Cho, Dong Hyeok; Chung, Dong Jin; Chung, Min Young

doi:10.3803/jkes.2009.24.3.217

Cited by 3 publications

(3 citation statements)

References 17 publications

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“…We have shown that cyanoacetylene is an excellent dense gas tracer (see also Morris et al 1976, Chung et al 1991, Bergin 1996. In particular, we find that the column density of HC 3 N in the hot core is up to two orders of magnitude higher than in the other Orion cloud components.…”

Section: Discussionmentioning

confidence: 94%

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N

Esplugues

Cernicharo

Viti

et al. 2013

A&A

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Context. We present a study of cyanoacetylene (HC 3 N) and cyanodiacetylene (HC 5 N) in Orion KL using observations from two line surveys performed with the IRAM 30-m telescope and the HIFI instrument onboard the Herschel telescope. The frequency ranges covered are 80−280 GHz and 480−1906 GHz. Aims. This study (divided by families of molecules) is part of a global analysis of the physical conditions of Orion KL and the molecular abundances in the different components of this cloud. Methods. We modeled the observed lines of HC 3 N, HC 5 N, their isotopologues (including DC 3 N), and vibrational modes using a non-local thermodynamic equilibrium (non-LTE) radiative transfer code. In addition, to investigate the chemical origin of HC 3 N and DC 3 N in Orion KL, we used a time-dependent chemical model. Results. We detect 40 lines of the ground vibrational state of HC 3 N and 68 lines of its 13 C isotopologues. We also detect 297 lines of six vibrational modes of this molecule (ν 7 , 2ν 7 , 3ν 7 , ν 6 , ν 5 , and ν 6 +ν 7 ) and 35 rotational lines of the ground vibrational state of HC 5 N. We report the first tentative detection of DC 3 N in a giant molecular cloud. We have obtained a DC 3 N/HC 3 N abundance ratio of 0.015 ± 0.009, similar to typical D/H ratios of cold dark clouds. We provide column densities for all species and derived isotopic and molecular abundances. We also made a 2 × 2 map around Orion IRc2 and present maps of the HC 3 N lines with energies from 34 to 154 K and of the HC 3 N vibrational modes ν 6 and ν 7 with energies between 354 and 872 K. In addition, a comparison of our results for HC 3 N with those in other clouds has allowed us to derive correlations between the column density, the FWHM, the mass, and the luminosity of the clouds. Conclusions. The high column densities of HC 3 N obtained in the hot core, in particular of the ground vibrational state and the vibrational mode ν 7 , make this molecule an excellent tracer of hot and dense gas. In addition, the wide frequency range covered reveals the need to consider a temperature and density gradient in the hot core to obtain better line fits. The high D/H ratio (similar to that obtained in cold clouds) that we derive suggests a deuterium enrichment. Our chemical models indicate that the possible deuterated HC 3 N in Orion KL is formed during the gas-phase. This fact provides new hints concerning the processes leading to deuteration.

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Section: Discussionmentioning

confidence: 94%

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N

Esplugues

Cernicharo

Viti

et al. 2013

A&A

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“…This was further confirmed by the carbon-bearing species HNCO, which is typically only seen in the hot cores around high-mass protostars once molecules have been liberated off dust grains by radiation or shocks (Brown et al 1988). HC 3 N is an excellent tracer of dense gas (Chung et al 1991;Bergin et al 1996) as it has high electric dipole moments (µ = 3.72 Debye).…”

Section: Other Lines and Siomentioning

confidence: 85%

A multi-transition molecular line study of infrared dark cloud G331.71+00.59

Yu¹,

Wang²

2013

Res. Astron. Astrophys.

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Using archive data from the Millimeter Astronomy Legacy Team Survey at 90 GHz (MALT90), carried out by Mopra 22-m telescope, we made a first multi-transition molecular line study of infrared dark cloud (IRDC) MSXDC G331.71+00.59. Two molecular cores were found embedded in this IRDC. Each of these cores is associated with a known "extended green object" (EGO), indicating places of massive star formation. The HCO + (1-0) and HNC (1-0) transitions show prominent blue or red asymmetric structures, suggesting outflow and inflow activities of young stellar objects (YSOs). Other detected molecule lines include H 13 CO + (1-0), C 2 H (1-0), HC 3 N (10-9), HNCO(4 0,4 -3 0,3 ), SiO (2-1) typical of hot cores and outflows. We regard the two EGOs are evolving from IRDC to hot cores. Using public GLIMPS data, we investigate the spectral energy distribution of EGO G331.71+0.60, supporting this EGO is a massive young stellar object (MYSO) driving outflow. G331.71+0.58 may be at an earlier evolutionary stage.

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“…The millimetre wavelength window is important for studying massive star formation, because it contains many useful molecular probes, such as shock tracers (SiO, SO, HNCO and H 2 CO; Schilke et al 1997;Esplugues et al 2013;Rizzo, Fuente & García-Burillo 2005), long carbon chain molecules (c-C 3 H 2 , HC 3 N and HC 5 N; Morris, Snell & vanden Bout 1977;Chung, Osamu & Masaki 1991;Bergin, Snell & Goldsmith 1996), deuterated molecules (DCN, DCO + , C 2 D and NH 2 D; Shah & Wootten 2001;Pety et al 2007;Parise et al 2009) and dense gas traces (HCN, HCO + , CS and C 2 H; Padovani et al 2009), etc.…”

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confidence: 99%

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Wang

Zhang

et al. 2017

Mon. Not. R. Astron. Soc.

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We present spectral line mapping observations towards four massive star-forming regionsCepheus A, DR21S, S76E and G34.26+0.15 -with the IRAM 30-m telescope at the 2 and 3 mm bands. In total, 396 spectral lines from 51 molecules, one helium recombination line, 10 hydrogen recombination lines and 16 unidentified lines were detected in these four sources. An emission line of nitrosyl cyanide (ONCN, 14 0, 14 -13 0, 13 ) was detected in G34.26+0.15, as the first detection in massive star-forming regions. We found that c-C 3 H 2 and NH 2 D show enhancement in shocked regions, as suggested by the evidence of SiO and/or SO emission. The column density and rotational temperature of CH 3 CN were estimated with the rotational diagram method for all four sources. Isotope abundance ratios of 12 C/ 13 C were derived using HC 3 N and its 13 C isotopologue, which were around 40 in all four massive star-forming regions and slightly lower than the local interstellar value (∼65). The 14 N/ 15 N and 16 O/ 18 O abundance ratios in these sources were also derived using the double isotopic method, which were slightly lower than in the local interstellar medium. Except for Cep A, the 33 S/ 34 S ratios in the other three targets were derived, which were similar to that in the local interstellar medium. The column density ratios of N(DCN)/N(HCN) and N(DCO + )/N(HCO + ) in these sources were more than two orders of magnitude higher than the elemental [D]/[H] ratio, which is 1.5 × 10 −5 . Our results show that the later stage sources, G34.26+0.15 in particular, present more molecular species than earlier stage sources. Evidence of shock activity is seen in all stages studied.

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Aortic Intramural Hematoma Associated with Primary Aldosteronism

Cited by 3 publications

References 17 publications

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N

A multi-transition molecular line study of infrared dark cloud G331.71+00.59

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

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Aortic Intramural Hematoma Associated with Primary Aldosteronism

Cited by 3 publications

References 17 publications

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC3N

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC3N

A multi-transition molecular line study of infrared dark cloud G331.71+00.59

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

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Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N