ASTE observations in the 345 GHz window towards the HII region N113 of the large magellanic cloud

Aims: The HII region N113 is located in the central part of the Large Magellanic Cloud (LMC) with an associated molecular cloud that is very rich in molecular species. Most of the previously observed molecular lines cover the frequency range 85-270 GHz. Thus, a survey and study of lines at the 345 G...

Descripción completa

Guardado en:

Detalles Bibliográficos
Publicado:	2014
Materias:	Galaxies:SM HII regions ISM: individual objects: N113 ISM: molecules Magellanic Clouds Clouds Density of gases Stars Excitation conditions H II regions ISM: individual objects Large magellanic clouds Local thermodynamic equilibrium Photo-dissociation regions Galaxies
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v572_n_p_Paron http://hdl.handle.net/20.500.12110/paper_00046361_v572_n_p_Paron
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00046361_v572_n_p_Paron
record_format	dspace
spelling	paper:paper_00046361_v572_n_p_Paron2023-06-08T14:28:08Z ASTE observations in the 345 GHz window towards the HII region N113 of the large magellanic cloud Galaxies:SM HII regions ISM: individual objects: N113 ISM: molecules Magellanic Clouds Clouds Density of gases Stars Excitation conditions H II regions ISM: individual objects ISM: molecules Large magellanic clouds Local thermodynamic equilibrium Magellanic Clouds Photo-dissociation regions Galaxies Aims: The HII region N113 is located in the central part of the Large Magellanic Cloud (LMC) with an associated molecular cloud that is very rich in molecular species. Most of the previously observed molecular lines cover the frequency range 85-270 GHz. Thus, a survey and study of lines at the 345 GHz window is required for a more complete understanding of the chemistry and excitation conditions of this region. Methods: We mapped a region of 2;5 × 2;5 centred at N113 using the Atacama Submillimeter Telescope Experiment in the 13CO J = 3-2 line with an angular and spectral resolution of 22″ and 0.11 km s-1. In addition, we observed 16 molecular lines as single pointings towards its centre. Results: From the 13CO J=3-2 map we estimate the local thermodynamic equilibrium (LTE) and virial masses in about 1 × 104 and 4.5 × 104M? for the molecular cloud associated with N113. From the dust continuum emission at 500 μm we additionally obtain a mass of gas of 7 × 103M?. Towards the cloud centre we detected emission from 12CO, 13CO, C18O (3-2), HCN, HNC, HCO+, C2H (4-3), and CS (7-6); these are the first reported detections of the HCN, HNC, and C2H (4-3) lines from this region. We confirm the detection of CS (7-6), which was previously tentatively detected. From analysing the HCN, HNC, and C2H lines we suggest that they might be emitted from a photodissociation region (PDR). Moreover, we suggest that the chemistry involving the C2H lines in N113 is probably similar to that in Galactic PDRs. We analysed the HCN J = 4-3, J = 3-2, and J = 1-0 lines with the code RADEX and we conclude that we observe very high density gas, between some 105 and 107 cm-3. © ESO, 2014. 2014 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v572_n_p_Paron http://hdl.handle.net/20.500.12110/paper_00046361_v572_n_p_Paron
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Galaxies:SM HII regions ISM: individual objects: N113 ISM: molecules Magellanic Clouds Clouds Density of gases Stars Excitation conditions H II regions ISM: individual objects ISM: molecules Large magellanic clouds Local thermodynamic equilibrium Magellanic Clouds Photo-dissociation regions Galaxies
spellingShingle	Galaxies:SM HII regions ISM: individual objects: N113 ISM: molecules Magellanic Clouds Clouds Density of gases Stars Excitation conditions H II regions ISM: individual objects ISM: molecules Large magellanic clouds Local thermodynamic equilibrium Magellanic Clouds Photo-dissociation regions Galaxies ASTE observations in the 345 GHz window towards the HII region N113 of the large magellanic cloud
topic_facet	Galaxies:SM HII regions ISM: individual objects: N113 ISM: molecules Magellanic Clouds Clouds Density of gases Stars Excitation conditions H II regions ISM: individual objects ISM: molecules Large magellanic clouds Local thermodynamic equilibrium Magellanic Clouds Photo-dissociation regions Galaxies
description	Aims: The HII region N113 is located in the central part of the Large Magellanic Cloud (LMC) with an associated molecular cloud that is very rich in molecular species. Most of the previously observed molecular lines cover the frequency range 85-270 GHz. Thus, a survey and study of lines at the 345 GHz window is required for a more complete understanding of the chemistry and excitation conditions of this region. Methods: We mapped a region of 2;5 × 2;5 centred at N113 using the Atacama Submillimeter Telescope Experiment in the 13CO J = 3-2 line with an angular and spectral resolution of 22″ and 0.11 km s-1. In addition, we observed 16 molecular lines as single pointings towards its centre. Results: From the 13CO J=3-2 map we estimate the local thermodynamic equilibrium (LTE) and virial masses in about 1 × 104 and 4.5 × 104M? for the molecular cloud associated with N113. From the dust continuum emission at 500 μm we additionally obtain a mass of gas of 7 × 103M?. Towards the cloud centre we detected emission from 12CO, 13CO, C18O (3-2), HCN, HNC, HCO+, C2H (4-3), and CS (7-6); these are the first reported detections of the HCN, HNC, and C2H (4-3) lines from this region. We confirm the detection of CS (7-6), which was previously tentatively detected. From analysing the HCN, HNC, and C2H lines we suggest that they might be emitted from a photodissociation region (PDR). Moreover, we suggest that the chemistry involving the C2H lines in N113 is probably similar to that in Galactic PDRs. We analysed the HCN J = 4-3, J = 3-2, and J = 1-0 lines with the code RADEX and we conclude that we observe very high density gas, between some 105 and 107 cm-3. © ESO, 2014.
title	ASTE observations in the 345 GHz window towards the HII region N113 of the large magellanic cloud
title_short	ASTE observations in the 345 GHz window towards the HII region N113 of the large magellanic cloud
title_full	ASTE observations in the 345 GHz window towards the HII region N113 of the large magellanic cloud
title_fullStr	ASTE observations in the 345 GHz window towards the HII region N113 of the large magellanic cloud
title_full_unstemmed	ASTE observations in the 345 GHz window towards the HII region N113 of the large magellanic cloud
title_sort	aste observations in the 345 ghz window towards the hii region n113 of the large magellanic cloud
publishDate	2014
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v572_n_p_Paron http://hdl.handle.net/20.500.12110/paper_00046361_v572_n_p_Paron
_version_	1768542247658192896

ASTE observations in the 345 GHz window towards the HII region N113 of the large magellanic cloud

Ejemplares similares