A multiwavelength study of the star forming region IRAS 18544+0112

Aims: This work aims at investigating the molecular and infrared components in the massive young stellar object (MYSO) candidate IRAS 18544+0112. The purpose is to determine the nature and the origin of this infrared source. Methods: To analyze the molecular gas towards IRAS 18544+0112, we have carr...

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Detalles Bibliográficos
Autores principales: Ortega, M.E., Paron, S., Cichowolski, S., Rubio, M., Castelletti, G., Dubner, G.
Formato: JOUR
Materias:
HII regions
ISM: molecules
Stars: formation
Angular resolution
Atacama
Emission profile
H II regions
High density
Infrared components
Infrared emissions
Infrared source
Ionized gas
Molecular analysis
Molecular clumps
Molecular gas
Molecular outflows
Multi-wavelength study
Near-infrared photometry
Non-detection
Point sources
Public data
Spitzer
Star-forming region
Submillimeters
Young stellar objects
Ionization of gases
Light sources
Molecules
Stars
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v510_n1_p_Ortega
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
Descripción
Sumario:Aims: This work aims at investigating the molecular and infrared components in the massive young stellar object (MYSO) candidate IRAS 18544+0112. The purpose is to determine the nature and the origin of this infrared source. Methods: To analyze the molecular gas towards IRAS 18544+0112, we have carried out observations in a 90″ × 90″ region around l = 34.°69, b = -0.°65, using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12CO J = 3-2, 13CO J = 3-2, HCO + J = 4-3 and CS J = 7-6 lines with an angular resolution of 22″. The infrared emission in the area has been analyzed using 2MASS and Spitzer public data. Results: From the molecular analysis, we find self-absorbed 12CO J = 3-2 profiles, which are typical in star forming regions, but we do not find any evidence of outflow activity. Moreover, we do not detect either HCO +J = 4-3 or CS J = 7-6 in the region, which are species normally enhanced in molecular outflows and high density envelopes. The 12CO J = 3-2 emission profile suggests the presence of expanding gas in the region. The Spitzer images reveal that the infrared source has a conspicuous extended emission bright at 8 μm with an evident shell-like morphology of ∼1.′5 in size (∼1.4 pc at the proposed distance of 3 kpc) that encircles the 24 μm emission. The non-detection of ionized gas related to IRAS 18544+0112 together with the fact that it is still embedded in a molecular clump suggest that IRAS 18544+0112 has not reached the UCHII region stage yet. Based on near infrared photometry we search for YSO candidates in the region and propose that 2MASS 18565878+0116233 is the infrared point source associated with IRAS 18544+0112. Finally, we suggest that the expansion of a larger nearby HII region, G034.8-0.7, might be related to the formation of IRAS 18544+0112. © 2010 ESO.

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