@Article{MachaieieViWuRaMyHi:2017:PrDeCo,
               author = "Machaieie, Dinelsa Antonio and Vilas Boas, Jos{\'e} Williams dos 
                         Santos and Wuensche, Carlos Alexandre and Racca, Germ{\'a}n A. 
                         and Myers, Philip C. and Hickel, Gabriel R.",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)} and {Universidade do Estado do Rio 
                         Grande do Norte (UERN)} and {Harvard-Smithsonian Center for 
                         Astrophysics} and {Universidade Federal de Itajub{\'a} 
                         (UNIFEI)}",
                title = "Properties of dense cores embedded in musca derived from 
                         extinction maps and 13CO, C18O, and NH3 emission lines",
              journal = "Astrophysical Journal",
                 year = "2017",
               volume = "836",
               number = "1",
                month = "Feb.",
             keywords = "dust, extinction, ISM: kinematics and dynamics, ISM: molecules, 
                         radio lines: ISM.",
             abstract = "Using near-infrared data from the Two Micron All Sky Survey 
                         catalog and the Near Infrared Color Excess method, we studied the 
                         extinction distribution in five dense cores of Musca, which show 
                         visual extinction greater than 10 mag and are potential sites of 
                         star formation. We analyzed the stability in four of them, fitting 
                         their radial extinction profiles with Bonnor-Ebert isothermal 
                         spheres, and explored their properties using the J. =. 1-0 
                         transition of (CO)-C-13 and (CO)-O-18 and the J = K = 1 transition 
                         of NH3. One core is not well described by the model. The stability 
                         parameter of the fitted cores ranges from 4.5 to 5.7 and suggests 
                         that all cores are stable, including Mu13, which harbors one young 
                         stellar object (YSO), the IRAS 12322-7023 source. However, the 
                         analysis of the physical parameters shows that Mu13 tends to have 
                         larger AV, nc, and Pext than the remaining starless cores. The 
                         other physical parameters do not show any trend. It is possible 
                         that those are the main parameters to explore in active 
                         star-forming cores. Mu13 also shows the most intense emission of 
                         NH3. Its (CO)-C-13 and (CO)-O-18 lines have double peaks, whose 
                         integrated intensity maps suggest that they are due to the 
                         superposition of clouds with different radial velocities seen in 
                         the line of sight. It is not possible to state whether these 
                         clouds are colliding and inducing star formation or are related to 
                         a physical process associated with the formation of the YSO.",
                  doi = "10.3847/1538-4357/836/1/19",
                  url = "http://dx.doi.org/10.3847/1538-4357/836/1/19",
                 issn = "0004-637X and 1538-4357",
             language = "en",
           targetfile = "machaieie_properties.pdf",
        urlaccessdate = "27 abr. 2024"
}