SIMBA survey of southern high-mass star forming regions. I. Physical parameters of the 1.2-mm/IRAS sources

By S. Faúndez, L. Bronfman, G. Garay, Rolf Chini, L. Nyman, J. May. 2004

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In Astronomy and Astrophysics

Citations in the corpus

The earliest phases of high-mass star formation: a 3 square degree millimeter continuum mapping of Cygnus X (2007, background): “In this way, studies by e.g., Molinari et al. (2000) and Sridharan et al. (2002) have identified massive young stellar objects harboring highluminosity infrared protostars (see also Mueller et al. 2002; Faúndez et al. 2004).”
STELLAR FEEDBACK IN MOLECULAR CLOUDS AND ITS INFLUENCE ON THE MASS FUNCTION OF YOUNG STAR CLUSTERS (2009, methodology): “In Figure 1, we plot Σ and Rh against M for starforming molecular clumps in the Milky Way, based on measurements of CS, C17O, and 1.2 mm dust emission in three independent surveys (Shirley et al. 2003; Faúndez et al. 2004; Fontani et al. 2005).”
Fragmentation of massive protostellar discs (2006, background): “…imply a column density Σcl of around 1 g cm −2 for the clumps that host massive star formation (Plume et al. 1997; Hillenbrand & Hartmann 1998; Figer et al. 1999; Kim et al. 2000; van den Bergh et al. 1991; Gilbert & Graham 2001; de Marchi et al. 1997; Turner et al. 2000; Faúndez et al. 2004).”
The simultaneous formation of massive stars and stellar clusters (2009, background): “…2000; Rathborne, Jackson & Simon 2006; Simon et al. 2006) and high-mass protostellar objects (HMPOs) (Beuther et al. 2002; Sridharan et al. 2002; Faúndez et al. 2004; Williams, Fuller & Sridharan 2004) have begun to probe the earliest stages of the massive clumps from which star clusters are…”
Fragmentation and mass segregation in the massive dense cores of Cygnus X (2009, background): “…of luminous IRAS or maser sources in the whole galactic plane (Molinari et al. 1996, Plume et al. 1997, Beuther et al. 2002b, Mueller et al. 2002, Faúndez et al. 2004), and more recently inside the dark filaments seen in the infrared surveys of the Galactic plane, the so-called IRDCs (e.g.…”
THE LONG-TERM EVOLUTION OF THE GALACTIC DISK TRACED BY DISSOLVING STAR CLUSTERS (2010, background): “Observations of gas-dominated cluster-forming regions show column densities of ∼ 0.1 − 3 g cm−2 (Plume et al. 1997; Mueller et al. 2002; Shirley et al. 2003; Faúndez et al. 2004; Fontani et al. 2005); the data are summarized in Figure 1 of Fall et al. (2010).”
RADIATION-HYDRODYNAMIC SIMULATIONS OF THE FORMATION OF ORION-LIKE STAR CLUSTERS. II. THE INITIAL MASS FUNCTION FROM WINDS, TURBULENCE, AND RADIATION (2012, background): “In contrast, the mean mass and radius of the star-forming regions studied by Faúndez et al. (2004) implies a volume density > 105 cm−3, a mass of ∼ 5000 M , and a column density of 2 g cm −2, such that multiple massive stars would be expected, and their radiation would be trapped effectively by…”
ATLASGAL - The APEX telescope large area survey of the galaxy at 870 μm (2009, background): “…showing far-infrared (FIR) colors typical of ultra-compact Hii regions (Wood & Churchwell 1989), e.g., in high-density molecular tracers (Bronfman et al. 1996; Molinari et al. 1996), dust continuum emission (Faúndez et al. 2004), or maser emission (e.g., Palla et al. 1993; Beuther et al. 2002).”
CHEMISTRY IN INFRARED DARK CLOUD CLUMPS: A MOLECULAR LINE SURVEY AT 3 mm (2011, background): “Considering the last point, since the size of the Mo- pra beam is 38′′, we are typically observing emission on physical scales ∼0.8 pc. Typical sizes of clumps in high-mass star-forming regions and in IRDCs are ∼0.4 pc (Faúndez et al. 2004) and ∼0.5 pc (Rathborne et al. 2006), respectively.”
Star Formation in the Milky Way and Nearby Galaxies (2012, result): “Very similar results were obtained from studies of millimeter continuum emission from dust (Faúndez et al. 2004) toward a sample of southern hemisphere sources surveyed in CS J = 2 → 1 (Bronfman et al. 1996).”