Massive Star Formation in NGC 2074

Fleener, Christine E.; Payne, James T.; Chu, You‐Hua; Chen, C.-H. Rosie; Gruendl, R. A.

doi:10.1088/0004-6256/139/1/158

Cited by 6 publications

(11 citation statements)

References 26 publications

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“…Infrared photometry from SAGE (Meixner et al 2006 Romita et al (2010), Chen et al (2010), Fleener et al (2010), Woods et al (2011), or Shimonishi et al (2008. Not all sources are well-represented in our SAGE photometry, and not all are well-fit.…”

Section: Allmentioning

confidence: 91%

“…Chen et al (2010) are probably MS stars in front of bright dust. Similarly, Fleener et al (2010) study high mass star formation in NGC 2074 and find 5 of the 10 GC09 YSO candidates show signs of multiplicity. Three 22-GHz water masers have also been observed.…”

Section: N160mentioning

confidence: 95%

“…Designations from Chen et al (2009) in N44 andChen et al (2010) in N159/N160 are preceded by Chen_... followed by the native designation; in N206 Romita_... for sources from Romita et al (2010);Fleener et al (2010) iii.…”

Section: Allmentioning

confidence: 99%

“…We consider 1045 sources to be well-fit YSOs, 127 of which are also selected by W08, GC09, Chen et al (2009), Romita et al (2010, Chen et al (2010), Fleener et al (2010), or some combination. For completeness, our images and photometric catalog include another 358 YSO candidates from those lists, most of which do meet our color-selection criteria but are not well fit by YSO models.…”

Section: Application To Nine Star-forming Regionsmentioning

confidence: 99%

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Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

Carlson

Sewiło

Meixner

et al. 2012

A&A

110

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We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine Hii regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, AJ, 132, 2268, combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997, AJ, 114, 1002 and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, PASJ, 59, 615). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007, ApJS, 169, 328) and estimate mass functions and SFRs for each region.

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Section: Allmentioning

confidence: 91%

Section: N160mentioning

confidence: 95%

Section: Allmentioning

confidence: 99%

Section: Application To Nine Star-forming Regionsmentioning

confidence: 99%

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Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

Carlson

Sewiło

Meixner

et al. 2012

A&A

110

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“…A trend is observed in YSOs in H II regions in the Milky Way and the LMC that in triggered star formation, the second generation is less massive than the first (e.g., Pomarès et al 2009;Fleener et al 2010). In N 159, the most massive YSO formed in the eastern GMC, 054004.40−694437.6, is O6 V (Indebetouw et al 2004), not as massive as the earliest type O4-6 Vn found in the central H II region (#54 in Fariña et al 2009).…”

Section: Massive Star Formation -Triggered or Spontaneous?mentioning

confidence: 99%

SPITZERVIEW OF YOUNG MASSIVE STARS IN THE LARGE MAGELLANIC CLOUD H II COMPLEXES. II. N 159

Chen

Indebetouw

Chu

et al. 2010

ApJ

Self Cite

161

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The H ii complex N 159 in the Large Magellanic Cloud is used to study massive star formation in different environments, as it contains three giant molecular clouds (GMCs) that have similar sizes and masses but exhibit different intensities of star formation. We identify candidate massive young stellar objects (YSOs) using infrared photometry, and model their spectral energy distributions to constrain mass and evolutionary state. Good fits are obtained for less evolved Type I, I/II, and II sources. Our analysis suggests that there are massive embedded YSOs in N 159B, a maser source, and several ultracompact H ii regions. Massive O-type YSOs are found in GMCs N 159-E and N 159-W, which are associated with ionized gas, i.e., where massive stars formed a few Myr ago. The third GMC, N 159-S, has neither O-type YSOs nor evidence of previous massive star formation. This correlation between current and antecedent formation of massive stars suggests that energy feedback is relevant. We present evidence that N 159-W is forming YSOs spontaneously, while collapse in N 159-E may be triggered. Finally, we compare star formation rates determined from YSO counts with those from integrated Hα and 24 μm luminosities and expected from gas surface densities. Detailed dissection of extragalactic GMCs like the one presented here is key to revealing the physics underlying commonly used star formation scaling laws.

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Velocity profiles of [C_II], [C_I], CO, and [O_I] and physical conditions in four star-forming regions in the Large Magellanic Cloud

Okada

Güsten

Requeña-Torres

et al. 2019

A&A

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Aims. The aim of our study is to investigate the physical properties of the star-forming interstellar medium (ISM) in the Large Magellanic Cloud (LMC) by separating the origin of the emission lines spatially and spectrally. The LMC provides a unique local template to bridge studies in the Galaxy and high redshift galaxies because of its low metallicity and proximity, enabling us to study the detailed physics of the ISM in spatially resolved individual star-forming regions. Following Okada et al. (2015, Paper I), we investigate different phases of the ISM traced by carbon-bearing species in four star-forming regions in the LMC, and model the physical properties using the KOSMA-τ PDR model. Methods. We mapped 3-13 arcmin 2 areas in 30 Dor, N158, N160 and N159 along the molecular ridge of the LMC in [C ii] 158 µm with GREAT on board SOFIA. We also observed the same area with CO(2-1) to (6-5), 13 CO(2-1) and (3-2), [C i] 3 P 1 -3 P 0 and 3 P 2 -3 P 1 with APEX. For selected positions in N159 and 30 Dor, we observed [O i] 145 µm and [O i] 63 µm with upGREAT. All spectra are velocity resolved. Results. In all four star-forming regions, the line profiles of CO, 13 CO, and [C i] emission are similar, being reproduced by a combination of Gaussian profiles defined by CO(3-2), whereas [C ii] typically shows wider line profiles or an additional velocity component. At several positions in N159 and 30 Dor, we observed the velocity-resolved [O i] 145 µm and 63 µm lines for the first time. At some positions, the [O i] line profiles match those of CO, at other positions they are more similar to the [C ii] profiles. We interpret the different line profiles of CO, [C ii] and [O i] as contributions from spatially separated clouds and/or clouds in different physical phases, which give different line ratios depending on their physical properties. We model the emission from the CO, [C i], [C ii], and [O i] lines and the far-infrared continuum emission using the latest KOSMA-τ PDR model, which treats the dust-related physics consistently and computes the dust continuum SED together with the line emission of the chemical species. We find that the line and continuum emissions are not well-reproduced by a single clump ensemble. Toward the CO peak at N159 W, we propose a scenario that the CO, [C ii], and [O i] 63 µm emission are weaker than expected because of mutual shielding among clumps.

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Massive Star Formation in NGC 2074

Cited by 6 publications

References 26 publications

Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

SPITZERVIEW OF YOUNG MASSIVE STARS IN THE LARGE MAGELLANIC CLOUD H II COMPLEXES. II. N 159

Velocity profiles of [C_II], [C_I], CO, and [O_I] and physical conditions in four star-forming regions in the Large Magellanic Cloud

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Massive Star Formation in NGC 2074

Cited by 6 publications

References 26 publications

Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

SPITZERVIEW OF YOUNG MASSIVE STARS IN THE LARGE MAGELLANIC CLOUD H II COMPLEXES. II. N 159

Velocity profiles of [CII], [CI], CO, and [OI] and physical conditions in four star-forming regions in the Large Magellanic Cloud

Contact Info

Product

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Velocity profiles of [C_II], [C_I], CO, and [O_I] and physical conditions in four star-forming regions in the Large Magellanic Cloud