Pillars of Creation among Destruction: Star Formation in Molecular Clouds near R136 in 30 Doradus

Kalari, V.; Rubio, M.; Elmegreen, Bruce G.; Guzmán, Viviana V.; Zinnecker, H.; Herrera, Cinthya N.

doi:10.3847/1538-4357/aa99dc

Cited by 20 publications

(17 citation statements)

References 52 publications

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“…Using the Atacama Large Millimeter Array and the Australia Telescope Compact Array, Indebetouw et al (2013), Anderson et al (2014) and Nayak et al (2016) find molecular clumps in the filamentary structure around R136 that seem to be gravitationally unstable and are likely to collapse to form the next generation of stars. This is in the same region where Walborn & Blades (1987) already identified knots of embedded young stars and where Kalari et al (2018) suggest that stars currently form. Also maser emission is found in these regions, indicative of young massive objects hidden from direct view (e.g.…”

Section: Overview Of Star Formation In 30 Dorsupporting

confidence: 58%

“…Walborn & Blades 1997;Grebel & Chu 2000;De Marchi et al 2011) whereas the youngest stars are still embedded in dense molecular clumps, primarily found to the north and west of R136 (e.g. Walborn & Blades 1987, 1997Hyland et al 1992;Rubio et al 1998;Brandner et al 2001;Walborn et al 2002;Maercker & Burton 2005;Nayak et al 2016;Kalari et al 2018). There are several star clusters such as Hodge 301 (15-30 Myr, e.g.…”

Section: Overview Of Star Formation In 30 Dormentioning

confidence: 99%

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The VLT-FLAMES Tarantula Survey

Schneider

Ramírez-Agudelo

Tramper

et al. 2018

A&A

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The 30 Doradus (30 Dor) nebula in the Large Magellanic Cloud (LMC) is the brightest HII region in the Local Group and a prototype starburst similar to those found in high redshift galaxies. It is thus a stepping stone to understand the complex formation processes of stars in starburst regions across the Universe. Here, we have studied the formation history of massive stars in 30 Dor using masses and ages derived for 452 mainly OB stars from the spectroscopic VLT-FLAMES Tarantula Survey (VFTS). We find that stars of all ages and masses are scattered throughout 30 Dor. This is remarkable because it implies that massive stars either moved large distances or formed independently over the whole field of view in relative isolation. We find that both channels contribute to the 30 Dor massive star population. Massive star formation rapidly accelerated about 8 Myr ago, first forming stars in the field before giving birth to the stellar populations in NGC 2060 and NGC 2070. The R136 star cluster in NGC 2070 formed last and, since then, about 1 Myr ago, star formation seems to be diminished with some continuing in the surroundings of R136. Massive stars within a projected distance of 8 pc of R136 are not coeval but show an age range of up to 6 Myr. Our mass distributions are well populated up to 200 M⊙. The inferred IMF is shallower than a Salpeter-like IMF and appears to be the same across 30 Dor. By comparing our sample of stars to stellar models in the Hertzsprung–Russell diagram, we find evidence for missing physics in the models above log L/L⊙ = 6 that is likely connected to enhanced wind mass loss for stars approaching the Eddington limit. Our work highlights the key information about the formation, evolution and final fates of massive stars encapsulated in the stellar content of 30 Dor, and sets a new benchmark for theories of massive star formation in giant molecular clouds.

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Section: Overview Of Star Formation In 30 Dorsupporting

confidence: 58%

Section: Overview Of Star Formation In 30 Dormentioning

confidence: 99%

The VLT-FLAMES Tarantula Survey

Schneider

Ramírez-Agudelo

Tramper

et al. 2018

A&A

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“…This ionizing photon flux is equivalent to the emission produced by ∼ 100 O5 stars in this HII region, and corresponds to the upper end of the incident UV fields modeled by Meijerink et al (2011); 10 5 G 0 , where G 0 = 1.6 × 10 −3 erg cm −2 s −1 (= one Habing). This would make TH6 a slightly more powerful version of the R136 cluster in the 30 Doradus region in the Large Magellanic Cloud (Kalari et al 2018).…”

Section: Radio Near-infrared and X-ray Diagnostics Of Dense Gas Heatingmentioning

confidence: 99%

Fire in the Heart: A Characterization of the High Kinetic Temperatures and Heating Sources in the Nucleus of NGC 253

Mangum

Ginsburg

Henkel

et al. 2019

ApJ

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“…11. Cut (a) goes through the so-called 'stapler nebula', where Kalari et al (2018) found three molecular clouds with CO(2-1). These authors suggested that we see the tails of pillarlike structures whose ionized heads are pointing toward R136, and that the large observed velocity dispersion can be explained by the velocity difference between the head and tail of a photoevaporating cloud.…”

Section: Dormentioning

confidence: 99%

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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Pillars of Creation among Destruction: Star Formation in Molecular Clouds near R136 in 30 Doradus

Cited by 20 publications

References 52 publications

The VLT-FLAMES Tarantula Survey

The VLT-FLAMES Tarantula Survey

Fire in the Heart: A Characterization of the High Kinetic Temperatures and Heating Sources in the Nucleus of NGC 253

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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Pillars of Creation among Destruction: Star Formation in Molecular Clouds near R136 in 30 Doradus

Cited by 20 publications

References 52 publications

The VLT-FLAMES Tarantula Survey

The VLT-FLAMES Tarantula Survey

Fire in the Heart: A Characterization of the High Kinetic Temperatures and Heating Sources in the Nucleus of NGC 253

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