The 30 Doradus Molecular Cloud at 0.4 pc Resolution with the Atacama Large Millimeter/submillimeter Array: Physical Properties and the Boundedness of CO-emitting Structures

Wong, Tony; Oudshoorn, Luuk; Eliyahu, Sofovich,; Green, Alex; Shah, Charmi; Indebetouw, R.; Meixner, Margaret; Hacar, A.; Nayak, Omnarayani; Tokuda, Kazuki; Bolatto, Alberto D.; Chevance, Mélanie; Marchi, Guido De; Fukui, Y.; Hirschauer, Alec S.; Jameson, Katherine; Kalari, V.; Lebouteiller, V.; Looney, Leslie W.; Madden, S. C.; Onishi, Toshikazu; Román-Duval, Julia; Rubio, M.; Tielens, A. G. G. M.

doi:10.3847/1538-4357/ac723a

Cited by 23 publications

(40 citation statements)

References 63 publications

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“…This result suggests that the super star cluster R136 and in general the massive-star formation to the north are not strongly affecting the physical conditions in the Ridge at this distance. This is consistent with the findings of Wong et al (2022) that there is little correlation with α vir for clouds in 30 Dor and their distance to R136.…”

Section: Spatial Dependencesupporting

confidence: 92%

“…This value of X 13CO is also consistent with using a typical galactic X CO factor of 2 × 10 20 cm −2 (K km s −1 ) −1 (Bolatto et al 2013) and a 13 CO (1-0)/ 12 CO (1-0) integrated intensity ratio of 0.12 (Finn et al 2021). The resulting column densities for 30 Dor also match the ranges of those calculated using LTE assumptions in Wong et al (2022).…”

Section: Derived Propertiessupporting

confidence: 86%

“…A mosaic of 30 Dor was observed as ALMA project 2019.1.00843.S and includes 12 m and 7 m interferometric data and total power data. Those data are presented and analyzed at their native resolution of 1 75 in Wong et al (2022). For this analysis, the resolution has been convolved to 13″ so that it can be directly compared with our data for the Molecular Ridge.…”

Section: Doradusmentioning

confidence: 99%

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Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud

Finn¹,

Indebetouw²,

Johnson³

et al. 2022

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We present a comparison of low-J 13CO and CS observations of four different regions in the LMC—the quiescent Molecular Ridge, 30 Doradus, N159, and N113, all at a resolution of ∼3 pc. The regions 30 Dor, N159, and N113 are actively forming massive stars, while the Molecular Ridge is forming almost no massive stars, despite its large reservoir of molecular gas and proximity to N159 and 30 Dor. We segment the emission from each region into hierarchical structures using dendrograms and analyze the sizes, masses, and line widths of these structures. We find that the Ridge has significantly lower kinetic energy at a given size scale and also lower surface densities than the other regions, resulting in higher virial parameters. This suggests that the Ridge is not forming massive stars as actively as the other regions because it has less dense gas and not because collapse is suppressed by excess kinetic energy. We also find that these physical conditions and energy balance vary significantly within the Ridge and that this variation appears only weakly correlated with distance from sites of massive-star formation such as R136 in 30 Dor, which is ∼1 kpc away. These variations also show only a weak correlation with local star formation activity within the clouds.

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Section: Spatial Dependencesupporting

confidence: 92%

Section: Derived Propertiessupporting

confidence: 86%

Section: Doradusmentioning

confidence: 99%

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Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud

Finn¹,

Indebetouw²,

Johnson³

et al. 2022

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“…To overcome this obstacle, our mass estimation method takes place in two parts (described in this section and Section 2.1.3). Additionally, our mass estimation method is similar to the approach taken by Wong et al (2022), who, in their study of the LMC's 30 Doradus region, found that 53% of CO-detected clumps were only traced by 12 CO and did not have corresponding 13 CO emission. The majority of the clumps in N90 with corresponding 13 CO emission are located in the northeast rim and nonrim sections near NGC 602, with several others on the northwest rim near the massive O3 star Sk 183 (see definitions of these subregions in Figure 7(a)).…”

Section: Molecular Column Densitymentioning

confidence: 86%

Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA

O'Neill

Indebetouw

Sandström

et al. 2022

ApJ

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NGC 602 is a young, low-metallicity star cluster in the “Wing” of the Small Magellanic Cloud. We reveal the recent evolutionary past of the cluster through analysis of high-resolution (∼0.4 pc) Atacama Large Millimeter/submillimeter Array observations of molecular gas in the associated H ii region N90. We identify 110 molecular clumps (R < 0.8 pc) traced by CO emission, and study the relationship between the clumps and associated young stellar objects (YSOs) and pre-main-sequence (PMS) stars. The clumps have high virial parameters (typical α vir = 4–11) and may retain signatures of a collision in the last ≲8 Myr between H i components of the adjacent supergiant shell SMC-SGS 1. We obtain a CO-bright-to-H2 gas conversion factor of X CO,B = (3.4 ± 0.2) × 1020 cm−2 (K km s−1)−1, and correct observed clump properties for CO-dark H2 gas to derive a total molecular gas mass in N90 of 16,600 ± 2400 M ⊙. We derive a recent (≲1 Myr) star formation rate of 130 ± 30 M ⊙ Myr−1 with an efficiency of 8% ± 3% assessed through comparing total YSO mass to total molecular gas mass. Very few significant radial trends exist between clump properties or PMS star ages and distance from NGC 602. We do not find evidence for a triggered star formation scenario among the youngest (≲2 Myr) stellar generations, and instead conclude that a sequential star formation process in which NGC 602 did not directly cause recent star formation in the region is likely.

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“…Although the large-scale H I flow scenario was originally designed to explain the R136 formation (Fukui et al 2017), the fact that the same flow distributes over kiloparsec scales motivates us to apply it describing the star formation history in N159. In a reimportation of this context, an ALMA wide-field imaging study found an N159-type conical molecular filament system around R136 (Wong et al 2022). These observational pieces of evidence may demonstrate that galaxy-scale (H I) gas flows and the subsequent more than a few ×10 pc scale filament system development are universally responsible for the super star cluster formation that can drive galaxy evolution itself.…”

Section: Muraoka Et Al 2020mentioning

confidence: 96%

An ALMA Study of the Massive Molecular Clump N159W-North in the Large Magellanic Cloud: A Possible Gas Flow Penetrating One of the Most Massive Protocluster Systems in the Local Group

Tokuda

Minami²,

Fukui

et al. 2022

ApJ

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Massive dense clumps in the Large Magellanic Cloud can be an important laboratory to explore the formation of populous clusters. We report multiscale ALMA observations of the N159W-North clump, which is the most CO-intense region in the galaxy. High-resolution CO isotope and 1.3 mm continuum observations with an angular resolution of ∼0.″25 (∼0.07 pc) revealed more than five protostellar sources with CO outflows within the main ridge clump. One of the thermal continuum sources, MMS-2, shows an especially massive/dense nature whose total H2 mass and peak column density are ∼104 M ⊙ and ∼1024 cm−2, respectively, and harbors massive (∼100 M ⊙) starless core candidates identified as its internal substructures. The main ridge containing this source can be categorized as one of the most massive protocluster systems in the Local Group. The CO high-resolution observations found several distinct filamentary clouds extending southward from the star-forming spots. The CO (1–0) data set with a larger field of view reveals a conical, ∼30 pc long complex extending toward the northern direction. These features indicate that a large-scale gas compression event may have produced the massive star-forming complex. Based on the striking similarity between the N159W-North complex and the other two previously reported high-mass star-forming clouds in the nearby regions, we propose a “teardrops inflow model” that explains the synchronized, extreme star formation across >50 pc, including one of the most massive protocluster clumps in the Local Group.

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The 30 Doradus Molecular Cloud at 0.4 pc Resolution with the Atacama Large Millimeter/submillimeter Array: Physical Properties and the Boundedness of CO-emitting Structures

Cited by 23 publications

References 63 publications

Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud

Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud

Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA

An ALMA Study of the Massive Molecular Clump N159W-North in the Large Magellanic Cloud: A Possible Gas Flow Penetrating One of the Most Massive Protocluster Systems in the Local Group

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