<i>HERschel</i>KEY PROGRAM HERITAGE: A FAR-INFRARED SOURCE CATALOG FOR THE MAGELLANIC CLOUDS

Seale, Jonathan; Meixner, Margaret; Sewiło, M.; Babler, B.; Engelbracht, C. W.; Gordon, K. D.; Hony, S.; Misselt, K. A.; Montiel, Edward; Okumura, K.; Panuzzo, P.; Roman-Duval, Julia; Sauvage, M.; Boyer, Martha L.; Chen, C.-H. Rosie; Indebetouw, R.; Matsuura, M.; Oliveira, J. M.; Srinivasan, S.; Loon, Jacco T H Van; Whitney, B. A.; Woods, Paul

doi:10.1088/0004-6256/148/6/124

Cited by 72 publications

(151 citation statements)

References 79 publications

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“…Rather, the underestimate of T ex by as- suming a filled beam and optically thick 12 CO emission, in addition to the somewhat high value of the H 2 / 13 CO ratio we adopt, is likely biasing the LTE masses high. The bright, compact CO source in the southern part of the PCC is associated with an infrared (IR) point source seen in the SAGE and HERITAGE surveys of the LMC, with a 24 µm flux of 4.87±0.09 mJy (Seale et al 2014). In conjunction with the unusually broad line profile seen in the CO spectra (Fig.…”

Section: Comparison With 13 Co-based Massesmentioning

confidence: 80%

“…4 and 5), this is indicative of a luminous young stellar object (YSO) or compact cluster that is driving a powerful wind or outflow. Seale et al (2014) obtain a far-IR luminosity of 330±74 L for this source (designated J81.048316−71.913885) based on graybody fitting to HERITAGE photometry. We further combined the available 2MASS, SAGE, and HERITAGE photometry with SED fitting to the models of Robitaille et al (2007) to estimate a total luminosity of ∼1000 L .…”

Section: Comparison With 13 Co-based Massesmentioning

confidence: 99%

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ALMA Observations of a Quiescent Molecular Cloud in the Large Magellanic Cloud

Wong

Hughes

Tokuda

et al. 2017

ApJ

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We present high-resolution (sub-parsec) observations of a giant molecular cloud in the nearest star-forming galaxy, the Large Magellanic Cloud. ALMA Band 6 observations trace the bulk of the molecular gas in 12 CO(2-1) and high column density regions in 13 CO(2-1). Our target is a quiescent cloud (PGCC G282.98−32.40, which we refer to as the "Planck cold cloud" or PCC) in the southern outskirts of the galaxy where star-formation activity is very low and largely confined to one location. We decompose the cloud into structures using a dendrogram and apply an identical analysis to matched-resolution cubes of the 30 Doradus molecular cloud (located near intense star formation) for comparison. Structures in the PCC exhibit roughly 10 times lower surface density and 5 times lower velocity dispersion than comparably sized structures in 30 Dor, underscoring the non-universality of molecular cloud properties. In both clouds, structures with relatively higher surface density lie closer to simple virial equilibrium, whereas lower surface density structures tend to exhibit super-virial line widths. In the PCC, relatively high line widths are found in the vicinity of an infrared source whose properties are consistent with a luminous young stellar object. More generally, we find that the smallest resolved structures ("leaves") of the dendrogram span close to the full range of line widths observed across all scales. As a result, while the bulk of the kinetic energy is found on the largest scales, the smallscale energetics tend to be dominated by only a few structures, leading to substantial scatter in observed size-linewidth relationships.

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Section: Comparison With 13 Co-based Massesmentioning

confidence: 80%

Section: Comparison With 13 Co-based Massesmentioning

confidence: 99%

ALMA Observations of a Quiescent Molecular Cloud in the Large Magellanic Cloud

Wong

Hughes

Tokuda

et al. 2017

ApJ

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“…Brightly illuminated arcs delineate the interfaces between the cold gas and the ionizing radiation, where subsequent generations of stars are thought to have been triggered (Walborn et al 2002). Studies at optical (De Marchi et al 2011;Kalari et al 2014), near-infrared (nIR; Rubio et al 1998;Brandner et al 2001), mid-infrared (mIR; Whitney et al 2008;Gruendl & Chu 2009;Walborn et al 2013), far-infrared (fIR; Seale et al 2014) and sub-millimeter (Johansson et al 1998;Indebetouw et al 2013) wavelengths have identified evidence for active star formation throughout the 30 Doradus nebula, consistent with the idea of multiple star formation episodes. We focus on the stapler nebula that lies 2-14 pc away from R 136 (see Fig.…”

Section: Introductionmentioning

confidence: 99%

“…Gruendl & Chu (2009) detect objects in the dense and nebulous surroundings using detailed aperture photometry (see Section 6.3 of Gruendl & Chu (2009) for a comparison). Photometry in the fIR at 100 and 160µm, and 250 and 350µm of point-like and extended sources in the stapler nebula is given in Seale et al (2014), using images taken by the Herschel space telescope PACS (Photoconductor Array Camera and Spectrometer), and SPIRE (Spectral and Photometric Imaging Receiver) instruments respectively as part of the Hershel large program HERITAGE (HERschel Inventory of The Agents of Galaxy Evolution; Meixner et al 2013). The FWHM for these images are 8 , 12 , 18 and 25 respectively.…”

Section: Introductionmentioning

confidence: 99%

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

Kalari

Rubio

Elmegreen

et al. 2018

ApJ

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New sensitive CO (2-1) observations of the 30 Doradus region in the Large Magellanic Cloud are presented. We identify a chain of three newly discovered molecular clouds we name KN1, KN2 and KN3 lying within 2-14 pc in projection from the young massive cluster R 136 in 30 Doradus. Excited H 2 2.12µm emission is spatially coincident with the molecular clouds, but ionized Brγ emission is not. We interpret these observations as the tails of pillar-like structures whose ionized heads are pointing towards R 136. Based on infrared photometry, we identify a new generation of stars forming within this structure.

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Complex Organic Molecules in Star-Forming Regions of the Magellanic Clouds

Sewiło

Charnley

Schilke

et al. 2019

ACS Earth Space Chem.

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The Large and Small Magellanic Clouds (LMC and SMC), gas-rich dwarf companions of the Milky Way, are the nearest laboratories for detailed studies on the formation and survival of complex organic molecules (COMs) under metal poor conditions. To date, only methanol, methyl formate, and dimethyl ether have been detected in these galaxies -all three toward two hot cores in the N113 star-forming region in the LMC, the only extragalactic sources exhibiting complex hot core chemistry. We describe a small and diverse sample of the LMC and SMC sources associated with COMs or hot core chemistry, and compare the observations to theoretical model predictions. Theoretical models accounting for the physical conditions and metallicity of hot molecular cores in the Magellanic Clouds have been able to broadly account for the existing observations, but fail to reproduce the dimethyl ether abundance by more than an order of magnitude. We discuss future prospects for research in the field of complex chemistry in the low-metallicity environment. The detection of COMs in the Magellanic Clouds has important implications for astrobiology. The metallicity of the Magellanic Clouds is similar to galaxies in the earlier epochs of the Universe, thus the presence of COMs in the LMC and SMC indicates that a similar prebiotic chemistry leading to the emergence of life, as it happened on Earth, is possible in lowmetallicity systems in the earlier Universe.

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HERschelKEY PROGRAM HERITAGE: A FAR-INFRARED SOURCE CATALOG FOR THE MAGELLANIC CLOUDS

Cited by 72 publications

References 79 publications

ALMA Observations of a Quiescent Molecular Cloud in the Large Magellanic Cloud

ALMA Observations of a Quiescent Molecular Cloud in the Large Magellanic Cloud

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

Complex Organic Molecules in Star-Forming Regions of the Magellanic Clouds

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