The SCUBA Legacy Catalogues: Submillimeter‐Continuum Objects Detected by SCUBA

Francesco, James Di; Johnstone, Doug; Kirk, Helen; Mackenzie, T.; Ledwosinska, Elizabeth

doi:10.1086/523645

Cited by 350 publications

(466 citation statements)

References 24 publications

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“…A careful comparison requires not only consideration of the differing beamsizes at each wavelength, but also proper treatment of the full beam profile, which, for the JCMT, includes a significant amount of flux in the "secondary" beam at 450 μm (Di Francesco et al 2008;Dempsey et al 2013). Using the procedure outlined in Pattle et al (2015) and Rumble et al (2015), D. Rumble et al(2017, in preparation) compiled temperature estimates for all of the GBS clouds based on the Legacy Release 1 reductions (see Section3.1 and Mairs et al 2015).…”

Section: Discussionmentioning

confidence: 99%

“…These original reductions are not directly available for comparison. The SCUBA Legacy Catalog reduction (Di Francesco et al 2008) of the Northern Streamer, however, is available in the archive and was used to verify that the SCUBA-2 GBS data sets presented here are in broad agreement with the lower sensitivity Kramer et al (2003) observations.…”

Section: Scuba-2mentioning

confidence: 98%

“…The pointing accuracy of the JCMT is smaller than the pixel sizes we adopt, with current rms pointing errors of 1 2 in azimuth and 1 6 in elevation (see http://www.eaobservatory. org/JCMT/telescope/pointing/pointing.html); JCMT pointing accuracy in the era of SCUBA is discussed by Di Francesco et al (2008).…”

Section: Scuba-2mentioning

confidence: 99%

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Alma Resolves the Torus of NGC 1068: Continuum and Molecular Line Emission

García‐Burillo

Combes

Almeida

et al. 2016

ApJL

219

235

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We present 450 and 850 μm submillimeter continuum observations of the IC 5146 star-forming region taken as part of the James Clerk Maxwell Telescope Gould Belt Survey. We investigate the location of bright submillimeter (clumped) emission with the larger-scale molecular cloud through comparison with extinction maps, and find that these denser structures correlate with higher cloud column density. Ninety-six individual submillimeter clumps are identified using FellWalker,and their physical properties are examined. These clumps are found to be relatively massive, ranging from 0.5  M to 116  M with a mean mass of 8  M and a median mass of 3.7  M . A stability analysis for the clumps suggests that the majority are (thermally) Jeans stable, withWe further compare the locations of known protostars with the observed submillimeter emission, finding that younger protostars, i.e., Class 0 and I sources, are strongly correlated with submillimeter peaks and that the clumps with protostars are among the most Jeans unstable. Finally, we contrast the evolutionary conditions in the two major star-forming regions within IC 5146: the young cluster associated with the Cocoon Nebula and the more distributed star formation associated with the Northern Streamer filaments. The Cocoon Nebula appears to have converted a higher fraction of its mass into dense clumps and protostars, the clumps are more likely to be Jeans unstable, and a larger fraction of these remaining clumps contain embedded protostars. The Northern Streamer, however, has a larger number of clumps in total and a larger fraction of the known protostars are still embedded within these clumps.

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Section: Discussionmentioning

confidence: 99%

Section: Scuba-2mentioning

confidence: 98%

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Alma Resolves the Torus of NGC 1068: Continuum and Molecular Line Emission

García‐Burillo

Combes

Almeida

et al. 2016

ApJL

219

235

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“…We have used Equations (15) and (17) to derive the dust opacity and the hydrogen column density of W51 and W3(OH) from the dust continuum emission from ATLASGAL (870 μm; Csengeri et al 2014) and SCUBA (850 μm; Di Francesco et al 2008) surveys, respectively. We have considered that the dust temperature is the same as the excitation temperature derived for PN, 35 K. We have adopted a gas-to-dust ratio of 100 and κ ν = 1.85 cm 2 g −1 , from interpolation of column 5 of Table 1 of Ossenkopf & Henning (1994).…”

Section: Discussionmentioning

confidence: 99%

The First Detections of the Key Prebiotic Molecule Po in Star-Forming Regions

Rivilla

Fontani

Beltrán

et al. 2016

ApJ

106

135

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Phosphorus is a crucial element in biochemistry, in particular the P−O bond, which is key in the formation of the backbone of deoxyribonucleic acid. So far, PO has only been detected toward the envelope of evolved stars, but never toward star-forming regions. We report the first detection of PO toward two massive star-forming regions, W51 e1/e2 and W3(OH), using data from the IRAM 30 m telescope. PN has also been detected toward the two regions. The abundance ratio PO/PN is 1.8 and 3 for W51 and W3(OH), respectively. Our chemical model indicates that the two molecules are chemically related and are formed via gas-phase ion-molecule and neutralneutral reactions during cold collapse. The molecules freeze out onto grains at the end of the collapse and desorb during the warm-up phase once the temperature reaches ∼35 K. Similar abundances of the two species are expected during a period of ∼5 × 10 4 yr at the early stages of the warm-up phase, when the temperature is in the range 35-90 K. The observed molecular abundances of 10 −10 are predicted by the model if a relatively high initial abundance of 5 × 10 −9 of depleted phosphorus is assumed.

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“…1), at a one-σ sensitivity of 50 to 70 mJy/beam. For comparison, the 9-year lifetime of the SCUBA instrument resulted in a total of 29.3 deg 2 mapped at 850 μm (Di Francesco et al 2008). A single observation consists in an on-the-fly map, 2 • long and 1 • wide, with 1.…”

Section: Observationsmentioning

confidence: 99%

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

Schüller¹,

Menten²,

Contreras

et al. 2009

A&A

712

927

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Context. Thanks to its excellent 5100 m high site in Chajnantor, the Atacama Pathfinder Experiment (APEX) systematically explores the southern sky at submillimeter wavelengths, in both continuum and spectral line emission. Studying continuum emission from interstellar dust is essential to locating the highest density regions in the interstellar medium, and deriving their masses, column densities, density structures, and large-scale morphologies. In particular, the early stages of (massive) star formation remain poorly understood, mainly because only small samples of high-mass proto-stellar or young stellar objects have been studied in detail so far. Aims. Our goal is to produce a large-scale, systematic database of massive pre-and proto-stellar clumps in the Galaxy, to understand how and under what conditions star formation takes place. Only a systematic survey of the Galactic Plane can provide the statistical basis for unbiased studies. A well characterized sample of Galactic star-forming sites will deliver an evolutionary sequence and a mass function of high-mass, star-forming clumps. This systematic survey at submillimeter wavelengths also represents a preparatory work for Herschel and ALMA. Methods. The APEX telescope is ideally located to observe the inner Milky Way. The Large APEX Bolometer Camera (LABOCA) is a 295-element bolometer array observing at 870 μm, with a beam size of 19. 2. Taking advantage of its large field of view (11. 4) and excellent sensitivity, we started an unbiased survey of the entire Galactic Plane accessible to APEX, with a typical noise level of 50−70 mJy/beam: the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL). Results. As a first step, we covered ∼95 deg 2 of the Galactic Plane. These data reveal ∼6000 compact sources brighter than 0.25 Jy, or 63 sources per square degree, as well as extended structures, many of them filamentary. About two thirds of the compact sources have no bright infrared counterpart, and some of them are likely to correspond to the precursors of (high-mass) proto-stars or protoclusters. Other compact sources harbor hot cores, compact H ii regions, or young embedded clusters, thus tracing more evolved stages after massive stars have formed. Assuming a typical distance of 5 kpc, most sources are clumps smaller than 1 pc with masses from a few 10 to a few 100 M . In this first introductory paper, we show preliminary results from these ongoing observations, and discuss the mid-and long-term perspectives of the survey.

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The SCUBA Legacy Catalogues: Submillimeter‐Continuum Objects Detected by SCUBA

Cited by 350 publications

References 24 publications

Alma Resolves the Torus of NGC 1068: Continuum and Molecular Line Emission

Alma Resolves the Torus of NGC 1068: Continuum and Molecular Line Emission

The First Detections of the Key Prebiotic Molecule Po in Star-Forming Regions

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

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