The JCMT Gould Belt Survey: properties of star-forming filaments in Orion A North

Salji, C.; Richer, J. S.; Buckle, Jane; Francesco, James Di; Hatchell, Jennifer; Hogerheijde, M. R.; Johnstone, Doug; Kirk, Helen; Ward-Thompson, Derek

doi:10.1093/mnras/stv369

Cited by 57 publications

(90 citation statements)

References 31 publications

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“…19 A number of previous studies find some variations in the filament-profile exponent p for different clouds. Nutter et al (2008) findp 3 for the Taurus molecular cloud, Pineda et al (2011) findp 4 for B5 in Perseus, Hacar, & Tafalla (2011) find p=2.7-3.4 for 4 filaments in L1517, Contreras et al (2013) find that p can vary between clump and inter-clump gas, and Salji et al (2015) find that the majority of filaments in Orion A North exhibit p=1.5-3, with a mode at p=2.2. filament profiles.…”

Section: Filament Profilesmentioning

confidence: 99%

The Link Between Turbulence, Magnetic Fields, Filaments, and Star Formation in the Central Molecular Zone Cloud G0.253+0.016

Federrath

Rathborne

Longmore

et al. 2016

ApJ

176

235

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Star formation is primarily controlled by the interplay between gravity, turbulence, and magnetic fields. However, the turbulence and magnetic fields in molecular clouds near the Galactic center may differ substantially compared to spiral-arm clouds. Here we determine the physical parameters of the central molecular zone (CMZ) cloud G0.253 +0.016, its turbulence, magnetic field, and filamentary structure. Using column density maps based on dust

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Section: Filament Profilesmentioning

confidence: 99%

The Link Between Turbulence, Magnetic Fields, Filaments, and Star Formation in the Central Molecular Zone Cloud G0.253+0.016

Federrath

Rathborne

Longmore

et al. 2016

ApJ

176

235

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“…The opacity of the dust is quite uncertain and a source of significant on-going research. Following the GBS standard (Pattle et al 2015;Rumble et al 2015Rumble et al , 2016Salji et al 2015aSalji et al , 2015bKirk et al 2016aKirk et al , 2016bLane et al 2016;Mairs et al 2016), we adopt k = 0.0125 850 cm 2 g −1 . Taking a fiducial value for the temperature from Appendix A,…”

Section: Large-scale Structurementioning

confidence: 99%

“…This imaging covered 50 square degrees of nearby clouds within the Gould Belt, including well-known regions such as Auriga (Broekhoven-Fiene et al 2016), Ophiuchus (Pattle et al 2015), Orion (Salji et al 2015a(Salji et al , 2015bKirk et al 2016aKirk et al , 2016bLane et al 2016;Mairs et al 2016), Perseus (Hatchell et al 2013;Sadavoy et al 2013;Chen et al 2016), SerpensMWC297 (Rumble et al 2015), Taurus (Buckle et al 2015;Ward-Thompson et al 2016), and W40 (Rumble et al 2016). Among these targets, the GBS survey covered approximately 2.5 square degrees of the IC 5146 starforming region.…”

Section: Introductionmentioning

confidence: 99%

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

García‐Burillo

Combes

Almeida

et al. 2016

ApJL

225

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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“…THz observations will have an advantage of observing continuum emission originating from prestellar cores and T Tauri sources at the wavelengths close to their SED peaks. Multi-wavelength continuum detectors anticipated to be onboard the GLT enable us to directly measure dust temperature and dust emissivity within filamentary molecular clouds such as demonstrated by the recent SCUBA-2 observations (Hatchell et al 2013;Rumble et al 2015;Salji et al 2015). As discussed in Section 3.2.1, adding THz observations to existing data sets will help us to estimate those quantities more precisely.…”

Section: Continuum Observations Of Star-forming Regions: Filamentary mentioning

confidence: 99%

First-generation science cases for ground-based terahertz telescopes

Hirashita

Koch

Matsushita

et al. 2015

Publications of the Astronomical Society of Japan

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Ground-based observations at terahertz (THz) frequencies are a newly explorable area of astronomy for the next ten years. We discuss science cases for a first-generation 10-m class THz telescope, focusing on the Greenland Telescope as an example of such a facility. We propose science cases and provide quantitative estimates for each case. The largest advantage of ground-based THz telescopes is their higher angular resolution (∼ 4 arcsec for a 10-m dish), as compared to space or airborne THz telescopes. Thus, high-resolution mapping is an important scientific argument. In particular, we can isolate zones of interest for Galactic and extragalactic star-forming regions. The THz windows are suitable for observations of high-excitation CO lines and [N II] 205 µm lines, which are scientifically relevant tracers of star formation and stellar feedback. Those lines are the brightest lines in the THz windows, so that they are suitable for the initiation of ground-based THz observations. THz polarization of star-forming regions can also be explored since it traces the dust population contributing to the THz spectral peak. For survey-type observations, we focus on "sub-THz" extragalactic surveys, whose uniqueness is to detect galaxies at redshifts z ∼ 1-2, where the dust emission per comoving volume is the largest in the history of the Universe. Finally we explore possibilities of flexible time scheduling, which enables us to monitor active galactic nuclei, and to target gamma-ray burst afterglows. c 2014. Astronomical Society of Japan. 2Publications of the Astronomical Society of Japan, (2014), Vol. 00, No. 0 For these objects, THz and submillimeter wavelength ranges have not yet been explored.

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The JCMT Gould Belt Survey: properties of star-forming filaments in Orion A North

Cited by 57 publications

References 31 publications

The Link Between Turbulence, Magnetic Fields, Filaments, and Star Formation in the Central Molecular Zone Cloud G0.253+0.016

The Link Between Turbulence, Magnetic Fields, Filaments, and Star Formation in the Central Molecular Zone Cloud G0.253+0.016

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

First-generation science cases for ground-based terahertz telescopes

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