Star formation in Perseus

Hatchell, Jennifer; Richer, J. S.; Fuller, G. A.; Qualtrough, C. J.; Ladd, E. F.; Chandler, Claire J.

doi:10.1051/0004-6361:20041836

Cited by 213 publications

(345 citation statements)

References 48 publications

Supporting

Mentioning

312

Contrasting

Order By: Relevance

“…The cumulative curve clearly shows that the SCUBA-2 flux predominantly traces the higher extinction regions within the cloud, with 85% of the mass derived from the submillimeter continuum residing at an extinction greater than A V =3 and 50% of the mass at an extinction greater than A V =6. This result is similar to those found for other star-forming regions (e.g., Onishi et al 1998;Johnstone et al 2004;Hatchell et al 2005;Enoch et al 2006Enoch et al , 2007Kirk et al 2006;Könyves et al 2013). Namely, the compact submillimeter emission within IC 5146 is intrinsically linked and heavily biased to regions of high dust column.…”

Section: Large-scale Structuresupporting

confidence: 78%

“…Figure 4 compares the cumulative mass, as determined from the extinction map within the Spitzer footprint, to the emergence of these YSOs as a function of the underlying extinction. It is clear that the YSOs are at least as biased to higher extinction regions as the clump mass in the cloud, reinforcing the notion that stars form where there is significant material (e.g., Johnstone et al 2004;Hatchell et al 2005;Kirk et al 2006;Könyves et al 2013). Furthermore, a large fraction of the most embedded YSOs, the protostellar Class 0/I and Flat, are found at extreme extinctions of > A 5 V , which is also where the SCUBA-2-derived mass resides.…”

Section: Dust Continuum and Ysosmentioning

confidence: 63%

See 1 more Smart Citation

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

García‐Burillo

Combes

Almeida

et al. 2016

ApJL

224

235

View full text Add to dashboard Cite

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.

show abstract

Section: Large-scale Structuresupporting

confidence: 78%

Section: Dust Continuum and Ysosmentioning

confidence: 63%

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

García‐Burillo

Combes

Almeida

et al. 2016

ApJL

224

235

View full text Add to dashboard Cite

show abstract

“…Cambrésy 1999), Perseus (e.g. Hatchell et al 2005), and S106 (e.g. Balsara, Ward-Thompson & Crutcher 2001).…”

Section: Properties Of Filamentsmentioning

confidence: 99%

Magnetohydrodynamical simulation of the formation of clumps and filaments in quiescent diffuse medium by thermal instability

Wareing

Pittard

Falle

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We have used the AMR hydrodynamic code, MG, to perform idealised 3D MHD simulations of the formation of clumpy and filamentary structure in a thermally unstable medium without turbulence. A stationary thermally unstable spherical diffuse atomic cloud with uniform density in pressure equilibrium with low density surroundings was seeded with random density variations and allowed to evolve. A range of magnetic field strengths threading the cloud have been explored, from β = 0.1 to β = 1.0 to the zero magnetic field case (β = ∞), where β is the ratio of thermal pressure to magnetic pressure. Once the density inhomogeneities had developed to the point where gravity started to become important, self-gravity was introduced to the simulation. With no magnetic field, clouds and clumps form within the cloud with aspect ratios of around unity, whereas in the presence of a relatively strong field (β = 0.1) these become filaments, then evolve into interconnected corrugated sheets that are predominantly perpendicular to the magnetic field. With magnetic and thermal pressure equality (β = 1.0), filaments, clouds and clumps are formed. At any particular instant, the projection of the 3D structure onto a plane parallel to the magnetic field, i.e. a line of sight perpendicular to the magnetic field, resembles the appearance of filamentary molecular clouds. The filament densities, widths, velocity dispersions and temperatures resemble those observed in molecular clouds. In contrast, in the strong field case β = 0.1, projection of the 3D structure along a line of sight parallel to the magnetic field reveals a remarkably uniform structure.

show abstract

“…Low-magnitude velocity fields have been observed in both, bound prestellar cores as well as unbound cores (see e.g., Motte et al 1998;Jijina, Myers, & Adams 1999;Hatchell et al 2005;Nutter & Ward-Thompson 2007;Enoch et al 2008; among a number of other authors working on the subject). It is commonly believed, this velocity field within cores is introduced during their natal phase itself, while they are yet accreting gas from their parent clouds.…”

Section: Discussionmentioning

confidence: 99%

“…Despite their relatively high levels of turbulence, some do indeed have a population of cores, most of which are unbound and therefore starless (see e.g., Hatchell et al 2005 for the Perseus MC; Hily-Blant & Falgarone 2009 for Polaris Flare; Roman-Duval et al 2010 for MCs in the Galactic ring survey; Ragan et al 2012 for a number of IRDCs 2 and Ripple et al 2013 for the Orion MC). Starless cores are believed to be supported by turbulence, and perhaps the magnetic field.…”

Section: Anathpindikamentioning

confidence: 99%

Formation of Prestellar Cores via Non-Isothermal Gas Fragmentation

Anathpindika

2015

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

Sheet-like clouds are common in turbulent gas and perhaps form via collisions between turbulent gas flows. Having examined the evolution of an isothermal shocked slab in an earlier contribution, in this work we follow the evolution of a sheet-like cloud confined by (thermal) pressure and gas in it is allowed to cool. The extant purpose of this endeavour is to study the early phases of core-formation. The observed evolution of this cloud supports the conjecture that molecular clouds themselves are three-phase media (comprising viz. a stable cold and warm medium, and a third thermally unstable medium), though it appears, clouds may evolve in this manner irrespective of whether they are gravitationally bound. We report, this sheet fragments initially due to the growth of the thermal instability (TI) and some fragments are elongated, filament-like. Subsequently, relatively large fragments become gravitationally unstable and sub-fragment into smaller cores. The formation of cores appears to be a three stage process: first, growth of the TI leads to rapid fragmentation of the slab; second, relatively small fragments acquire mass via gas-accretion and/or merger and third, sufficiently massive fragments become susceptible to the gravitational instability and sub-fragment to form smaller cores. We investigate typical properties of clumps (and smaller cores) resulting from this fragmentation process. Findings of this work support the suggestion that the weak velocity field usually observed in dense clumps and smaller cores is likely seeded by the growth of dynamic instabilities. Simulations were performed using the smooth particle hydrodynamics algorithm.

show abstract

Star formation in Perseus

Cited by 213 publications

References 48 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

Magnetohydrodynamical simulation of the formation of clumps and filaments in quiescent diffuse medium by thermal instability

Formation of Prestellar Cores via Non-Isothermal Gas Fragmentation

Contact Info

Product

Resources

About