Galactic cold cores

Rivera-Ingraham, A.; Ristorcelli, I.; Juvela, M.; Montillaud, J.; Men’shchikov, A.; Malinen, J.; Pelkonen, V. M.; Marston, A. P.; Martín, P. G.; Pagani, L.; Paladini, R.; Paradis, D.; Ysard, N.; Ward-Thompson, Derek; Bernard, J.-P.; Marshall, D. J.; Montier, L.; Tóth, L. V.

doi:10.1051/0004-6361/201526263

Cited by 38 publications

(47 citation statements)

References 45 publications

(66 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This means that the fields typically contain a few Planck clumps but also a significant area of the surrounding cloud and even diffuse medium. This has enabled, for example, the study of the filamentary structure of the clouds around the clumps (Rivera-Ingraham et al 2016Malinen et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Herscheland SCUBA-2 observations of dust emission in a sample ofPlanckcold clumps

Juvela

Pattle

et al. 2018

A&A

View full text Add to dashboard Cite

Context. Analysis of all-sky Planck submillimetre observations and the IRAS 100 µm data has led to the detection of a population of Galactic cold clumps. The clumps can be used to study star formation and dust properties in a wide range of Galactic environments. Aims. Our aim is to measure dust spectral energy distribution (SED) variations as a function of the spatial scale and the wavelength. Methods. We examine the SEDs at large scales using IRAS, Planck, and Herschel data. At smaller scales, we compare with JCMT/SCUBA-2 850 µm maps with Herschel data that are filtered using the SCUBA-2 pipeline. Clumps are extracted using the Fellwalker method and their spectra are modelled as modified blackbody functions. Results. According to IRAS and Planck data, most fields have dust colour temperatures T C ∼ 14 − 18 K and opacity spectral index values of β = 1.5 − 1.9. The clumps/cores identified in SCUBA-2 maps have T ∼ 13 K and similar β values. There are some indications of the dust emission spectrum becoming flatter at wavelengths longer than 500 µm. In fits involving Planck data, the significance is limited by the uncertainty of the corrections for CO line contamination. The fits to the SPIRE data give a median β value slightly above 1.8. In the joint SPIRE and SCUBA-2 850 µm fits the value decreases to β ∼1.6. Most of the observed T -β anticorrelation can be explained by noise. Conclusions. The typical submillimetre opacity spectral index β of cold clumps is found to be ∼1.7. This is above the values of diffuse clouds but lower than in some previous studies of dense clumps. There is only tentative evidence of T -β anticorrelation and β decreasing at millimetre wavelengths.

show abstract

Section: Introductionmentioning

confidence: 99%

Herscheland SCUBA-2 observations of dust emission in a sample ofPlanckcold clumps

Juvela

Pattle

et al. 2018

A&A

View full text Add to dashboard Cite

show abstract

“…In Rivera-Ingraham et al (2016) (Paper I hereafter), the data acquired by the Herschel Galactic Cold Cores Key Programme (GCC; P.I: M. Juvela et al 2012) was used to extract a sample of filaments for Galactic fields located at D ≤ 500 pc. This study complemented the work presented in Juvela et al (2012), and aimed to provide a robust characterisation of the physical properties of the filament population under different environmental conditions.…”

Section: Introductionmentioning

confidence: 99%

Galactic cold cores

Rivera-Ingraham

Ristorcelli

Juvela

et al. 2017

A&A

Self Cite

View full text Add to dashboard Cite

Context. The onset of star formation is intimately linked with the presence of massive, unstable filaments. These structures are therefore key for theoretical models aiming to reproduce the observed characteristics of the star formation process. Aims. As part of the filament study carried out by the Herschel Galactic Cold Cores Key Programme, here we study the filament properties presented in GCC VII (Paper I) in context with theoretical models of filament formation and evolution. Methods. A conservative sample of filaments at a distance D < 500 pc was extracted with the getfilaments algorithm. The physical structure of the filaments was quantified according to two main components: the central (Gaussian) region (core component), and the power-law like region dominating the filament column density profile at larger radii (wing component). The properties and behaviour of these components relative to the total linear mass density of the filament and its environmental column density were compared with the predictions from theoretical models describing the evolution of filaments under gravity-dominated conditions. Results. The feasibility of a transition from a subcritical to supercritical state by accretion is dependent on the combined effect of filament intrinsic properties and environmental conditions. Reasonably self-gravitating (high M line,core ) filaments in dense environments (A V ≈3 mag) can become supercritical in timescales of t ∼ 1 Myr by accreting mass at constant or decreasing width. The trend of increasing M line,tot (M line,core and M line,wing ), and ridge A V with background also indicates that the precursors of star-forming filaments evolve coevally with their environment. The simultaneous increase of environment and filament A V explains the association between dense environments and high M line,core values, and argues against filaments remaining in constant single-pressure equilibrium states. The simultaneous growth of filament and background in locations with efficient mass assembly, predicted in numerical models of collapsing clouds, presents a suitable scenario for the fulfillment of the combined filament mass−environment criterium that is in quantitative agreement with Herschel observations.

show abstract

“…Independent studies of filament widths in nearby clouds have generally confirmed this result when using submillimeter continuum data (e.g. Koch & Rosolowsky, 2015;Salji et al, 2015;Rivera-Ingraham et al, 2016), even if factor of ∼ 2-4 variations around the mean inner width of ∼ 0.1 pc have been found along the main axis of a given filament (e.g. Juvela et al, 2012;Ysard et al, 2013).…”

Section: Insights From Herschel and Planck: A Filamentary Paradigm Fomentioning

confidence: 83%

Probing the cold magnetised Universe with SPICA-POL (B-BOP)

André

Hughes

Guillet

et al. 2019

Publ. Astron. Soc. Aust.

Self Cite

View full text Add to dashboard Cite

SPICA, the cryogenic infrared space telescope recently pre-selected for a "Phase A" concept study as one of the three remaining candidates for ESA's fifth medium class (M5) mission, is foreseen to include a far-infrared polarimetric imager (SPICA-POL, now called B-BOP), which would offer a unique opportunity to resolve major issues in our understanding of the nearby, cold magnetized Universe. This paper presents an overview of the main science drivers for B-BOP, including high dynamic range polarimetric imaging of the cold interstellar medium (ISM) in both our Milky Way and nearby galaxies. Thanks to a cooled telescope, B-BOP will deliver wide-field 100-350 µm images of linearly polarized dust emission in Stokes Q and U with a resolution, signal-to-noise ratio, and both intensity and spatial dynamic ranges comparable to those achieved by Herschel images of the cold ISM in total intensity (Stokes I). The B-BOP 200 µm images will also have a factor ∼ 30 higher resolution than Planck polarization data. This will make B-BOP a unique tool for characterizing the statistical properties of the magnetized interstellar medium and probing the role of magnetic fields in the formation and evolution of the interstellar web of dusty molecular filaments giving birth to most stars in our Galaxy. B-BOP will also be a powerful instrument for studying the magnetism of nearby galaxies and testing galactic dynamo models, constraining the physics of dust grain alignment, informing the problem of the interaction of cosmic rays with molecular clouds, tracing magnetic fields in the inner layers of protoplanetary disks, and monitoring accretion bursts in embedded protostars.

show abstract

Galactic cold cores

Cited by 38 publications

References 45 publications

Herscheland SCUBA-2 observations of dust emission in a sample ofPlanckcold clumps

Herscheland SCUBA-2 observations of dust emission in a sample ofPlanckcold clumps

Galactic cold cores

Probing the cold magnetised Universe with SPICA-POL (B-BOP)

Contact Info

Product

Resources

About