Adaptable radiative transfer innovations for submillimetre telescopes (ARTIST)

Padovani, M.; Brinch, Christian; Girart, J. M.; Jørgensen, J. K.; Frau, P.; Hennebelle, P.; Kuiper, Rolf; Vlemmings, Wouter; Bertoldi, F.; Hogerheijde, M. R.; Juhász, A.; Schaaf, R.

doi:10.1051/0004-6361/201219028

Cited by 45 publications

(50 citation statements)

References 58 publications

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“…This is suggestive of a toroidal magnetic field that is being wrapped by the rotation of the disk (Hennebelle & Ciardi 2009;Kataoka et al 2012). As a qualitative comparison, Figure 3b shows the synthetic map of the expected magnetic field pattern in a rotating circumstellar disk with a face-on configuration for the case of a low mass protostar located at 140 pc, and thus is at a distance not too different from our target, obtained by Padovani et al (2012). Interestingly, the I16293B magnetic field pattern roughly resembles the expected configuration for a magnetized rotating, disk.…”

Section: Discussionmentioning

confidence: 74%

Detection of a Magnetized Disk Around a Very Young Protostar

Rao¹,

Girart

Lai

et al. 2013

ApJ

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We present subarcsecond resolution polarimetric observations of the 878 µm thermal dust continuum emission obtained with the Submillimeter Array (SMA) towards the IRAS 16293−2422 protostellar binary system. We report the detection of linearly polarized dust emission arising from the circumstellar disk associated with the IRAS 16293−2422 B protostar. The fractional polarization of ≃ 1.4% is only slightly lower than that expected from theoretical calculations in such disks. The magnetic field structure on the plane of the sky derived from the dust polarization suggests a complex magnetic field geometry in the disk, possibly associated with a rotating disk that is wrapping the field lines as expected from the simulations. The polarization around IRAS 16293−2422 A at sub-arcsecond angular resolution is only marginally detected.

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Section: Discussionmentioning

confidence: 74%

Detection of a Magnetized Disk Around a Very Young Protostar

Rao¹,

Girart

Lai

et al. 2013

ApJ

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“…13) through the rotated simulation cube, following the method in Wardle & Königl (1990), Fiege & Pudritz (2000), Pelkonen et al (2009), andPadovani et al (2012). Because of a number of inconsistencies in the literature, we give the correct derivation in Appendix B, drawing on the works of Lee & Draine (1985) and Wardle & Königl (1990).…”

Section: Simulated Planck Observationsmentioning

confidence: 99%

“…Note that the corrective term in Eq. (5) is incorrectly written in Fiege & Pudritz (2000), Gonçalves et al (2005), Pelkonen et al (2009), andPadovani et al (2012), with p 0 /2 instead of p 0 .…”

Section: Simulated Planck Observationsmentioning

confidence: 99%

Planckintermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Ade

Aghanim

Alina

et al. 2015

A&A

126

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Polarized emission observed by Planck HFI at 353 GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions p and angles ψ. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction p max decreases with column density N H in the more opaque fields with N H > 10 21 cm −2 ; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction p max in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the maximum polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function S. However, the dispersion of the polarization angle for a given polarization fraction is found to be larger in the simulations than in the observations, suggesting a shortcoming in the physical content of these numerical models. In summary, we find that the turbulent structure of the magnetic field is able to reproduce the main statistical properties of the dust polarization as observed in a variety of nearby clouds, dense cores excluded, and that the large-scale field orientation with respect to the line of sight plays a major role in the quantitative analysis of these statistical properties.

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“…The ARTIST (Adaptable Radiative Transfer Innovations for Submillimeter Telescopes) project 1 was designed as a general model suite for comprehensive multidimensional radiative transfer calculations of dust and molecular line emission (Padovani et al 2011). In addition to the model suite, which is based on the full three-dimensional radiative transfer code LIME (Line Modeling Engine, Brinch and Hogerheijde 2010), the ARTIST project will also provide the tools for modeling polarization at (sub-)millimetre wavelength.…”

Section: Alma Polarization Analysis Tools: the Artist Projectmentioning

confidence: 99%

“…The dust polarization module (DustPol) is described in detail in Padovani et al (2012). As it is based on LIME, DustPol can be combined with analytical as well as pregridded models and output from, e.g., magneto-hydrodynamical (MHD) models.…”

Section: Alma Polarization Analysis Tools: the Artist Projectmentioning

confidence: 99%

Magnetic Fields with the Atacama Large Millimeter/Submillimeter Array

Vlemmings

2014

Astrophysics and Space Science Library

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The Atacama Large Millimeter/submillimeter Array (ALMA) is one of the largest radio telescopes and is located at 5;000 m altitude in the Atacama desert in Chile. Its unprecedented sensitivity at extremely high angular and spectral resolution in the (sub-)millimetre wavelength regime, allows for countless advances in astrophysics. One of the areas in which ALMA can make unique contributions, is in that of the study of astrophysical magnetic fields. ALMA is expected to map the magnetic field geometry, and in some cases strength, in a large number of star forming regions, around evolved stars and planetary nebulae, and in nearby galaxies. This chapter provides examples of the amount of improvement ALMA offers the study of magnetic fields based on the current state-of-the-art and shortly introduces new tools that will be available to analyse (sub-)millimetre polarimetric observations. The Atacama Large Millimeter/Submillimeter ArrayThe Atacama Large Millimeter/submillimeter Array (ALMA) is a large international (sub-)millimeter-wavelength radio telescope array in the Atacama Desert of northern Chile. It consists of a total of 66 antennas operating in the wavelength range from 0:4 to 4 mm. Because of its unmatched sensitivity at very high spectral and spatial resolution, ALMA provides new insights into many astrophysical topics, from the formation of stars and planets to the evolution of the most distant galaxies. As ALMA is able to observe in full polarization mode, it can also reveal the magnetic field with a sensitivity and resolution that has not previously been possible.ALMA is a partnership between Europe, North America (USA and Canada) and East Asia (Japan and Taiwan) in cooperation with the Republic of Chile. The ALMA project is coordinated by the Joint ALMA Office based in Santiago de Chile. The ALMA observatory is operated from the Operation Support Facility (OSF), which is situated at 2,900 m altitude. The array itself and the correlator are located at the W. Vlemmings ( )

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Adaptable radiative transfer innovations for submillimetre telescopes (ARTIST)

Cited by 45 publications

References 58 publications

Detection of a Magnetized Disk Around a Very Young Protostar

Detection of a Magnetized Disk Around a Very Young Protostar

Planckintermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Magnetic Fields with the Atacama Large Millimeter/Submillimeter Array

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