# 2011A&A...530A.101M

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 Query : 2011A&A...530A.101M

2011A&A...530A.101M - Astronomy and Astrophysics, volume 530A, 101-101 (2011/6-1)

Accuracy of core mass estimates in simulated observations of dust emission.

MALINEN J., JUVELA M., COLLINS D.C., LUNTTILA T. and PADOAN P.

Abstract (from CDS):

We study the reliability of the mass estimates obtained for molecular cloud cores using sub-millimetre and infrared dust emission. We use magnetohydrodynamic simulations and radiative transfer to produce synthetic observations with spatial resolution and noise levels typical of Herschel surveys. We estimate dust colour temperatures using different pairs of intensities, calculate column densities with opacity at one wavelength, and compare the estimated masses with the true values. We compare these results to the case when all five Herschel wavelengths are available. We investigate the effects of spatial variations of dust properties and the influence of embedded heating sources. Wrong assumptions of dust opacity and its spectral index β can cause significant systematic errors in mass estimates. These are mainly multiplicative and leave the slope of the mass spectrum intact, unless cores with very high optical depth are included. Temperature variations bias the colour temperature estimates and, in quiescent cores with optical depths higher than for normal stable cores, masses can be underestimated by up to one order of magnitude. When heated by internal radiation sources, the dust in the core centre becomes visible and the observations recover the true mass spectra. The shape, although not the position, of the mass spectrum is reliable against observational errors and biases introduced in the analysis. This changes only if the cores have optical depths much higher than expected for basic hydrostatic equilibrium conditions. Observations underestimate the value of β whenever there are temperature variations along the line of sight. A bias can also be observed when the true β varies with wavelength. Internal heating sources produce an inverse correlation between colour temperature and β that may be difficult to separate from any intrinsic β(T) relation of the dust grains. This suggests caution when interpreting the observed mass spectra and the spectral indices.

Journal keyword(s): ISM: structure - ISM: clouds - stars: formation - radiative transfer - magnetohydrodynamics (MHD) - submillimeter: ISM

Full paper

 Number of rows : 1
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 IC 5146 OpC 21 53 29 +47 14.8           ~ 444 2

 Query : 2011A&A...530A.101M

Basic data :
', {sourceSize:12, color:'#30a090'})); aladin.on('objectClicked', function(object) { var objName=object.data.MAIN_ID; aladin.showPopup(object.ra,object.dec,'',''+ objName+''); });" title="Show Simbad objects"> Overlay points in this preview
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 Some important notes on this object about identifications and objects associations. notes: cluster embedded in nebula

Hierarchy : number of linked objects
whatever the membership probability is (see description here ) :

 The count displayed here is the number of children objects. The list obtained by clicking the button may be larger, as some children may be linked with different references or probability. %This number is the number of distinct objets linked, by using this button, you will obtain all links (may be more than one) from that object to his children : 854 Display criteria : All >=90% stars galaxies radio IR <2 arcsec #ref>50

 The link on the acronym of the identifiers give access to the information for this acronym in the dictionary of nomenclature. Identifiers (12) :
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 IC 5146 LBN 424 NAME Cocoon Nebula OCl 213.0 C 2151+470 LBN 094.43-05.58 OCISM 43 [KC2019] Theia 88 Cl Collinder 470 Min 2-70 OCl 213 [KPS2012] MWSC 3571

 References (444 between 1850 and 2023) (Total 444) Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system). Follow new references on this object
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Collections of Measurements

velocities : 5    distance : 5    Fe_H : 3    PLX : 6    PM : 7

Observing logs

herschel : 4    ISO : 12

External archives :

 Indications mainly about references on other documents Notes (1) :

• message of Brent A. Archinal (27.12.2005):
the IC makes no mention of a star cluster here, and neither do the discoverersof the IC 5146 nebula (the "Cocoon Nebula"), Espin (1900) and Wolf (1904).Collinder appears to have been the first to identify a star cluster here(even though he also used the IC 5146 name incorrectly), so the preferred namewould seem to be Collinder 470. Details of this are given in Brent A. Archinaland Steven's Hynes book "Star Clusters", pp. 127-128.
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2023.02.04-13:12:44