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Erratum
This article is an erratum for: [this article]

Issue
A&A
Volume 568, August 2014
Article Number C1
Number of page(s) 3
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201323293e
Published online 28 August 2014

Errors occurred during the production process. Figures 4, 16, 18, and 20 were published twice. The correct Figs. 3, 4, 15, 16, 17, 18, 19, and 20 are published below.

thumbnail Fig. 3

Relationship between submillimeter optical-depth and NIR extinction in Orion A. The best linear fit, used to calibrate the data, is shown together with the expected 3σ region, as calculated from direct error propagation in the extinction map.

Open with DEXTER

thumbnail Fig. 4

Same as Fig. 3 for Orion B.

Open with DEXTER

thumbnail Fig. 15

Integral area-extinction relation for Orion A, i.e., the physical cloud area above a given extinction threshold (top panel), and the logarithmic derivative of this quantity (bottom panel). The solid black line shows the result for the entire field, while the solid gray line shows the region covered by Herschel alone. For comparison we also plot as a dashed gray line the same quantity as obtained from the 2MASS/Nicest extinction map and a simple S( > relation as a red line.

Open with DEXTER

thumbnail Fig. 16

Same as Fig. 15 for Orion B.

Open with DEXTER

thumbnail Fig. 17

Function S′(>AK), that is, the probability distribution function (pdf) of the measured column densities for Orion A. In this log–log plot a log-normal distribution would appear as a parabola, and a power law as a straight line. The red line shows the slope of the power law .

Open with DEXTER

thumbnail Fig. 18

Same as Fig. 17 for Orion B.

Open with DEXTER

thumbnail Fig. 19

Integral mass-extinction relation for Orion A, i.e. the cloud mass above a given extinction threshold. The color codes follow the same convention as in Fig. 15.

Open with DEXTER

thumbnail Fig. 20

Same as Fig. 19 for Orion B.

Open with DEXTER


© ESO, 2014

All Figures

thumbnail Fig. 3

Relationship between submillimeter optical-depth and NIR extinction in Orion A. The best linear fit, used to calibrate the data, is shown together with the expected 3σ region, as calculated from direct error propagation in the extinction map.

Open with DEXTER
In the text
thumbnail Fig. 4

Same as Fig. 3 for Orion B.

Open with DEXTER
In the text
thumbnail Fig. 15

Integral area-extinction relation for Orion A, i.e., the physical cloud area above a given extinction threshold (top panel), and the logarithmic derivative of this quantity (bottom panel). The solid black line shows the result for the entire field, while the solid gray line shows the region covered by Herschel alone. For comparison we also plot as a dashed gray line the same quantity as obtained from the 2MASS/Nicest extinction map and a simple S( > relation as a red line.

Open with DEXTER
In the text
thumbnail Fig. 16

Same as Fig. 15 for Orion B.

Open with DEXTER
In the text
thumbnail Fig. 17

Function S′(>AK), that is, the probability distribution function (pdf) of the measured column densities for Orion A. In this log–log plot a log-normal distribution would appear as a parabola, and a power law as a straight line. The red line shows the slope of the power law .

Open with DEXTER
In the text
thumbnail Fig. 18

Same as Fig. 17 for Orion B.

Open with DEXTER
In the text
thumbnail Fig. 19

Integral mass-extinction relation for Orion A, i.e. the cloud mass above a given extinction threshold. The color codes follow the same convention as in Fig. 15.

Open with DEXTER
In the text
thumbnail Fig. 20

Same as Fig. 19 for Orion B.

Open with DEXTER
In the text

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