Herschel-Planck dust optical-depth and column-density maps (Corrigendum)

Marco Lombardi; Hervé Bouy; João Alves; Charles J. Lada

doi:10.1051/0004-6361/201323293e

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Volume 568 (August 2014)

A&A, 568 (2014) C1

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/201323293]

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

A&A 568, C1 (2014)

I. Method description and results for Orion

Marco Lombardi¹^,4, Hervé Bouy², João Alves³ and Charles J. Lada⁴

¹ University of Milan, Department of Physics, via Celoria 16, 20133 Milan, Italy
e-mail: marco.lombardi@unimi.it
² Centro de Astrobiología, INTA-CSIC, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain
³ University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
⁴ Harvard-Smithsonian Center for Astrophysics, Mail Stop 72, 60 Garden Street, Cambridge, MA 02138, USA

Key words: ISM: clouds / dust, extinction / ISM: structure / ISM: individual objects: Orion molecular cloud / errata, addenda

Erratum for: A&A 566, A45 (2014), DOI: 10.1051/0004-6361/201323293

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.

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.

Fig. 4

Same as Fig. 3 for Orion B.

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( > $A_{K}) \propto A_{K}^{-2}$ $\hbox{$A_K) \propto A_K^{-2}$}$ relation as a red line.

Fig. 16

Same as Fig. 15 for Orion B.

Fig. 17

Function − S′(>A_K), 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 $- S^{'} (A_{K}) \propto A_{K}^{-3}$ $\hbox{$-S'(A_K) \propto A_K^{-3}$}$ .

Fig. 18

Same as Fig. 17 for Orion B.

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.

Fig. 20

Same as Fig. 19 for Orion B.

© ESO, 2014

All Figures

	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.
In the text

	Fig. 4 Same as Fig. 3 for Orion B.
In the text

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( > $A_{K}) \propto A_{K}^{-2}$ $\hbox{$A_K) \propto A_K^{-2}$}$ relation as a red line.

In the text

	Fig. 16 Same as Fig. 15 for Orion B.
In the text

	Fig. 17 Function − S′(>A_K), 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 $- S^{'} (A_{K}) \propto A_{K}^{-3}$ $\hbox{$-S'(A_K) \propto A_K^{-3}$}$ .
In the text

	Fig. 18 Same as Fig. 17 for Orion B.
In the text

	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.
In the text

	Fig. 20 Same as Fig. 19 for Orion B.
In the text

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