Erratum: “Dust and Gas in the Magellanic Clouds from the HERITAGE Herschel Key Project. I. Dust Properties and Insights into the Origin of the Submm Excess Emission” (2014, ApJ, 797, 85)

Karl D. Gordon; Julia Roman-Duval; Caroline Bot; Margaret Meixner; Brian Babler; Jean-Philippe Bernard; Alberto Bolatto; Martha L. Boyer; Geoffrey C. Clayton; Charles Engelbracht; Yasuo Fukui; Maud Galametz; Frederic Galliano; Sacha Hony; Annie Hughes; Remy Indebetouw; Frank P. Israel; Katie Jameson; Akiko Kawamura; Vianney Lebouteiller; Aigen Li; Suzanne C. Madden; Mikako Matsuura; Karl Misselt; Edward Montiel; K. Okumura; Toshikazu Onishi; Pasquale Panuzzo; Deborah Paradis; Monica Rubio; Karin Sandstrom; Marc Sauvage; Jonathan Seale; Marta Sewiło; Kirill Tchernyshyov; Ramin Skibba

doi:10.3847/1538-4357/aa6042

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Erratum: "Dust and Gas in the Magellanic Clouds from the HERITAGE Herschel Key Project. I. Dust Properties and Insights into the Origin of the Submm Excess Emission" (2014, ApJ, 797, 85)

Karl D. Gordon^1,2, Julia Roman-Duval¹, Caroline Bot³, Margaret Meixner¹, Brian Babler⁴, Jean-Philippe Bernard^5,6, Alberto Bolatto⁷, Martha L. Boyer^8,9, Geoffrey C. Clayton¹⁰, Charles Engelbracht^11,12, Yasuo Fukui¹³, Maud Galametz¹⁴, Frederic Galliano¹⁵, Sacha Hony¹⁵, Annie Hughes¹⁶, Remy Indebetouw¹⁷, Frank P. Israel¹⁸, Katie Jameson⁷, Akiko Kawamura¹⁹, Vianney Lebouteiller¹⁵, Aigen Li²⁰, Suzanne C. Madden¹⁵, Mikako Matsuura²¹, Karl Misselt¹¹, Edward Montiel^10,11, K. Okumura¹⁵, Toshikazu Onishi²², Pasquale Panuzzo^15,23, Deborah Paradis^5,6, Monica Rubio²⁴, Karin Sandstrom¹¹, Marc Sauvage¹⁵, Jonathan Seale^1,25, Marta Sewiło²⁵, Kirill Tchernyshyov²⁵, and Ramin Skibba^11,26

Published 2017 March 7 • © 2017. The American Astronomical Society. All rights reserved.
The Astrophysical Journal, Volume 837, Number 1 Citation Karl D. Gordon et al 2017 ApJ 837 98 DOI 10.3847/1538-4357/aa6042

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¹ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA

² Sterrenkundig Observatorium, Universiteit Gent, Gent, Belgium

³ Observatoire astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l Université, F-67000 Strasbourg, France

⁴ Department of Astronomy, 475 North Charter Street, University of Wisconsin, Madison, WI 53706, USA

⁵ CESR, Université de Toulouse, UPS, 9 Avenue du Colonel Roche, F-31028 Toulouse, Cedex 4, France

⁶ Université de Toulouse, UPS-OMP, IRAP, 31028 Toulouse Cedex 4, France

⁷ Department of Astronomy, Lab for Millimeter-wave Astronomy, University of Maryland, College Park, MD 20742, USA

⁸ Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

⁹ Oak Ridge Associated Universities (ORAU), Oak Ridge, TN 37831, USA

¹⁰ Louisiana State University, Department of Physics & Astronomy, 233-A Nicholson Hall, Tower Dr., Baton Rouge, LA 70803, USA

¹¹ Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA

¹² Raytheon Company, 1151 East Hermans Road, Tucson, AZ 85756, USA

¹³ Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan

¹⁴ European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching-bei-Mnchen, Germany

¹⁵ CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France

¹⁶ Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany

¹⁷ Department of Astronomy, University of Virginia, and National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA

¹⁸ Sterrewacht Leiden, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands

¹⁹ National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo, 181-8588, Japan

²⁰ 314 Physics Building, Department of Physics and Astronomy, University of Missouri, Columbia, MO 65211, USA

²¹ Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

²² Department of Astrophysics, Graduate School of Science, Osaka Prefecture University, Sakai, Osaka 599-8531, Japan

²³ CNRS, Observatoire de Paris—Lab. GEPI, Bat. 11, 5, place Jules Janssen, 92195 Meudon CEDEX, France

²⁴ Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile

²⁵ The Johns Hopkins University, Department of Physics and Astronomy, 366 Bloomberg Center, 3400 N. Charles Street, Baltimore, MD 21218, USA

²⁶ Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Dr, La Jolla, San Diego, CA 92093, USA

ORCID iDs

Karl D. Gordon https://orcid.org/0000-0001-5340-6774

Julia Roman-Duval https://orcid.org/0000-0001-6326-7069

Brian Babler https://orcid.org/0000-0002-6984-5752

Alberto Bolatto https://orcid.org/0000-0002-5480-5686

Martha L. Boyer https://orcid.org/0000-0003-4850-9589

Geoffrey C. Clayton https://orcid.org/0000-0002-0141-7436

Maud Galametz https://orcid.org/0000-0002-0283-8689

Sacha Hony https://orcid.org/0000-0003-4358-0925

Remy Indebetouw https://orcid.org/0000-0002-4663-6827

Akiko Kawamura https://orcid.org/0000-0001-7813-0380

Vianney Lebouteiller https://orcid.org/0000-0002-7716-6223

Aigen Li https://orcid.org/0000-0002-1119-642X

Suzanne C. Madden https://orcid.org/0000-0003-3229-2899

Mikako Matsuura https://orcid.org/0000-0002-5529-5593

Karin Sandstrom https://orcid.org/0000-0002-4378-8534

Dates

Received 2017 February 10
Accepted 2017 February 10
Published 2017 March 7

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The values of ${\kappa }_{\mathrm{eff},160}$ given in the original paper are missing a factor of π. This is because the routine used to compute ${B}_{\lambda }(T)$ was the IDL Astronomer User's Library²⁷ planck.pro and it returns $\pi {B}_{\lambda }(T)$ . While this is explicitly documented in the planck.pro function, it was not realized by the first author until after the paper was published. This does not impact the results or conclusions of the paper as the values of ${\kappa }_{\mathrm{eff},160}$ used were determined based on fitting Milky Way observations using the same code that was used to fit the Magellanic Cloud observations. Thus, the correct values of ${\kappa }_{\mathrm{eff},160}$ are a factor of π larger than the ones quoted in the paper. Using Equation (5) from the paper with the values of ${\kappa }_{\mathrm{eff},160}$ given in the corrected Table 2 will reproduce the dust surface density result from the paper. The detailed fit parameter maps used in the paper are available online.²⁸

Table 2. MW Diffuse Fit Results

Model	${\kappa }_{\mathrm{eff},160}$ ^a	Other Parameters	Expectation Values
	[cm² g⁻¹]
SMBB	30.2 ± 1.3 ± 2.5	$({T}_{\mathrm{eff},{\rm{d}}},{\beta }_{\mathrm{eff}})$	(17.2 ± 0.4 K, 1.96 ± 0.10)
BEMBB	36.4 ± 4.7 ± 2.5	$({T}_{\mathrm{eff},{\rm{d}}},{\beta }_{\mathrm{eff},1},{\lambda }_{b},{e}_{500})$	(16.8 ± 0.6 K, 2.27 ± 0.15, 294 ± 29 μm, 0.48 ± 0.11)
TTMBB	1620 ± 672 ± 2.5	$({T}_{\mathrm{eff},d1},{T}_{\mathrm{eff},d2},{\beta }_{\mathrm{eff}},{e}_{500})$	(15.0 ± 0.7 K, 6.0 ± 0.8 K, 2.9 ± 0.1, 0.91 ± 0.25)
TTMBB	30.2 ± 1.3 ± 2.5	adopted

Note.

^aThe results are given as value ± fitting uncertainty ± systematic uncertainty.

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The correct values of ${\kappa }_{\mathrm{eff},160}$ are approximately a factor of two larger than the values calculated from full dust grain models and discussed in Section 5.3 of the paper. This difference may be due to the simple models in our paper, which did not include the full physical treatment (e.g., multiple grain sizes/compositions with different temperatures) or, less likely, some issues with the assumptions in the dust grain models. We are carrying out work to investigate such issues for the dust in the Magellanic Clouds (and Milky Way) using more complicated dust grain models and additional observations. This work will be discussed in future papers.

There was a typo in Equation (4) with a factor of π missing from the denominator. This does not affect Equation (5) as it was derived correctly including this factor of π. The correct equation is

$\begin{eqnarray}&&{S}_{\lambda }=\displaystyle \frac{{{\rm{\Sigma }}}_{d}}{\tfrac{4}{3}\pi {a}^{3}\rho }\pi {a}^{2}{Q}_{\lambda }{B}_{\lambda }({T}_{d}).\end{eqnarray} \tag{ 4 }$

Last, there was a typo in Equation (15). The correct equation is

$\begin{eqnarray}&&{S}_{\mathrm{band}}=\displaystyle \frac{\int {S}_{\nu }{R}_{E}(\nu )d\nu }{\int ({\nu }_{o}/\nu ){R}_{E}(\nu )d\nu }.\end{eqnarray} \tag{ 15 }$