Erratum: “The Herschel Inventory of the Agents of Galaxy Evolution (Heritage) in the Magellanic Clouds, a Herschel Open Time Key Program” (2013, AJ, 146, 62)

M. Meixner, P. Panuzzo, J. Roman-Duval, C. W Engelbracht, B. Babler, J.

Seale, S. Hony, E. Montiel, M. Sauvage, K. Gordon, et al.

► To cite this version:

M. Meixner, P. Panuzzo, J. Roman-Duval, C. W Engelbracht, B. Babler, et al. Erratum: “The Herschel Inventory of the Agents of Galaxy Evolution (Heritage) in the Magellanic Clouds, a Herschel Open Time Key Program” (2013, AJ, 146, 62). The Astronomical Journal, 2015, 149 (2), pp.88. 10.1088/0004-6256/149/2/88 . hal-02469845

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ERRATUM: “THE HERSCHEL INVENTORY OF THE AGENTS OF GALAXY EVOLUTION (HERITAGE) IN THE MAGELLANIC CLOUDS, A HERSCHEL OPEN TIME KEY PROGRAM” (2013, AJ, 146, 62)

M. MEIXNER¹,², P. PANUZZO³,⁴, J. ROMAN-DUVAL¹, C. ENGELBRACHT⁵,⁶, B. BABLER⁷, J. SEALE¹, S. HONY³, E. MONTIEL⁵,⁸,
M. SAUVAGE³, K. GORDON¹, K. MISSELT⁵, K. OKUMURA³, P. CHANIAL³, T. BECK¹, J.-P. BERNARD⁹,¹⁰, A. BOLATTO¹¹, C. BOT¹²,¹³,
M. L. BOYER¹,¹⁴,¹⁵, L. R. CARLSON¹⁶, G. C. CLAYTON⁸, C.-H. R. CHEN¹⁷, D. CORMIER³, Y. FUKUI¹⁸, M. GALAMETZ¹⁹,
F. GALLIANO³, J. L. HORA²⁰, A. HUGHES²¹, R. INDEBETOUW²², F. P. ISRAEL¹⁶, A. KAWAMURA²³, F. KEMPER²⁴, S. KIM²⁵, E. KWON²⁵,
V. LEBOUTEILLER³, A. LI²⁶, K. S. LONG¹, S. C. MADDEN³, M. MATSUURA²⁷, E. MULLER²³, J. M. OLIVEIRA²⁸, T. ONISHI²⁹,
M. OTSUKA²⁴, D. PARADIS⁹,¹⁰, A. POGLITSCH³⁰, W. T. REACH³¹, T. P. ROBITAILLE²¹, M. RUBIO³², B. SARGENT¹,³³, M. SEWILO²,
R. SKIBBA⁵, L. J. SMITH³⁴, S. SRINIVASAN³⁵,²⁴, A. G. G. M. TIELENS¹⁶, J. TH. VAN LOON²⁸, AND B. WHITNEY⁷
¹Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; meixner@stsci.edu

²The Johns Hopkins University, Department of Physics and Astronomy, 366 Bloomberg Center, 3400 N. Charles Street, Baltimore, MD 21218, USA

³CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France

⁴CNRS, Observatoire de Paris — Lab. GEPI, Bat. 11, 5, place Jules Janssen, F-92195 Meudon CEDEX, FRANCE, France

⁵Steward Observatory, University of Arizona, 933 North Cherry Ave., Tucson, AZ 85721, USA

⁶Raytheon Company, 1151 East Hermans Road, Tucson, AZ 85756, USA

⁷Department of Astronomy, 475 North Charter St., University of Wisconsin, Madison, WI 53706, USA

⁸Louisiana State University, Department of Physics & Astronomy, 233-A Nicholson Hall, Tower Dr., Baton Rouge, LA 70803-4001, USA

CNRS, IRAP, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France

¹⁰Universit de Toulouse, UPS-OMP, IRAP, 31028 Toulouse Cedex 4, France

¹¹Department of Astronomy, Lab for Millimeter-wave Astronomy, University of Maryland, College Park, MD 20742-2421, USA

¹²Université de Strasbourg, Observatoire Astronomique de Strasbourg, 11, rue de l'université, F-67000 Strasbourg, France

¹³CNRS, Observatoire Astronomique de Strasbourg, UMR7550, F-67000 Strasbourg, France

¹⁴Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

¹⁵Oak Ridge Associated Universities (ORAU), Oak Ridge, TN 37831, USA

¹⁶Sterrewacht Leiden, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands

¹⁷Max-Planck-Institut für Radioastronomie Auf dem Hügel 69, 53121 Bonn, Germany

¹⁸Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602, Japan

¹⁹Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK

²⁰Center for Astrophysics, 60 Garden St., MS 67, Harvard University, Cambridge, MA 02138, USA

²¹Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany

²²Department of Astronomy, University of Virginia, and National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA

²³National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan

²⁴Academia Sinica, Institute of Astronomy and Astrophysics, PO Box 23-141, Taipei 10617, Taiwan

²⁵Department of Astronomy and Space Science, Sejong University, 98 Gunja-dong, Gwangjin-gu, 143-747, Seoul, Korea

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

²⁷Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

²⁸School of Physical & Geographical Sciences, Lennard-Jones Laboratories, Keele University, Staffordshire ST5 5BG, UK

²⁹Department of Physical Science, Osaka Prefecture University, Gakuen 1-1, Sakai, Osaka 599-8531, Japan

³⁰Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße D-85748 Garching, Germany

³¹Stratospheric Observatory for Infrared Astronomy, Universities Space Research Association, Mail Stop 232-11, Moffett Field, CA 94035, USA

³²Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile

³³Center for Imaging Science and Laboratory for Multiwavelength Astrophysics, Rochester Institute of Technology,

54 Lomb Memorial Drive, Rochester, NY 14623, USA

³⁴Space Telescope Science Institute and European Space Agency, 3700 San Martin Drive, Baltimore, MD 21218, USA

³⁵UMPC-CNRS UMR7095, Institute d'Astrophysique de Paris, F-75014 Paris, France

*Received 2014 December 17; accepted 2014 December 26; published 2015 February 2*

We provide a corrected Table 4 that lists the total galaxy fluxes for the HERTIAGE bands and corresponding Figure 19 which plots these fluxes in comparison to prior measurements. These corrected fluxes differ by up to 41% to what we reported in the original paper. These revised fluxes utilize a more appropriate subtraction of the Milky Way Foreground Cirrus emission which contaminates especially the PACS 100 and 160 µm bands. The subtraction process uses the HI 21 cm emission to develop a model for the MW cirrus dust emission. In addition, the better subtraction process corrected for an over subtraction of the background in the SPIRE images of the SMC that occured during the original data processing. The need for these better foreground subtractions was realized while working on an analysis of the dust masses and gas-to-dust ratios in the LMC and SMC reported by Gordon et al. (2014) and Roman-Duval et al. (2014). After the subtraction has been done, the fluxes were derived by simply summing up all the pixels in the image. The errors we quote for the fluxes reflect the absolute flux calibration errors for extended sources which are ~10% for PACS and ~8% for SPIRE. In the revised Figure 19, we confirm that these corrected global fluxes remain within the range of prior global measurements for both the LMC and SMC. Indeed, the shape of the corrected spectral energy distributions appears better aligned with prior measurements.
<figure><img src="image_2.png" /><figcaption>**Figure 19.** The spectral energy distributions of the whole LMC and SMC cover the UV to radio wavelengths. Prior work summarized by Israel et al. (2010) includes data from ground and space based missions such as *IRAS*, *DIRBE*, *TopHat*, and *WMAP*. For the SMC, we also include prior work (blue squares) from Gordon et al. (2011). The HERITAGE photometry measured in the PACS and SPIRE bands listed in Table 4 are shown in red. The Planck measurements are shown in green (Planck collaboration 2011).</figcaption></figure>

<table><caption>**Table 4**
Total Galaxy Fluxes in SED</caption><thead><tr><th rowspan="2">Parameter</th><th colspan="2">PACS λ (μm)</th><th colspan="3">SPIRE λ (μm)</th></tr><tr><th>100</th><th>160</th><th>250</th><th>350</th><th>500</th></tr></thead><tbody><tr><td>LMC flux (Jy)</td><td>2.2 ± 0.2 × 10<sup>5</sup></td><td>2.6 ± 0.3 × 10<sup>5</sup></td><td>1.4 ± 0.1 × 10<sup>5</sup></td><td>7.3 ± 0.6 × 10<sup>4</sup></td><td>3.1 ± 0.3 × 10<sup>4</sup></td></tr><tr><td>SMC flux (Jy)</td><td>1.6 ± 0.2 × 10<sup>4</sup></td><td>2.1 ± 0.2 × 10<sup>4</sup></td><td>1.5 ± 0.1 × 10<sup>4</sup></td><td>8.3 ± 0.7 × 10<sup>3</sup></td><td>3.9 ± 0.3 × 10<sup>3</sup></td></tr></tbody></table>

REFERENCES

Gordon, K. D., Meixner, M., Meade, M. R., et al. 2011, AJ, 142, 102

Gordon, K. D., Roman-Duval, J., Bot, C., et al. 2014, ApJ, 797, 85

Israel, F. P., Wall, W. F., Raban, D., et al. 2010, A&A, 519, A67

Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2011, A&A, 536, A17

Roman-Duval, J., Gordon, K. D., Meixner, M., et al. 2014, ApJ, 797, 86