# Water in star-forming regions with Herschel (WISH) (Corrigendum). V. The physical conditions in low-mass protostellar outflows revealed by multi-transition water observations

J. C. Mottram, L. E. Kristensen, E. F. van Dishoeck, S. Bruderer, I. San José-García, A. Karska, R. Visser, G. Santangelo, A. O. Benz, E. A. Bergin, et al.

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J. C. Mottram, L. E. Kristensen, E. F. van Dishoeck, S. Bruderer, I. San José-García, et al. Water in star-forming regions with Herschel (WISH) (Corrigendum). V. The physical conditions in low-mass protostellar outflows revealed by multi-transition water observations. Astronomy and Astrophysics - A&A, 2015, 574, pp.id.C3. 10.1051/0004-6361/201424267e. hal-01112644

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# Water in star-forming regions with Herschel (WISH)\*

## V. The physical conditions in low-mass protostellar outflows revealed by multi-transition water observations

### (Corrigendum)

J. C. Mottram<fnref n="1" />, L. E. Kristensen<fnref n="2" />, E. F. van Dishoeck<fnref n="1" />,<fnref n="3" />, S. Bruderer<fnref n="3" />, I. San José-García<fnref n="1" />, A. Karska<fnref n="3" />, R. Visser<fnref n="4" />, G. Santangelo<fnref n="5" />,<fnref n="6" />, A. O. Benz<fnref n="7" />, E. A. Bergin<fnref n="4" />, P. Caselli<fnref n="8" />,<fnref n="3" />, F. Herpin<fnref n="9" />,<fnref n="10" />, M. R. Hogerheijde<fnref n="1" />, D. Johnstone<fnref n="11" />,<fnref n="12" />,<fnref n="13" />, T. A. van Kempen<fnref n="1" />, R. Liseau<fnref n="14" />, B. Nisini<fnref n="6" />, M. Tafalla<fnref n="15" />, F. F. S. van der Tak<fnref n="16" />,<fnref n="17" />, and F. Wyrowski<fnref n="18" />

A&A 572, A21 (2014), DOI: 10.1051/0004-6361/201424267

**Key words.** stars: formation – ISM: jets and outflows – ISM: molecules – stars: protostars – errata, addenda

The original calculation of the fraction of the total integrated intensity in each component type presented in Table 4 of Mottram et al. (2014) did not correctly take into account the different distance corrections for the cavity shock compared to the spot shock and envelope components. For the cavity shock components a correction of (d/200 pc) was used, assuming that the emission is extended along the outflow axis but point-like perpendicular to it, while for the other components (d/200 pc)<fnref n="2" /> was used, assuming that both are point-like. The table given below provides the corrected values.

This primarily affects the contribution of the envelope, which is decreased in the corrected version, leading to a slight increase in the relative contribution of the cavity shock component. The correction does not change the discussion of the results or the conclusions drawn from them.

## References

Mottram, J. C., Kristensen, L. E., van Dishoeck, E. F., et al. 2014, A&A, 572, A21

<footnote n="1">¹ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
e-mail: mottram@strw.leidenuniv.nl</footnote>

<footnote n="2">² Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</footnote>

<footnote n="3">³ Max Planck Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany</footnote>

<footnote n="4">⁴ Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109-1042, USA</footnote>

<footnote n="5">⁵ Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Florence, Italy</footnote>

<footnote n="6">⁶ Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monteporzio Catone, Italy</footnote>

<footnote n="7">⁷ Institute for Astronomy, ETH Zurich, 8093 Zurich, Switzerland</footnote>

<footnote n="8">⁸ School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK</footnote>

<footnote n="9">⁹ Université de Bordeaux, Observatoire Aquitain des Sciences de l'Univers, 2 rue de l'Observatoire, BP 89, 33270 Floirac Cedex, France</footnote>

<footnote n="10">¹⁰ CNRS, LAB, UMR 5804, Laboratoire d'Astrophysique de Bordeaux, 2 rue de l'Observatoire, BP 89, 33270 Floirac Cedex, France</footnote>

<footnote n="11">¹¹ Joint Astronomy Centre, 660 North Aohoku Place, University Park, Hilo, HI 96720, USA</footnote>

<footnote n="12">¹² Department of Physics and Astronomy, University of Victoria, PO Box 3055 STN CSC, Victoria, BC V8W 3P6, Canada</footnote>

<footnote n="13">¹³ NRC-Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada</footnote>

<footnote n="14">¹⁴ Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden</footnote>

<footnote n="15">¹⁵ Observatorio Astronómico Nacional (IGN), Alfonso XII 3, 28014 Madrid, Spain</footnote>

<footnote n="16">¹⁶ SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV Groningen, The Netherlands</footnote>

<footnote n="17">¹⁷ Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands</footnote>

<footnote n="18">¹⁸ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany</footnote>

<footnote>\* Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.</footnote>
<table><caption>**Table 4.** Detection statistics and average fraction of the total integrated intensity that each component contributes for each transition.</caption><thead><tr><th rowspan="3">Line</th><th colspan="6">Class 0</th><th colspan="6">Class I</th></tr><tr><th colspan="2">Envelope<sup>a</sup></th><th colspan="2">Cavity shock</th><th colspan="2">Spot shock</th><th colspan="2">Envelope<sup>a</sup></th><th colspan="2">Cavity shock</th><th colspan="2">Spot shock</th></tr><tr><th>D<sup>b</sup></th><th>I<sub>comp</sub>/I<sub>tot</sub></th><th>D<sup>b</sup></th><th>I<sub>comp</sub>/I<sub>tot</sub></th><th>D<sup>b</sup></th><th>I<sub>comp</sub>/I<sub>tot</sub></th><th>D<sup>b</sup></th><th>I<sub>comp</sub>/I<sub>tot</sub></th><th>D<sup>b</sup></th><th>I<sub>comp</sub>/I<sub>tot</sub></th><th>D<sup>b</sup></th><th>I<sub>comp</sub>/I<sub>tot</sub></th></tr></thead><tbody><tr><td>H<sub>2</sub>O 1<sub>11</sub>-0<sub>00</sub></td><td>14</td><td>-0.1 ± 0.1</td><td>14</td><td>0.9 ± 0.1</td><td>9</td><td>0.2 ± 0.1</td><td>4</td><td>0.0 ± 0.1</td><td>4</td><td>1.0 ± 0.1</td><td>0</td><td>-</td></tr><tr><td>H<sub>2</sub>O 1<sub>10</sub>-1<sub>01</sub></td><td>15</td><td>-0.1 ± 0.1</td><td>15</td><td>0.9 ± 0.1</td><td>8</td><td>0.2 ± 0.1</td><td>12</td><td>0.1 ± 0.1</td><td>11</td><td>1.1 ± 0.3</td><td>3</td><td>-0.2 ± 0.2</td></tr><tr><td>H<sub>2</sub>O 2<sub>12</sub>-1<sub>01</sub></td><td>5</td><td>-0.2 ± 0.1</td><td>5</td><td>1.0 ± 0.1</td><td>5</td><td>0.2 ± 0.2</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td></tr><tr><td>H<sub>2</sub>O 2<sub>02</sub>-1<sub>11</sub></td><td>14</td><td>0.0 ± 0.1</td><td>14</td><td>0.7 ± 0.1</td><td>10</td><td>0.3 ± 0.1</td><td>8</td><td>0.2 ± 0.1</td><td>7</td><td>0.8 ± 0.1</td><td>1</td><td>0.0 ± 0.0</td></tr><tr><td>H<sub>2</sub>O 2<sub>11</sub>-2<sub>02</sub></td><td>11</td><td>0.0 ± 0.1</td><td>11</td><td>0.7 ± 0.1</td><td>8</td><td>0.3 ± 0.1</td><td>7</td><td>0.3 ± 0.2</td><td>5</td><td>0.7 ± 0.2</td><td>0</td><td>-</td></tr><tr><td>H<sub>2</sub>O 3<sub>12</sub>-2<sub>21</sub></td><td>7</td><td>0.0 ± 0.1</td><td>7</td><td>0.8 ± 0.1</td><td>5</td><td>0.2 ± 0.1</td><td>3</td><td>0.0 ± 0.1</td><td>3</td><td>1.0 ± 0.1</td><td>0</td><td>-</td></tr><tr><td>H<sub>2</sub>O 3<sub>12</sub>-3<sub>03</sub></td><td>8</td><td>0.0 ± 0.1</td><td>8</td><td>0.8 ± 0.1</td><td>7</td><td>0.2 ± 0.1</td><td>2</td><td>0.0 ± 0.1</td><td>2</td><td>1.0 ± 0.1</td><td>0</td><td>-</td></tr></tbody></table>

**Notes.** (a) Calculated for all sources with detected emission as $I_{tot} - I_{cavity\ shock} - I_{spot\ shock}$. May include emission and absorption. (b) No. of sources with detections in this component.