A network of filaments detected by Herschel in the Serpens core - A laboratory to test simulations of low-mass star formation

V. Roccatagliata; J. E. Dale; T. Ratzka; L. Testi; A. Burkert; C. Koepferl; A. Sicilia-Aguilar; C. Eiroa; B. Gaczkowski

doi:10.1051/0004-6361/201425253

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Volume 584 (December 2015)

A&A, 584 (2015) A119

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Issue		A&A Volume 584, December 2015


Article Number		A119
Number of page(s)		16
Section		Galactic structure, stellar clusters and populations
DOI		https://doi.org/10.1051/0004-6361/201425253
Published online		07 December 2015

Online material

Appendix A: The control field

In the observations and the simulations we consider a control region where neither filamentary structures nor cores are present (box 0 in Figs. 2 and 3). Figure A.1 shows the histograms of the column density distributions on the left, and the PDFs on the right. Since only a few bins are covered in the column

density distribution, these plots are shown here in the Appendix. However, the small error bar in each bin emphasizes that the column density distributions show only a peak without any additional structure. This peak at A_V ~ 0.5 mag is very narrow in the observations, while in the simulations the peak is much broader.

	Fig. A.1 Left panel: histograms of the column density distributions of the control field, right panel: PDFs. The dashed lines overplotted on the PDFs show the best Gaussian fit of the data. The red lines are for the observations, the blue for the simulations.
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Appendix B: Filamentary structures in the Serpens core

Figure B.1 shows the zoom on filament number 1: starting from the left side, the first five panels show the Herschel, PACS and

SPIRE mosaics, while the last two panels show the column density and the temperature map. An additional box identifies the position of a core structure along the filament.

Figures B.2–B.9 show the enlargements on each filament as in Fig. B.1.

Fig. B.1

Filament number 1. From left to right: Herschel/PACS 70 μm, 160 μm, and SPIRE 250 μm, 350 μm, and 500 μm. The images all use units of Jy/arcsec². Last two panels: column density map (N_H) in [×10⁺²⁰ cm^-2] and the temperature map in K. The box identifies the extension of the filament and its size is given in Table 2. The smaller box identifies the position of the cores along the filament.

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	Fig. B.2 Filament number 2. The panels and the units are as in Fig. B.1.
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	Fig. B.3 Filament number 3. The panels and the units are as in Fig. B.1.
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	Fig. B.4 Filament number 4. The panels and the units are as in Fig. B.1.
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	Fig. B.5 Filament number 5. The panels and the units are as in Fig. B.1.
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	Fig. B.6 Filament number 6. The panels and the units are as in Fig. B.1.
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	Fig. B.7 Filament number 7. The panels and the units are as in Fig. B.1. The smaller box identifies the position of the core along the filament.
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	Fig. B.8 Filament number 8. The panels and the units are as in Fig. B.1.
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	Fig. B.9 Filament number 9. The panels and the units are as in Fig. B.1.
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© ESO, 2015

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