Infrared emission of young HII regions: a Herschel/Hi-GAL study

R. Cesaroni; M. Pestalozzi; M. T. Beltrán; M. G. Hoare; S. Molinari; L. Olmi; M. D. Smith; G. S. Stringfellow; L. Testi; M. A. Thompson

doi:10.1051/0004-6361/201525953

Free Access

Issue		A&A Volume 579, July 2015


Article Number		A71
Number of page(s)		46
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201525953
Published online		30 June 2015

Online material

Appendix A

Table A.1

Flux densities of the Hii regions classified as “ultracompact” and “compact” in the CORNISH catalogue.

Table A.2

Distances, Lyman continuum photon rates, bolometric luminosities, and clump masses of the 200 Hii regions of our sample for which a distance estimate was possible.

	Fig. A.1 Spectral energy distributions of the CORNISH Hii regions with Hi-GAL counterparts of at least three bands. In addition to Hi-GAL, the MSX 21 μm, WISE 22 μm, ATLASGAL 870 μm, and BGPS 1.1 mm flux densities have also been used. The number in each box identifies the source according to the numbering in Table A.1.
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	Fig. A.2 Hi-GAL images of the sources lying above the blackbody curve in Fig. 5. The sources are identified by the numbers in Col. 1 of Table A.1. The black circles represent the CORNISH Hii regions in the field of view, with diameter equal to the angular size given in Col. 8 of Table 3 in Purcell et al. (2013). The HPBW at each wavelength is shown in the bottom right of the top panels.
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	Fig. A.3 Same as Fig. A.2 for the sources lying between the blackbody curve (dashed line) and the single ZAMS star curve (solid line) in Fig. 5.
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	Fig. A.4 Same as Fig. A.2 for the sources lying inside the cluster region (hatched area) in Fig. 5.
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	Fig. A.5 Same as Fig. A.2 for the sources lying below the cluster region in Fig. 5.
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	Fig. A.6 Same as Fig. A.2 for the sources without distance estimates.
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© ESO, 2015

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