The dust properties of bubble H II regions as seen by<i>Herschel</i>

Anderson, L. D.; Zavagno, A.; Deharveng, L.; Abergel, A.; Motte, F.; André, Ph.; Bernard, J.-P.; Bontemps, Sylvain; Hennemann, M.; Hill, T.; Rodón, J. A.; Roussel, H.; Russeil, D.

doi:10.1051/0004-6361/201117283

Cited by 109 publications

(138 citation statements)

References 104 publications

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“…There is growing evidence of an inverse relationship between the dust emissivity spectral index, β and the dust temperature, T d (Dupac et al 2003;Désert et al 2008;Paradis et al 2010;Veneziani et al 2010;Anderson et al 2012). We investigate this for the region associated with IRAS 20286+4105.…”

Section: Variation In Dust Emissivity Indexmentioning

confidence: 85%

Radio and infrared study of the star-forming region IRAS 20286+4105

Ramachandran

Das

Tej

et al. 2016

Mon. Not. R. Astron. Soc.

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A multi-wavelength investigation of the star forming complex IRAS 20286+4105, located in the Cygnus-X region, is presented here. Near-infrared K-band data is used to revisit the cluster / stellar group identified in previous studies. The radio continuum observations, at 610 and 1280 MHz show the presence of a HII region possibly powered by a star of spectral type B0 -B0.5. The cometary morphology of the ionized region is explained by invoking the bow-shock model where the likely association with a nearby supernova remnant is also explored. A compact radio knot with non-thermal spectral index is detected towards the centre of the cloud. Mid-infrared data from the Spitzer Legacy Survey of the Cygnus-X region show the presence of six Class I YSOs inside the cloud. Thermal dust emission in this complex is modelled using Herschel far-infrared data to generate dust temperature and column density maps. Herschel images also show the presence of two clumps in this region, the masses of which are estimated to be ∼ 175 M and 30 M . The mass-radius relation and the surface density of the clumps do not qualify them as massive star forming sites. An overall picture of a runaway star ionizing the cloud and a triggered population of intermediate-mass, Class I sources located toward the cloud centre emerges from this multiwavelength study. Variation in the dust emissivity spectral index is shown to exist in this region and is seen to have an inverse relation with the dust temperature.

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Section: Variation In Dust Emissivity Indexmentioning

confidence: 85%

Radio and infrared study of the star-forming region IRAS 20286+4105

Ramachandran

Das

Tej

et al. 2016

Mon. Not. R. Astron. Soc.

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“…For the other pointings, with RADEX we only obtain lower limits to the column density, and correspondingly, the average values from the Anderson et al (2012) map are higher than the RADEX values. In particular, pointing C6 shows a large difference between the two estimations, in line with the suggestion made in Sect.…”

Section: Discussionmentioning

confidence: 64%

“…On the other hand, using the column density map obtained by Anderson et al (2012) for RCW 120, we averaged their column density values obtained at the position of the different pointings within the beam of the central pixel of the SLW array (∼36 at 350 μm, Makiwa et al 2013), obtaining the total hydrogen column densities shown in Col. 2 of Table 8.…”

Section: Discussionmentioning

confidence: 99%

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HerschelSPIRE-FTS observations of RCW 120

Rodón

Zavagno

Baluteau

et al. 2015

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Context. The expansion of Galactic H ii regions can trigger the formation of a new generation of stars. However, little is know about the physical conditions that prevail in these regions.Aims. We study the physical conditions that prevail in specific zones towards expanding H ii regions that trace representative media such as the photodissociation region, the ionized region, and condensations with and without ongoing star formation.Methods. We use the SPIRE Fourier Transform Spectrometer (FTS) on board Herschel to observe the H ii region RCW 120.Continuum and lines are observed in the 190−670 μm range. Line intensities and line ratios are obtained and used as physical diagnostics of the gas. We used the Meudon PDR code and the RADEX code to derive the gas density and the radiation field at nine distinct positions including the PDR surface and regions with and without star-formation activity. Results. For the different regions we detect the atomic lines [NII] at 205 μm and [CI]at 370 and 609 μm, the 12 CO ladder between the J = 4 and J = 13 levels and the 13 CO ladder between the J = 5 and J = 14 levels, as well as CH + in absorption. We find gas temperatures in the range 45−250 K for densities of 10 4 −10 6 cm −3 , and a high column density on the order of N H ∼ 10 22 cm −2 that is in agreement with dust analysis. The ubiquitousness of the atomic and CH + emission suggests the presence of a low-density PDR throughout RCW 120. High-excitation lines of CO indicate the presence of irradiated dense structures or small dense clumps containing young stellar objects, while we also find a less dense medium (N H ∼ 10 20 cm −2 ) with high temperatures (80−200 K).

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“…As can be noticed, the emission observed in the three different bands is similar, in the sense that it forms a shell-like structure, instead of having, as observed in several H ii regions, the emission at 70 µm brighter in the interior of the bubble, where the hotter material is expected to be present, and the SPIRE emission, mapping the cooler dust, outside it (e.g. Rodón et al 2010;Deharveng et al 2010;Anderson et al 2012). In this context, the observed largescale distribution of the infrared emission at the periphery of the ionized gas represents matter accumulated during the expansion of the ionized gas.…”

Section: Infrared Emission and Dust Propertiesmentioning

confidence: 73%

The infrared and molecular environment surrounding the Wolf-Rayet star WR 130

Cichowolski

Suad

Pineault

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present a study of the molecular CO gas and mid/far infrared radiation arising from the environment surrounding the Wolf-Rayet (W-R) star 130. We use the multi-wavelength data to analyze the properties of the dense gas and dust, and its possible spatial correlation with that of Young Stellar Objects (YSOs). We use CO J=1-0 data from the FCRAO survey as tracer of the molecular gas, and mid/far infrared data from the recent WISE and Herschel space surveys to study the dust continuum radiation and to identify a population of associated candidate YSOs. The spatial distribution of the molecular gas shows a ring-like structure very similar to that observed in the H i gas, and over the same velocity interval. The relative spatial distribution of the H i and CO components is consistent with a photo-dissociation region. We have identified and characterized four main and distinct molecular clouds that create this structure. Cold dust is coincident with the dense gas shown in the CO measurements. We have found several cYSOs that lie along the regions with the highest gas column density, and suggest that they are spatially correlated with the shell. These are indicative of regions of star formation induced by the strong wind and ionization of the WR star.

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The dust properties of bubble H II regions as seen byHerschel

Cited by 109 publications

References 104 publications

Radio and infrared study of the star-forming region IRAS 20286+4105

Radio and infrared study of the star-forming region IRAS 20286+4105

HerschelSPIRE-FTS observations of RCW 120

The infrared and molecular environment surrounding the Wolf-Rayet star WR 130

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