Star formation around RCW 120, the perfect
 bubble

Deharveng, L.; Zavagno, A.; Schüller, F.; Caplan, J.; Pomarès, M.; Breuck, C. De

doi:10.1051/0004-6361/200811337

Cited by 151 publications

(237 citation statements)

References 33 publications

(41 reference statements)

Supporting

Mentioning

212

Contrasting

Unclassified

Order By: Relevance

“…Moreover, not all massive dust condensations appear as infrared dark clouds. For example, the two most massive condensations (with masses of 200 and 800 M at a distance of 1.3 kpc) observed at 870 μm in the photo-dissociation region (PDR) bordering the RCW 120 H ii region (Deharveng et al 2009) are not detected as IRDCs at 8 or 24 μm. They are hidden, at these wavelengths, by the bright emission of the adjacent foreground PDR.…”

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

Schüller¹,

Menten²,

Contreras

et al. 2009

A&A

Self Cite

725

927

View full text Add to dashboard Cite

Context. Thanks to its excellent 5100 m high site in Chajnantor, the Atacama Pathfinder Experiment (APEX) systematically explores the southern sky at submillimeter wavelengths, in both continuum and spectral line emission. Studying continuum emission from interstellar dust is essential to locating the highest density regions in the interstellar medium, and deriving their masses, column densities, density structures, and large-scale morphologies. In particular, the early stages of (massive) star formation remain poorly understood, mainly because only small samples of high-mass proto-stellar or young stellar objects have been studied in detail so far. Aims. Our goal is to produce a large-scale, systematic database of massive pre-and proto-stellar clumps in the Galaxy, to understand how and under what conditions star formation takes place. Only a systematic survey of the Galactic Plane can provide the statistical basis for unbiased studies. A well characterized sample of Galactic star-forming sites will deliver an evolutionary sequence and a mass function of high-mass, star-forming clumps. This systematic survey at submillimeter wavelengths also represents a preparatory work for Herschel and ALMA. Methods. The APEX telescope is ideally located to observe the inner Milky Way. The Large APEX Bolometer Camera (LABOCA) is a 295-element bolometer array observing at 870 μm, with a beam size of 19. 2. Taking advantage of its large field of view (11. 4) and excellent sensitivity, we started an unbiased survey of the entire Galactic Plane accessible to APEX, with a typical noise level of 50−70 mJy/beam: the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL). Results. As a first step, we covered ∼95 deg 2 of the Galactic Plane. These data reveal ∼6000 compact sources brighter than 0.25 Jy, or 63 sources per square degree, as well as extended structures, many of them filamentary. About two thirds of the compact sources have no bright infrared counterpart, and some of them are likely to correspond to the precursors of (high-mass) proto-stars or protoclusters. Other compact sources harbor hot cores, compact H ii regions, or young embedded clusters, thus tracing more evolved stages after massive stars have formed. Assuming a typical distance of 5 kpc, most sources are clumps smaller than 1 pc with masses from a few 10 to a few 100 M . In this first introductory paper, we show preliminary results from these ongoing observations, and discuss the mid-and long-term perspectives of the survey.

show abstract

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

Schüller¹,

Menten²,

Contreras

et al. 2009

A&A

Self Cite

725

927

View full text Add to dashboard Cite

show abstract

“…Observations in mm and sub-mm wavelengths (Zavagno et al 2007;Deharveng et al 2009) show a fragmented neutral layer along its PDR, which contains five of the nine mmcondensations found by Zavagno et al (2007). According to Deharveng et al (2009) the mass of the layer is ∼2000 M .…”

Section: Introductionmentioning

confidence: 93%

HerschelSPIRE-FTS observations of RCW 120

Rodón

Zavagno

Baluteau

et al. 2015

A&A

Self Cite

View full text Add to dashboard Cite

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).

show abstract

“…In the infrared, Churchwell et al (2006) and Churchwell et al (2007) found many 0.1 -10 pc size shells in the GLIMPSE survey covering only a part of the plane of the Milky Way. Deharveng et al (2003), Zavagno et al (2006), Sidorin (2008), and Deharveng et al (2009) identified shells observationally in optical, infrared, radio and other wavebands, some of them appear to have triggered star formation at their borders. Watson et al (2009) analyzed some of the shells from the GLIMPSE survey to determine properties of YSOs related to them.…”

Section: Outside Of a Star Clustermentioning

confidence: 98%

Action of Winds Inside and Outside of Star Clusters

et al. 2010

View full text Add to dashboard Cite

Abstract. The feedback form pre-main sequence and young stars influences their vicinity. The stars are formed in clusters, which implies that the winds of individual stars collide with each other. Inside of a star cluster, winds thermalize a fraction of their kinetic energy, forming a very hot medium able to escape from the cluster in the form of a large-scale wind. Outside of the cluster, the cluster wind forms a shock front as it interacts with the ambient medium which is accreted onto the expanding shell. A variety of instabilities may develop in such shells, and in some cases they fragment, triggering second generation of star formation. However, if the cluster surpasses a certain mass (depending on the radius and other parameters) the hot medium starts to be thermally unstable even inside of the cluster, forming dense warm clumps. The formation of next generations of stars may start if the clumps are big enough to self-shield against stellar radiation creating cold dense cores.

show abstract

Star formation around RCW 120, the perfect bubble

Cited by 151 publications

References 33 publications

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

HerschelSPIRE-FTS observations of RCW 120

Action of Winds Inside and Outside of Star Clusters

Contact Info

Product

Resources

About