Interactions of the Infrared Bubble N4 With Its Surroundings

Liu, Hong Li; Li, Jin Zeng; Wu, Yuefang; Yuan, Jinghua; Li, Shipeng; Dubner, G.; Paron, S.; Ortega, M. E.; Molinari, S.; Huang, M.; Zavagno, A.; Samal, M. R.; Huang, Y.; Zhang, Si Ju

doi:10.3847/0004-637x/818/1/95

Cited by 39 publications

(65 citation statements)

References 104 publications

(123 reference statements)

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…This spatial distribution is in good agreement with the fact that 24 µm emission mainly arises from hot dust, which can reach rather high temperatures after absorbing high-energy photons (e.g. Deharveng et al 2010;Liu et al 2016). …”

Section: Presentation Of Rcw 79supporting

confidence: 86%

“…It is difficult to distinguish stars formed by triggering from those forming spontaneously (Elmegreen 2011;Dale et al 2015). The high surface density of YSOs observed at the edge of H ii regions or bubbles is often assumed to be a result of triggered star formation (Zavagno et al 2006;Deharveng et al 2009;Thompson et al 2012;Kendrew et al 2012;Liu et al 2015Liu et al , 2016Yadav et al 2016;Nandakumar et al 2016). However, these YSOs might either be redistributed by the expansion of H ii regions or bubbles, or they might form in situ (Elmegreen 2011;Liu et al 2015;Dale et al 2015).…”

Section: Taking Advantage Of the Spitzer-glimpse (Benjaminmentioning

confidence: 99%

“…Taking advantage of the high-resolution column density map, we modeled 870 µm emission according to Eq. 1 of Liu et al (2016). The resulting map is displayed in Fig.…”

Section: Condensations In Rcw 79mentioning

confidence: 99%

See 2 more Smart Citations

Herschelobservations of the Galactic H ii region RCW 79

Liu

Figueira

Zavagno

et al. 2017

A&A

Self Cite

View full text Add to dashboard Cite

Context. Triggered star formation around H ii regions could be an important process. The Galactic H ii region RCW 79 is a prototypical object for triggered high-mass star formation. Aims. We aim to obtain a census of the young stellar population observed at the edges of the H ii region and to determine the properties of the young sources in order to characterize the star formation processes that take place at the edges of this ionized region. Methods. We take advantage of Herschel data from the surveys HOBYS, "Evolution of Interstellar Dust", and Hi-Gal to extract compact sources. We use the algorithm getsources. We complement the Herschel data with archival 2MASS, Spitzer, and WISE data to determine the physical parameters of the sources (e.g., envelope mass, dust temperature, and luminosity) by fitting the spectral energy distribution. Results. We created the dust temperature and column density maps along with the column density probability distribution function (PDF) for the entire RCW 79 region. We obtained a sample of 50 compact sources in this region, 96% of which are situated in the ionization-compressed layer of cold and dense gas that is characterized by the column density PDF with a double-peaked lognormal distribution. The 50 sources have sizes of ∼ 0.1 − 0.4 pc with a typical value of ∼ 0.2 pc, temperatures of ∼ 11 − 26 K, envelope masses of ∼ 6 − 760 M , densities of ∼ 0.1 − 44 × 10 5 cm −3 , and luminosities of ∼ 19 − 12712 L . The sources are classified into 16 class 0, 19 intermediate, and 15 class I objects. Their distribution follows the evolutionary tracks in the diagram of bolometric luminosity versus envelope mass (L bol − Menv) well. A mass threshold of 140 M , determined from the L bol − Menv diagram, yields 12 candidate massive dense cores that may form high-mass stars. The core formation efficiency (CFE) for the 8 massive condensations shows an increasing trend of the CFE with density. This suggests that the denser the condensation, the higher the fraction of its mass transformation into dense cores, as previously observed in other high-mass star-forming regions.

show abstract

Section: Presentation Of Rcw 79supporting

confidence: 86%

Section: Taking Advantage Of the Spitzer-glimpse (Benjaminmentioning

confidence: 99%

See 1 more Smart Citation

Herschelobservations of the Galactic H ii region RCW 79

Liu

Figueira

Zavagno

et al. 2017

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Further, the location of the four clumps in the periphery of S10 strongly suggests a fragmented shell interacting and shaped by the expansion of the bubble. Similar dust clumps have been observed at the borders of several IR bubbles Ji et al 2012;Liu et al 2016).…”

Section: Introductionsupporting

confidence: 80%

High-Mass Star Formation Toward Southern Infrared Bubble S10

Das

Tej

Vig

et al. 2016

View full text Add to dashboard Cite

An investigation in radio and infrared wavelengths of two high-mass star forming regions toward the southern Galactic bubble S10 is presented here. The two regions under study are associated with the broken bubble S10 and Extended Green Object, G345.99-0.02, respectively. Radio continuum emission mapped at 610 and 1280 MHz using the Giant Metrewave Radio Telescope, India is detected towards both the regions. These regions are estimated to be ionized by early B to late O type stars. Spitzer GLIMPSE mid-infrared data is used to identify young stellar objects associated with these regions. A Class I/II type source, with an estimated mass of 6.2 M ⊙ , lies ∼ 7 ′′ from the radio peak. Pixel-wise, modified blackbody fits to the thermal dust emission using Herschel far-infrared data is performed to construct dust temperature and column density maps. Eight clumps are detected in the two regions using the 250 µm image. The masses and linear diameter of these range between ∼ 300 -1600 M ⊙ and 0.2 -1.1 pc, respectively which qualifies them as high-mass star forming clumps. Modelling of the spectral energy distribution of these clumps indicates the presence of high luminosity, high accretion rate, massive young stellar objects possibly in the accelerating accretion phase. Further, based on the radio and MIR morphology, the occurrence of a possible bow-wave towards the likely ionizing star is explored.Subject headings: stars: formation -ISM: HII region -ISM -radio continuum -ISM: individual objects (S10 -IRAS 17036-4033): individual objects (G345.99-0.02)

show abstract

“…3 we show the surface density maps for each star-forming object type. We note that radial velocity measurements of YSOs and clumps that are spatially associated with bubbles have been found to be consistent with ionized gas of H ii regions (e.g., Martins et al 2010;Hou & Gao 2014;Deharveng et al 2015;Liu et al 2015Liu et al , 2016. We therefore assumed that star-forming objects that are found within the edges of bubbles are physically associated with them.…”

Section: Distribution Of Star-forming Sources Related To Ionized Regionsmentioning

confidence: 98%

Spatial distribution of star formation related to ionized regions throughout the inner Galactic plane

Palmeirim

Zavagno

Elia

et al. 2017

A&A

View full text Add to dashboard Cite

We present a comprehensive statistical analysis of star-forming objects located in the vicinities of 1360 bubble structures throughout the Galactic plane and their local environments. The compilation of ∼70 000 star-forming sources, found in the proximity of the ionized (Hii) regions and detected in both Hi-GAL and GLIMPSE surveys, provided a broad overview of the different evolutionary stages of star-formation in bubbles, from prestellar objects to more evolved young stellar objects (YSOs). Surface density maps of star-forming objects clearly reveal an evolutionary trend where more evolved star-forming objects (Class II YSO candidates) are found spatially located near the center, while younger star-forming objects are found at the edge of the bubbles. We derived dynamic ages for a subsample of 182 H ii regions for which kinematic distances and radio continuum flux measurements were available. We detect approximately 80% more star-forming sources per unit area in the direction of bubbles than in the surrounding fields. We estimate the clump formation efficiency (CFE) of Hi-GAL clumps in the direction of the shell of the bubbles to be ∼15%, around twice the value of the CFE in fields that are not affected by feedback effects. We find that the higher values of CFE are mostly due to the higher CFE of protostellar clumps, in particular in younger bubbles, whose density of the bubble shells is higher. We argue that the formation rate from prestellar to protostellar phase is probably higher during the early stages of the (H ii ) bubble expansion. Furthermore, we also find a higher fraction of massive YSOs (MYSOs) in bubbles at the early stages of expansion (<2 Myr) than older bubbles. Evaluation of the fragmentation time inside the shell of bubbles advocates the preexistence of clumps in the medium before the bubble expansion in order to explain the formation of MYSOs in the youngest H ii regions (<1 Myr), as supported by numerical simulations. Approximately 23% of the Hi-GAL clumps are found located in the direction of a bubble, with 15% for prestellar clumps and 41% for protostellar clumps. We argue that the high fraction of protostellar clumps may be due to the acceleration of the star-formation process cause by the feedback of the (Hii) bubbles.

show abstract

Interactions of the Infrared Bubble N4 With Its Surroundings

Cited by 39 publications

References 104 publications

Herschelobservations of the Galactic H ii region RCW 79

Herschelobservations of the Galactic H ii region RCW 79

High-Mass Star Formation Toward Southern Infrared Bubble S10

Spatial distribution of star formation related to ionized regions throughout the inner Galactic plane

Contact Info

Product

Resources

About