A multiwavelength investigation of the H ii region S311: young stellar population and star formation

Yadav, R. K. S.; Pandey, A. K.; Sharma, Saurabh; Ojha, D. K.; Samal, M. R.; Mallick, K. K.; Jose, Jessy; Ogura, K.; Richichi, A.; Irawati, P.; Kobayashi, Naoto; Eswaraiah, Chakali

doi:10.1093/mnras/stw1356

Cited by 10 publications

(7 citation statements)

References 76 publications

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“…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%

Herschelobservations of the Galactic H ii region RCW 79

Liu

Figueira

Zavagno

et al. 2017

A&A

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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.

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Section: Taking Advantage Of the Spitzer-glimpse (Benjaminmentioning

confidence: 99%

Herschelobservations of the Galactic H ii region RCW 79

Liu

Figueira

Zavagno

et al. 2017

A&A

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“…All of these features hint towards a recent star forming activities in the region. As there are many active star-forming regions in the literature where massive stars have triggered the formation of YSOs (Zavagno et al 2006;Pomarès et al 2009;Yadav et al 2016;Sharma et al 2017;Pandey et al 2020b;Kaur et al 2020, and references therein), in the present work we also explored the impact of massive stars on the star formation activities in the S301 region.…”

Section: Feedback Pressure From Massive Starmentioning

confidence: 99%

Sh 2-301: a blistered H II region undergoing star formation

Pandey,

Sharma,

Dewangan

et al. 2021

Preprint

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We present a multiwavelength study of the H ii region Sh 2-301 (S301) using deep optical data, near-infrared data, radio continuum data and other archival data at longer wavelengths. A cluster of young stellar objects (YSOs) is identified in the north-east (NE) direction of S301. The Hα and radio continuum images trace the distribution of the ionized gas surrounding a massive star ALS 207, and the S301 H ii region is bounded by an arc-like structure of gas and dust emission in the south-eastern direction. The north-western part of S301 seems to be devoid of gas and dust emission, while the presence of molecular material between the NE cluster and the central massive star ALS 207 is found. The distribution of warm dust emission, ionized gas, and neutral hydrogen together suggests a blistered morphology of the S301 H ii region powered by ALS 207, which appears to be located near the edge of the cloud. The location of the NE cluster embedded in the cold molecular cloud is found opposite to the blistered morphology. There is a noticeable age difference investigated between the massive star and the NE cluster. This age difference, pressure calculation, photodissociation regions (PDRs), and the distribution of YSOs favour the positive feedback of the massive star ALS 207 in S301. On a wider scale of S301, the H ii region and the young stellar cluster are depicted toward the central region of a hub-filamentary system, which is evident in the infrared images.

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“…We acquired the corrected basic calibrated data (cbcd), uncertainty (cbunc), and imask (bimsk) files. In order to create the final mosaic images with a pixel scale of 1.2 arcsec pixel −1 , and to obtain the aperture photometry of the point sources, we followed the steps mentioned in Yadav et al (2016) and used sources with uncertainty < 0.2 mag for our analysis.…”

Section: Ancillary Archival Data Setsmentioning

confidence: 99%

A Comprehensive Study of the Young Cluster IRAS 05100+3723: Properties, Surrounding Interstellar Matter, and Associated Star Formation

Yadav,

Samal,

Semenko

et al. 2021

Preprint

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We present a comprehensive multiwavelength investigation of a likely massive young cluster 'IRAS 05100+3723' and its environment with the aim to understand its formation history and feedback effects. We find that IRAS 05100+3723 is a distant (∼3.2 kpc), moderate mass (∼500 M ), young (∼3 Myr) cluster with its most massive star being an O8.5V-type. From spectral modeling, we estimate the effective temperature and log g of the star as ∼33,000 K and ∼3.8, respectively. Our radio continuum observations reveal that the star has ionized its environment forming an H II region of size ∼2.7 pc, temperature ∼5,700 K, and electron density ∼165 cm −3 . However, our large-scale dust maps reveal that it has heated the dust up to several parsecs (∼10 pc) in the range 17−28 K and the morphology of warm dust emission resembles a bipolar H II region. From dust and 13 CO gas analyses, we find evidences that the formation of the H II region has occurred at the very end of a long filamentary cloud around 3 Myr ago, likely due to edge collapse of the filament. We show that the H II region is currently compressing a clump of mass ∼2700 M at its western outskirts, at the junction of the H II region and filament. We observe several 70 µm point sources of intermediate-mass and class 0 nature within the clump. We attribute these sources as the second generation stars of the complex. We propose that the star formation in the clump is either induced or being facilitated by the compression of the expanding H II region onto the inflowing filamentary material.

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A multiwavelength investigation of the H ii region S311: young stellar population and star formation

Cited by 10 publications

References 76 publications

Herschelobservations of the Galactic H ii region RCW 79

Herschelobservations of the Galactic H ii region RCW 79

Sh 2-301: a blistered H II region undergoing star formation

A Comprehensive Study of the Young Cluster IRAS 05100+3723: Properties, Surrounding Interstellar Matter, and Associated Star Formation

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