The HII region G35.673-00.847: another case of triggered star formation?

Paron, S.; Petriella, A.; Ortega, M. E.

doi:10.1051/0004-6361/201015312

Cited by 22 publications

(47 citation statements)

References 31 publications

(51 reference statements)

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“…Based on the MIR and radio continuum emission, the G35.6 site has an almost semi-ring-like appearance with a radius of about 1. 5 (∼1.6 pc at a distance of 3.7 kpc) (Paron et al 2011), which is associated with the main radio continuum source detected in the region (see Figures 1a and 1b). In the direction of the G35.6 H ii region, the velocity of the ionized gas is estimated to be 60.7±2.6 km s −1 (Lockman 1989).…”

Section: Introductionmentioning

confidence: 70%

The Embedded Ring-like Feature and Star Formation Activities in G35.673-00.847

Dewangan

Devaraj

Ojha

2018

ApJ

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We present a multi-wavelength study to probe the star formation (SF) process in the molecular cloud linked with the G35.673-00.847 site (hereafter MCG35.6), which is traced in a velocity range of 53-62 km s −1 . Multi-wavelength images reveal a semi-ring-like feature (associated with ionized gas emission) and an embedded face-on ring-like feature (without the NVSS 1.4 GHz radio emission; where 1σ ∼0.45 mJy beam −1 ) in the MCG35.6. The semi-ring-like feature is originated by the ionizing feedback from a star with spectral type B0.5V-B0V. The central region of the ring-like feature does not contain detectable ionized gas emission, indicating that the ring-like feature is unlikely to be produced by the ionizing feedback from a massive star. Several embedded Herschel clumps and young stellar objects (YSOs) are identified in the MCG35.6, tracing the ongoing SF activities within the cloud. The polarization information from the Planck and GPIPS data trace the plane-of-sky magnetic field, which is oriented parallel to the major axis of the ring-like feature. At least five clumps (having M clump ∼740-1420 M ) seem to be distributed in an almost regularly spaced manner along the ringlike feature and contain noticeable YSOs. Based on the analysis of the polarization and molecular line data, three subregions containing the clumps are found to be magnetically supercritical in the ring-like feature. Altogether, the existence of the ring-like feature and the SF activities on its edges can be explained by the magnetic field mediated process as simulated by .

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Section: Introductionmentioning

confidence: 70%

The Embedded Ring-like Feature and Star Formation Activities in G35.673-00.847

Dewangan

Devaraj

Ojha

2018

ApJ

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“…In previous studies toward several H II regions (e.g., Zavagno et al 2006;Deharveng et al 2008;Paron et al 2009Paron et al , 2011Pomarès et al 2009;Dirienzo et al 2012), an initial number density of ∼10 3 cm −3 was determined. Alexander et al (2013) Fig.…”

Section: Discussionmentioning

confidence: 99%

Triggered massive and clustered star formation by combined H II regions G38.91-0.44 and G39.30-1.04

Xu¹,

Wang²,

Liu³

2013

A&A

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Aims. We investigate the triggered star formation occurring in the infrared dark clouds (IRDC) G38.95-0.47 between H II regions G38.91-0.44 and G39.30-1.04, and study the detailed morphology, distribution, and physical parameters of the molecular gas and dust in this region. Methods. We present the radio continuum, infrared, and CO molecular observations of IRDC G38.95-0.47 and its adjacent H II regions G38.91-0.44 (N74), G38.93-0.39 (N75), and G39.30-1.04. The Purple Mountain Observation (PMO) 13.7 m radio telescope was used to detect 12 CO J = 1−0, 13 CO J = 1−0 and C 18 O J = 1−0 lines. The carbon monoxide (CO) molecular observations can ensure the real association between the ionized gas and the neutral material observed nearby. To select young stellar objects (YSOs) associated this region, we used the GLIMPSE I catalog. Results. The 13 CO J = 1−0 emission presents two large cloud clumps. The clump consistent with IRDC G38.95-0.47 shows a triangle-like shape, and has a steep integrated-intensity gradient toward H II regions G38.91-0.44 and G39.30-1.04, suggesting that the two H II regions have expanded into the IRDC. Four submillmeter continuum sources have been detected in the IRDC G38.95-0.47. Only the G038.95-00.47-M1 source with a mass of 117 M has outflow and infall motions, indicating a newly forming massive star. We detected a new collimated outflow in the clump compressed by G38.93-0.39. The derived ages of the three H II regions are 6.1 × 10 5 yr, 2.5 × 10 5 yr, and 9.0 × 10 5 yr, respectively. In the IRDC G38.95-0.47, the significant enhancement of several Class I YSOs indicates the presence of some recently formed stars. Comparing the ages of these H II regions with YSOs (Class I sources and massive G038.95-00.47-M1 source), we suggest that YSOs may be triggered by G38.91-0.44 and G39.30-1.04 together, which supports the radiatively driven implosion model. It may be the first time that the triggered star formation has occurred in the IRDC compressed by two H II regions. The new detected outflow may be driven by a star cluster.

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“…Hence, this result only provides a lower limit, since the emission at 1390 MHz could be partially optically thick as is evident from our radio spectral index estimations. In addition to this, several studies show that there could be appreciable absorption of Lyman continuum photons by dust (Inoue, Hirashita & Kamaya 2001;Arthur et al 2004;Paron, Petriella & Ortega 2011). It is further noticed that if the total infrared luminosity of G12.42+0.50 (2.8 × 10 4 , Section 3.3.2) were to be produced by a ZAMS star, it would correspond to a star with spectral type between B0 − O9.5 (Panagia 1973).…”

Section: Uc H II Regionmentioning

confidence: 95%

Initial phases of high-mass star formation: a multiwavelength study towards the extended green object G12.42+0.50

Issac

Tej

Varricatt

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a multiwavelength study of the extended green object, G12.42+0.50 in this paper. The associated ionized, dust, and molecular components of this source are studied in detail employing various observations at near-, mid-and far-infrared, submillimeter and radio wavelengths. Radio continuum emission mapped at 610 and 1390 MHz, using the Giant Meterwave Radio Telescope, India, advocates for a scenario of coexistence of an UC H II region and an ionized thermal jet possibly powered by the massive young stellar object, IRAS 18079-1756 with an estimated spectral type of B1 − B0.5. Shock-excited lines of H 2 and [FeII], as seen in the near-infrared spectra obtained with UKIRT-UIST, lend support to this picture. Cold dust emission shows a massive clump of mass 1375 M enveloping G12.42+0.50. Study of the molecular gas kinematics using the MALT90 and JCMT archival data unravels the presence of both infall activity and large-scale outflow suggesting an early stage of massive star formation in G12.42+0.50. A network of filamentary features are also revealed merging with the massive clump mimicking a hub-filament layout. Velocity structure along these indicate bulk inflow motion.

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The HII region G35.673-00.847: another case of triggered star formation?

Cited by 22 publications

References 31 publications

The Embedded Ring-like Feature and Star Formation Activities in G35.673-00.847

The Embedded Ring-like Feature and Star Formation Activities in G35.673-00.847

Triggered massive and clustered star formation by combined H II regions G38.91-0.44 and G39.30-1.04

Initial phases of high-mass star formation: a multiwavelength study towards the extended green object G12.42+0.50

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