A multi-wavelength analysis of the diffuse H ii region G25.8700+0.1350

Cichowolski, Silvina; Duronea, N. U.; Suad, Laura Andrea; Reynoso, E. M.; Dorda, R.

doi:10.1093/mnras/stx2676

Cited by 6 publications

(3 citation statements)

References 58 publications

(63 reference statements)

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“…Proposed examples of triggered star formation abound in the literature over a variety of scales. In particular, the high quality infrared observations from the Spitzer and Herschel space observatories over the last decade and a half have provided abundant support for the actual existence of triggered star formation along the edges of bubble-like HII regions (Deharveng & Zavagno 2011;Samal et al 2014;Liu et al 2016;Gama et al 2016;Cichowolski et al 2018). Examples at larger scales where star formation appears to have been caused by expanding supershells seen in HI in the disk of our Galaxy also exist (Megeath et al 2003;Oey et al 2005;Arnal & Corti 2007;Lee & Chen 2009), although the evidence is more elusive, largely due to confusion and crowdedness along the line of sight.…”

Section: Discussionmentioning

confidence: 99%

The possible common origin of M 16 and M 17

Comerón

Torra

2018

A&A

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Context. It has been suggested that the well-studied giant HII regions M16 and M17 may have had a common origin, being an example of large-scale triggered star formation. While some features of the distribution of the interstellar medium in the region support this interpretation, no definitive detection of an earlier population of massive stars responsible for the triggering has been made thus far. Aims. We have carried out observations looking for red supergiants in the area covered by a giant shell seen in HI and CO centered on galactic coordinates l ∼ 14 • 5, b ∼ +1 • that peaks near the same radial velocity as the bulk of the emission from both giant HII regions, which are located along the shell. Red supergiants have ages in the range expected for the parent association whose most massive members could have triggered the formation of the shell and of the giant HII regions along its rim. Methods. We have obtained spectroscopy in the visible of a sample of red stars selected on the basis of their infrared colors, whose magnitudes are consistent with them being red supergiants if they are located at the distance of M16 and M17. Spectroscopy is needed to distinguish red supergiants from AGB stars and RGB stars, which are expected to be abundant along the line of sight.Results. Out of a sample of 37 bright red stars, we identify four red supergiants that confirm the existence of massive stars in the age range between ∼ 10 and ∼ 30 Myr in the area. At least three of them have Gaia DR2 parallaxes consistent with them being at the same distance as M16 and M17. Conclusions. The evidence of past massive star formation within the area of the gaseous shell lends support to the idea that it was formed by the combined action of stellar winds and ionizing radiation of the precursors of the current red supergiants. These could be the remnants of a richer population, whose most massive members have exploded already as core-collapse supernovae. The expansion of the shell against the surrounding medium, perhaps combined with the overrun of preexisting clouds, is thus a plausible trigger of the formation of a second generation of stars currently responsible for the ionization of M16 and M17.F. Comerón and J. Torra: On the possible common origin of M16 and M17 selection criteria and our findings, through which we produce a crude estimate of the overall massive star content of the association and the mechanical energy deposited in the bubble, which suggest that the scenario of triggered formation of M16 and M17 is indeed plausible.

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Section: Discussionmentioning

confidence: 99%

The possible common origin of M 16 and M 17

Comerón

Torra

2018

A&A

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“…In the same way, several analysis of the energy values involved in the formation of these regions show that many highmass stars seem to be missing or have not been detected (e.g. Cichowolski et al 2018). On the other side, observational studies have confirmed that massive stars are not usually isolated but are, in fact, members of binary systems or other stellar groups (Roberts 1957;Maíz-Apellániz 2004;Barbá et al 2017).…”

Section: Introductionmentioning

confidence: 97%

Stellar population in the vicinity of the H ii region G331.03-00.15

Cárdenas

Blanco

Gamen

et al. 2022

A&A

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We present a multi-wavelength study of the H II region G331.03-00.15, with the aim of identifying the population of massive stars associated with it. The distributions of ionised gas and heated dust both exhibit similar spherical forms, while the bordering photodissociating region follows a very ring-like distribution, indicating the presence of abundant neighbouring molecular material being photo-dissociated. There is only one high-mass star catalogued in the region, namely, the WR star 1051-67L. Based on an energy analysis of the detected radio continuum emission, we deduced that additional high-mass stars could be interacting with G331.03-00.15. We conducted a search of massive star candidates by applying a series of colour criteria to a sample of highly reddened infrared (IR) point sources projected over the radio continuum morphology, with the additional condition that they be located at the same distance assumed for the region. Fourteen candidate sources were selected and classified using low-resolution, near-infrared (NIR) spectroscopic data in the H and K bands, obtained with Gemini/FLAMINGOS-2. We identified one massive star and classified it as an O7 V star. Adding the contribution from this new star to the total ionising radiation available, we concluded that it would be possible for the H II region to be powered solely by these two massive stars. However, we do not rule out the possibility that there could be more early-type stars that remain undetected in this highly obscured part of the Galaxy. Additionally, we searched for primary tracers of star-forming activity and identified several class I and II candidate young stellar objects (YSOs), positioned over the dense clouds and clumps of molecular material found in the area. The presence of several maser species located in the densest cloud are also indicative of massive star formation taking place in the vicinity of G331.03-00.15.

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“…The structure and physical properties of molecular clouds can be significantly influenced by feedback from massive stars (>8 M e ), such as outflows, radiation pressure, stellar winds, and supernova explosions (Zinnecker & Yorke 2007;Raskutti et al 2017;Cichowolski et al 2018). Radiation from H II regions and expansion of supernova remnants can create expanding shells in their surroundings and the expanding shells can sweep up diffuse molecular gas into dense shells which may subsequently undergo fragmentation and form a new generation of stars (Whitworth et al 1994;Kim et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Molecular Clouds Associated with H ii Regions and Candidates within l = 106.°65 to 109.°50 and b = −1.°85 to 0.°95

Li¹,

Wang²,

Ma³

et al. 2022

Res. Astron. Astrophys.

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We present a large-scale simultaneous survey of the CO isotopologues ($\rm {}^{12}{CO}$, $\rm{}^{13}{CO}$, and $\rm{C}{}^{18}{O}$) J = 1 ${-}$ 0 line emission toward the Galactic plane region of l = 106.65$^\circ$ to 109.50$^\circ$ and b = ${-}$1.85$^\circ$ to 0.95$^\circ$ using the Purple Mountain Observatory 13.7 m millimeter-wavelength telescope. Except for the molecular gas in the solar neighborhood, the emission from the molecular gas in this region is concentrated in the velocity range of [${-}$60, ${-}$35] $\rm km~s^{-1}$. The gas in the region can be divided into four clouds, with mass in the range of $\sim$10$^{3}$ to 10$^{4}$\,${M_{\sun}}$. We have identified 25 filaments based on the $\rm {}^{13}{CO}$ data. The median excitation temperature, length, line mass, line width, and virial parameter of the filaments are 10.89 K, 8.49 pc, 146.11 ${M}_{\odot}~ \rm pc^{-1}$, 1.01 $\rm km~s^{-1}$, and 3.14, respectively. Among these filaments, eight have virial parameters of $<$~2, suggesting that they are gravitationally bound and can lead to star formation. Nineteen {H \small {II}} regions or candidates have previously been found in the region and we investigate the relationships between these {H \small {II}} regions/candidates and surrounding molecular clouds in detail. Using morphology similarity and radial velocity consistency between {H \small {II}} regions/candidates and molecular clouds as evidence for association, and raised temperature and velocity broadening as signatures of interaction, we propose that 12 {H \small {II}} regions/candidates are associated with their surrounding molecular clouds. In the case of the {H \small {II}} region of S142, the energy of the {H \small {II}}region is sufficient to maintain the turbulence in the surrounding molecular gas.

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A multi-wavelength analysis of the diffuse H ii region G25.8700+0.1350

Cited by 6 publications

References 58 publications

The possible common origin of M 16 and M 17

The possible common origin of M 16 and M 17

Stellar population in the vicinity of the H ii region G331.03-00.15

Molecular Clouds Associated with H ii Regions and Candidates within l = 106.°65 to 109.°50 and b = −1.°85 to 0.°95

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