The H i  supershell GS 118+01−44  and its role in the interstellar medium

Suad, Laura Andrea; Cichowolski, Silvina; Noriega-Crespo, A.; Arnal, E. M.; Testori, J. C.; Flagey, Nicolas

doi:10.1051/0004-6361/201425409

Cited by 11 publications

(6 citation statements)

References 45 publications

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“…The mass value and the E kin are consistent with others HI shells studied in the literature (e.g. McClure-Griffiths et al 2002;Suad et al 2016).…”

Section: Kinetic Energy Stored In the Hi Shellsupporting

confidence: 90%

Studying the interstellar medium to look for relics of triggered star formation among stellar clusters

Paron,

Granada,

Areal

2021

Preprint

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Evidence of triggered star formation at large spatial scales involving stellar clusters is scarce. We investigate a Galactic region (l = 130. • 0, b = 0. • 35) populated by several open stellar clusters that according to the last GAIA data release, are located at a distance of about 2.9 kpc. By analyzing the interstellar medium (ISM) at infrared, centimeter, and millimeter wavelengths towards this group of clusters we discovered a shell of material of about 2 • in size at the same distance. We suggest that the shell, mainly observed at 12 µm and in the HI emission at 21 cm, was generated by the action of massive stars belonging to clusters Berkeley 7 and UBC 414, that lie at its center. Five clusters (MWSC0152, Czernik 6, Czernik 7, Berkeley 6, NGC 663, and NGC 654) lie at the border of this shell. From the comparison between the dynamical time of the discovered HI shell and the analysis of the ages of stellar populations in these clusters, we conclude that the expansion of the shell could have triggered in the past the formation of stars in some of them. We point out that in order to find physical evidence supporting a genetic connection between stellar clusters, it is necessary not only to study the individual clusters and their stellar populations, but also to investigate their surrounding ISM at a large spatial scale.

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“…The mass value and the E kin are consistent with others HI shells studied in the literature (e.g. McClure-Griffiths et al 2002;Suad et al 2016).…”

Section: Kinetic Energy Stored In the Hi Shellsupporting

confidence: 90%

Studying the interstellar medium to look for relics of triggered star formation among stellar clusters

Paron,

Granada,

Areal

2021

Preprint

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“…1 and 2), suggesting that the expanding bubble may have triggered the formation of a second generation of stars. There is evidence of star forming activity in the shells of SBs (Suad et al 2016(Suad et al , 2012. This is not straightforward for the SB associated with HESS J1857+026.…”

Section: Discussionmentioning

confidence: 99%

Radio study of HESS J1857+026: Gamma-rays from a superbubble?

Petriella

Duvidovich

Giacani

2021

A&A

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Aims. We provide new insights into the nature of HESS J1857+026, a very-high-energy γ-ray source whose complex morphology in the TeV band was attributed to the superposition of two distinct sources. Methods. We performed radio continuum observations to look for the pulsar wind nebula and the supernova remnant associated with the pulsar PSR J1856+0245, which might be powering part of the γ-ray emission. We observed HESS J1857+026 with the Karl G. Jansky Very Large Array (VLA) at 1.5 GHz in the C configuration. In addition, using the same array configuration, we observed a region of 0.4° × 0.4° towards PSR J1856+0245 at 6.0 GHz. We obtained complementary data for the neutral hydrogen and molecular gas emission from public surveys in order to investigate the properties of the interstellar medium in the direction of HESS J1857+026. Results. The new observations at 1.5 GHz do not show evidence of emission above the noise level of 0.7 mJy beam−1 that could be associated with either HESS J1857+026 or PSR J1856+0245. Also, in the new image at 6.0 GHz we do not detect radio emission from a pulsar wind nebula powered by PSR J1856+0245. The neutral gas analysis shows the existence of a superbubble in the direction of the γ-ray source. We suggest that this structure is located at ~5.5 kpc, compatible with the distance to the pulsar PSR J1856+0245. Conclusions. We conclude that TeV emission from HESS J1857+026 originates in a superbubble, arguing in favour of a single γ-ray source rather than the superposition of two distinct sources. The pulsar PSR J1856+0245 could also be contributing as a source of γ-rays within the bubble.

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“…Figure 5 shows the H i emission distribution averaged in the velocity range from −43.3 to −38.1 km s −1 , where the large H i features located at distances similar to GS 121−05−037 are marked with ellipses. Although two of these structures, GSH 117.8+1.5-35 (Cichowolski et al 2009) and GS 118+01-44 (Suad et al 2016), are observed in the same region of the sky, they are present in a different velocity range, as discussed in Suad et al (2016). On the other hand, the expansion of these two large shells was associated with the origin of the H ii regions Sh2-173 and Sh2-172, indicated as E and G in Fig.…”

Section: Discussionmentioning

confidence: 84%

“…Then, following the procedure described by Suad et al (2016), we estimated the amount of atomic mass present in GS 121−05−037, as well as the kinetic energy stored in it. Assuming solar abundances, we obtained M t = (1.7 ± 0.9) × 10 5 M ⊙ and E k = (2.1 ± 1.3) × 10 50 erg.…”

Section: H I Emission Distributionmentioning

confidence: 99%

GS 121–05–037: A new Galactic chimney candidate with signs of triggered star formation

Suad

Lera

Cichowolski

2022

A&A

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Aims. The goal of this study is to analyze the H i supershell GS 121−05−037 and its role in triggering star formation. Methods. To characterize the supershell, we analyzed the H i 21-cm line and the far-infrared emission distributions. In addition, to study the star formation processes related to GS 121−05−037, we used the Gaia survey, together with spectrophotometric calculations, and derived a method to look for massive OB-type stars.Results. The H i characterization of GS 121−05−037 shows an expanding structure centered at (l, b) ∼ (121 • .3, −4 • .8) in the velocity range from −47.8 to −25.2 km s −1 . It is located at 3.2 ± 1.0 kpc from the Sun and has a kinetic energy of E k = (2.1 ± 1.3) × 10 50 erg. GS 121−05−037 presents, in the H i emission distribution, an open morphology toward the Galactic halo. The analysis of the IR emission reveals the presence of 32 H ii regions seen projected into the borders of GS 121−05−037. A spectrophotometric analysis to look for the ionizing stars of these regions reveals that 12 of them would be located at a similar distance to GS 121−05−037. Conclusions. The relative location between GS 121−05−037 and the H ii regions, together with their age difference, led us to conclude that the ionizing stars could have been created due to the expansion of the H i supershell. On the other hand, the H ii regions located on the interface of two or more supershells could have originated from the collision of the H i structures. Finally, the open morphology of GS 121−05−037 toward the halo suggests that this large structure could be a Galactic chimney.

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The H i supershell GS 118+01−44 and its role in the interstellar medium

Cited by 11 publications

References 45 publications

Studying the interstellar medium to look for relics of triggered star formation among stellar clusters

Studying the interstellar medium to look for relics of triggered star formation among stellar clusters

Radio study of HESS J1857+026: Gamma-rays from a superbubble?

GS 121–05–037: A new Galactic chimney candidate with signs of triggered star formation

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