GS305+04-26: revisiting the interstellar medium around the Centaurus OB1 stellar association

Corti, Mariela Alejandra; Arnal, E. M.; Orellana, R. B.

doi:10.1051/0004-6361/201118455

Cited by 6 publications

(21 citation statements)

References 33 publications

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“…In these new spectroscopic and astrometric studies we found 56 members of Cen OB1 and NGC 4755, while in Corti et al (2012) 54 members of Cen OB1 and NGC 4755 were found, so between both works there are 43 members in common. For this reason the total energy supplied to the interstellar medium by this new group of members of Cen OB1 and NGC 4755 is 17% lower than the energy published in Corti et al (2012).…”

Section: Membershipmentioning

confidence: 62%

“…For this reason the total energy supplied to the interstellar medium by this new group of members of Cen OB1 and NGC 4755 is 17% lower than the energy published in Corti et al (2012). With the contribution of energy to the Hi shell GS305+04-26 given by the pulsars, it is sufficient to generate this Hi shell, as was stated in Corti et al (2012).…”

Section: Membershipmentioning

confidence: 75%

“…12 it is possible to see that several members of Cen OB1 are in the galactic plane of our Galaxy. According to the research about the Hi shell GS305+04-26, published in Corti et al (2012) the possible generators of this Hi shell were the members of Cen OB1, through their winds. Some members of Cen OB1 and the NGC 4755 cluster are inside the Hi, and it has two supergiant members (one of them a possible binary system) and one giant member sharing the location with the members of the association.…”

Section: Size and Agementioning

confidence: 99%

“…As part of a project in which the investigation of the possible link between star sets and Hi shells is proposed, the Hi GS305+04−26, centred in (l,b) = (305 • , +4 • ) (Corti et al 2012) was investigated. In a study of this kind it was determined that the Hi GS305+04−26, could have been generated by the open cluster NGC 4755 and the stellar association Cen OB1.…”

Section: Introductionmentioning

confidence: 99%

“…The distance estimated was 1976 pc. - Corti et al (2012) incorporated the PSRJ 1253−5820 and PSRJ 1254−6150 pulsars as members of Cen OB1. Both could have arisen as a result of the explosion as supernovae (SNe) of two stars that are possible members of Cen OB1.…”

Section: Introductionmentioning

confidence: 99%

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Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies

Corti

Orellana

2013

A&A

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Context. An OB association is a gravitationally unbound group of stars. The identification of the members of the association is an important aspect of its study. There are few astrometric membership studies for OB associations, but the combination of these studies with astrophysical techniques becomes a very powerful tool for this type of research. Aims. We perform new spectroscopic and astrometric studies of the members of the association Centaurus OB1 (Cen OB1) and the open cluster NGC 4755. Methods. To carry out this study we used new spectroscopic optical observations obtained at CASLEO, and proper motion and photometric data from the Tycho-2 Catalogue and other databases available via the Internet.Results. With this investigation we found 52 members of Cen OB1 (l = 303.• 7, b = 0.• 4) and four members of NGC 4755 (l = 303.• 2, b = 2.• 5), an open cluster integrated into the Cen OB1 stellar association. The distance, heliocentric radial velocity, proper motion, and age of Cen OB1 are 2.6 ± 0.5 kpc, ∼−20 km s −1 , μ α cos δ = −4.78 ± 0.10 mas yr −1 , μ δ = −0.93 ± 0.10 mas yr −1 , and ∼20 × 10 6 years old, respectively. The same parameters found for NGC 4755 are 1.9 ± 0.5 kpc, −18 ± 2 km s −1 , μ α cos δ = −4.14 ± 0.19 mas yr −1 , μ δ = −1.09 ± 0.12 mas yr −1 , and ∼15 × 10 6 years old. The pulsars PSR J1253−5820 and PSR J1254−6150 could have been born as the result of supernovae explosions that occurred in the past by massive members of Cen OB1. We have seen Infrared Astronomical Satellite (IRAS) sources near Cen OB1, that show that star formation is still occurring. The age gradient observed between the different members of Cen OB1 makes it likely that the stellar association and IRAS sources represent different stages of a sequential formation process.

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Section: Membershipmentioning

confidence: 62%

Section: Membershipmentioning

confidence: 75%

Section: Size and Agementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies

Corti

Orellana

2013

A&A

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Massive stellar content of the Galactic supershell GSH 305+01−24

Kaltcheva¹,

Golev²,

Moran³

2014

A&A

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Aims. The distribution of OB stars along with Hα, 12 CO, dust infrared emission, and neutral hydrogen is carried out to provide a more complete picture of interactions of the young massive stars and the observed supershell GSH 305+01−24. Methods. The studied field is located between 299The investigation is based on nearly 700 O-B9 stars with currently available uvbyβ photometry. The derived stellar physical parameters were used to establish a homogeneous scale for the distances and extinction of light for major apparent groups and layers of foreground and background stars in Centaurus and to study the interaction with the surrounding interstellar medium. Results. The distance to the entire Centaurus star-forming complex is revised, and a maximum of the OB-star distance distribution is found at 1.8 ± 0.4 (rms) kpc. The massive star component of GSH 305+01−24 is identified at about 85−90% completeness up to 11.5−12 mag. The projected coincidence of the OB stars with the shell and the similarities between the shell's morphology and the OB-star distribution indicate a strong interaction of the stellar winds with the superbubble material. We demonstrate that these stars contribute enough wind injection energy to explain the observed size and expansion velocity of the supershell. The derived stellar ages suggest an age gradient over the Coalsack Loop. Continuous star formation might be taking place within the shell with the youngest stars located toward its periphery, and the open cluster NGC 4755 is the oldest. A layer of very young stars at 1 kpc is detected, and its connection to both GSH 305+01−24 and the foreground GSH 304−00−12 H i shells is investigated.

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A deep and wide-field view at the IC 2944/2948 complex in Centaurus*

Baume

Rodríguez

Corti

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We employed the ESO MPI wide-field camera and obtained deep images in the VI C passbands in the region of the IC 2944/2948 complex (l ∼ 294. • 8; b ∼ −1. • 6), and complemented them with literature and archival data. We used this material to derive the photometric, spectroscopic and kinematic properties of the brightest (V < 16) stars in the region. The VI deep photometry on the other end, helped us to unravel the lower main sequence of a few, possibly physical, star groups in the area.Our analysis confirmed previous suggestions that the extinction toward this line of sight follows the normal law (R V = 3.1). We could recognize B-type stars spread in distance from a few hundred pc to at least 2 kpc. We found two young groups (age ∼ 3 Myr) located respectively at about 2.3 and 3.2 kpc from the Sun. They are characterized by a significant variable extinction (E B−V ranging from 0.28 to 0.45 mag), and host a significant pre-main sequence population. We computed the initial mass functions for these groups and obtained slopes Γ from -0.94 to -1.02 (e Γ = 0.3), in a scale where the classical Salpeter law is -1.35. We estimated the total mass of both main stellar groups in ∼ 1100 and ∼ 500 M ⊙ , respectively. Our kinematic analysis indicated that both groups of stars deviate from the standard rotation curve of the Milky Way, in line with literature results for this specific Galactic direction.Finally, along the same line of sight we identified a third group of early-type stars located at ∼ 8 kpc from the Sun. This group might be located in the far side of the Sagittarius-Carina spiral arm.

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GS305+04-26: revisiting the interstellar medium around the Centaurus OB1 stellar association

Cited by 6 publications

References 33 publications

Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies

Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies

Massive stellar content of the Galactic supershell GSH 305+01−24

A deep and wide-field view at the IC 2944/2948 complex in Centaurus*

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