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

Corti, Mariela Alejandra; Orellana, R. B.

doi:10.1051/0004-6361/201220743

Cited by 13 publications

(14 citation statements)

References 34 publications

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“…Our derived distance of 2.6 +0.4 −0.3 kpc is larger than the 2.3±0.4 kpc estimated by Negueruela et al (2011), but again consistent within the 1σ uncertainties. However, the distance estimate of Negueruela et al (2011) was based on the best previous determination of the distance to Cen OB1, which has recently been revised upwards to 2.6 ± 0.5 kpc (Corti & Orellana 2013). Hence our distance remains fully consistent with the PSR B1259−63/LS 2883 system having originated from that OB association (see also Shannon et al 2014).…”

Section: Discussionsupporting

confidence: 56%

The geometric distance and binary orbit of PSR B1259–63

Miller-Jones

Deller

Shannon

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The pulsar/massive star binary system PSR B1259−63/LS 2883 is one of the beststudied gamma-ray binaries, a class of systems whose bright gamma-ray flaring can provide important insights into high-energy physics. Using the Australian Long Baseline Array we have conducted very long baseline interferometric observations of PSR B1259−63 over 4.4 years, fully sampling the 3.4-year orbital period. From our measured parallax of 0.38 ± 0.05 mas we use a Bayesian approach to infer a distance of 2.6 +0.4 −0.3 kpc. We find that the binary orbit is viewed at an angle of 154 ± 3 • to the line of sight, implying that the pulsar moves clockwise around its orbit as viewed on the sky. Taking our findings together with previous results from pulsar timing observations, all seven orbital elements for the system are now fully determined. We use our measurement of the inclination angle to constrain the mass of the stellar companion to lie in the range 15-31M . Our measured distance and proper motion are consistent with the system having originated in the Cen OB1 association and receiving a modest natal kick, causing it to have moved ∼ 8 pc from its birthplace over the past ∼ 3 × 10 5 years. The orientation of the orbit on the plane of the sky matches the direction of motion of the X-ray synchrotron-emitting knot observed by the Chandra X-ray Observatory to be moving away from the system.

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Section: Discussionsupporting

confidence: 56%

The geometric distance and binary orbit of PSR B1259–63

Miller-Jones

Deller

Shannon

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…The average color excess is E(b − y) = 0.29 (±0.03 sd; ±0.0041 se). These estimates are in perfect agreement with other authors (see Corti & Orellana 2013, and the reference therein).…”

Section: Distribution Of O-b9 Stars Toward Centaurussupporting

confidence: 93%

“…Corti & Orellana (2013) give the distance to the cluster as 1.9±0.5 kpc and the age of ∼15 Myr. Bonatto et al (2006) estimated the cluster's age as 14 ± 2 Myr and concluded that the star formation in NGC 4755 began ≈14 Myr ago and proceeded for about the same length of time.…”

Section: Wind-blown Energy Deposit Of the Most Massive Stars Within Gmentioning

confidence: 97%

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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“…At the same time, young star aggregates help us to probe the Galactic spiral structure, being one of the most prominent spiral arm tracers, together with gas, in the form of HI, HII, or CO (Carraro 2013 -see e.g. Shorlin 1 (Carraro & Costa 2009), Danks 1 and 2 (Baume et al 2009), NGC 6193/6167 (Baume et al 2011) or CenOB1/NGC 4755 (Corti & Orellana 2013). In this paper we extend our study to the remarkable IC 2944/2948 region, located at l ∼ 294.…”

Section: Introductionmentioning

confidence: 99%

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

Cited by 13 publications

References 34 publications

The geometric distance and binary orbit of PSR B1259–63

The geometric distance and binary orbit of PSR B1259–63

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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