Outer pseudoring in the galaxy

Melnik, A. M.

doi:10.1134/s1063773706010026

Cited by 34 publications

(46 citation statements)

References 29 publications

(26 reference statements)

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“…The absorption estimate of the source is A K = 0.59, which yields a distance of 2.0 kpc, compatible with the distance quoted above. In the same field we find the OB association Sct OB3 (see Mel'Nik & Efremov 1995), with ten members in a region of 25.8 × 33.6 pc 2 , and an estimated distance of 1.5 kpc. This distance is compatible with the estimate in Dambis et al (2001), obtained from a parallax measurement, of 1.4 kpc.…”

Section: The Origin Of Ls 5039 and Psr J1825−1446mentioning

confidence: 72%

On the origin of LS 5039 and PSR J1825−1446

Moldón

Ribó

Paredes

et al. 2012

A&A

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Context. The gamma-ray binary LS 5039 and the isolated pulsar PSR J1825−1446 were proposed to have been formed in the supernova remnant (SNR) G016.8−01.1. Aims. We aim to obtain the Galactic trajectory of LS 5039 and PSR J1825−1446 to find their origin in the Galaxy, and in particular to check their association with SNR G016.8−01.1 to restrict their age. Methods. By means of radio and optical observations we obtained the proper motion and the space velocity of the sources. Results. The proper motion of PSR J1825−1446 corresponds to a transverse space velocity of 690 km s −1 at a distance of 5 kpc. Its Galactic velocity at different distances is not compatible with the expected Galactic rotation. The velocity and characteristic age of PSR J1825−1446 make it incompatible with SNR G016.8−01.1. There are no clear OB associations or SNRs crossing the past trajectory of PSR J1825−1446. We estimate the age of the pulsar to be 80-245 kyr, which is compatible with its characteristic age. The proper motion of LS 5039 is μ α cos δ = 7.09 and μ δ = −8.82 mas yr −1 . The association of LS 5039 with SNR G016.8−01.1 is unlikely, although we cannot discard it. The system would have had to be formed in the association Ser OB2 (at 2.0 kpc) if the age of the system is 1.0-1.2 Myr, or in the association Sct OB3 (distance 1.5-2 kpc) for an age of 0.1-0.2 Myr. If the system were not formed close to Ser OB2, the pseudo-synchronization of the orbit would be unlikely. Conclusions. PSR J1825−1446 is a high-velocity isolated pulsar ejected from the Galaxy. The distance to LS 5039, which needs to be constrained by future astrometric missions such as Gaia, is a key parameter for restricting its origin and age.

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Section: The Origin Of Ls 5039 and Psr J1825−1446mentioning

confidence: 72%

On the origin of LS 5039 and PSR J1825−1446

Moldón

Ribó

Paredes

et al. 2012

A&A

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“…Turner (1985) provided a similar estimate of 1.88±0.24 kpc to Cen OB1 based mainly on Hβ photometry of ten members of Cen OB1 with reliable luminosities. The partition of Cen OB1 into five groups by Mel'nik & Efremov (1995) is not apparent. The overall impression is that beyond 1 kpc an extended star-forming complex of many OB stars is located.…”

Section: Distribution Of O-b9 Stars Toward Centaurusmentioning

confidence: 99%

“…In their new delineation of Galactic OB associations, Mel'nik & Efremov (1995) propose five groups (Cen 1A to Cen 1E) located between 303 • ≤ l ≤ 306 • at distances varying from 1.8 to 2.2 kpc. Their Cen 1A group consists of 37 stars, almost all belonging to NGC 4755.…”

Section: Distribution Of O-b9 Stars Toward Centaurusmentioning

confidence: 99%

“…There have been several attempts to establish the distance to Cen OB1 (Humphreys 1978;Blaha & Humphreys 1989;Garmany & Stencel 1992;Mel'nik & Efremov 1995), most of which were based on the photometric data of Blaha & Humphreys (1989) or on earlier studies. All estimates used UBV photometry and spectrophotometric calibrations and placed the association 1.9 to 2.5 kpc from the Sun.…”

Section: Introductionmentioning

confidence: 99%

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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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“…According to Humphreys (1978) this region is dominated by the Car OB1 association (284.2 • < l < 288 • , −2.2 • < b < 0.9 • ) at 2.5 kpc. In their revision of the list of Galactic OB associations Mel'nik & Efremov (1995) break down Car OB1 into five groups at distances between 2.2 and 2.8 kpc.…”

Section: Distribution Perpendicular To the Galactic Planementioning

confidence: 99%

The Carina spiral feature: Strömgren-β photometry approach

Kaltcheva¹,

Scorcio²

2010

A&A

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Aims. In recent years a significant development has become evident in the study of the stellar structure of the Galactic disk. This is especially true for the 3rd Galactic quadrant, where the stellar population was extensively investigated beyond 10 kpc, revealing details about the warped geometry of the thin and thick disks and outer arm. The 4th Galactic quadrant offers even better opportunity to follow the distribution of the young stellar populace to a large distance, since the line of sight is parallel to the largest single segment of a spiral arm seen from our position in the Galaxy: the Carina spiral feature. This paper further contributes to the study of the structure of the Galactic disk in the direction of Carina field utilizing homogeneous photometric distances of a sample of about 600 bright early-type stars seen in this direction up to 6 kpc. Methods. The derived stellar distances are based on uvbyβ photometry. All O and B type stars with uvbyβ data presently available are included in the study. Results. The photometry-derived parameters allow us to study the structure and characteristics of this segment of the Carina arm. We find that the stellar distribution is consistent with a location of the apparent edge of the arm at l = 287 • . Toward the edge of the arm the warp of the Galactic plane can be traced up to 6 kpc where it reaches negative 200 pc. The field toward the edge seems to be much more complex than harboring just one OB association, and it is likely that some of the apparent concentrations in this field represent parts of long segments of the edge. In the 284 • -289 • longitude range an interarm space about 1 kpc wide is found beyond 850 pc from the Sun. The giant molecular clouds and open clusters do not follow the edge of the arm as defined by the OB stars and indicate a possible presence of an age gradient in a direction perpendicular to the formal Galactic plane.

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Outer pseudoring in the galaxy

Cited by 34 publications

References 29 publications

On the origin of LS 5039 and PSR J1825−1446

On the origin of LS 5039 and PSR J1825−1446

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

The Carina spiral feature: Strömgren-β photometry approach

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