Revisiting the birth locations of pulsars B1929+10, B2020+28, and B2021+51

Kirsten, F.; Vlemmings, Wouter; Campbell, R. M.; Krämer, M.; Chatterjee, Shami

doi:10.1051/0004-6361/201425562

Cited by 39 publications

(37 citation statements)

References 27 publications

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“…Such a situation is not unusual (Yao et al 2017). For instance, the very long baseline interferometry (VLBI) parallax measurements for two pulsars revealed 65% lower distances than followed from the NE2001 model (Kirsten et al 2015). Subsequent extensive VLBI parallax analysis of 57 pulsar under the PSRπ project also suggests that the accuracy of the DM-based distance predictions is significantly overestimated (Deller et al 2018).…”

Section: Pulsar Distance and The Galactic Electron Density Distributionmentioning

confidence: 99%

Tracking the Footprints of the Radio Pulsar B1727–47: Proper Motion, Host Supernova Remnant, and the Glitches

Shternin

Kirichenko

Zyuzin

et al. 2019

ApJ

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The bright radio pulsar B1727−47 with a characteristic age of 80 kyr is among the first pulsars discovered 50 yr ago. Using its regular timing observations and interferometric positions at three epochs, we measured, for the first time, the pulsar proper motion of 151 ± 19 mas yr −1 . At the dispersion measure distance of 2.7 kpc, this would suggest a record transverse velocity of the pulsar 1900 km s −1 . However, a backward extrapolation of the pulsar track to its birth epoch points remarkably close to the center of the evolved nearby supernova remnant RCW 114, which suggests genuine association of the two objects. In this case, the pulsar is substantially closer (∼ 0.6 kpc) and younger (∼ 50 kyr), and its velocity (∼ 400 km s −1 ) is compatible with the observed pulsar velocity distribution. We also identified two new glitches of the pulsar. We discuss implications of our results on the pulsar and remnant properties.

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Section: Pulsar Distance and The Galactic Electron Density Distributionmentioning

confidence: 99%

Tracking the Footprints of the Radio Pulsar B1727–47: Proper Motion, Host Supernova Remnant, and the Glitches

Shternin

Kirichenko

Zyuzin

et al. 2019

ApJ

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“…van Buren & McCray 1988). It was claimed that this star was part of a binary and was ejected when its companion (now the pulsar PSR B1929+10) exploded as a supernova about 1 Myr ago (van Rensbergen et al 1996;Hoogerwerf et al 2001;Tetzlaff et al 2010), but Kirsten et al (2015) recently refuted this hypothesis. In any case, it appears to be currently single; we found no significant RV variation in the data.…”

Section: C28 Hd 149757mentioning

confidence: 99%

Chemical abundances of fast-rotating massive stars

Cazorla

Morel

Nazé

et al. 2017

A&A

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Aims. Recent observations have challenged our understanding of rotational mixing in massive stars by revealing a population of fastrotating objects with apparently normal surface nitrogen abundances. However, several questions have arisen because of a number of issues, which have rendered a reinvestigation necessary; these issues include the presence of numerous upper limits for the nitrogen abundance, unknown multiplicity status, and a mix of stars with different physical properties, such as their mass and evolutionary state, which are known to control the amount of rotational mixing. Methods. We have carefully selected a large sample of bright, fast-rotating early-type stars of our Galaxy (40 objects with spectral types between B0.5 and O4). Their high-quality, high-resolution optical spectra were then analysed with the stellar atmosphere modelling codes DETAIL/SURFACE or CMFGEN, depending on the temperature of the target. Several internal and external checks were performed to validate our methods; notably, we compared our results with literature data for some well-known objects, studied the effect of gravity darkening, or confronted the results provided by the two codes for stars amenable to both analyses. Furthermore, we studied the radial velocities of the stars to assess their binarity.Results. This first part of our study presents our methods and provides the derived stellar parameters, He, CNO abundances, and the multiplicity status of every star of the sample. It is the first time that He and CNO abundances of such a large number of Galactic massive fast rotators are determined in a homogeneous way.

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“…This worked well only when increasing the error bars for the measured (input) data as they were known at that time (2000) to 10 σ (see also Tetzlaff et al ). Later on, when more precise values for proper motion and parallax of the pulsar became known, including smaller error bars, it did not work well anymore (Bobylev ; Kirsten et al ; Tetzlaff et al ). In this context, it is important to mention that a wide range of RVs (from −35 to +30 km s −1 , as summarized in Table ) have been published for ζ Oph in the literature.…”

Section: Introductionmentioning

confidence: 99%

The radial and rotational velocity of ζ Ophiuchi

Zehe¹,

Mugrauer²,

Neuhäuser³

et al. 2018

Astron Nachr

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We present the results of our spectroscopic monitoring campaign of Oph, carried out at the University observatory Jena with the spectrograph FLECHAS between July 2015 and September 2016. The main aim of the project was to determine the radial velocity of the star precisely, as a wide range of radial velocity measurements of Oph are given in the literature. Besides the proper motion and parallax, the radial velocity is an important input parameter for the calculation of the space motion of the star. Oph is considered to be a runaway star and potential former companion of the progenitor star of the pulsar PSR J1932+1059, both of which may have been located in a binary system and were then released during a supernova explosion about 1 Myr ago in the Upper Scorpius OB association. For the conclusion that the pulsar and Oph could have been at the same place, a radial velocity of −9.0 km s −1 for Oph was used in the literature. By analyzing the hydrogen and helium lines in 48 FLECHAS spectra, we determined the radial velocity of Oph to be 12.2 ± 3.3 km s −1 and the projected rotational velocity to be 432 ± 16 km s −1 with no indication of variability.

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Revisiting the birth locations of pulsars B1929+10, B2020+28, and B2021+51

Cited by 39 publications

References 27 publications

Tracking the Footprints of the Radio Pulsar B1727–47: Proper Motion, Host Supernova Remnant, and the Glitches

Tracking the Footprints of the Radio Pulsar B1727–47: Proper Motion, Host Supernova Remnant, and the Glitches

Chemical abundances of fast-rotating massive stars

The radial and rotational velocity of ζ Ophiuchi

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