The line-of-sight velocities of OB associations and molecular clouds in a wide solar neighborhood: The streaming motions of stars and gas in the Perseus arm

Sitnik, T. G.

doi:10.1134/1.1573280

Cited by 15 publications

(13 citation statements)

References 13 publications

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“…According to Sitnik (2003), the radial velocity of Cas OB4 with respect to the local standard of rest (LSR) is −29.1 km s −1 . If BD +60 73 is associated with Cas OB4, it has a radial velocity of 62 km s −1 with respect to the association.…”

Section: Discussionmentioning

confidence: 99%

Orbit and properties of the massive X-ray binary BD +60 73=IGR J00370+6122

Grunhut

Bolton

McSwain

2014

A&A

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Context. High-energy X-rays generated in massive binary systems can arise from several different mechanisms. Constraints on the orbital parameters of these systems are therefore necessary to properly understand and interpret the X-ray phenomena. Aims. In this study we aim to determine a spectroscopic orbit for the high-mass X-ray binary system BD +60 73=IGR J00370+6122, to infer the properties of the optical and compact companion, and to interpret the characteristics of the X-ray light curve within the context of our findings. Methods. We acquired 123 spectroscopic observations with the David Dunlap Observatory and Kitt Peak National Observatory telescopes in the optical domain. Using a cross-correlation technique, we measured the radial velocity of each of these spectra relative to the heliocentric rest-frame. An orbital solution was obtained from the resulting radial velocity measurements. Spectra of several spectral standards were also acquired to reassess the spectral classification of the optical companion. Results. The best-fit orbital parameters suggest an eccentricity of e = 0.48 +0.02−0.03 and a mass-function of f (M) = 0.009 ± 0.002, lending further support to the assumption that the companion is a low-mass compact star. We find that the X-ray maximum occurs just after the time of periastron passage, but before the time of superior conjunction when the optical companion could eclipse the compact companion. The spectrum of the optical companion is best matched by the B1Ib spectral standard HD 24398, which reaffirms the original classification. Conclusions. The mass-function combined with a plausible range of possible masses for a neutron star companion yields primary masses within the range expected for the spectral type of BD +60 73 for high orbital inclinations. The compact companion cannot be a black hole unless the supergiant has an exceptionally high mass for its B1Ib spectral type or if the inclination of its orbit is very low. The X-ray timing and characteristics can potentially be explained by accretion variations on the compact object; but this would require the companion to be a magnetar.

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Section: Discussionmentioning

confidence: 99%

Orbit and properties of the massive X-ray binary BD +60 73=IGR J00370+6122

Grunhut

Bolton

McSwain

2014

A&A

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“…The estimates of the corotation radius (CR) of the Galactic bar do not exceed 5 kpc, which gives the lower limit for its angular velocity Ω b > 40 km s −1 kpc −1 (Weiner & Sellwood 1999). However, this model cannot explain the kinematics of the Perseus region: the direction of the velocities of young stars in the Perseus region, if interpreted in terms of the density-wave concept (Lin, Yuan & Shu 1969), indicates that a fragment of a Perseus arm must be located inside the corotation circle (CR) (Burton & Bania 1974;Mel'nik, Dambis & Rastorguev 2001;Mel'nik 2003;Sitnik 2003) implying an upper limit Ω s < 25 km s −1 kpc −1 for its pattern speed, which is inconsistent with the one mentioned above. Attempts have been undertaken to overcome this contradiction by introducing an analytical spiral potential rotating slower than the bar (Bissantz, Englmaier & Gerhard 2003).…”

Section: Introductionmentioning

confidence: 99%

Classical Cepheids in the Galactic outer ring R₁R ′₂

et al. 2015

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The kinematics and distribution of classical Cepheids within ∼ 3 kpc from the Sun suggest the existence of the outer ring R1R ′ 2 in the Galaxy. The optimum value of the solar position angle with respect to the major axis of the bar, θ b , providing the best agreement between the distribution of Cepheids and model particles is θ b = 37 ± 13• . The kinematical features obtained for Cepheids with negative Galactocentric radial velocity VR are consistent with the solar location near the descending segment of the outer ring R2. The sharp rise of extinction toward of the Galactic center can be explained by the presence of the outer ring R1 near the Sun.

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“…We do not give any kinematic distance corresponding to the velocity -34 km s −1 because CO clouds and star-forming regions in the Perseus Arm considerably depart from the circular rotation that is due to streaming and expanding motions (Sitnik 2003;Vallée 2008;Choi et al 2014;Foster & Brunt 2015).…”

Section: Discussionmentioning

confidence: 99%

Dark clouds in the vicinity of the emission nebula Sh2-205: interstellar extinction and distances

Straižys

Čepas

Boyle

et al. 2016

A&A

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Results of CCD photometry in the seven-colour Vilnius system for 922 stars down to V = 16-17 mag and for 302 stars down to 19.5 mag are used to investigate the interstellar extinction in an area of 1.5 square degrees in the direction of the P7 and P8 clumps of the dark cloud TGU H942, which lies in the vicinity of the emission nebula Sh2-205. In addition, we used 662 red clump giants that were identified by combining the 2MASS and WISE infrared surveys. The resulting plots of extinction versus distance were compared with previous results of the distribution and radial velocities of CO clouds and with dust maps in different passbands of the IRAS and WISE orbiting observatories. A possible distance of the front edge of the nearest cloud layer at 130 ± 10 pc was found. This dust layer probably covers all the investigated area, which results in extinction of up to 1.8 mag in some directions. A second rise of the extinction seems to be present at 500-600 pc. Within this layer, the clumps P7 and P8 of the dust cloud TGU H942, the Sh2-205 emission nebula, and the infrared cluster FSR 655 are probably located. In the direction of these clouds, we identified 88 young stellar objects and a new infrared cluster.

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The line-of-sight velocities of OB associations and molecular clouds in a wide solar neighborhood: The streaming motions of stars and gas in the Perseus arm

Cited by 15 publications

References 13 publications

Orbit and properties of the massive X-ray binary BD +60 73=IGR J00370+6122

Orbit and properties of the massive X-ray binary BD +60 73=IGR J00370+6122

Classical Cepheids in the Galactic outer ring R₁R ′₂

Dark clouds in the vicinity of the emission nebula Sh2-205: interstellar extinction and distances

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The line-of-sight velocities of OB associations and molecular clouds in a wide solar neighborhood: The streaming motions of stars and gas in the Perseus arm

Cited by 15 publications

References 13 publications

Orbit and properties of the massive X-ray binary BD +60 73=IGR J00370+6122

Orbit and properties of the massive X-ray binary BD +60 73=IGR J00370+6122

Classical Cepheids in the Galactic outer ring R1R ′2

Dark clouds in the vicinity of the emission nebula Sh2-205: interstellar extinction and distances

Contact Info

Product

Resources

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Classical Cepheids in the Galactic outer ring R₁R ′₂