The Properties of the Galactic Bar Implied by Gas Kinematics in the Inner Milky Way

Weiner, Benjamin J.; Sellwood, J. A.

doi:10.1086/307786

Cited by 124 publications

(179 citation statements)

References 54 publications

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“…Mass and orientation of the bar Several studies suggest that the mass of the COBE/DIRBE bar is in the range 0.98-2×10 10 M (Weiner & Sellwood 1999;Dwek et al 1995;Matsumoto et al 1982;Zhao 1996). Given that the bar is formed from the bulge, we assume the mass of the bar is in the range 9.8 × 10 9 − 1.4 × 10 10 M .…”

Section: Galactic Bar Parametersmentioning

confidence: 99%

Radial migration of the Sun in the Milky Way: a statistical study

Martínez-Barbosa

Brown

Zwart

2014

Monthly Notices of the Royal Astronomical Society

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The determination of the birth radius of the Sun is important to understand the evolution and consequent disruption of the Sun's birth cluster in the Galaxy. Motivated by this fact, we study the motion of the Sun in the Milky Way during the last 4.6 Gyr in order to find its birth radius. We carried out orbit integrations backward in time using an analytical model of the Galaxy which includes the contribution of spiral arms and a central bar. We took into account the uncertainty in the parameters of the Milky Way potential as well as the uncertainty in the present day position and velocity of the Sun. We find that in general the Sun has not migrated from its birth place to its current position in the Galaxy (R ). However, significant radial migration of the Sun is possible when: 1) The 2 : 1 Outer Lindblad resonance of the bar is separated from the corrotation resonance of spiral arms by a distance ∼ 1 kpc. 2) When these two resonances are at the same Galactocentric position and further than the solar radius. In both cases the migration of the Sun is from outer regions of the Galactic disk to R , placing the Sun's birth radius at around 11 kpc. We find that in general it is unlikely that the Sun has migrated significantly from the inner regions of the Galactic disk to R .

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Section: Galactic Bar Parametersmentioning

confidence: 99%

Radial migration of the Sun in the Milky Way: a statistical study

Martínez-Barbosa

Brown

Zwart

2014

Monthly Notices of the Royal Astronomical Society

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“…An examination of the Galactic-longitude-velocity diagrams of CO emission (Dame et al 2001), H i (see Fig. 1 in Weiner & Sellwood 1999), Galactic planetary nebulae (Durand et al 1998) and OH/IR and SiO-maser stars (Habing et al 2006) shows that the observed velocities of V383 Sco and V381 Sco fall into regions close to the Galactic centre with very high velocities. The kinematics of the gas in these regions is inconsistent with purely circular motion (Dame et al 2001;Weiner & Sellwood 1999, and references therein).…”

Section: High-resolution Spectramentioning

confidence: 99%

A new look at the long-period eclipsing binary V383 Scorpii

Gałan

Tomov

Katô

et al. 2013

A&A

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Context. The system V383 Sco was discovered to be an eclipsing binary star at the beginning of the twentieth century. This system has one of the longest orbital periods known (13.5 yr) and was initially classified as a ζAur-type eclipsing variable. It was then forgotten about for decades, with no progress made in understanding it. Aims. This study provides a detailed look at the system V383 Sco, using new data obtained before, during, and after the last eclipse, which occurred in 2007/8. There was a suspicion that this system could be similar to eclipsing systems with extensive dusty disks like EE Cep and ε Aur. This and other, alternative hypotheses are considered here. Methods. The All Sky Automated Survey (ASAS-3) V and I light curves have been used to examine apparent magnitude and colour changes. Low-and high-resolution spectra have been obtained and used for spectral classification, to analyse spectral line profiles, as well as to determine the reddening, radial velocities and the distance to the system. The spectral energy distribution (SED) was analysed using all available photometric and spectroscopic data. Using our own original numerical code, we performed a very simplified model of the eclipse, taking into account the pulsations of one of the components. Results. The low-resolution spectrum shows apparent traces of molecular bands, characteristic of an M-type supergiant. The presence of this star in the system is confirmed by the SED, by a strong dependence of the eclipse depth on the photometric bands, and by the nature of pulsational changes. The presence of a very low excitation nebula around the system has been inferred from [O i] 6300 Å emission in the high-resolution spectrum. Analysis of the radial velocities, reddening, and period-luminosity relation for Mira-type stars imply a distance to the V383 Sco system of 8.4 ± 0.6 kpc. The distance to the nearby V381 Sco is 6.4 ± 0.8 kpc. The very different and oppositely directed radial velocities of these two systems (89.8 km s −1 vs. −178.8 km s −1 ) seem to be in agreement with a bulge/bar kinematic model of the Galactic centre and inconsistent with purely circular motion. Conclusions. We have found strong evidence for the presence of a pulsating M-type supergiant in the V383 Sco system. This supergiant periodically obscures the much more luminous F0 I-type star, causing the deep (possibly total) eclipses which vary in duration and shape.

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“…(Pichardo et al 2003 References. ( * ) Weiner & Sellwood (1999), Fux (1999), Ibata & Gilmore (1995), Englmaier & Gerhard (1999). We emphasize that the absolute PM presented here is based on direct observations of background galaxies, used to define the absolute reference frame.…”

Section: Observations Data Reduction Proper Motionsmentioning

confidence: 99%

Absolute proper motion of the Galactic open cluster M 67

Bellini

Bedin

Pichardo

et al. 2010

A&A

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We derived the absolute proper motion (PM) of the old, solar-metallicity Galactic open cluster M 67 using observations collected with CFHT (1997) and with LBT (2007). About 50 galaxies with relatively sharp nuclei allow us to determine the absolute PM of the cluster. We find (μ α cos δ, μ δ ) J2000.0 = (−9.6 ± 1.1, −3.7 ± 0.8) mas yr −1 . By adopting a line-of-sight velocity of 33.78 ± 0.18 km s −1 , and assuming a distance of 815 ± 50 pc, we explore the influence of the Galactic potential, with and without the bar and/or spiral arms, on the galactic orbit of the cluster.

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The Properties of the Galactic Bar Implied by Gas Kinematics in the Inner Milky Way

Cited by 124 publications

References 54 publications

Radial migration of the Sun in the Milky Way: a statistical study

Radial migration of the Sun in the Milky Way: a statistical study

A new look at the long-period eclipsing binary V383 Scorpii

Absolute proper motion of the Galactic open cluster M 67

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