The rotation of the Galaxy within the solar circle

Álvarez, H.; May, J.; Bronfman, L.

doi:10.1086/168258

Cited by 47 publications

(82 citation statements)

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“…I HI, CO Gunn et al (1979) quad. I HI Clemens (1985) North CO, HI for R < R 0 CO, HII for R > R 0 Rohlfs et al (1986) North + South HI for R < R 0 HII for R > R 0 Fich et al (1989) North HI, CO-HII Alvarez et al (1990) quad. IV CO Merrifield (1992) Ext.…”

Section: Referencementioning

confidence: 99%

“…Velocity anomalies in the Perseus and Carina arms have been known for a long time (Rickard 1968;Humphreys 1970Humphreys , 1972; more recently Alvarez et al (1990) have shown molecular velocity excesses of 12 km s −1 in the Carina arm and Heyer & Terebey (1998) show evidence that expanding motions are present within the Perseus arm. These velocity departures were studied in the radial velocity and seemed to be localized.…”

Section: Deviations From Circular Rotationmentioning

confidence: 99%

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Star-forming complexes and the spiral structure of our Galaxy

Russeil¹

2002

A&A

459

598

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Abstract.We have carried out a multiwavelength study of the plane of our Galaxy in order to establish a star-forming-complex catalogue which is as complete as possible. Features observed include Hα, H109α, CO, the radio continuum and absorption lines. For each complex we have determined the position, the systemic velocity, the kinematic distance and, when possible, the stellar distance and the corresponding uncertainties. All of these parameters were determined as homogeneously as possible, in particular all the stellar distances have been (re)calculated with the same calibration and the kinematic distances with the same mean Galactic rotation curve. Through the complexes with stellar distance determination, a rotation curve has been fitted. It is in good agreement with the one of Brand & Blitz (1993). We also investigated the residual velocities relative to the circular rotation model. We find that departures exist over large areas of the arms, with different values from one arm to another. From our data and in good agreement with previous studies, the Galactic warp is observed. It does not seem correlated with the departures from circular rotation. Finally, as segment-like features are noted from the complexes' distribution, we tried to find if they are indicative of a larger underlying structure. Then, we attempted to interpret the complexes' distribution in terms of spiral structure by fitting models with two, three and four logarithmic spiral arms. The four-arm model seems more appropriate to represent the grand design of our Galaxy. In this model the Norma arm and the external arm appear as being the two extremities of a single arm called the Norma-Cygnus arm. The new data and fitted model confirm the four-segment model of Georgelin & Georgelin (1976), clarifying the arms' design and extension and doubling their known length.

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Section: Referencementioning

confidence: 99%

Section: Deviations From Circular Rotationmentioning

confidence: 99%

Star-forming complexes and the spiral structure of our Galaxy

Russeil¹

2002

A&A

459

598

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“…However, we discuss it here since it has been used to constrain several dynamical models of the Milky Way (Binney et al 1991;Weiner & Sellwood 1999;Englmaier & Gerhard 1999;Bissantz et al 2003). There have been different determinations of the TVC using CO and HI data (Fich et al 1989;Burton & Liszt 1993;Clemens 1985;Alvarez et al 1990). The dispersion of the TVC points derived by different authors is typically 10 km s −1 (see for instance Fig.…”

Section: The Terminal Velocity Curvementioning

confidence: 99%

Gas flow models in the Milky Way embedded bars

Rodríguez-Fernández¹,

Combes

2008

A&A

164

212

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Context. The gas distribution and dynamics in the inner Galaxy present many unknowns, such as the origin of the asymmetry of the lv-diagram of the Central Molecular Zone (CMZ). On the other hand, there is recent evidence in the stellar component of the presence of a nuclear bar that may be slightly lopsided. Aims. Our goal is to characterize the nuclear bar observed in 2MASS maps and to study the gas dynamics in the inner Milky Way taking into account this secondary bar. Methods. We have derived a realistic mass distribution by fitting the 2MASS star count map with a model including three components (disk, bulge and nuclear bar) and we have simulated the gas dynamics in the deduced gravitational potential using a sticky-particles code.Results. Our simulations of the gas dynamics successfully reproduce the main characteristics of the Milky Way for a bulge orientation of 20• -35• with respect to the Sun-Galactic Center (GC) line and a pattern speed of 30-40 km s −1 kpc −1 . In our models the Galactic Molecular Ring (GMR) is not an actual ring but the inner parts of the spiral arms, while the 3-kpc arm and its far side counterpart are lateral arms that extend around the bar. Our simulations reproduce, for the first time, the parallelogram shape of the lv-diagram of the CMZ as the gas response to the nuclear bar. This bar should be oriented by an angle of ∼60• -75• with respect to the Sun-GC line and its mass amounts to (2-5.5) 10 9 M . We show that the observed asymmetry of the CMZ cannot be due to lopsidedness of the nuclear bar as suggested by the 2MASS maps. Conclusions. We do not find clear evidence of lopsidedness in the stellar potential. We propose that the observed asymmetry of the central gas layer can be due to the infalling of gas into the CMZ in the l = 1.3• -complex.

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“…We estimate the kinematic distance using the rotation curve determined by Alvarez et al (1990), with a Galactocentric solar distance of 8.5 kpc and a solar LSR velocity of 220 km s −1 . Considering a Galactic longitude of 345.…”

Section: Gmc G3455+10mentioning

confidence: 99%

Massive star formation in the GMC G345.5+1.0: spatial distribution of the dust emission

López¹,

Bronfman²,

Nyman³

et al. 2011

A&A

Self Cite

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Context. Massive condensations in giant molecular clouds (GMCs) are linked to the formation of high mass stars, which are the principal source of heavy elements and UV radiation, playing an important role in the evolution of galaxies. Aims. We attemp to make a complete census of massive-star formation within all of GMC G345.5+1.0. This cloud is located one degree above the Galactic plane and at 1.8 kpc from the Sun, thus there is little superposition of dust along the line-of-sight, minimizing confusion effects in identifying individual clumps. Methods. We observed the 1.2 mm continuum emission across the whole GMC using the Swedish-ESO Submillimetre Telescope (SEST) Imaging Bolometer Array (SIMBA) mounted on the SEST. Observations have a spatial resolution of 0.2 pc and cover 1.• 8 × 2.• 2 in the sky with a noise of 20 mJy beam −1 . Results. We identify 201 clumps with diameters between 0.2 and 0.6 pc, masses between 3.0 and 1.3 × 10 3 M , and densities between 5 × 10 3 and 4 × 10 5 cm −3 . The total mass of the clumps is 1.2 × 10 4 M , thus the efficiency in forming these clumps, estimated as the ratio of the total clump mass to the total GMC mass, is ∼0.02. The clump mass distribution for masses between 10 and 10 3 M is well-fitted by a power law dN/dM ∝ M −α , with a spectral mass index α of 1.7 ± 0.1. Given their mass distribution, clumps do not appear to be the direct progenitors of single stars. Comparing the 1.2 mm continuum emission with infrared images taken by the Midcourse Space Experiment (MSX) and by the Spitzer satellite, we find that at least ∼20% of the clumps are forming stars, and at most ∼80% are starless. Six massive-star forming regions (MSFRs) embedded in clumps and associated with IRAS point sources have mean densities of ∼10 5 cm −3 , luminosities >10 3 L , and spectral energy distributions that can be modeled with two dust components at different mean temperatures of 28 ± 5 and 200 ± 10 K.

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The rotation of the Galaxy within the solar circle

Cited by 47 publications

References 0 publications

Star-forming complexes and the spiral structure of our Galaxy

Star-forming complexes and the spiral structure of our Galaxy

Gas flow models in the Milky Way embedded bars

Massive star formation in the GMC G345.5+1.0: spatial distribution of the dust emission

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