Searching for the in-plane Galactic bar and ring in DENIS

López-Corredoira, Martín; Hammersley, P. L.; Garzón, F.; Cabrera-Lavers, A.; Castro-Rodríguez, N.; Schultheis, M.; Mahoney, T. J.

doi:10.1051/0004-6361:20010560

Cited by 44 publications

(69 citation statements)

References 51 publications

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“…The extension in longitude of the extra density and its confinement very close to the galactic plane may suggest an inplane bar shape, as is argued in Hammersley et al (2000) and López-Corredoira et al (2001). Supposing that it does correspond to a bar, one can estimate its bar angle and its half-length, using the distance of excess stars from the Sun at its top end.…”

Section: Discussionmentioning

confidence: 94%

“…To continue this research work (see also López-Corredoira et al 2001) in the field of the structure of the inner Galaxy we have made use in this paper of the large NIR star count database obtained with the CAIN camera at the Teide Observatory together with the Besançon model of the Galaxy (Robin & Crézé 1986;Bienaymé et al 1987;Robin et al 2003) to examine the excesses in both the magnitude and the colour histograms of the data with respect to the model predictions. This study permits us on the one hand to confirm with an independent method the existence of this extra density, and allows us on the other hand to derive considerations about its structure.…”

Section: Introductionmentioning

confidence: 99%

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Stellar density distribution in the NIR on the Galactic plane at longitudes 15–27 deg. Clues for the Galactic bar?

Picaud

Cabrera-Lavers

Garzón

2003

A&A

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Abstract. Garzón et al. (1997), López-Corredoira et al. (1999) and Hammersley et al. (2000) have identified in TMGS and DENIS data a large excess of stars at l = 27• and b = 0 • which might correspond to an in-plane bar. We compared near infrared CAIN star counts and simulations from the Besançon Model of Galaxy on 15 fields between 15• and 45• in longitude and −2• and 2• in latitude. Comparisons confirm the existence of an overdensity at longitudes lower than 27• which is inhomogeneous and decreases very steeply off the Galactic plane. The observed excess in the star distribution over the predicted density is even higher than 100%. Its distance from the sun is estimated to be lower than 6 kpc. If this overdensity corresponds to the stellar population of the bar, we estimate its half-length to 3.9 ± 0.4 kpc and its angle from the Sun-center direction to 45 ± 9 degrees.

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Section: Discussionmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Stellar density distribution in the NIR on the Galactic plane at longitudes 15–27 deg. Clues for the Galactic bar?

Picaud

Cabrera-Lavers

Garzón

2003

A&A

Self Cite

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“…For the luminosity function we will adopt the model of Wainscoat et al (1992). The density distribution will be built using a truncated exponential disk (Lopez−Corredoira et al 2001) and a triaxial bar model with a power law profile. This bar model has an inclination of 20 deg with respect to the line of sight, and axis ratio: x0 y0 3 and z0 y0 0.7 (Dwek et al 1995).…”

Section: Discussionmentioning

confidence: 99%

Another bar in the Bulge

Alard

2001

A&A

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Abstract.A map of the projected density of the old stellar population of the Galactic Bulge region is reconstructed using 2MASS data. By making a combination of the H and K photometric bands, it is possible to overcome the effect of reddening, and thus penetrate the inner structure of the Galactic Bulge. The main structure in the map corresponds to the well documented peanut shaped bar which is formed by the inner parts of the Galactic disk as a result of dynamical instabilities. As suggested by numerical simulations, the projected Z profile of the bar, has an almost exponential shape. After subtracting the exponential profile associated with the bar, a large residual appear near the Galactic Center. This residual is elongated and asymmetrical, which suggest a bar structure. Thus we arrive at the conclusion that in addition to the main bar a smaller bar with a different orientation may exist in the central region of the Milky Way. This finding makes the Milky Way very similar to a large number of barred spiral Galaxies which show as well a smaller bar in their central regions.

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“…• (Weiner & Sellwood 1999;Sevenster 1999;López-Corredoira et al 2001) with a number of works giving values in the range 15…”

Section: Introductionmentioning

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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Searching for the in-plane Galactic bar and ring in DENIS

Cited by 44 publications

References 51 publications

Stellar density distribution in the NIR on the Galactic plane at longitudes 15–27 deg. Clues for the Galactic bar?

Stellar density distribution in the NIR on the Galactic plane at longitudes 15–27 deg. Clues for the Galactic bar?

Another bar in the Bulge

Gas flow models in the Milky Way embedded bars

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