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Modelling the Galactic Bar Using Red Clump Giants
Astrophysics · Submitted 27 May 1996
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that almost regardless of the analytical function used to describe the 3-D stars distribution of the Galactic bar, the resulting models have the major axis inclined to the line of sight by $20-30\deg$, with axis ratios corresponding to $x_0:y_0:z_0=3.5:1.5:1$.
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The abstract, sentence by sentence
The color-magnitude diagrams of $\sim 7 \times 10^5$ stars obtained for 12 fields across the Galactic bulge with the OGLE project reveal a well-defined population of bulge red clump giants. We find that the distributions of the apparent magnitudes of the red clump stars are systematically fainter when moving towards lower galactic $l$ fields. The most plausible explanation of this distinct trend is that the Galactic bulge is a bar, whose nearest end lies at positive galactic longitude. We model this Galactic bar by fitting for all fields the observed luminosity functions in the red clump region of the color-magnitude diagram. We find that almost regardless of the analytical function used to describe the 3-D stars distribution of the Galactic bar, the resulting models have the major axis inclined to the line of sight by $20-30\deg$, with axis ratios corresponding to $x_0:y_0:z_0=3.5:1.5:1$. This puts a strong constraint on the possible range of the Galactic bar models. Gravitational microlensing can provide us with additional constrains on the structure of the Galactic bar.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The color-magnitude diagrams of $\sim 7 \times 10^5$ stars obtained for 12 fields across the Galactic bulge with the OGLE project reveal a well-defined population of bulge red clump giants. | method 0.51 | 0.61 | 0.03 | asserted 1.00 |
| s1 | We find that the distributions of the apparent magnitudes of the red clump stars are systematically fainter when moving towards lower galactic $l$ fields. | result 1.00 | 0.95 | 0.06 | asserted 1.00 |
| s2 | The most plausible explanation of this distinct trend is that the Galactic bulge is a bar, whose nearest end lies at positive galactic longitude. | interpretation 1.00 | 0.55 | 0.75 | hedged possibility 0.93 |
| s3 | We model this Galactic bar by fitting for all fields the observed luminosity functions in the red clump region of the color-magnitude diagram. | method 0.97 | 0.96 | 0.05 | asserted 0.95 |
| s4 | We find that almost regardless of the analytical function used to describe the 3-D stars distribution of the Galactic bar, the resulting models have the major axis inclined to the line of sight by $20-30\deg$, with axis ratios corresponding to $x_0:y_0:z_0=3.5:1.5:1$. | result 1.00 | 0.96 | 0.39 | asserted 1.00 |
| s5 | This puts a strong constraint on the possible range of the Galactic bar models. | interpretation 0.96 | 0.59 | 0.14 | asserted 0.99 |
| s6 | Gravitational microlensing can provide us with additional constrains on the structure of the Galactic bar. | future work 0.71 | 0.07 | 0.02 | hedged possibility 0.87 |
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The paper
Original abstract
The color-magnitude diagrams of $\sim 7 \times 10^5$ stars obtained for 12 fields across the Galactic bulge with the OGLE project reveal a well-defined population of bulge red clump giants. We find that the distributions of the apparent magnitudes of the red clump stars are systematically fainter when moving towards lower galactic $l$ fields. The most plausible explanation of this distinct trend is that the Galactic bulge is a bar, whose nearest end lies at positive galactic longitude. We model this Galactic bar by fitting for all fields the observed luminosity functions in the red clump region of the color-magnitude diagram. We find that almost regardless of the analytical function used to describe the 3-D stars distribution of the Galactic bar, the resulting models have the major axis inclined to the line of sight by $20-30\deg$, with axis ratios corresponding to $x_0:y_0:z_0=3.5:1.5:1$. This puts a strong constraint on the possible range of the Galactic bar models. Gravitational microlensing can provide us with additional constrains on the structure of the Galactic bar.
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How the literature uses it
5 arXiv papers cite this in 7 sentences
Papers citing it · 5 sentences without a confident label
Uses its method or tool 1 paper
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We follow the same type of calculation as in [ref] and all the parameters of the E2 fitting formula except the total normalization are fixed according to [ref] .
Bayesian reconstruction of the Milky Way dark matter distribution · The visible component (baryonic morphology) · 0.83
Cites it as background 1 paper
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Evidence has been emerging that each of these is subdivided into thin/thick disks of various metallicities [ref] , inner/outer halos displaying abundance gradients [ref] , and a complicated bulge plus bar structure [ref] .
Chemodynamical evidence of the HR 1614 moving group as a bar resonance · Introduction · 0.86
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