Star counts redivivus. I - A new look at the galaxy at faint magnitudes

Reid, Neill; Majewski, S. R.

doi:10.1086/172695

Cited by 170 publications

(240 citation statements)

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“…We use the same model as starting point to build a theoretical CMD of field stars in the direction of NGC 1252. This model has been described in more detail by Reid & Majewski (1993) and Santiago et al (1996b). A recent application of the method to Galactic fields was carried out by Kerber et al (2001).…”

Section: Comparison With a Field Modelmentioning

confidence: 99%

Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Pavani

Bica

Dutra

et al. 2001

A&A

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Abstract. Photometry in the B and V bands is presented for the southern stellar groups NGC 1901 and NGC 1252. NGC 1901 is often described as an open cluster while NGC 1252 consists of a concentration of about 20 stars centered ≈20 north of the original New General Catalogue coordinates, and at the southwest edge of the large region previously assigned to this object in the literature. NGC 1901 has a clear main sequence and shares similarities with the Hyades. We derive a reddening value E(B −V ) = 0.04, a distance from the Sun d = 0.45 kpc (Z = −0.23 kpc) and an age 0.6 ± 0.1 Gyr. NGC 1901 is conclusively a physical system, dynamically comparable to or more evolved than the Hyades. The colour-magnitude diagram of NGC 1252 suggests a turnoff and main sequence, and a total of 12 probable members. We simulated the Galactic field colour-magnitude diagram in the same direction and found it to be a poor match to NGC 1252, suggesting that NGC 1252 is not a field fluctuation. Isochrone fitting to the probable members is consistent with E(B − V ) = 0.02, d = 0.64 kpc (Z = −0.46 kpc) and an age 3 ± 1 Gyr. NGC 1252 cannot be ruled out as a physical group with the available data. If so, evidence is found that it is not a classical open cluster, but rather an open cluster remnant.

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Section: Comparison With a Field Modelmentioning

confidence: 99%

Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Pavani

Bica

Dutra

et al. 2001

A&A

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“…This population has been explored extensively, mainly through star counts (e.g., Gilmore & Reid 1983;Reid & Majewski 1993;Buser et al 1999;Norris 1999;Siegel et al 2002). However, the thick disk scale height and local density normalization are still uncertain ( Norris 1999), with values of h thick ranging from $700 to 1500 pc and local normalizations between 2% and 15%.…”

Section: Introductionmentioning

confidence: 99%

“…The scale length of the thick disk is also uncertain, although typically scale lengths larger than the thin disk are inferred (Chen et al 2001;Larsen & Humphreys 2003). The thick disk is thought to be an older, metal-poor population (Reid & Majewski 1993;Chiba & Beers 2000). Metallicity differences, such as -element enhancement, have been explored ), but other observables, such as photometric color and chromospheric activity trends, have yet to be studied in detail.…”

Section: Introductionmentioning

confidence: 99%

Exploring the Local Milky Way: M Dwarfs as Tracers of Galactic Populations

et al. 2007

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We have assembled a spectroscopic sample of low-mass dwarfs observed as part of the Sloan Digital Sky Survey along one Galactic sight line, designed to investigate the observable properties of the thin and thick disks. This sample of $7400 K and M stars also has measured ugriz photometry, proper motions, and radial velocities. We compute UVW space-motion distributions, and investigate their structure with respect to vertical distance from the Galactic plane. We place constraints on the velocity dispersions of the thin and thick disks, using two-component Gaussian fits. We also compare these kinematic distributions to a leading Galactic model. Finally, we investigate other possible observable differences between the thin and thick disks, such as color, active fraction, and metallicity.

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“…This model works well in reproducing existing star counts at high Galactic latitude for V < 19, but predicts too many stars at fainter magnitudes (Reid and Majewski 1993). Some combination of a flatter spheroid and/or a shorter scale length is indicated.…”

Section: Halomentioning

confidence: 63%

A Survey of Surveys

Kent

1996

Symp. - Int. Astron. Union

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Abstract. A new era for the field of Galactic structure is about to be opened with the advent of wide-area digital sky surveys. In this article, I will review the status and prospects for research for 3 new ground-based surveys: the Sloan Digital Sky Survey (SDSS), the Deep Near-Infrared Survey of the Southern Sky (DENIS) and the Two Micron All Sky Survey (2MASS). These surveys will permit detailed studies of Galactic structure and stellar populations in the Galaxy with unprecedented detail. Extracting the information, however, will be challenging.

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Star counts redivivus. I - A new look at the galaxy at faint magnitudes

Cited by 170 publications

References 0 publications

Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Exploring the Local Milky Way: M Dwarfs as Tracers of Galactic Populations

A Survey of Surveys

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