NGC 2401: a template of the young population of the Norma–Cygnus arm in the Third Galactic Quadrant

Baume, G.; Moitinho, A.; Vazquez, R. A.; Solivella, G. R.; Carraro, G.; Villanova, S.

doi:10.1111/j.1365-2966.2006.09985.x

Cited by 11 publications

(41 citation statements)

References 32 publications

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“…The CMDs in Figure 1 sample objects that are many magnitudes fainter than those studied by Baume et al (2006), and a rich population of faint cPMS stars is detected (see below). The GMOS CMD of objects in Regions 1, 2, and 3 is compared with the CMD of sources in the same area but based on the Baume et al (2006) photometry in Figure 3.…”

Section: A Deep Color-magnitude Diagram Of Ngc 2401mentioning

confidence: 99%

“…The luminosity function (LF) of the center of NGC 2401 in K was matched by a model that assumes a Chabrier (2001) MF. Baume et al (2006) also concluded that stars more massive than solar in NGC 2401 follow a solar neighborhood-like MF. In the present study, deep g 0 and i 0 images obtained with the Gemini Multiobject Spectrograph (GMOS) on Gemini South are used to examine the photometric properties and spatial distributions of MS and PMS objects in NGC 2401.…”

Section: Introductionmentioning

confidence: 99%

“…It has been the subject of four recent photometric studies, and the ages, distances, and reddenings obtained in these are summarized in Table 1. Sujatha et al (2004), Baume et al (2006), and Hasegawa et al (2008) estimate the age of NGC 2401 from the main sequence turn-off (MSTO), while Davidge (2014) measure an age using the faintest MS stars, which define the MS cut-off (MSCO). The dispersion in the ages found from these studies is almost certainly linked to the problematic nature of distinguishing between cluster and noncluster members in the NGC 2401 CMD.…”

Section: Introductionmentioning

confidence: 99%

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The Distribution of Main Sequence and Premain Sequence Stars in the Young Anticenter Cluster NGC 2401

Davidge¹

2015

Publications of the Astronomical Society of the Pacific

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ABSTRACT. Images obtained with the Gemini Multiobject Spectrograph on Gemini South are used to examine the photometric properties and spatial distributions of main sequence (MS) and premain sequence (PMS) objects in the star cluster NGC 2401. The data sample several magnitudes fainter than previous studies and a large population of candidate PMS (cPMS) stars are identified. The cPMS stars are traced out to 2.4′ from the cluster center and have a flatter spatial distribution than the brightest MS stars near the cluster center. The luminosity function of all MS and candidate PMS stars can be matched by a model that assumes a solar neighborhood mass function, suggesting that NGC 2401 has not yet shed significant numbers of members with masses ≥0:5 M ⊙ . The frequency of wide binaries among the MS stars is ∼3× higher than among the cPMS stars. It is argued that the difference in the spatial distributions of MS and PMS objects is not the consequence of secular dynamical evolution or structural evolution driven by near-catastrophic mass loss. Rather, it is suggested that the different spatial distributions of these objects is the fossil imprint of primordial subclustering that arises naturally if massive stars form preferentially in the highest density central regions of a protocluster.

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Section: A Deep Color-magnitude Diagram Of Ngc 2401mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Distribution of Main Sequence and Premain Sequence Stars in the Young Anticenter Cluster NGC 2401

Davidge¹

2015

Publications of the Astronomical Society of the Pacific

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“…Baume et al 2004Baume et al , 2006Baume et al , 2009 Individual positions of all stars down to V = 14 were simultaneously examined in all the diagrams. At fainter magnitudes, UCAC3 does not provide reliable solutions.…”

Section: Optical Photometric Diagramsmentioning

confidence: 99%

The Ara OB1a association

Baume

Carraro²,

Comerón³

et al. 2011

A&A

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Context. The Ara OB1a association is a nearby complex in the fourth Galactic quadrant where a number of young/embedded star clusters are projected close to more evolved, intermediate age clusters. It is also rich in interstellar matter, and contains evidence of the interplay between massive stars and their surrounding medium, such as the rim HII region NGC 6188. Aims. We provide robust estimates of the fundamental parameters (age and distance) of the two most prominent stellar clusters, NGC 6167 and NGC 6193, that may be used as a basis for studing the star formation history of the region. Methods. The study is based on a photometric optical survey (UBVIH α ) of NGC 6167 and NGC 6193 and their nearby field, complemented with data from 2MASS-VVV, UCAC3, and IRAC-Spitzer in this region. Results. We produce a uniform photometric catalogue and estimate more robustly the fundamental parameters of NGC 6167 and NGC 6193, in addition to the IRAS 16375-4854 source. As a consequence, all of them are located at approximately the same distance from the Sun in the Sagittarius-Carina Galactic arm. However, the ages we estimate differ widely: NGC 6167 is found to be an intermediate-age cluster (20-30 Myr), NGC 6193 a very young one (1-5 Myr) with PMS, H α emitters and class II objects, and the IRAS 16375-4854 source is the youngest of the three containing several YSOs. Conclusions. These results support a picture in which Ara OB1a is a region where star formation has proceeded for several tens of Myr until the present. The difference in the ages of the different stellar groups can be interpreted as a consequence of a triggered star formation process. In the specific case of NGC 6193, we find evidence of possible non-coeval star formation.

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“…These results rely not only on the fundamental parameters derived for the clusters themselves, but also on careful analysis of the characteristics of the field population. From the sample described in Paper I, only NGC 2425, NGC 2635 (Moitinho et al 2006a, Paper II of this series), NGC 2588 (Baume et al 2004) and NGC 2401 (Baume et al 2006) have been the subject of publications dedicated to their detailed photometric analysis and derivation of main physical parameters. In this paper we present a detailed analysis of the fields of four open candidate cluster pairs.…”

Section: Introductionmentioning

confidence: 99%

Open clusters in the Third Galactic Quadrant III. Alleged binary clusters

Vazquez

Moitinho

Carraro³

et al. 2010

A&A

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Aims. We aim to determine accurate distances and ages of eight open clusters in order to: (1) assess their possible binarity (2) provide probes to trace the structure of the Third Galactic Quadrant. Methods. Cluster reddenings, distances, ages and metallicities are derived from ZAMS and isochrone fits in UBVRI photometric diagrams. Field contamination is reduced by restricting analysis to stars within the cluster limits derived from star counts. Further membership control is done by requiring that stars have consistent positions in several diagrams and by using published spectral types. Results. The derived distances, ages and metallicities have shown that none of the analysed clusters compose binary/double systems. Of the four candidate pairs, only NGC 2383/NGC 2384 are close to each other, but have different metallicities and ages. Ruprecht 72 and Ruprecht 158 are not clusters but fluctuations of the field stellar density. Haffner 18 is found to be the superposition of two stellar groups at different distances: Haffner 18(1) at 4.5 kpc and Haffner 18(2) between 9.5 and 11.4 kpc from the Sun. The derived distances and ages have been used to situate the clusters in the Galactic context. In particular, young stellar groups trace spiral structure at large Galactocentric radii. At least two clusters formed during the last few 10 8 yr in an interstellar medium with less than solar abundances. Conclusions. In contrast with the LMC, double clusters are apparently rare, or even non existent, in the undisturbed environment of the Third Galactic Quadrant. This leaves open the question of whether binary clusters form more easily toward denser and more violent regions of the Milky Way such as the inner Galaxy.

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NGC 2401: a template of the young population of the Norma–Cygnus arm in the Third Galactic Quadrant

Cited by 11 publications

References 32 publications

The Distribution of Main Sequence and Premain Sequence Stars in the Young Anticenter Cluster NGC 2401

The Distribution of Main Sequence and Premain Sequence Stars in the Young Anticenter Cluster NGC 2401

The Ara OB1a association

Open clusters in the Third Galactic Quadrant III. Alleged binary clusters

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