Spectroscopy of the open cluster Blanco 1

Panagi, P. M.; Odell, Mark

doi:10.1051/aas:1997316

Cited by 26 publications

(55 citation statements)

References 22 publications

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“…Panagi & O'Dell (1997) found it is similar to or slighty older than that of the well-studied Pleiades cluster of 120 Myr, while other authors used an age of 100 Myr (e.g. Pillitteri et al 2003).…”

Section: Introductionmentioning

confidence: 77%

The lower mass function of the young open cluster Blanco 1: from 30 M$\mathsf{_{Jup}}$ to 3 M$\mathsf{_{\odot}}$

Moraux¹,

Bouvier²,

Stauffer

et al. 2007

A&A

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Aims. We performed a deep wide field optical survey of the young (∼ 100 − 150 Myr) open cluster Blanco 1 to study its low mass population well down into the brown dwarf regime and estimate its mass function over the whole cluster mass range. Methods. The survey covers 2.3 square degrees in the I and z-bands down to I ≃ z ≃ 24 with the CFH12K camera. Considering two different cluster ages (100 and 150 Myr), we selected cluster member candidates on the basis of their location in the (I, I − z) CMD relative to the isochrones, and estimated the contamination by foreground late-type field dwarfs using statistical arguments, infrared photometry and lowresolution optical spectroscopy. Results. We find that our survey should contain about 57% of the cluster members in the 0.03 − 0.6M ⊙ mass range, including 30-40 brown dwarfs. The candidate's radial distribution presents evidence that mass segregation has already occured in the cluster. We took it into account to estimate the cluster mass function across the stellar/substellar boundary. We find that, between 0.03M ⊙ and 0.6M ⊙ , the cluster mass distribution does not depend much on its exact age, and is well represented by a single power-law, with an index α = 0.69 ± 0.15. Over the whole mass domain, from 0.03M ⊙ to 3M ⊙ , the mass function is better fitted by a log-normal function with m 0 = 0.36 ± 0.07M ⊙ and σ = 0.58 ± 0.06. Conclusions. Comparison between the Blanco 1 mass function, other young open clusters' MF, and the galactic disc MF suggests that the IMF, from the substellar domain to the higher mass part, does not depend much on initial conditions. We discuss the implications of this result on theories developed to date to explain the origin of the mass distribution.

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Section: Introductionmentioning

confidence: 77%

The lower mass function of the young open cluster Blanco 1: from 30 M$\mathsf{_{Jup}}$ to 3 M$\mathsf{_{\odot}}$

Moraux¹,

Bouvier²,

Stauffer

et al. 2007

A&A

View full text Add to dashboard Cite

show abstract

“…In fact, Blanco 1 is a young open cluster, with an age estimated in the range 50−100 Myr (de Epstein & Epstein 1985;Westerlund et al 1988;Edvardsson et al 1995;Panagi & O'Dell 1997), a metallicity higher than the solar one ([Fe/H] ∼ +0.23, Edvardsson et al 1995) and also peculiar is its location out of the galactic plane (b = −79…”

Section: Introductionmentioning

confidence: 99%

“…In the following we will assume that the age of Blanco 1 is 100 Myr in agreement with Panagi & O'Dell (1997). The temperature scale adopted by Edvardsson et al (1995) to derive the metallicity of Blanco 1 is different from that used in studying other clusters like the Pleiades (see Boesgaard & Friel 1990).…”

Section: Introductionmentioning

confidence: 99%

“…Previous membership studies have been largely based on photometric criteria (Epstein 1968;de Epstein & Epstein 1985;Westerlund et al 1988;Panagi & O'Dell 1997). To date, the most complete published member list is due to Panagi & O'Dell (1997).…”

Section: Introductionmentioning

confidence: 99%

“…To date, the most complete published member list is due to Panagi & O'Dell (1997). This list does not include dM stars.…”

Section: Introductionmentioning

confidence: 99%

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The X-ray Luminosity Distributions of the high-metallicity open cluster Blanco 1

Pillitteri

Micela

Sciortino

et al. 2003

A&A

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Abstract. We present X-ray Luminosity Distributions (XLDs) of late-type members (dF, dG, dK, dM) of the Blanco 1 cluster, based on ROSAT-HRI data and new astrometric-photometric membership obtained from the GSC-II project. For the first time we present the XLD of dM stars of this cluster. The high metallicity of Blanco 1 allows us to investigate the role of chemical composition on the coronal emission of late-type stars. Comparison between X-ray Luminosity Distributions of Blanco 1 and Pleiades, NGC 2516 and α Per suggests a possible metallicity effect in dM stars.

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TheGaia-ESO Survey: Metallicity of the Chamaeleon I star-forming region

Spina

Randich

Palla

et al. 2014

A&A

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Context. Recent metallicity determinations in young open clusters and star-forming regions suggest that the latter may be characterized by a slightly lower metallicity than the Sun and older clusters in the solar vicinity. However, these results are based on small statistics and inhomogeneous analyses. The Gaia-ESO Survey is observing and homogeneously analyzing large samples of stars in several young clusters and star-forming regions, hence allowing us to further investigate this issue. Aims. We present a new metallicity determination of the Chamaeleon I star-forming region, based on the products distributed in the first internal release of the Gaia-ESO Survey. Methods. The 48 candidate members of Chamaeleon I have been observed with the high-resolution, spectrograph UVES. We use the surface gravity, lithium line equivalent width, and position in the Hertzsprung-Russell diagram to confirm the cluster members, and we use the iron abundance to derive the mean metallicity of the region. Results. Out of the 48 targets, we confirm 15 high probability members. Considering the metallicity measurements for nine of them, we find that the iron abundance of Chamaeleon I is slightly subsolar with a mean value [Fe/H] = −0.08 ± 0.04 dex. This result agrees with the metallicity determination of other nearby star-forming regions and suggests that the chemical pattern of the youngest stars in the solar neighborhood is indeed more metal-poor than the Sun. We argue that this evidence may be related to the chemical distribution of the Gould Belt that contains most of the nearby star-forming regions and young clusters.

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Spectroscopy of the open cluster Blanco 1

Cited by 26 publications

References 22 publications

The lower mass function of the young open cluster Blanco 1: from 30 M$\mathsf{_{Jup}}$ to 3 M$\mathsf{_{\odot}}$

The lower mass function of the young open cluster Blanco 1: from 30 M$\mathsf{_{Jup}}$ to 3 M$\mathsf{_{\odot}}$

The X-ray Luminosity Distributions of the high-metallicity open cluster Blanco 1

TheGaia-ESO Survey: Metallicity of the Chamaeleon I star-forming region

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