A deep<i>IZ</i>survey of 1.1 deg<sup>2</sup>of the Pleiades cluster: three candidate members with

Dobbie, P. D.; Kenyon, F.; Jameson, R. F.; Hodgkin, S. T.; Pinfield, D. J.; Osborne, Samantha

doi:10.1046/j.1365-8711.2002.05650.x

Cited by 37 publications

(28 citation statements)

References 62 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A similar study in the Upper Sco association favors a turn-down in the mass function below 10 M J (Lodieu et al 2011). In the Pleiades Casewell et al (2007) reported several L/T-type candidates with masses as low as 10 M J , implying that the slope of the mass function in this mass regime agrees, within the uncertainties, with the values inferred from earlier studies at higher masses (Dobbie et al 2002;Moraux et al 2003;Lodieu et al 2007;Casewell et al 2007). Finally, Kirkpatrick et al (2012) find tantalizing hints that the number of BDs in the field continues to rise from late-T to early-Y.…”

Section: Introductionsupporting

confidence: 80%

Searching for planetary-mass T-dwarfs in the core of Serpens

Spezzi

Oliveira

Moraux

et al. 2012

A&A

View full text Add to dashboard Cite

Context. The knowledge of the present-day mass function of young clusters and the mass of their coolest substellar members is essential to clarify the brown dwarf formation mechanism, which still remains a matter of debate. Aims. We searched for isolated planetary-mass T-dwarfs in the ∼3 Myr old Serpens Core cluster. Methods. We performed a deep imaging survey of the central part of this cluster using the WIRCam camera at the CFHT. Observations were performed through the narrow-band CH 4 off and CH 4 on filters, to identify young T-dwarfs from their 1.6 μm methane absorption bands, and the broad-band JHK S filters, to better characterize the selected candidates. We complemented our WIRCam photometry with optical imaging data from MegaCam at CFHT and Suprime-Cam at the Subaru telescope and mid-infrared flux measurements from the Spitzer "core to disk" (c2d) Legacy Survey. Results. We report four faint T-dwarf candidates in the direction of the Serpens Core with CH 4 on−CH 4 off above 0.2 mag, estimated visual extinction in the range 1−9 mag and spectral type in the range T1−T5 based on their dereddened CH 4 on−CH 4 off colors. Comparisons with T-dwarf spectral models and optical to mid-infrared color-color and color-magnitude diagrams, indicate that two of our candidates (ID 1 and 2) are background contaminants (most likely heavily reddened low-redshift quasars). The properties of the other two candidates (ID 3 and 4) are consistent with them being young members of the Serpens Core cluster, although our analysis can not be considered conclusive. In particular, ID 3 may also be a foreground T-dwarf. It is detected by the Spitzer c2d survey but only flux upper limits are available above 5.8 μm and, hence, we can not assess the presence of a possible disk around this object. However, it presents some similarities with other young T-dwarf candidates (S Ori 70 in the σ Orionis cluster and CFHT_J0344+3206 in the direction of IC 348). If ID 3 and 4 belong to Serpens, they would have a mass of a few Jupiter masses and would be amongst the youngest, lowest mass objects detected in a star-forming region so far.

show abstract

Section: Introductionsupporting

confidence: 80%

Searching for planetary-mass T-dwarfs in the core of Serpens

Spezzi

Oliveira

Moraux

et al. 2012

A&A

View full text Add to dashboard Cite

show abstract

“…However, the mass spectrum remains somewhat uncertain in the low-mass and substellar regimes. Most studies conducted in Pleiades-like open clusters suggest a power law index α in the range 0.5−1.0 across the hydrogen-burning limit Bouvier et al 1998;Tej et al 2002;Dobbie et al 2002;Moraux et al 2003;Barrado y Navascués et al 2001a;Barrado y Navascués et al 2002). A comparable result is obtained for the mass function in the solar neighbourhood (Kroupa et al 1993;Reid et al 1999).…”

Section: Introductionmentioning

confidence: 74%

“…Cruz et al 2003), as companions to low-mass stars (Burgasser et al 2003;Gizis et al 2003;Close et al 2003;Bouy et al 2003), in star-forming regions (Lucas & Roche 2000;Briceño et al 2002;Luhman et al 2003), and in open clusters (Bouvier et al 1998;Zapatero Osorio et al 2000;Barrado y Navascués et al 2001a;Barrado y Navascués et al 2002;Oliveira et al 2003, and references therein). Since the discovery of the first BDs in the Pleiades (Rebolo et al 1995(Rebolo et al , 1996, numerous open clusters have been targeted in the optical and in the near-infrared to uncover their low-mass and substellar populations, including the Pleiades (Bouvier et al 1998;Tej et al 2002;Dobbie et al 2002;Moraux et al 2003), α Per (Stauffer et al 1999;Barrado y Navascués et al 2002), M 35 (Barrado y Navascués et al 2001a, IC 2391 (Barrado y Navascués et al 2001b), and NGC 2547 (Oliveira et al 2003).…”

Section: Introductionmentioning

confidence: 99%

A deep wide-field optical survey in the young open cluster Collinder 359

Lodieu

Bouvier

James

et al. 2006

A&A

View full text Add to dashboard Cite

We present the first deep, optical, wide-field imaging survey of the young open cluster Collinder 359, complemented by near-infrared follow-up observations. This study is part of a large programme aimed at examining the dependence of the mass function on environment and time. We have surveyed 1.6 square degrees in the cluster, in the I and z filters, with the CFH12K camera on the Canada-France-Hawaii 3.6-m telescope down to completeness and detection limits in both filters of 22.0 and 24.0 mag, respectively. Based on their location in the optical (I − z, I) colour-magnitude diagram, we have extracted new cluster member candidates in Collinder 359 spanning 1.3−0.03 M , assuming an age of 60 Myr and a distance of 450 pc for the cluster. We have used the 2MASS database as well as our own near-infrared photometry to examine the membership status of the optically-selected cluster candidates. Comparison of the location of the most massive members in Collinder 359 in a (B − V, V) diagram with theoretical isochrones suggests that Collinder 359 is older than α Per but younger than the Pleiades. We discuss the possible relationship between Collinder 359 and IC 4665 as both clusters harbour similar parameters, including proper motion, distance, and age.

show abstract

“…The second type of large-scale surveys also applies to the aforementioned clusters like the Pleiades [20,46], Alpha Per [4], Hyades [9,22], Praesepe [17,24,47] but also to regions with small proper motions i.e. hard to distinguish from field stars on a few year baseline.…”

Section: Wide-field Surveysmentioning

confidence: 99%

“…We have cross-correlated 12 square degrees surveyed in ZY J H K in the Pleiades by the GCS with previous optical surveys from the Isaac Newton Telescope (INT; [20]) and Canada-France-Hawaii Telescope (CFHT; [46]) to extract proper motion members from 0.6 to 0.03 M [38]. Our selection of cluster candidates has recovered a large number of published Pleiades members, in particular all the bright ones with masses greater than 0.1 M [1,19,27].…”

Section: The Pleiades Seen By the Gcsmentioning

confidence: 99%

Brown dwarfs in wide-field surveys

Lodieu

2011

EPJ Web of Conferences

View full text Add to dashboard Cite

Abstract. In this invited talk, I briefly summarise early photometric and proper motion surveys carried out in the nearest and youngest open clusters to introduce the motivation behind the Galactic Cluster component of the UKIRT Infrared Deep Sky Survey. Afterwards, I focus on the latest results that we obtained in the Upper Sco association and in the Pleiades. To finish, I show a comparison of the luminosity and mass functions obtained in the Upper Sco association, the Pleiades cluster, and Orionis from the homogeneous set of data publicly available from the Galactic Clusters Survey.

show abstract

A deepIZsurvey of 1.1 deg²of the Pleiades cluster: three candidate members with

Cited by 37 publications

References 62 publications

Searching for planetary-mass T-dwarfs in the core of Serpens

Searching for planetary-mass T-dwarfs in the core of Serpens

A deep wide-field optical survey in the young open cluster Collinder 359

Brown dwarfs in wide-field surveys

Contact Info

Product

Resources

About

A deepIZsurvey of 1.1 deg2of the Pleiades cluster: three candidate members with

Cited by 37 publications

References 62 publications

Searching for planetary-mass T-dwarfs in the core of Serpens

Searching for planetary-mass T-dwarfs in the core of Serpens

A deep wide-field optical survey in the young open cluster Collinder 359

Brown dwarfs in wide-field surveys

Contact Info

Product

Resources

About

A deepIZsurvey of 1.1 deg²of the Pleiades cluster: three candidate members with