2012A&A...545A.105S


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.20CEST06:16:13

2012A&A...545A.105S - Astronomy and Astrophysics, volume 545A, 105-105 (2012/9-1)

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

SPEZZI L., ALVES DE OLIVEIRA C., MORAUX E., BOUVIER J., WINSTON E., HUDELOT P., BOUY H. and CUILLANDRE J.-C.

Abstract (from CDS):

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. We searched for isolated planetary-mass T-dwarfs in the ∼3 Myr old Serpens Core cluster. 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 CH4off and CH4on filters, to identify young T-dwarfs from their 1.6 µm methane absorption bands, and the broad-band JHKS 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. We report four faint T-dwarf candidates in the direction of the Serpens Core with CH4on-CH4off above 0.2mag, estimated visual extinction in the range 1-9 mag and spectral type in the range T1-T5 based on their dereddened CH4on-CH4off 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 5.8µm 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.

Abstract Copyright:

Journal keyword(s): stars: formation - brown dwarfs - ISM: clouds - ISM: individual objects: Serpens Core - stars: low-mass

CDS comments: CFHT J0344+3206 is [BMB2009] IC348 CH4 2 in SIMBAD.

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1268 1
2 IC 348 OpC 03 44 34 +32 09.8           ~ 1257 1
3 [BMB2009] IC348 CH4 2 BD? 03 44 49.52 +32 06 35.4           ~ 4 0
4 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 3094 0
5 [BZR99] S Ori 70 BD* 05 38 10.10 -02 36 26.0           T6-7 46 0
6 NAME sigma Orionis Cluster MGr 05 38 42 -02 36.0           ~ 502 0
7 NAME Upper Sco Association As* 16 12 -23.4           ~ 1105 1
8 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 975 2
9 SSTc2d J182956.6+011836 BD? 18 29 56.580 +01 18 35.93           ~ 1 0
10 SSTc2d J182957.6+011941 BD? 18 29 57.640 +01 19 40.61           ~ 1 0
11 SSTc2d J183027.9+011452 BD? 18 30 27.890 +01 14 52.22           ~ 1 0
12 SSTc2d J183037.2+011837 BD? 18 30 37.240 +01 18 37.68           ~ 1 0

    Equat.    Gal    SGal    Ecl

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