No substellar objects at the center of the Lupus 3 star-forming cloud

Comerón, F.

doi:10.1051/0004-6361/201116523

Cited by 10 publications

(7 citation statements)

References 67 publications

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“…The results of Scholz et al (2012) indicate that there may be as few as one 5-15 M Jup object for every 20-50 stars in the young (∼ 1 Myr) association NGC 1333, in strong contradiction with other results mentioned above. Similar but less constraining results have been obtained by Muzic et al (2015) for the ∼ 2 Myr-old Chamaeleon I region, and by Comerón (2011) and Muzic et al (2015) for the ∼ 1 Myr-old Lupus 3 region. Results by Marsh et al (2010) yielded estimates of planetary-mass to main-sequence population ratios in the ∼ 1 Myr ρ Oph cloud core region that are more in line with our findings for TWA (see Figure 15).…”

Section: The Space Density Of Isolated Planetary-mass Objects In Tw Hyasupporting

confidence: 83%

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

Gagné

Faherty

Mamajek

et al. 2017

ApJS

102

106

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A determination of the initial mass function (IMF) of the current, incomplete census of the 10 Myrold TW Hya association (TWA) is presented. This census is built from a literature compilation supplemented with new spectra and 17 new radial velocities from on-going membership surveys, as well as a re-analysis of Hipparcos data that confirmed HR 4334 (A2 Vn) as a member. Though the dominant uncertainty in the IMF remains census incompleteness, a detailed statistical treatment is carried out to make the IMF determination independent of binning, while accounting for small number statistics. The currently known high-likelihood members are fitted by a log-normal distribution with a central mass of 0.21−0.06 M and a characteristic width of 0.8 +0.2 −0.1 dex in the 12 M Jup -2 M range, whereas a Salpeter power law with α = 2.2 +1.1 −0.5 best describes the IMF slope in the 0.1-2 M range. This characteristic width is higher than other young associations, which may be due to incompleteness in the current census of low-mass TWA stars. A tentative overpopulation of isolated planetary-mass members similar to 2MASS J11472421-2040204 and 2MASS J11193254-1137466 is identified: this indicates that there might be as many as 10 +13 −5 similar members of TWA with hot-start modeldependent masses estimated at ∼ 5-7 M Jup , most of which would be too faint to be detected in 2MASS . Our new radial velocity measurements corroborate the membership of 2MASS J11472421-2040204, and secure TWA 28 (M8.5 γ), TWA 29 (M9.5 γ) and TWA 33 (M4.5 e) as members. The discovery of 2MASS J09553336-0208403, a young L7-type interloper unrelated to TWA, is also presented.

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Section: The Space Density Of Isolated Planetary-mass Objects In Tw Hyasupporting

confidence: 83%

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

Gagné

Faherty

Mamajek

et al. 2017

ApJS

102

106

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“…Furthermore, in Lupus 3, we find evidence for a turn-down of the IMF in the substellar regime. This cluster seems to produce fewer BDs than other clusters we have studied (Mužić et al 2015;Comerón 2011).…”

Section: Introductionmentioning

confidence: 59%

The low-mass content of the massive young star cluster RCW 38

Mužić

Schödel

Scholz

et al. 2017

Monthly Notices of the Royal Astronomical Society

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RCW 38 is a deeply embedded young (∼1 Myr), massive star cluster located at a distance of 1.7 kpc. Twice as dense as the Orion Nebula Cluster, orders of magnitude denser than other nearby star forming regions, and rich in massive stars, RCW 38 is an ideal place to look for potential differences in brown dwarf formation efficiency as a function of environment. We present deep, high resolution adaptive optics data of the central ∼ 0.5 × 0.5 pc 2 obtained with NACO at the Very Large Telescope. Through comparison with evolutionary models we determine masses and extinction for ∼ 480 candidate members, and derive the first Initial Mass Function (IMF) of the cluster extending into the substellar regime. Representing the IMF as a set of power laws in the form dN/dM ∝ M −α , we derive the slope α = 1.60 ± 0.13 for the mass range 0.5 -20 M ⊙ which is shallower than the Salpeter slope, but in agreement with results in several other young massive clusters. At the low-mass side, we find α = 0.71 ± 0.11 for masses between 0.02 and 0.5 M ⊙ , or α = 0.81 ± 0.08 for masses between 0.02 and 1 M ⊙ . Our result is in agreement with the values found in other young star-forming regions, revealing no evidence that a combination of high stellar densities and the presence of numerous massive stars affect the formation efficiency of brown dwarfs and very-low mass stars. We estimate that the Milky Way galaxy contains between 25 and 100 billion brown dwarfs (with masses > 0.03 M ⊙ ).

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“…Because the sample included candidate BD's, a few objects included in the observed sample have turned out not to be stellar or sub-stellar objects with disks, including four found to be extragalactic and one that may be at an earlier evolutionary state with a substantial envelope or extragalactic (ChaJ11080397-7730382). The four extragalactic objects include 2MASSJ16080175-3912316 and IRACJ16084679-3902074 from the study by Allen et al (2007) and found to be extragalactic by Comerón, Spezzi & López Martí (2009) and Comerón (2011). The source 2MASSJ1129140-7546256 was found by Luhman & Muench (2008) to exhibit emission lines characteristic of a galaxy.…”

Section: The Samplementioning

confidence: 92%

AHERSCHELSURVEY OF COLD DUST IN DISKS AROUND BROWN DWARFS AND LOW-MASS STARS

Harvey

Henning

Liu

et al. 2012

ApJ

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We report the complete photometric results from our Herschel study which is the first comprehensive program to search for far-infrared emission from cold dust around young brown dwarfs. We surveyed 50 fields containing 51 known or suspected brown dwarfs and very low mass stars that have evidence of circumstellar disks based on Spitzer photometry and/or spectroscopy. The objects with known spectral types range from M3 to M9.5. Four of the candidates were subsequently identified as extragalactic objects. Of the remaining 47 we have successfully detected 36 at 70µm and 14 at 160µm with S/N greater than 3, as well as several additional possible detections with low S/N. The objects exhibit a range of [24]-[70] micron colors suggesting a range in mass and/or structure of the outer disk. We present modeling of the spectral energy distributions of the sample and discuss trends visible in the data. Using two Monte Carlo radiative transfer codes we investigate disk masses and geometry. We find a very wide -2 -range in modeled total disk masses from less than 10 −6 M ⊙ up to 10 −3 M ⊙ with a median disk mass of order 3 × 10 −5 M ⊙ , suggesting that the median ratio of disk mass to central object mass may be lower than for T Tauri stars. The disk scale heights and flaring angles, however, cover a range consistent with those seen around T Tauri stars. The host clouds in which the young brown dwarfs and low-mass stars are located span a range in estimated age from ∼1-3 Myr to ∼10 Myr and represent a variety of star-forming environments. No obvious dependence on cloud location or age is seen in the disk properties, though the statistical significance of this conclusion is not strong.

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No substellar objects at the center of the Lupus 3 star-forming cloud

Cited by 10 publications

References 67 publications

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

The low-mass content of the massive young star cluster RCW 38

AHERSCHELSURVEY OF COLD DUST IN DISKS AROUND BROWN DWARFS AND LOW-MASS STARS

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