FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2093974519> ?p ?o ?g. }

• W2093974519 endingPage "1811" @default.
• W2093974519 startingPage "1793" @default.
• W2093974519 abstract "We present the results of a survey of the low-mass star and brown dwarf population of the 25 Orionis group. Using optical photometry from the CIDA (Centro de Investigaciones de Astronomía ‘Francisco J. Duarte’, Mérida, Venezuela) Deep Survey of Orion, near-IR photometry from the Visible and Infrared Survey Telescope for Astronomy and low-resolution spectroscopy obtained with Hectospec at the MMT telescope, we selected 1246 photometric candidates to low-mass stars and brown dwarfs with estimated masses within 0.02 ≲ M/M⊙ ≲ 0.8 and spectroscopically confirmed a sample of 77 low-mass stars as new members of the cluster with a mean age of ∼7 Myr. We have obtained a system initial mass function of the group that can be well described by either a Kroupa power-law function with indices α3 = −1.73 ± 0.31 and α2 = 0.68 ± 0.41 in the mass ranges 0.03 ≤ M/M⊙ ≤ 0.08 and 0.08 ≤ M/M⊙ ≤ 0.5, respectively, or a Scalo lognormal function with coefficients |$m_{rm c}=0.21^{+0.02}_{-0.02}$| and σ = 0.36 ± 0.03 in the mass range 0.03 ≤ M/M⊙ ≤ 0.8. From the analysis of the spatial distribution of this numerous candidate sample, we have confirmed the east–west elongation of the 25 Orionis group observed in previous works, and rule out a possible southern extension of the group. We find that the spatial distributions of low-mass stars and brown dwarfs in 25 Orionis are statistically indistinguishable. Finally, we found that the fraction of brown dwarfs showing IR excesses is higher than for low-mass stars, supporting the scenario in which the evolution of circumstellar discs around the least massive objects could be more prolonged." @default.
• W2093974519 created "2016-06-24" @default.
• W2093974519 creator A5002607342 @default.
• W2093974519 creator A5029976640 @default.
• W2093974519 creator A5041053065 @default.
• W2093974519 creator A5042101566 @default.
• W2093974519 creator A5049690883 @default.
• W2093974519 creator A5053918712 @default.
• W2093974519 creator A5069072777 @default.
• W2093974519 creator A5075661751 @default.
• W2093974519 creator A5088057202 @default.
• W2093974519 date "2014-09-01" @default.
• W2093974519 modified "2023-09-23" @default.
• W2093974519 title "The low-mass star and sub-stellar populations of the 25 Orionis group" @default.
• W2093974519 cites W1575766262 @default.
• W2093974519 cites W1965814985 @default.
• W2093974519 cites W1970404523 @default.
• W2093974519 cites W1970660289 @default.
• W2093974519 cites W1975762335 @default.
• W2093974519 cites W1975889887 @default.
• W2093974519 cites W1977043243 @default.
• W2093974519 cites W1992204357 @default.
• W2093974519 cites W1993244509 @default.
• W2093974519 cites W1995779538 @default.
• W2093974519 cites W1996501974 @default.
• W2093974519 cites W1997255077 @default.
• W2093974519 cites W2000949154 @default.
• W2093974519 cites W2009868804 @default.
• W2093974519 cites W2013081905 @default.
• W2093974519 cites W2022429968 @default.
• W2093974519 cites W2024047931 @default.
• W2093974519 cites W2024913339 @default.
• W2093974519 cites W2030154533 @default.
• W2093974519 cites W2030554090 @default.
• W2093974519 cites W2033504756 @default.
• W2093974519 cites W2047272174 @default.
• W2093974519 cites W2051156670 @default.
• W2093974519 cites W2052937506 @default.
• W2093974519 cites W2056887900 @default.
• W2093974519 cites W2062610118 @default.
• W2093974519 cites W2063090834 @default.
• W2093974519 cites W2068121261 @default.
• W2093974519 cites W2070602613 @default.
• W2093974519 cites W2078129074 @default.
• W2093974519 cites W2078854057 @default.
• W2093974519 cites W2082215603 @default.
• W2093974519 cites W2091777812 @default.
• W2093974519 cites W2092380306 @default.
• W2093974519 cites W2094650116 @default.
• W2093974519 cites W2100833883 @default.
• W2093974519 cites W2102049225 @default.
• W2093974519 cites W2107028611 @default.
• W2093974519 cites W2110567652 @default.
• W2093974519 cites W2111817932 @default.
• W2093974519 cites W2112937078 @default.
• W2093974519 cites W2115884632 @default.
• W2093974519 cites W2116904425 @default.
• W2093974519 cites W2119621846 @default.
• W2093974519 cites W2120684453 @default.
• W2093974519 cites W2126513432 @default.
• W2093974519 cites W2129078510 @default.
• W2093974519 cites W2129760210 @default.
• W2093974519 cites W2140930823 @default.
• W2093974519 cites W2142220522 @default.
• W2093974519 cites W2142755350 @default.
• W2093974519 cites W2167635287 @default.
• W2093974519 cites W2171238799 @default.
• W2093974519 cites W2953307733 @default.
• W2093974519 cites W3023536260 @default.
• W2093974519 cites W3098231028 @default.
• W2093974519 cites W3098484406 @default.
• W2093974519 cites W3099219513 @default.
• W2093974519 cites W3099488042 @default.
• W2093974519 cites W3099758390 @default.
• W2093974519 cites W3100021782 @default.
• W2093974519 cites W3100024326 @default.
• W2093974519 cites W3100597667 @default.
• W2093974519 cites W3102091167 @default.
• W2093974519 cites W3102169206 @default.
• W2093974519 cites W3103012355 @default.
• W2093974519 cites W3103063951 @default.
• W2093974519 cites W3103458148 @default.
• W2093974519 cites W3103795556 @default.
• W2093974519 cites W3103855903 @default.
• W2093974519 cites W3104385902 @default.
• W2093974519 cites W3105870319 @default.
• W2093974519 cites W3105995887 @default.
• W2093974519 cites W3157917098 @default.
• W2093974519 cites W1975218600 @default.
• W2093974519 doi "https://doi.org/10.1093/mnras/stu1553" @default.
• W2093974519 hasPublicationYear "2014" @default.
• W2093974519 type Work @default.
• W2093974519 sameAs 2093974519 @default.
• W2093974519 citedByCount "24" @default.
• W2093974519 countsByYear W20939745192015 @default.
• W2093974519 countsByYear W20939745192016 @default.
• W2093974519 countsByYear W20939745192017 @default.
• W2093974519 countsByYear W20939745192018 @default.

• next