Protoplanetary disks around young stellar and substellar objects in the $${\sigma }$$ Orionis cluster

Damian, Belinda; Jose, Jessy; Biller, Beth; Paul, K. T.

doi:10.1007/s12036-023-09968-2

Cited by 6 publications

(2 citation statements)

References 60 publications

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“…Investigations on the substellar mass populations show that if substellar mass objects form as an extension of the star formation process, we shall expect an indistinguishable spatial distribution of the substellar mass population in a particular SFR (Parker & Andersen 2014;Parker & Alves de Oliveira 2023). Recent studies show that disks are ubiquitous around the substellar objects (Jayawardhana et al 2003;Luhman & Mamajek 2012;Scholz et al 2023;Damian et al 2023). Subsequent works elaborate that the BDs' disks are capable of planet formation (Testi et al 2016;Jung et al 2018).…”

Section: Clues On the Formation Of Very-low-mass Stellar And Substell...mentioning

confidence: 99%

Low-mass Stellar and Substellar Content of the Young Cluster Berkeley 59

Panwar,

C.,

Sharma

et al. 2024

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We present a multiwavelength analysis of the young star cluster Berkeley 59, based on Gaia data and deep IR observations with the 3.58 m Telescopio Nazionale Galileo and Spitzer space telescope. The mean proper motion of the cluster is found to be μ α cosδ ∼ −0.63 mas yr−1 and μ δ ∼ −1.83 mas yr−1, and the kinematic distance of the cluster, ∼1 kpc, is in agreement with previous photometric studies. The present data are the deepest available near-IR observations for the cluster so far and reach below 0.03 M ⊙. The mass function of the cluster region is calculated using the statistically cleaned color–magnitude diagram and is similar to the Salpeter value for the member stars above 0.4 M ⊙. In contrast, the slope becomes shallower (Γ ∼ 0.01 ± 0.18) in the mass range 0.04–0.4 M ⊙, comparable to other nearby clusters. The spatial distribution of young brown dwarfs (BDs) and stellar candidates shows a nonhomogeneous distribution. This suggests that the radiation feedback from massive stars may be a prominent factor contributing to the BD population in the cluster Berkeley 59. We also estimated the star-to-BD ratio for the cluster, which is found to be ∼3.6. The Kolmogorov–Smirnov test shows that the stellar and BD populations significantly differ, and stellar candidates are nearer the cluster center compared to the BDs, suggesting mass segregation in the cluster toward the substellar mass regime.

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Section: Clues On the Formation Of Very-low-mass Stellar And Substell...mentioning

confidence: 99%

Low-mass Stellar and Substellar Content of the Young Cluster Berkeley 59

Panwar,

C.,

Sharma

et al. 2024

View full text Add to dashboard Cite

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“…The studies by Haisch et al (2001), Sicilia-Aguilar et al (2006), Hernández et al (2007, Meyer et al (2007), Mamajek (2009), Ribas et al (2014Ribas et al ( , 2015, Jose et al (2016), Richert et al (2018), and Damian et al (2023 showed that disk fraction varies with age, while Yasui et al (2009Yasui et al ( , 2010Yasui et al ( , 2021 have proposed that the disk fraction is influenced by metallicity.…”

Section: Disk Fraction As a Function Of Cluster Age And Metallicitymentioning

confidence: 99%

Does Metallicity Affect the Protoplanetary Disk Fraction? Answers from the Outer Milky Way

Patra,

Jose,

Evans

2024

ApJ

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The role of metallicity in shaping protoplanetary disk evolution remains poorly comprehended. This study analyzes the disk fraction of 10 young (0.9–2.1 Myr) and low-metallicity (0.34–0.83 Z ⊙) clusters located in the outer Milky Way with Galactocentric distances between 10 and 13 kpc. Using JHK data obtained from UKIDSS, the calculated disk fraction values for low-mass stars (0.2–2 M ⊙) ranged from 42% to 7%. To enhance the statistical reliability of our analysis, eight additional low-metallicity clusters are sourced from previous studies with metallicity range 0.25–0.85 Z ⊙ along with our sample, resulting in a total of 18 regions with low metallicity. We find that low-metallicity clusters exhibit on average a 2.6 ± 0.2 times lower disk fraction compared to solar-metallicity clusters in all the age bins we have. Within the age range we can probe, our study does not find evidence of faster disk decay in subsolar-metallicity regions compared to solar-metallicity regions. Furthermore, we observe a positive correlation between cluster disk fraction and metallicity for two different age groups of 0.3–1.4 and 1.4–2.5 Myr. We emphasize that both cluster age and metallicity significantly affect the fraction of stars with evidence of inner disks.

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Testing external photoevaporation in the σ-Orionis cluster with spectroscopy and disk mass measurements

Maucó,

Manara,

Ansdell

et al. 2023

A&A

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Context. The evolution of protoplanetary disks is regulated by an interplay of several processes, either internal to the system or related to the environment. As most of the stars and planets, including our own Solar System, have formed in massive stellar clusters that contain OB-type stars, studying the effects of UV radiation on disk evolution is of paramount importance. Aims. For this work, we tested the impact of external photoevaporation on the evolution of disks in the mid-age (~3–5 Myr) σ-Orionis cluster by conducting the first combined large-scale UV to IR spectroscopic and millimeter-continuum survey of this region. Methods. We studied a sample of 50 targets located at increasing distances from the central, massive OB system σ-Ori. We combined new spectra obtained with VLT/X-shooter, used to measure mass accretion rates and stellar masses, with new and previously published ALMA measurements of disk dust and gas fluxes and masses. Results. We confirm the previously found decrease in Mdust in the inner ~0.5 pc of the cluster. This is particularly evident when considering the disks around the more massive stars (≥0.4 M⊙), where those located in the inner part (<0.5 pc) of the cluster have Mdust about an order of magnitude lower than the more distant ones. About half of the sample is located in the region of the Ṁacc versus Mdisk expected by models of external photoevaporation, namely showing shorter disk lifetimes than expected for their ages. The shorter disk lifetimes is observed for all targets with a projected separation from σ-Ori < 0.5 pc, proving that the presence of a massive stellar system affects disk evolution. Conclusions. External photoevaporation is a viable mechanism to explain the observed shorter disk lifetimes and lower Mdust in the inner ~0.5 pc of the σ-Orionis cluster, where the effects of this process are more pronounced. Follow-up observations of the low stellar mass targets are crucial to constrain disk dispersion timescales in the cluster and to confirm the dependence of the external photoevaporation process with stellar host mass. This work confirms that the effects of external photoevaporation are significant down to at least impinging radiation as low as ~104 G0.

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Protoplanetary disks around young stellar and substellar objects in the $${\sigma }$$ Orionis cluster

Cited by 6 publications

References 60 publications

Low-mass Stellar and Substellar Content of the Young Cluster Berkeley 59

Low-mass Stellar and Substellar Content of the Young Cluster Berkeley 59

Does Metallicity Affect the Protoplanetary Disk Fraction? Answers from the Outer Milky Way

Testing external photoevaporation in the σ-Orionis cluster with spectroscopy and disk mass measurements

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