Search for brown dwarfs in IC 1396 with Subaru HSC: interpreting the impact of environmental factors on substellar population
brown dwarfs; catalogues; Hertzsprung-Russell and colour-magnitude diagrams; methods: data analysis; stars: pre-main-sequence; techniques: photometric
Young stellar clusters are predominantly the hub of star formation and hence, ideal to perform comprehensive studies over the least explored substellar regime. Various unanswered questions like the mass distribution in brown dwarf regime and the effect of diverse cluster environment on brown dwarf formation efficiency still plague the scientific community. The nearby young cluster, IC 1396 with its feedback-driven environment, is ideal to conduct such study. In this paper, we adopt a multiwavelength approach, using deep Subaru HSC along with other data sets and machine learning techniques to identify the cluster members complete down to ? 0.03 M? in the central 22 arcmin area of IC 1396. We identify 458 cluster members including 62 brown dwarfs which are used to determine mass distribution in the region. We obtain a star-to-brown dwarf ratio of ? 6 for a stellar mass range 0.03-1 M? in the studied cluster. The brown dwarf fraction is observed to increase across the cluster as radial distance from the central OB-stars increases. This study also compiles 15 young stellar clusters to check the variation of star-to-brown dwarf ratio relative to stellar density and ultraviolet (UV) flux ranging within 4-2500 stars pc?2 and 0.7-7.3 G0, respectively. The brown dwarf fraction is observed to increase with stellar density but the results about the influence of incident UV flux are inconclusive within this range. This is the deepest study of IC 1396 as of yet and it will pave the way to understand various aspects of brown dwarfs using spectroscopic observations in future. 2024 The Author(s).
Gupta S.; Jose J.; Das S.R.; Guo Z.; Damian B.; Prakash P.; Samal M.R.
Monthly Notices of the Royal Astronomical Society, Vol-528, No. 4, pp. 5633-5648.
All Open Access; Green Open Access; Hybrid Gold Open Access
https://doi.org/10.1093/mnras/stae369 https://www.scopus.com/inward/record.uri?eid=2-s2.0-85185398687&doi=10.1093%2fmnras%2fstae369&partnerID=40&md5=491bb99a8186a70a36a05274142801c9
Gupta S., Department of Physics, Indian Institute of Science Education and Research (IISER) Tirupati, Rami Reddy Nagar, Karakambadi Road, Mangalam (PO), Tirupati, 517 507, India; Jose J., Department of Physics, Indian Institute of Science Education and Research (IISER) Tirupati, Rami Reddy Nagar, Karakambadi Road, Mangalam (PO), Tirupati, 517 507, India; Das S.R., Departamento de Astronom, Universidad de Chile, Las Condes, Santiago, 7591245, Chile; Guo Z., Instituto de Fica y Astronom, Universidad de Valparao, ave. Gran Breta, 1111, Casilla 5030, Valparao, Chile, Nleo Milenio de Formaci Planetaria (NPF), ave. Gran Breta, 1111, Casilla 5030, Valparao, Chile, Centre for Astrophysics Research, University of Hertfordshire, Hatfield, AL10 9AB, United Kingdom, Departamento de Fica, Universidad TecnicFederico Santa Mar, Avenida Espa 1680, Valparao, Chile; Damian B., Department of Physics and Electronics, Christ (Deemed to be University), Bangalore, 560029, India; Prakash P., Department of Inter Disciplinary, Indian Institute of Technology Hyderabad, Sangareddy, Telangana, Kandi, India; Samal M.R., Astronomy and Astrophysics Division, Physical Research Laboratory (PRL), Navrangpura, Gujarat, Ahmedabad, 380 009, India