Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Articles Article Faculty Publications -Articles Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Disentangling the two sub-populations of early Herbig Be stars using VLT/X-shooter spectra Subject The topic of the resource Circumstellar matter; Methods: data analysis; Stars: emission-line, Be; Techniques: spectroscopic Description An account of the resource Context. Early Herbig Be (HBe) stars are massive, young stars accreting through the boundary layer mechanism. However, given the rapid (&lt;2 Myr) evolution of early Herbig stars to the main-sequence phase, studying the evolution of the circumstellar medium around these stars can be a cumbersome exercise. Aims. In this work, we study the sample of early (B0-B5) HBe stars using the correlation between H? emission strength and near-infrared excess, complemented by the analysis of various emission features in the X-shooter spectra. Methods. We segregate the sample of 37 early HBe stars based on the median values of H? equivalent width (EW) and near-infrared index (n(J-H)) distributions. The stars with |H? EW| &gt; 50and n(J-H) &gt; -2 are classified as intense HBe stars and stars with |H? EW| &lt; 50and n(J-H) &lt; -2 as weak HBe stars. Using the VLT/X-shooter spectra of five intense and eight weak HBe stars, we visually checked for the differences in intensity and profiles of various HI and metallic emission lines commonly observed in Herbig stars. Results. We propose that the intense HBe stars possess an inner disk close to the star (as apparent from the high near-infrared excess) and an active circumstellar environment (as seen from the high H? EW value and presence of emission lines belonging to FeII, CaII, OI, and [OI]). However, for weak HBe stars, the inner disk has cleared, and the circumstellar environment appears more evolved than for intense HBe stars. Furthermore, we compiled a sample of ~58 000 emission-line stars published in Gaia DR3 to identify more intense HBe candidates. Further spectroscopic studies of these candidates will help us to understand the evolution of the inner (approximately a few au) disk in early HBe stars. The Authors 2023. Creator An entity primarily responsible for making the resource Shridharan B.; Mathew B.; Arun R.; Cysil T.B.; Subramaniam A.; Manoj P.; Maheswar G.; Sudheesh T.P. Source A related resource from which the described resource is derived Astronomy and Astrophysics, Vol-679 Publisher An entity responsible for making the resource available EDP Sciences Date A point or period of time associated with an event in the lifecycle of the resource 2023-01-01 Identifier An unambiguous reference to the resource within a given context <a href="https://doi.org/10.1051/0004-6361/202346811" target="_blank" rel="noreferrer noopener">https://doi.org/10.1051/0004-6361/202346811</a> <br /><br /><a href="https://www.scopus.com/inward/record.uri?eid=2-s2.0-85178195856&amp;doi=10.1051%2F0004-6361%2F202346811&amp;partnerID=40&amp;md5=ebf87ad4364622c6de17e09e330b438c" target="_blank" rel="noreferrer noopener">https://www.scopus.com/inward/record.uri?eid=2-s2.0-85178195856&amp;doi=10.1051%2f0004-6361%2f202346811&amp;partnerID=40&amp;md5=ebf87ad4364622c6de17e09e330b438c</a> Rights Information about rights held in and over the resource All Open Access; Green Open Access; Hybrid Gold Open Access Relation A related resource ISSN: 46361; CODEN: AAEJA Format The file format, physical medium, or dimensions of the resource Online Language A language of the resource English Type The nature or genre of the resource Article Coverage The spatial or temporal topic of the resource, the spatial applicability of the resource, or the jurisdiction under which the resource is relevant Shridharan B., Department of Physics and Electronics, Christ (Deemed to Be University), Bangalore, 560029, India; Mathew B., Department of Physics and Electronics, Christ (Deemed to Be University), Bangalore, 560029, India; Arun R., Indian Institute of Astrophysics, Sarjapur Road, Koramangala, Bangalore, 560034, India; Cysil T.B., Department of Physics and Electronics, Christ (Deemed to Be University), Bangalore, 560029, India; Subramaniam A., Indian Institute of Astrophysics, Sarjapur Road, Koramangala, Bangalore, 560034, India; Manoj P., Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai, 400005, India; Maheswar G., Indian Institute of Astrophysics, Sarjapur Road, Koramangala, Bangalore, 560034, India; Sudheesh T.P., Department of Physics and Electronics, Christ (Deemed to Be University), Bangalore, 560029, India