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 Hi line analysis of Herbig Ae/Be stars using X-Shooter spectra Subject The topic of the resource case B recombination; emission-line stars; Spectroscopy Description An account of the resource Herbig Ae/Be stars are intermediate-mass pre-main sequence stars undergoing accretion through their circumstellar disk. The optical and infrared (IR) spectra of HAeBe stars show Hi emission lines belonging to Balmer, Paschen and Brackett series. We used the archival X-Shooter spectra available for 109 HAeBe stars from Vioque et al. (2018) and analysed the various Hi lines present in them. We segregated the stars into different classes based on the presence of higher-order lines in different Hi series. We discussed the dependence of the appearance of higher-order lines on the stellar parameters. We found that most massive and younger stars show all the higher-order lines in emission. The stars showing only lower-order lines have Teff&lt; 12 , 000 K and an age range of 510 Myr. We performed a case B line ratio analysis for a sub-sample of stars showing most of the Hi lines in emission. We noted that all but four stars belonging to the sub-sample show lower Hi line ratios than theoretical values, owing to the emitting medium being optically thick. The Hiline flux ratios do not depend on the stars spectral type. Further, from the line ratios of lower-order lines and Paschen higher-order lines, we note that line ratios of most HAeBe stars match with electron density value in the range of 10 9 10 11 cm - 3 . The electron temperature, however, could not be ascertained with confidence using the line ratios studied in this work. 2023, Indian Academy of Sciences. Creator An entity primarily responsible for making the resource Shridharan B.; Mathew B.; Arun R.; Cysil T.B. Source A related resource from which the described resource is derived Journal of Astrophysics and Astronomy, Vol-44, No. 2 Publisher An entity responsible for making the resource available Springer 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/10.1007/s12036-023-09952-w" target="_blank" rel="noreferrer noopener">https://doi.org/10.1007/s12036-023-09952-w</a> <br /><br /><a href="https://www.scopus.com/inward/record.uri?eid=2-s2.0-85162872808&amp;doi=10.1007%2Fs12036-023-09952-w&amp;partnerID=40&amp;md5=46ba2328b8c5eac4fbfc33730f414831" target="_blank" rel="noreferrer noopener">https://www.scopus.com/inward/record.uri?eid=2-s2.0-85162872808&amp;doi=10.1007%2fs12036-023-09952-w&amp;partnerID=40&amp;md5=46ba2328b8c5eac4fbfc33730f414831</a> Rights Information about rights held in and over the resource All Open Access; Green Open Access Relation A related resource ISSN: 2506335 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., CHRIST (Deemed to be University), Bangalore, India; Mathew B., CHRIST (Deemed to be University), Bangalore, India; Arun R., Indian Institute of Astrophysics, Bangalore, India; Cysil T.B., CHRIST (Deemed to be University), Bangalore, India