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 Are Narrow-line Seyfert 1 Galaxies Powered by Low-mass Black Holes? Subject The topic of the resource accretion, accretion disks; galaxies: active; galaxies: Seyfert Description An account of the resource Narrow-line Seyfert 1 galaxies (NLS1s) are believed to be powered by the accretion of matter onto low-mass black holes (BHs) in spiral host galaxies with BH masses M BH ? 106-108 M o. However, the broadband spectral energy distribution of the ?-ray-emitting NLS1s are found to be similar to flat-spectrum radio quasars. This challenges our current notion of NLS1s having low M BH. To resolve this tension of low M BH values in NLS1s, we fitted the observed optical spectrum of a sample of radio-loud NLS1s (RL-NLS1s), radio-quiet NLS1s (RQ-NLS1s), and radio-quiet broad-line Seyfert 1 galaxies (RQ-BLS1s) of ?500 each with the standard Shakura-Sunyaev accretion disk (AD) model. For RL-NLS1s we found a mean log() of 7.98 0.54. For RQ-NLS1s and RQ-BLS1s we found mean log() of 8.00 0.43 and 7.90 0.57, respectively. While the derived values of RQ-BLS1s are similar to their virial masses, for NLS1s the derived values are about an order of magnitude larger than their virial estimates. Our analysis thus indicates that NLS1s have M BH similar to RQ-BLS1s and their available virial M BH values are underestimated, influenced by their observed relatively small emission line widths. Considering Eddington ratio as an estimation of the accretion rate and using , we found the mean accretion rate of our RQ-NLS1s, RL-NLS1s, and RQ-BLS1s as , and , respectively. Our results therefore suggest that NLS1s have BH masses and accretion rates that are similar to BLS1s. 2019. The American Astronomical Society. All rights reserved. Creator An entity primarily responsible for making the resource Viswanath G.; Stalin C.S.; Rakshit S.; Kurian K.S.; Ujjwal K.; Gudennavar S.B.; Kartha S.S. Source A related resource from which the described resource is derived Astrophysical Journal Letters, Vol-881, No. 1 Publisher An entity responsible for making the resource available Institute of Physics Publishing Date A point or period of time associated with an event in the lifecycle of the resource 2019-01-01 Identifier An unambiguous reference to the resource within a given context <a href="https://doi.org/10.3847/2041-8213/ab365e" target="_blank" rel="noreferrer noopener">https://doi.org/10.3847/2041-8213/ab365e</a> <br /><br /><a href="https://www.scopus.com/inward/record.uri?eid=2-s2.0-85071224038&amp;doi=10.3847%2F2041-8213%2Fab365e&amp;partnerID=40&amp;md5=2ee9e3e92bbaf0221226e1dc8c52cee8" target="_blank" rel="noreferrer noopener">https://www.scopus.com/inward/record.uri?eid=2-s2.0-85071224038&amp;doi=10.3847%2f2041-8213%2fab365e&amp;partnerID=40&amp;md5=2ee9e3e92bbaf0221226e1dc8c52cee8</a> Rights Information about rights held in and over the resource All Open Access; Bronze Open Access; Green Open Access Relation A related resource ISSN: 20418205 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 Viswanath G., Department of Physics and Electronics, CHRIST (Deemed to Be University), Bengaluru, Karnataka, 560029, India; Stalin C.S., Indian Institute of Astrophysics, Block II, Koramangala, Bengaluru, Karnataka, 560034, India; Rakshit S., Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Quantum, Vesilinnantie 5, FI-20014, Finland; Kurian K.S., Indian Institute of Astrophysics, Block II, Koramangala, Bengaluru, Karnataka, 560034, India; Ujjwal K., Department of Physics and Electronics, CHRIST (Deemed to Be University), Bengaluru, Karnataka, 560029, India; Gudennavar S.B., Department of Physics and Electronics, CHRIST (Deemed to Be University), Bengaluru, Karnataka, 560029, India; Kartha S.S., Department of Physics and Electronics, CHRIST (Deemed to Be University), Bengaluru, Karnataka, 560029, India