Choi, YunyiFu, YumingIm, MyungshinWu, Xue BingOnken, Christopher A.Wolf, ChristianChang, Seo WonChoi, HyeonhoJeong, MankeunKim, YongjungLim, GuPang, YuxuanKim, TaewanSohn, JubeeKim, DohyeongKim, Ji HoonKo, EunheePaek, Gregory S.H.Jung, Sungho2025-12-162025-12-160067-0049WOS:001591385000001ORCID:/0000-0002-4569-016X/work/196077493https://hdl.handle.net/1885/733795061We present the second catalog of bright quasars from the All-sky BRIght, Complete Quasar Survey (AllBRICQS), focusing on spectroscopically observed quasars in the Northern Hemisphere with Galactic latitude |b| > 10 degrees. This catalog includes their spectral data, redshifts, and luminosities. AllBRICQS aims to identify the last remaining optically bright quasars using data from the Wide-field Infrared Survey Explorer and Gaia all-sky survey Data Release 3 (DR3). AllBRICQS searches for quasars that are brighter than B-P = 16.5 or R-P = 16 mag in Gaia DR3, based on simple selection criteria. Here, we report 62 new AllBRICQS quasars spanning various types, which include typical broad emission line quasars and the most luminous iron low-ionization broad absorption line quasars discovered to date. Spectroscopic observations were conducted using the Long-Slit Spectrograph on the 1.8 m telescope at Bohyunsan Optical Astronomy Observatory, the Yunnan Faint Object Spectrograph and Camera on the 2.4 m telescope at Lijiang Observatory, and the Beijing Faint Object Spectrograph and Camera on the 2.16 m telescope at Xinglong Observatory. We applied flux calibration using Zwicky Transient Facility broadband photometry to correct for attenuation due to intermittent thin clouds during the observations. Redshifts were determined using inverse-variance weighted cross-correlation methods. Our targets span the bolometric luminosity range of 44.9 < log (L-bol/erg s(-1)) < 48.0 at redshifts between 0.09 and 2.48. These confirmed AllBRICQS quasars provide a valuable resource for future research into quasar evolution, black holes, their environments, and their host galaxies across multiple wavelengths.This work was supported by the National Research Foundation of Korea (NRF) grant No. 2021M3F7A1084525, funded by the Korean government (MSIT). We also made use of data obtained at the Bohyunsan Optical Astronomy Observatory, which is operated by the Korea Astronomy and Space Science Institute.We acknowledge the support of the staff of the Xinglong 2.16 m telescope. This work was partially supported by the National Astronomical Observatories, Chinese Academy of Sciences. We also acknowledge the support of the staff of the Lijiang 2.4 m telescope. Funding for the Lijiang telescope has been provided by the Chinese Academy of Sciences and the People’s Government of Yunnan Province.This work has made use of data from the European Space Agency (ESA) mission Gaia,16 16 https://www.cosmos.esa.int/gaia processed by the Gaia Data Processing and Analysis Consortium (DPAC).17 17 https://www.cosmos.esa.int/web/gaia/dpac/consortium Funding for DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement.This publication also makes use of data products from WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration (NASA).We additionally used data obtained with the Samuel Oschin 48 inch and the 60 inch telescopes at Palomar Observatory as part of the ZTF project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and by a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington (UW), Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratory. Operations are conducted by Caltech Optical Observatories, IPAC, and UW.Y.C., M.I., S.W.C., H.C., M.J., and J.H.K. acknowledge support from NRF grant No. 2021M3F7A1084525. S.W.C. also acknowledges support from the Basic Science Research Program through the NRF, funded by the Ministry of Education (grant No. RS-2023-00245013). H.C. acknowledges support from NRF grant No. RS-2025-00573214 funded by the Korean government (MSIT). J.H.K. also acknowledges support from NRF grant No. 2020R1A2C3011091 and from the Institute of Information & Communications Technology Planning & Evaluation (IITP) grant No. RS-2021-II212068, funded by the Korean government (MSIT). G.L. acknowledges support from the Basic Science Research Program through the NRF, funded by MSIT (grant No. 2022R1A6A3A01085930). Y.K. was supported by NRF grant No. 2021R1C1C2091550, funded by the Korean government (MSIT). G.S.H.P. acknowledges support from the Pan-STARRS project, which is operated by the Institute for Astronomy of the University of Hawaii and supported by NASA’s Near-Earth Object Observation Program under grants 80NSSC18K0971, NNX14AM74G, NNX12AR65G, NNX13AQ47G, NNX08AR22G, and 80NSSC21K1572, as well as by the State of Hawaii. T.K. and J.S. are supported by the NRF grant funded by the Korean government (MSIT) (grant No. RS-2023-00210597). D.K. acknowledges support from NRF grant No. 2021R1C1C1013580, funded by the Korean government (MSIT).19en© 2025. The Author(s).Bolometric luminosityCatalogData releaseDust-obscured quasarsEddington ratiosFinding quasarsOptical snuqsoSpectrographSpectroscopic identificationsSurvey 1st data202510.3847/1538-4365/adf8ed105018476861