[{"publication_status":"published","author":[{"full_name":"Cheng, Sihao","last_name":"Cheng","first_name":"Sihao"},{"last_name":"Schlaufman","first_name":"Kevin C.","full_name":"Schlaufman, Kevin C."},{"full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","orcid":"0000-0002-4770-5388","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"}],"department":[{"_id":"IlCa"}],"external_id":{"arxiv":["2408.03985"],"isi":["001514518100001"]},"date_created":"2025-07-06T22:01:22Z","status":"public","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"month":"07","type":"journal_article","file":[{"date_created":"2025-07-08T06:40:54Z","date_updated":"2025-07-08T06:40:54Z","file_name":"2025_AstronomicalJour_Cheng.pdf","relation":"main_file","access_level":"open_access","content_type":"application/pdf","file_size":931173,"success":1,"file_id":"19975","checksum":"144b0e46aa3dff0cdf8c6ee7d4fe2fe4","creator":"dernst"}],"arxiv":1,"isi":1,"OA_place":"publisher","title":"A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars","citation":{"ista":"Cheng S, Schlaufman KC, Caiazzo I. 2025. A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars. The Astronomical Journal. 170(1), 47.","short":"S. Cheng, K.C. Schlaufman, I. Caiazzo, The Astronomical Journal 170 (2025).","mla":"Cheng, Sihao, et al. “A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars.” <i>The Astronomical Journal</i>, vol. 170, no. 1, 47, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-3881/addd21\">10.3847/1538-3881/addd21</a>.","ieee":"S. Cheng, K. C. Schlaufman, and I. Caiazzo, “A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars,” <i>The Astronomical Journal</i>, vol. 170, no. 1. IOP Publishing, 2025.","apa":"Cheng, S., Schlaufman, K. C., &#38; Caiazzo, I. (2025). A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars. <i>The Astronomical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-3881/addd21\">https://doi.org/10.3847/1538-3881/addd21</a>","ama":"Cheng S, Schlaufman KC, Caiazzo I. A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars. <i>The Astronomical Journal</i>. 2025;170(1). doi:<a href=\"https://doi.org/10.3847/1538-3881/addd21\">10.3847/1538-3881/addd21</a>","chicago":"Cheng, Sihao, Kevin C. Schlaufman, and Ilaria Caiazzo. “A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars.” <i>The Astronomical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-3881/addd21\">https://doi.org/10.3847/1538-3881/addd21</a>."},"oa":1,"date_updated":"2026-02-19T09:31:41Z","scopus_import":"1","file_date_updated":"2025-07-08T06:40:54Z","license":"https://creativecommons.org/licenses/by/4.0/","_id":"19964","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"1","article_number":"47","day":"01","acknowledgement":"We thank Jay Farihi, Guangwei Fu, J. J. Hermes, Mary Anne Limbach, and Daniel Thorngren for useful discussions. S.C. thanks Siyu Yao for her constant inspiration and encouragement. S.C. acknowledges the support of the Martin A. and Helen Chooljian Member Fund, funding from the Zurich Insurance Company, and the Fund for Natural Sciences at the Institute for Advanced Study. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This publication makes use of data products from the Wide-field Infrared Survey Explorer, 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. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of NASA’s Astrophysics Data System.\r\nFacilities: ADS - , ESO:VISTA - European Southern Observatory's 4.1 meter Visible and Infrared Survey Telescope for Astronomy, Exoplanet Archive - , Gaia - , IRSA - , NEOWISE - , Spitzer - Spitzer Space Telescope satellite, UKIRT - United Kingdom Infrared Telescope, WISE - Wide-field Infrared Survey Explorer.\r\nSoftware: astropy (Astropy Collaboration et al. 2013, 2018, 2022), numpy (C. R. Harris et al. 2020), matplotlib (J. D. Hunter 2007), R (R Core Team 2024), SciPy (P. Virtanen et al. 2020).","oa_version":"Published Version","ddc":["520"],"article_type":"original","year":"2025","doi":"10.3847/1538-3881/addd21","quality_controlled":"1","has_accepted_license":"1","publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"article_processing_charge":"Yes","DOAJ_listed":"1","language":[{"iso":"eng"}],"abstract":[{"lang":"eng","text":"It has been suggested that giant planet occurrence peaks for stars with M* ≈ 3 M⊙ at a value a factor of 4 higher than observed for solar-mass stars. This population of giant planets predicted to frequently orbit main-sequence B stars at a ≈ 10 au is difficult to characterize during the few hundred million years while fusion persists in their host stars. By the time those stars become massive, young white dwarfs, any giant planets present would still be luminous as a consequence of their recent formation. From an initial sample of 2195 Gaia-identified massive, young white dwarfs, we use homogeneous Spitzer Infrared Array Camera (IRAC) photometry to search for evidence of unresolved giant planets. For 30 systems, these IRAC data provide sensitivity to objects with M ≲ 10 MJup, and we identify one candidate with M ≈ 4 MJup orbiting the white dwarf GALEX J071816.4+373139. Correcting for the possibility that some of the white dwarfs in our sample result from mergers, we find a giant planet occurrence  n GP = 0.11+0.13-0.07 for stars with initial masses M* ≳ 3 M⊙. Our occurrence inference is consistent with both the Doppler-inferred occurrence of giant planets orbiting M* ≈ 2 M⊙ giant stars and the theoretically predicted factor of 4 enhancement in the occurrence of giant planets orbiting M* ≈ 3 M⊙ stars relative to solar-mass stars. Future James Webb Space Telescope NIRCam observations of our sample would provide sensitivity to Saturn-mass planets and thereby a definitive estimate of the occurrence of giant planets orbiting stars with M* ≳ 3 M⊙."}],"publisher":"IOP Publishing","volume":170,"publication":"The Astronomical Journal","date_published":"2025-07-01T00:00:00Z","intvolume":"       170","OA_type":"gold"},{"publication_identifier":{"issn":["0004-6256"],"eissn":["1538-3881"]},"quality_controlled":"1","doi":"10.3847/1538-3881/ac166a","year":"2021","article_type":"original","oa_version":"Preprint","intvolume":"       162","date_published":"2021-10-21T00:00:00Z","publication":"The Astronomical Journal","volume":162,"publisher":"IOP Publishing","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2107.06301"}],"abstract":[{"text":"The NASA Transiting Exoplanet Survey Satellite (TESS) is observing tens of millions of stars with time spans ranging from ∼27 days to about 1 yr of continuous observations. This vast amount of data contains a wealth of information for variability, exoplanet, and stellar astrophysics studies but requires a number of processing steps before it can be fully utilized. In order to efficiently process all the TESS data and make it available to the wider scientific community, the TESS Data for Asteroseismology working group, as part of the TESS Asteroseismic Science Consortium, has created an automated open-source processing pipeline to produce light curves corrected for systematics from the short- and long-cadence raw photometry data and to classify these according to stellar variability type. We will process all stars down to a TESS magnitude of 15. This paper is the next in a series detailing how the pipeline works. Here, we present our methodology for the automatic variability classification of TESS photometry using an ensemble of supervised learners that are combined into a metaclassifier. We successfully validate our method using a carefully constructed labeled sample of Kepler Q9 light curves with a 27.4 days time span mimicking single-sector TESS observations, on which we obtain an overall accuracy of 94.9%. We demonstrate that our methodology can successfully classify stars outside of our labeled sample by applying it to all ∼167,000 stars observed in Q9 of the Kepler space mission.","lang":"eng"}],"language":[{"iso":"eng"}],"article_processing_charge":"No","type":"journal_article","month":"10","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"external_id":{"arxiv":["2107.06301"]},"date_created":"2022-07-18T11:54:55Z","extern":"1","author":[{"first_name":"J.","last_name":"Audenaert","full_name":"Audenaert, J."},{"full_name":"Kuszlewicz, J. S.","last_name":"Kuszlewicz","first_name":"J. S."},{"last_name":"Handberg","first_name":"R.","full_name":"Handberg, R."},{"full_name":"Tkachenko, A.","first_name":"A.","last_name":"Tkachenko"},{"full_name":"Armstrong, D. J.","first_name":"D. J.","last_name":"Armstrong"},{"first_name":"M.","last_name":"Hon","full_name":"Hon, M."},{"first_name":"R.","last_name":"Kgoadi","full_name":"Kgoadi, R."},{"last_name":"Lund","first_name":"M. N.","full_name":"Lund, M. N."},{"full_name":"Bell, K. J.","first_name":"K. J.","last_name":"Bell"},{"full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"full_name":"Bowman, D. M.","first_name":"D. M.","last_name":"Bowman"},{"full_name":"Johnston, C.","last_name":"Johnston","first_name":"C."},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"last_name":"Stello","first_name":"D.","full_name":"Stello, D."},{"full_name":"Molnár, L.","last_name":"Molnár","first_name":"L."},{"full_name":"Plachy, E.","last_name":"Plachy","first_name":"E."},{"full_name":"Buzasi, D.","first_name":"D.","last_name":"Buzasi"},{"last_name":"Aerts","first_name":"C.","full_name":"Aerts, C."}],"publication_status":"published","acknowledgement":"The research leading to these results has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 670519: MAMSIE), from the KU Leuven Research Council (grant C16/18/005: PARADISE), from the Research Foundation Flanders (FWO) under grant agreement G0H5416N (ERC Runner Up Project), as well as from the BELgian federal Science Policy Office (BELSPO) through PRODEX grant PLATO. D.J.A acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement No.: DNRF106). R.H. and M.N.L. acknowledge the ESA PRODEX program. This research was supported by the National Aeronautics and Space Administration (80NSSC18K1585 and 80NSSC19K0379) awarded through the TESS Guest Investigator Program. K.J.B. is supported by the National Science Foundation under Award AST-1903828. J.S.K and K.J.B. were supported by funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 338251 (StellarAges). D.M.B. gratefully acknowledges funding from a senior postdoctoral fellowship from the Research Foundation Flanders (FWO) with grant agreement No. 1286521N. The research leading to these results has received funding from the Research Foundation Flanders (FWO) under grant agreement G0A2917N (BlackGEM). R.A.G. acknowledges support from the GOLF and PLATO CNES grants. L.M. was supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. The research leading to these results has been supported by the Hungarian National Research, Development, and Innovation Office (NKFIH) grant KH_18 130405 and the Lendület LP2014-17 and LP2018-7/2020 grants of the Hungarian Academy of Sciences. D.B. acknowledges support from the NASA TESS Guest Investigator Program under award 80NSSC19K0385.\r\n\r\nThis paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate. This research has made use of NASA's Astrophysics Data System as well as the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for the TESS Asteroseismic Science Operations Centre is provided by the Danish National Research Foundation (Grant agreement no.: DNRF106), ESA PRODEX (PEA 4000119301), and the Stellar Astrophysics Centre (SAC) at Aarhus University. We thank the TESS team and staff and TASC/TASOC for their support of the present work.\r\n\r\nThis paper includes data collected by the Kepler mission. Funding for the Kepler and K2 mission was provided by NASA's Science Mission Directorate. The authors acknowledge the efforts of the Kepler Mission team in obtaining the light-curve data and data validation products used in this publication. These data were generated by the Kepler Mission science pipeline through the efforts of the Kepler Science Operations Center and Science Office. The Kepler light curves are archived at the Mikulski Archive for Space Telescopes.\r\n\r\nThe numerical results presented in this work were obtained at the Centre for Scientific Computing, Aarhus. 37 This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013, 2018).\r\n\r\nSoftware: Scikit-learn (Pedregosa et al. 2011), Numpy (Harris et al. 2020), Astropy (Astropy Collaboration et al. 2013, 2018), Scipy (Virtanen et al. 2020), Pandas (McKinney 2010; Pandas Development Team 2020), Lightkurve (Lightkurve Collaboration et al. 2018), XGBoost (Chen & Guestrin 2016), Tensorflow (Abadi et al. 2015).","day":"21","article_number":"209","issue":"5","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11604","scopus_import":"1","date_updated":"2022-08-19T10:01:56Z","oa":1,"citation":{"apa":"Audenaert, J., Kuszlewicz, J. S., Handberg, R., Tkachenko, A., Armstrong, D. J., Hon, M., … Aerts, C. (2021). TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. <i>The Astronomical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-3881/ac166a\">https://doi.org/10.3847/1538-3881/ac166a</a>","chicago":"Audenaert, J., J. S. Kuszlewicz, R. Handberg, A. Tkachenko, D. J. Armstrong, M. Hon, R. Kgoadi, et al. “TESS Data for Asteroseismology (T’DA) Stellar Variability Classification Pipeline: Setup and Application to the Kepler Q9 Data.” <i>The Astronomical Journal</i>. IOP Publishing, 2021. <a href=\"https://doi.org/10.3847/1538-3881/ac166a\">https://doi.org/10.3847/1538-3881/ac166a</a>.","ama":"Audenaert J, Kuszlewicz JS, Handberg R, et al. TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. <i>The Astronomical Journal</i>. 2021;162(5). doi:<a href=\"https://doi.org/10.3847/1538-3881/ac166a\">10.3847/1538-3881/ac166a</a>","short":"J. Audenaert, J.S. Kuszlewicz, R. Handberg, A. Tkachenko, D.J. Armstrong, M. Hon, R. Kgoadi, M.N. Lund, K.J. Bell, L.A. Bugnet, D.M. Bowman, C. Johnston, R.A. García, D. Stello, L. Molnár, E. Plachy, D. Buzasi, C. Aerts, The Astronomical Journal 162 (2021).","ista":"Audenaert J, Kuszlewicz JS, Handberg R, Tkachenko A, Armstrong DJ, Hon M, Kgoadi R, Lund MN, Bell KJ, Bugnet LA, Bowman DM, Johnston C, García RA, Stello D, Molnár L, Plachy E, Buzasi D, Aerts C. 2021. TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. The Astronomical Journal. 162(5), 209.","mla":"Audenaert, J., et al. “TESS Data for Asteroseismology (T’DA) Stellar Variability Classification Pipeline: Setup and Application to the Kepler Q9 Data.” <i>The Astronomical Journal</i>, vol. 162, no. 5, 209, IOP Publishing, 2021, doi:<a href=\"https://doi.org/10.3847/1538-3881/ac166a\">10.3847/1538-3881/ac166a</a>.","ieee":"J. Audenaert <i>et al.</i>, “TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data,” <i>The Astronomical Journal</i>, vol. 162, no. 5. IOP Publishing, 2021."},"title":"TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data","arxiv":1},{"date_created":"2023-08-03T10:11:57Z","external_id":{"arxiv":["2103.13642"]},"extern":"1","author":[{"full_name":"Wang, Luqian","last_name":"Wang","first_name":"Luqian"},{"full_name":"Gies, Douglas R.","last_name":"Gies","first_name":"Douglas R."},{"full_name":"Peters, Geraldine J.","last_name":"Peters","first_name":"Geraldine J."},{"full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg"},{"full_name":"Chojnowski, S. Drew","first_name":"S. Drew","last_name":"Chojnowski"},{"last_name":"Lester","first_name":"Kathryn V.","full_name":"Lester, Kathryn V."},{"full_name":"Howell, Steve B.","last_name":"Howell","first_name":"Steve B."}],"publication_status":"published","month":"05","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","date_updated":"2023-08-21T11:35:50Z","citation":{"apa":"Wang, L., Gies, D. R., Peters, G. J., Götberg, Y. L. L., Chojnowski, S. D., Lester, K. V., &#38; Howell, S. B. (2021). The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-3881/abf144\">https://doi.org/10.3847/1538-3881/abf144</a>","ama":"Wang L, Gies DR, Peters GJ, et al. The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy. <i>The Astronomical Journal</i>. 2021;161(5). doi:<a href=\"https://doi.org/10.3847/1538-3881/abf144\">10.3847/1538-3881/abf144</a>","chicago":"Wang, Luqian, Douglas R. Gies, Geraldine J. Peters, Ylva Louise Linsdotter Götberg, S. Drew Chojnowski, Kathryn V. Lester, and Steve B. Howell. “The Detection and Characterization of Be+sdO Binaries from HST/STIS FUV Spectroscopy.” <i>The Astronomical Journal</i>. American Astronomical Society, 2021. <a href=\"https://doi.org/10.3847/1538-3881/abf144\">https://doi.org/10.3847/1538-3881/abf144</a>.","short":"L. Wang, D.R. Gies, G.J. Peters, Y.L.L. Götberg, S.D. Chojnowski, K.V. Lester, S.B. Howell, The Astronomical Journal 161 (2021).","ista":"Wang L, Gies DR, Peters GJ, Götberg YLL, Chojnowski SD, Lester KV, Howell SB. 2021. The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy. The Astronomical Journal. 161(5), 248.","ieee":"L. Wang <i>et al.</i>, “The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy,” <i>The Astronomical Journal</i>, vol. 161, no. 5. American Astronomical Society, 2021.","mla":"Wang, Luqian, et al. “The Detection and Characterization of Be+sdO Binaries from HST/STIS FUV Spectroscopy.” <i>The Astronomical Journal</i>, vol. 161, no. 5, 248, American Astronomical Society, 2021, doi:<a href=\"https://doi.org/10.3847/1538-3881/abf144\">10.3847/1538-3881/abf144</a>."},"oa":1,"title":"The detection and characterization of Be+sdO binaries from HST/STIS FUV spectroscopy","arxiv":1,"day":"04","article_number":"248","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"5","_id":"13459","scopus_import":"1","year":"2021","article_type":"original","oa_version":"Preprint","publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"doi":"10.3847/1538-3881/abf144","quality_controlled":"1","publisher":"American Astronomical Society","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2103.13642"}],"abstract":[{"text":"The B emission-line stars are rapid rotators that were probably spun up by mass and angular momentum accretion through mass transfer in an interacting binary. Mass transfer will strip the donor star of its envelope to create a small and hot subdwarf remnant. Here we report on Hubble Space Telescope/STIS far-ultraviolet spectroscopy of a sample of Be stars that reveals the presence of the hot sdO companion through the calculation of cross-correlation functions of the observed and model spectra. We clearly detect the spectral signature of the sdO star in 10 of the 13 stars in the sample, and the spectral signals indicate that the sdO stars are hot, relatively faint, and slowly rotating as predicted by models. A comparison of their temperatures and radii with evolutionary tracks indicates that the sdO stars occupy the relatively long-lived, He-core burning stage. Only 1 of the 10 detections was a known binary prior to this investigation, which emphasizes the difficulty of finding such Be+sdO binaries through optical spectroscopy. However, these results and others indicate that many Be stars probably host hot subdwarf companions.","lang":"eng"}],"article_processing_charge":"No","language":[{"iso":"eng"}],"intvolume":"       161","volume":161,"publication":"The Astronomical Journal","date_published":"2021-05-04T00:00:00Z"},{"intvolume":"       162","volume":162,"publication":"The Astronomical Journal","date_published":"2021-08-19T00:00:00Z","publisher":"American Astronomical Society","main_file_link":[{"url":"https://arxiv.org/abs/2105.02261","open_access":"1"}],"abstract":[{"lang":"eng","text":"AM CVn systems are a rare type of accreting binary that consists of a white dwarf and a helium-rich, degenerate donor star. Using the Zwicky Transient Facility (ZTF), we searched for new AM CVn systems by focusing on blue, outbursting stars. We first selected outbursting stars using the ZTF alerts. We cross matched the candidates with Gaia and Pan-STARRS catalogs. The initial selection of candidates based on the Gaia BP-RP contains 1751 unknown objects. We used the Pan-STARRS g-r and r-i color in combination with the Gaia color to identify 59 strong AM CVn candidates. We obtained identification spectra of 35 sources, of which 18 are high-priority candidates, and discovered nine new AM CVn systems and one magnetic CV that shows only He-ii lines. Using the outburst recurrence time, we estimate the orbital periods of the nine new AM CVn systems that are in the range of 29–50 minutes. We conclude that targeted follow up of blue, outbursting sources is an efficient method to find new AM CVn systems and we plan to follow up all candidates we identified to systematically study the population of outbursting AM CVn systems."}],"article_processing_charge":"No","language":[{"iso":"eng"}],"publication_identifier":{"issn":["0004-6256"],"eissn":["1538-3881"]},"doi":"10.3847/1538-3881/ac0622","quality_controlled":"1","year":"2021","article_type":"original","oa_version":"Preprint","day":"19","article_number":"113","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"3","_id":"15216","scopus_import":"1","date_updated":"2024-04-02T07:28:50Z","citation":{"apa":"van Roestel, J., Creter, L., Kupfer, T., Szkody, P., Fuller, J., Green, M. J., … Masci, F. J. (2021). A systematic search for outbursting AM CVn systems with the Zwicky transient facility. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-3881/ac0622\">https://doi.org/10.3847/1538-3881/ac0622</a>","chicago":"Roestel, Jan van, Leah Creter, Thomas Kupfer, Paula Szkody, Jim Fuller, Matthew J. Green, R. Michael Rich, et al. “A Systematic Search for Outbursting AM CVn Systems with the Zwicky Transient Facility.” <i>The Astronomical Journal</i>. American Astronomical Society, 2021. <a href=\"https://doi.org/10.3847/1538-3881/ac0622\">https://doi.org/10.3847/1538-3881/ac0622</a>.","ama":"van Roestel J, Creter L, Kupfer T, et al. A systematic search for outbursting AM CVn systems with the Zwicky transient facility. <i>The Astronomical Journal</i>. 2021;162(3). doi:<a href=\"https://doi.org/10.3847/1538-3881/ac0622\">10.3847/1538-3881/ac0622</a>","ista":"van Roestel J, Creter L, Kupfer T, Szkody P, Fuller J, Green MJ, Rich RM, Sepikas J, Burdge K, Caiazzo I, Mróz P, Prince TA, Duev DA, Graham MJ, Shupe DL, Laher RR, Mahabal AA, Masci FJ. 2021. A systematic search for outbursting AM CVn systems with the Zwicky transient facility. The Astronomical Journal. 162(3), 113.","short":"J. van Roestel, L. Creter, T. Kupfer, P. Szkody, J. Fuller, M.J. Green, R.M. Rich, J. Sepikas, K. Burdge, I. Caiazzo, P. Mróz, T.A. Prince, D.A. Duev, M.J. Graham, D.L. Shupe, R.R. Laher, A.A. Mahabal, F.J. Masci, The Astronomical Journal 162 (2021).","ieee":"J. van Roestel <i>et al.</i>, “A systematic search for outbursting AM CVn systems with the Zwicky transient facility,” <i>The Astronomical Journal</i>, vol. 162, no. 3. American Astronomical Society, 2021.","mla":"van Roestel, Jan, et al. “A Systematic Search for Outbursting AM CVn Systems with the Zwicky Transient Facility.” <i>The Astronomical Journal</i>, vol. 162, no. 3, 113, American Astronomical Society, 2021, doi:<a href=\"https://doi.org/10.3847/1538-3881/ac0622\">10.3847/1538-3881/ac0622</a>."},"oa":1,"title":"A systematic search for outbursting AM CVn systems with the Zwicky transient facility","arxiv":1,"type":"journal_article","month":"08","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","external_id":{"arxiv":["2105.02261"]},"date_created":"2024-03-26T10:32:25Z","extern":"1","author":[{"last_name":"van Roestel","first_name":"Jan","full_name":"van Roestel, Jan"},{"full_name":"Creter, Leah","last_name":"Creter","first_name":"Leah"},{"last_name":"Kupfer","first_name":"Thomas","full_name":"Kupfer, Thomas"},{"last_name":"Szkody","first_name":"Paula","full_name":"Szkody, Paula"},{"first_name":"Jim","last_name":"Fuller","full_name":"Fuller, Jim"},{"last_name":"Green","first_name":"Matthew J.","full_name":"Green, Matthew J."},{"last_name":"Rich","first_name":"R. Michael","full_name":"Rich, R. Michael"},{"full_name":"Sepikas, John","first_name":"John","last_name":"Sepikas"},{"full_name":"Burdge, Kevin","first_name":"Kevin","last_name":"Burdge"},{"full_name":"Caiazzo, Ilaria","first_name":"Ilaria","orcid":"0000-0002-4770-5388","last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"},{"first_name":"Przemek","last_name":"Mróz","full_name":"Mróz, Przemek"},{"full_name":"Prince, Thomas A.","last_name":"Prince","first_name":"Thomas A."},{"last_name":"Duev","first_name":"Dmitry A.","full_name":"Duev, Dmitry A."},{"last_name":"Graham","first_name":"Matthew J.","full_name":"Graham, Matthew J."},{"full_name":"Shupe, David L.","first_name":"David L.","last_name":"Shupe"},{"first_name":"Russ R.","last_name":"Laher","full_name":"Laher, Russ R."},{"full_name":"Mahabal, Ashish A.","first_name":"Ashish A.","last_name":"Mahabal"},{"first_name":"Frank J.","last_name":"Masci","full_name":"Masci, Frank J."}],"publication_status":"published"},{"scopus_import":"1","_id":"17528","issue":"6","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_number":"284","day":"29","title":"Optimizing simulation parameters for weak lensing analyses involving non-Gaussian observables","oa":1,"citation":{"chicago":"Matilla, José Manuel Zorrilla, Stefan Waterval, and Zoltán Haiman. “Optimizing Simulation Parameters for Weak Lensing Analyses Involving Non-Gaussian Observables.” <i>The Astronomical Journal</i>. American Astronomical Society, 2020. <a href=\"https://doi.org/10.3847/1538-3881/ab8f8c\">https://doi.org/10.3847/1538-3881/ab8f8c</a>.","ama":"Matilla JMZ, Waterval S, Haiman Z. Optimizing simulation parameters for weak lensing analyses involving non-Gaussian observables. <i>The Astronomical Journal</i>. 2020;159(6). doi:<a href=\"https://doi.org/10.3847/1538-3881/ab8f8c\">10.3847/1538-3881/ab8f8c</a>","apa":"Matilla, J. M. Z., Waterval, S., &#38; Haiman, Z. (2020). Optimizing simulation parameters for weak lensing analyses involving non-Gaussian observables. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-3881/ab8f8c\">https://doi.org/10.3847/1538-3881/ab8f8c</a>","ieee":"J. M. Z. Matilla, S. Waterval, and Z. Haiman, “Optimizing simulation parameters for weak lensing analyses involving non-Gaussian observables,” <i>The Astronomical Journal</i>, vol. 159, no. 6. American Astronomical Society, 2020.","mla":"Matilla, José Manuel Zorrilla, et al. “Optimizing Simulation Parameters for Weak Lensing Analyses Involving Non-Gaussian Observables.” <i>The Astronomical Journal</i>, vol. 159, no. 6, 284, American Astronomical Society, 2020, doi:<a href=\"https://doi.org/10.3847/1538-3881/ab8f8c\">10.3847/1538-3881/ab8f8c</a>.","short":"J.M.Z. Matilla, S. Waterval, Z. Haiman, The Astronomical Journal 159 (2020).","ista":"Matilla JMZ, Waterval S, Haiman Z. 2020. Optimizing simulation parameters for weak lensing analyses involving non-Gaussian observables. The Astronomical Journal. 159(6), 284."},"date_updated":"2024-09-11T09:03:15Z","status":"public","type":"journal_article","month":"05","publication_status":"published","author":[{"full_name":"Matilla, José Manuel Zorrilla","first_name":"José Manuel Zorrilla","last_name":"Matilla"},{"first_name":"Stefan","last_name":"Waterval","full_name":"Waterval, Stefan"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán"}],"extern":"1","date_created":"2024-09-05T09:35:49Z","publication":"The Astronomical Journal","date_published":"2020-05-29T00:00:00Z","volume":159,"intvolume":"       159","language":[{"iso":"eng"}],"article_processing_charge":"No","abstract":[{"lang":"eng","text":"We performed a series of numerical experiments to quantify the sensitivity of the predictions for weak lensing statistics obtained in ray-tracing dark matter (DM)-only simulations, to two hyper-parameters that influence the accuracy as well as the computational cost of the predictions: the thickness of the lens planes used to build past light cones and the mass resolution of the underlying DM simulation. The statistics considered are the power spectrum (PS) and a series of non-Gaussian observables, including the one-point probability density function, lensing peaks, and Minkowski functionals. Counterintuitively, we find that using thin lens planes (< 60 h−1 Mpc on a 240 h−1 Mpc simulation box) suppresses the PS over a broad range of scales beyond what would be acceptable for a survey comparable to the Large Synoptic Survey Telescope (LSST). A mass resolution of 7.2 × 1011 h−1 M⊙ per DM particle (or 2563 particles in a (240 h−1 Mpc)3 box) is sufficient to extract information using the PS and non-Gaussian statistics from weak lensing data at angular scales down to 1' with LSST-like levels of shape noise."}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.3847/1538-3881/ab8f8c"}],"publisher":"American Astronomical Society","quality_controlled":"1","doi":"10.3847/1538-3881/ab8f8c","publication_identifier":{"issn":["0004-6256","1538-3881"]},"oa_version":"Published Version","article_type":"original","year":"2020"},{"oa":1,"citation":{"apa":"Huber, D., Chaplin, W. J., Chontos, A., Kjeldsen, H., Christensen-Dalsgaard, J., Bedding, T. R., … Zohrabi, F. (2019). A hot Saturn orbiting an oscillating late subgiant discovered by TESS. <i>The Astronomical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-3881/ab1488\">https://doi.org/10.3847/1538-3881/ab1488</a>","chicago":"Huber, Daniel, William J. Chaplin, Ashley Chontos, Hans Kjeldsen, Jørgen Christensen-Dalsgaard, Timothy R. Bedding, Warrick Ball, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS.” <i>The Astronomical Journal</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-3881/ab1488\">https://doi.org/10.3847/1538-3881/ab1488</a>.","ama":"Huber D, Chaplin WJ, Chontos A, et al. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. <i>The Astronomical Journal</i>. 2019;157(6). doi:<a href=\"https://doi.org/10.3847/1538-3881/ab1488\">10.3847/1538-3881/ab1488</a>","ista":"Huber D et al. 2019. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. The Astronomical Journal. 157(6), 245.","short":"D. Huber, W.J. Chaplin, A. Chontos, H. Kjeldsen, J. Christensen-Dalsgaard, T.R. Bedding, W. Ball, R. Brahm, N. Espinoza, T. Henning, A. Jordán, P. Sarkis, E. Knudstrup, S. Albrecht, F. Grundahl, M.F. Andersen, P.L. Pallé, I. Crossfield, B. Fulton, A.W. Howard, H.T. Isaacson, L.M. Weiss, R. Handberg, M.N. Lund, A.M. Serenelli, J. Rørsted Mosumgaard, A. Stokholm, A. Bieryla, L.A. Buchhave, D.W. Latham, S.N. Quinn, E. Gaidos, T. Hirano, G.R. Ricker, R.K. Vanderspek, S. Seager, J.M. Jenkins, J.N. Winn, H.M. Antia, T. Appourchaux, S. Basu, K.J. Bell, O. Benomar, A. Bonanno, D.L. Buzasi, T.L. Campante, Z. Çelik Orhan, E. Corsaro, M.S. Cunha, G.R. Davies, S. Deheuvels, S.K. Grunblatt, A. Hasanzadeh, M.P. Di Mauro, R. A. García, P. Gaulme, L. Girardi, J.A. Guzik, M. Hon, C. Jiang, T. Kallinger, S.D. Kawaler, J.S. Kuszlewicz, Y. Lebreton, T. Li, M. Lucas, M.S. Lundkvist, A.W. Mann, S. Mathis, S. Mathur, A. Mazumdar, T.S. Metcalfe, A. Miglio, M.J.P. F. G. Monteiro, B. Mosser, A. Noll, B. Nsamba, J.M. Joel Ong, S. Örtel, F. Pereira, P. Ranadive, C. Régulo, T.S. Rodrigues, I.W. Roxburgh, V.S. Aguirre, B. Smalley, M. Schofield, S.G. Sousa, K.G. Stassun, D. Stello, J. Tayar, T.R. White, K. Verma, M. Vrard, M. Yıldız, D. Baker, M. Bazot, C. Beichmann, C. Bergmann, L.A. Bugnet, B. Cale, R. Carlino, S.M. Cartwright, J.L. Christiansen, D.R. Ciardi, O. Creevey, J.A. Dittmann, J.-D.D. Nascimento, V.V. Eylen, G. Fürész, J. Gagné, P. Gao, K. Gazeas, F. Giddens, O.J. Hall, S. Hekker, M.J. Ireland, N. Latouf, D. LeBrun, A.M. Levine, W. Matzko, E. Natinsky, E. Page, P. Plavchan, M. Mansouri-Samani, S. McCauliff, S.E. Mullally, B. Orenstein, A.G. Soto, M. Paegert, J.L. van Saders, C. Schnaible, D.R. Soderblom, R. Szabó, A. Tanner, C.G. Tinney, J. Teske, A. Thomas, R. Trampedach, D. Wright, T.T. Yuan, F. Zohrabi, The Astronomical Journal 157 (2019).","mla":"Huber, Daniel, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS.” <i>The Astronomical Journal</i>, vol. 157, no. 6, 245, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-3881/ab1488\">10.3847/1538-3881/ab1488</a>.","ieee":"D. Huber <i>et al.</i>, “A hot Saturn orbiting an oscillating late subgiant discovered by TESS,” <i>The Astronomical Journal</i>, vol. 157, no. 6. IOP Publishing, 2019."},"date_updated":"2022-08-22T07:38:34Z","arxiv":1,"title":"A hot Saturn orbiting an oscillating late subgiant discovered by TESS","issue":"6","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawai'ian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We thank Andrei Tokovinin for helpful information on the Speckle observations obtained with SOAR. D.H. acknowledges support by the National Aeronautics and Space Administration through the TESS Guest Investigator Program (80NSSC18K1585) and by the National Science Foundation (AST-1717000). A.C. acknowledges support by the National Science Foundation under the Graduate Research Fellowship Program. W.J.C., W.H.B., A.M., O.J.H., and G.R.D. acknowledge support from the Science and Technology Facilities Council and UK Space Agency. H.K. and F.G. acknowledge support from the European Social Fund via the Lithuanian Science Council grant No. 09.3.3-LMT-K-712-01-0103. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant DNRF106). A.J. acknowledges support from FONDECYT project 1171208, CONICYT project BASAL AFB-170002, and by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). R.B. acknowledges support from FONDECYT Post-doctoral Fellowship Project 3180246, and from the Millennium Institute of Astrophysics (MAS). A.M.S. is supported by grants ESP2017-82674-R (MINECO) and SGR2017-1131 (AGAUR). R.A.G. and L.B. acknowledge the support of the PLATO grant from the CNES. The research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP72007-2013)ERC grant agreement No. 338251 (StellarAges). S.M. acknowledges support from the European Research Council through the SPIRE grant 647383. This work was also supported by FCT (Portugal) through national funds and by FEDER through COMPETE2020 by these grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672, PTDC/FIS-AST/30389/2017, and POCI-01-0145-FEDER-030389. T.L.C. acknowledges support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 792848 (PULSATION). E.C. is funded by the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 664931. V.S.A. acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B). D.S. acknowledges support from the Australian Research Council. S.B. acknowledges NASA grant NNX16AI09G and NSF grant AST-1514676. T.R.W. acknowledges support from the Australian Research Council through grant DP150100250. A.M. acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, G.A. n. 772293). S.M. acknowledges support from the Ramon y Cajal fellowship number RYC-2015-17697. M.S.L. is supported by the Carlsberg Foundation (grant agreement No. CF17-0760). A.M. and P.R. acknowledge support from the HBCSE-NIUS programme. J.K.T. and J.T. acknowledge that support for this work was provided by NASA through Hubble Fellowship grants HST-HF2-51399.001 and HST-HF2-51424.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. T.S.R. acknowledges financial support from Premiale 2015 MITiC (PI B. Garilli). This project has been supported by the NKFIH K-115709 grant and the Lendület Program of the Hungarian Academy of Sciences, project No. LP2018-7/2018.\r\n\r\nBased on observations made with the Hertzsprung SONG telescope operated on the Spanish Observatorio del Teide on the island of Tenerife by the Aarhus and Copenhagen Universities and by the Instituto de Astrofísica de Canarias. Funding for the TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST).\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2018), Matplotlib (Hunter 2007), DIAMONDS (Corsaro & De Ridder 2014), isoclassify (Huber et al. 2017), EXOFASTv2 (Eastman 2017), ktransit (Barclay 2018).","article_number":"245","day":"30","scopus_import":"1","_id":"11616","extern":"1","external_id":{"arxiv":["1901.01643"]},"date_created":"2022-07-18T14:29:07Z","publication_status":"published","author":[{"last_name":"Huber","first_name":"Daniel","full_name":"Huber, Daniel"},{"first_name":"William J.","last_name":"Chaplin","full_name":"Chaplin, William J."},{"full_name":"Chontos, Ashley","last_name":"Chontos","first_name":"Ashley"},{"full_name":"Kjeldsen, Hans","last_name":"Kjeldsen","first_name":"Hans"},{"last_name":"Christensen-Dalsgaard","first_name":"Jørgen","full_name":"Christensen-Dalsgaard, Jørgen"},{"full_name":"Bedding, Timothy R.","first_name":"Timothy R.","last_name":"Bedding"},{"first_name":"Warrick","last_name":"Ball","full_name":"Ball, Warrick"},{"last_name":"Brahm","first_name":"Rafael","full_name":"Brahm, Rafael"},{"first_name":"Nestor","last_name":"Espinoza","full_name":"Espinoza, Nestor"},{"full_name":"Henning, Thomas","last_name":"Henning","first_name":"Thomas"},{"full_name":"Jordán, Andrés","first_name":"Andrés","last_name":"Jordán"},{"full_name":"Sarkis, Paula","last_name":"Sarkis","first_name":"Paula"},{"first_name":"Emil","last_name":"Knudstrup","full_name":"Knudstrup, Emil"},{"first_name":"Simon","last_name":"Albrecht","full_name":"Albrecht, Simon"},{"full_name":"Grundahl, Frank","last_name":"Grundahl","first_name":"Frank"},{"last_name":"Andersen","first_name":"Mads Fredslund","full_name":"Andersen, Mads Fredslund"},{"last_name":"Pallé","first_name":"Pere L.","full_name":"Pallé, Pere L."},{"first_name":"Ian","last_name":"Crossfield","full_name":"Crossfield, Ian"},{"last_name":"Fulton","first_name":"Benjamin","full_name":"Fulton, Benjamin"},{"full_name":"Howard, Andrew W.","last_name":"Howard","first_name":"Andrew W."},{"first_name":"Howard T.","last_name":"Isaacson","full_name":"Isaacson, Howard T."},{"full_name":"Weiss, Lauren M.","last_name":"Weiss","first_name":"Lauren M."},{"first_name":"Rasmus","last_name":"Handberg","full_name":"Handberg, Rasmus"},{"first_name":"Mikkel N.","last_name":"Lund","full_name":"Lund, Mikkel N."},{"full_name":"Serenelli, Aldo M.","last_name":"Serenelli","first_name":"Aldo M."},{"full_name":"Rørsted Mosumgaard, Jakob","last_name":"Rørsted Mosumgaard","first_name":"Jakob"},{"first_name":"Amalie","last_name":"Stokholm","full_name":"Stokholm, Amalie"},{"full_name":"Bieryla, Allyson","first_name":"Allyson","last_name":"Bieryla"},{"last_name":"Buchhave","first_name":"Lars A.","full_name":"Buchhave, Lars A."},{"full_name":"Latham, David W.","last_name":"Latham","first_name":"David W."},{"last_name":"Quinn","first_name":"Samuel N.","full_name":"Quinn, Samuel N."},{"first_name":"Eric","last_name":"Gaidos","full_name":"Gaidos, Eric"},{"first_name":"Teruyuki","last_name":"Hirano","full_name":"Hirano, Teruyuki"},{"full_name":"Ricker, George R.","first_name":"George R.","last_name":"Ricker"},{"full_name":"Vanderspek, Roland K.","last_name":"Vanderspek","first_name":"Roland K."},{"full_name":"Seager, Sara","first_name":"Sara","last_name":"Seager"},{"last_name":"Jenkins","first_name":"Jon M.","full_name":"Jenkins, Jon M."},{"full_name":"Winn, Joshua N.","first_name":"Joshua N.","last_name":"Winn"},{"full_name":"Antia, H. M.","first_name":"H. M.","last_name":"Antia"},{"full_name":"Appourchaux, Thierry","last_name":"Appourchaux","first_name":"Thierry"},{"full_name":"Basu, Sarbani","last_name":"Basu","first_name":"Sarbani"},{"full_name":"Bell, Keaton J.","first_name":"Keaton J.","last_name":"Bell"},{"last_name":"Benomar","first_name":"Othman","full_name":"Benomar, Othman"},{"last_name":"Bonanno","first_name":"Alfio","full_name":"Bonanno, Alfio"},{"first_name":"Derek L.","last_name":"Buzasi","full_name":"Buzasi, Derek L."},{"full_name":"Campante, Tiago L.","last_name":"Campante","first_name":"Tiago L."},{"first_name":"Z.","last_name":"Çelik Orhan","full_name":"Çelik Orhan, Z."},{"first_name":"Enrico","last_name":"Corsaro","full_name":"Corsaro, Enrico"},{"full_name":"Cunha, Margarida S.","first_name":"Margarida S.","last_name":"Cunha"},{"full_name":"Davies, Guy R.","first_name":"Guy R.","last_name":"Davies"},{"first_name":"Sebastien","last_name":"Deheuvels","full_name":"Deheuvels, Sebastien"},{"first_name":"Samuel K.","last_name":"Grunblatt","full_name":"Grunblatt, Samuel K."},{"last_name":"Hasanzadeh","first_name":"Amir","full_name":"Hasanzadeh, Amir"},{"last_name":"Di Mauro","first_name":"Maria Pia","full_name":"Di Mauro, Maria Pia"},{"last_name":"A. García","first_name":"Rafael","full_name":"A. García, Rafael"},{"last_name":"Gaulme","first_name":"Patrick","full_name":"Gaulme, Patrick"},{"full_name":"Girardi, Léo","first_name":"Léo","last_name":"Girardi"},{"full_name":"Guzik, Joyce A.","first_name":"Joyce A.","last_name":"Guzik"},{"full_name":"Hon, Marc","first_name":"Marc","last_name":"Hon"},{"last_name":"Jiang","first_name":"Chen","full_name":"Jiang, Chen"},{"full_name":"Kallinger, Thomas","last_name":"Kallinger","first_name":"Thomas"},{"full_name":"Kawaler, Steven D.","last_name":"Kawaler","first_name":"Steven D."},{"first_name":"James S.","last_name":"Kuszlewicz","full_name":"Kuszlewicz, James S."},{"full_name":"Lebreton, Yveline","first_name":"Yveline","last_name":"Lebreton"},{"full_name":"Li, Tanda","last_name":"Li","first_name":"Tanda"},{"full_name":"Lucas, Miles","first_name":"Miles","last_name":"Lucas"},{"full_name":"Lundkvist, Mia S.","last_name":"Lundkvist","first_name":"Mia S."},{"first_name":"Andrew W.","last_name":"Mann","full_name":"Mann, Andrew W."},{"full_name":"Mathis, Stéphane","first_name":"Stéphane","last_name":"Mathis"},{"full_name":"Mathur, Savita","last_name":"Mathur","first_name":"Savita"},{"last_name":"Mazumdar","first_name":"Anwesh","full_name":"Mazumdar, Anwesh"},{"full_name":"Metcalfe, Travis S.","first_name":"Travis S.","last_name":"Metcalfe"},{"last_name":"Miglio","first_name":"Andrea","full_name":"Miglio, Andrea"},{"last_name":"F. G. Monteiro","first_name":"Mário J. P.","full_name":"F. G. Monteiro, Mário J. P."},{"full_name":"Mosser, Benoit","first_name":"Benoit","last_name":"Mosser"},{"full_name":"Noll, Anthony","last_name":"Noll","first_name":"Anthony"},{"first_name":"Benard","last_name":"Nsamba","full_name":"Nsamba, Benard"},{"last_name":"Joel Ong","first_name":"Jia Mian","full_name":"Joel Ong, Jia Mian"},{"last_name":"Örtel","first_name":"S.","full_name":"Örtel, S."},{"first_name":"Filipe","last_name":"Pereira","full_name":"Pereira, Filipe"},{"last_name":"Ranadive","first_name":"Pritesh","full_name":"Ranadive, Pritesh"},{"full_name":"Régulo, Clara","first_name":"Clara","last_name":"Régulo"},{"last_name":"Rodrigues","first_name":"Thaíse S.","full_name":"Rodrigues, Thaíse S."},{"last_name":"Roxburgh","first_name":"Ian W.","full_name":"Roxburgh, Ian W."},{"full_name":"Aguirre, Victor Silva","last_name":"Aguirre","first_name":"Victor Silva"},{"first_name":"Barry","last_name":"Smalley","full_name":"Smalley, Barry"},{"first_name":"Mathew","last_name":"Schofield","full_name":"Schofield, Mathew"},{"last_name":"Sousa","first_name":"Sérgio G.","full_name":"Sousa, Sérgio G."},{"full_name":"Stassun, Keivan G.","first_name":"Keivan G.","last_name":"Stassun"},{"full_name":"Stello, Dennis","first_name":"Dennis","last_name":"Stello"},{"last_name":"Tayar","first_name":"Jamie","full_name":"Tayar, Jamie"},{"full_name":"White, Timothy R.","first_name":"Timothy R.","last_name":"White"},{"full_name":"Verma, Kuldeep","first_name":"Kuldeep","last_name":"Verma"},{"last_name":"Vrard","first_name":"Mathieu","full_name":"Vrard, Mathieu"},{"full_name":"Yıldız, M.","first_name":"M.","last_name":"Yıldız"},{"first_name":"David","last_name":"Baker","full_name":"Baker, David"},{"full_name":"Bazot, Michaël","first_name":"Michaël","last_name":"Bazot"},{"last_name":"Beichmann","first_name":"Charles","full_name":"Beichmann, Charles"},{"full_name":"Bergmann, Christoph","first_name":"Christoph","last_name":"Bergmann"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet"},{"last_name":"Cale","first_name":"Bryson","full_name":"Cale, Bryson"},{"last_name":"Carlino","first_name":"Roberto","full_name":"Carlino, Roberto"},{"full_name":"Cartwright, Scott M.","last_name":"Cartwright","first_name":"Scott M."},{"full_name":"Christiansen, Jessie L.","first_name":"Jessie L.","last_name":"Christiansen"},{"full_name":"Ciardi, David R.","first_name":"David R.","last_name":"Ciardi"},{"first_name":"Orlagh","last_name":"Creevey","full_name":"Creevey, Orlagh"},{"first_name":"Jason A.","last_name":"Dittmann","full_name":"Dittmann, Jason A."},{"full_name":"Nascimento, Jose-Dias Do","first_name":"Jose-Dias Do","last_name":"Nascimento"},{"full_name":"Eylen, Vincent Van","first_name":"Vincent Van","last_name":"Eylen"},{"first_name":"Gabor","last_name":"Fürész","full_name":"Fürész, Gabor"},{"last_name":"Gagné","first_name":"Jonathan","full_name":"Gagné, Jonathan"},{"last_name":"Gao","first_name":"Peter","full_name":"Gao, Peter"},{"full_name":"Gazeas, Kosmas","last_name":"Gazeas","first_name":"Kosmas"},{"full_name":"Giddens, Frank","first_name":"Frank","last_name":"Giddens"},{"last_name":"Hall","first_name":"Oliver J.","full_name":"Hall, Oliver J."},{"full_name":"Hekker, Saskia","last_name":"Hekker","first_name":"Saskia"},{"full_name":"Ireland, Michael J.","first_name":"Michael J.","last_name":"Ireland"},{"last_name":"Latouf","first_name":"Natasha","full_name":"Latouf, Natasha"},{"first_name":"Danny","last_name":"LeBrun","full_name":"LeBrun, Danny"},{"last_name":"Levine","first_name":"Alan M.","full_name":"Levine, Alan M."},{"last_name":"Matzko","first_name":"William","full_name":"Matzko, William"},{"first_name":"Eva","last_name":"Natinsky","full_name":"Natinsky, Eva"},{"full_name":"Page, Emma","last_name":"Page","first_name":"Emma"},{"full_name":"Plavchan, Peter","last_name":"Plavchan","first_name":"Peter"},{"full_name":"Mansouri-Samani, Masoud","first_name":"Masoud","last_name":"Mansouri-Samani"},{"full_name":"McCauliff, Sean","last_name":"McCauliff","first_name":"Sean"},{"first_name":"Susan E.","last_name":"Mullally","full_name":"Mullally, Susan E."},{"first_name":"Brendan","last_name":"Orenstein","full_name":"Orenstein, Brendan"},{"first_name":"Aylin Garcia","last_name":"Soto","full_name":"Soto, Aylin Garcia"},{"first_name":"Martin","last_name":"Paegert","full_name":"Paegert, Martin"},{"full_name":"van Saders, Jennifer L.","first_name":"Jennifer L.","last_name":"van Saders"},{"first_name":"Chloe","last_name":"Schnaible","full_name":"Schnaible, Chloe"},{"full_name":"Soderblom, David R.","last_name":"Soderblom","first_name":"David R."},{"last_name":"Szabó","first_name":"Róbert","full_name":"Szabó, Róbert"},{"first_name":"Angelle","last_name":"Tanner","full_name":"Tanner, Angelle"},{"full_name":"Tinney, C. G.","first_name":"C. G.","last_name":"Tinney"},{"full_name":"Teske, Johanna","first_name":"Johanna","last_name":"Teske"},{"full_name":"Thomas, Alexandra","first_name":"Alexandra","last_name":"Thomas"},{"first_name":"Regner","last_name":"Trampedach","full_name":"Trampedach, Regner"},{"last_name":"Wright","first_name":"Duncan","full_name":"Wright, Duncan"},{"full_name":"Yuan, Thomas T.","last_name":"Yuan","first_name":"Thomas T."},{"full_name":"Zohrabi, Farzaneh","last_name":"Zohrabi","first_name":"Farzaneh"}],"month":"05","type":"journal_article","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"abstract":[{"lang":"eng","text":"We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V = 8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (R⋆ = 2.943 ± 0.064 R⊙), mass (M⋆ = 1.212 ± 0.074 M⊙), and age (4.9 ± 1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a \"hot Saturn\" (Rp = 9.17 ± 0.33 R⊕) with an orbital period of ∼14.3 days, irradiance of F = 343 ± 24 F⊕, and moderate mass (Mp = 60.5 ± 5.7 M⊕) and density (ρp = 0.431 ± 0.062 g cm−3). The properties of HD 221416 b show that the host-star metallicity–planet mass correlation found in sub-Saturns (4–8 R⊕) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology."}],"publisher":"IOP Publishing","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1901.01643"}],"language":[{"iso":"eng"}],"article_processing_charge":"No","publication":"The Astronomical Journal","date_published":"2019-05-30T00:00:00Z","volume":157,"intvolume":"       157","year":"2019","oa_version":"Preprint","article_type":"original","publication_identifier":{"issn":["0004-6256"]},"quality_controlled":"1","doi":"10.3847/1538-3881/ab1488"},{"date_updated":"2024-09-25T09:22:09Z","oa":1,"citation":{"apa":"Tanaka, T., Haiman, Z., &#38; Menou, K. (2010). Witnessing the birth of a quasar. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1088/0004-6256/140/2/642\">https://doi.org/10.1088/0004-6256/140/2/642</a>","chicago":"Tanaka, Takamitsu, Zoltán Haiman, and Kristen Menou. “Witnessing the Birth of a Quasar.” <i>The Astronomical Journal</i>. American Astronomical Society, 2010. <a href=\"https://doi.org/10.1088/0004-6256/140/2/642\">https://doi.org/10.1088/0004-6256/140/2/642</a>.","ama":"Tanaka T, Haiman Z, Menou K. Witnessing the birth of a quasar. <i>The Astronomical Journal</i>. 2010;140(2):642-651. doi:<a href=\"https://doi.org/10.1088/0004-6256/140/2/642\">10.1088/0004-6256/140/2/642</a>","short":"T. Tanaka, Z. Haiman, K. Menou, The Astronomical Journal 140 (2010) 642–651.","ista":"Tanaka T, Haiman Z, Menou K. 2010. Witnessing the birth of a quasar. The Astronomical Journal. 140(2), 642–651.","ieee":"T. Tanaka, Z. Haiman, and K. Menou, “Witnessing the birth of a quasar,” <i>The Astronomical Journal</i>, vol. 140, no. 2. American Astronomical Society, pp. 642–651, 2010.","mla":"Tanaka, Takamitsu, et al. “Witnessing the Birth of a Quasar.” <i>The Astronomical Journal</i>, vol. 140, no. 2, American Astronomical Society, 2010, pp. 642–51, doi:<a href=\"https://doi.org/10.1088/0004-6256/140/2/642\">10.1088/0004-6256/140/2/642</a>."},"title":"Witnessing the birth of a quasar","day":"15","issue":"2","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","_id":"17686","scopus_import":"1","date_created":"2024-09-06T08:21:37Z","extern":"1","author":[{"first_name":"Takamitsu","last_name":"Tanaka","full_name":"Tanaka, Takamitsu"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán","full_name":"Haiman, Zoltán"},{"full_name":"Menou, Kristen","first_name":"Kristen","last_name":"Menou"}],"publication_status":"published","page":"642-651","month":"07","type":"journal_article","status":"public","publisher":"American Astronomical Society","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1088/0004-6256/140/2/642"}],"abstract":[{"lang":"eng","text":"The coalescence of a supermassive black hole binary (SMBHB) is thought to be accompanied by an electromagnetic (EM) afterglow, produced by the viscous infall of the surrounding circumbinary gas disk after the merger. It has been proposed that once the merger has been detected in gravitational waves (GWs) by LISA, follow-up EM searches for this afterglow can help identify the EM counterpart of the LISA source. Here we study whether the afterglows may be sufficiently bright and numerous to be detectable in EM surveys alone. The viscous afterglow, which lasts for years to decades for SMBHBs in LISA's sensitivity window, is characterized by rapid increases in both the bolometric luminosity and in the spectral hardness of the source. If quasar activity is triggered by the same major galaxy mergers that produce SMBHBs, then the afterglow could be interpreted as a signature of the birth of a quasar. Using an idealized model for the post-merger viscous spreading of the circumbinary disk and the resulting light curve, and using the observed luminosity function of quasars as a proxy for the SMBHB merger rate, we delineate the survey requirements for identifying such birthing quasars. If circumbinary disks have a high disk surface density and viscosity, an all-sky soft X-ray survey with a sensitivity of ~<3x10^-14 erg s^-1 cm^-2 and a time resolution of ~months could identify dozens of birthing quasars with sustained brightening rates of >10%/yr. If >1% of the X-ray emission is reprocessed into optical frequencies, birthing quasars could also be identified in optical transient surveys such as the LSST. Distinguishing a birthing quasar from other variable sources may be facilitated by the monotonic hardening of its spectrum, but will likely remain challenging. This reinforces the notion that joint EM-plus-GW observations offer the best prospects for identifying the EM signatures of SMBHB mergers."}],"language":[{"iso":"eng"}],"article_processing_charge":"No","intvolume":"       140","publication":"The Astronomical Journal","date_published":"2010-07-15T00:00:00Z","volume":140,"year":"2010","article_type":"original","oa_version":"Published Version","publication_identifier":{"issn":["0004-6256","1538-3881"]},"quality_controlled":"1","doi":"10.1088/0004-6256/140/2/642"},{"main_file_link":[{"url":"https://doi.org/10.1086/498063","open_access":"1"}],"publisher":"American Astronomical Society","abstract":[{"text":"We report on i-band snapshot observations of 157 Sloan Digital Sky Survey (SDSS) quasars at 4<z<5.4 using the Advanced Camera for Surveys on the Hubble Space Telescope (HST) to search for evidence of gravitational lensing of these sources. None of the quasars appear to be strongly lensed and multiply imaged at the angular resolution (~0.1\") and sensitivity of HST. The non-detection of strong lensing in these systems constrains the z=4-5 luminosity function to an intrinsic slope of beta>-3.8 (3 sigma), assuming a break in the quasar luminosity function at M*_145=-24.5. This constraint is considerably stronger than the limit of beta>-4.63 obtained from the absence of lensing in four z>5.7 quasars. Such constraints are important for our understanding of the true space density of high-redshift quasars and the ionization state of the early universe.","lang":"eng"}],"article_processing_charge":"No","language":[{"iso":"eng"}],"intvolume":"       131","volume":131,"publication":"The Astronomical Journal","date_published":"2006-01-01T00:00:00Z","year":"2006","article_type":"original","oa_version":"Published Version","publication_identifier":{"issn":["0004-6256","1538-3881"]},"doi":"10.1086/498063","quality_controlled":"1","date_updated":"2024-11-12T09:57:35Z","oa":1,"citation":{"mla":"Richards, Gordon T., et al. “A Snapshot Survey for Gravitational Lenses among z ≥ 4.0 Quasars. II. Constraints on the 4.0 &#60; z &#60; 5.4 Quasar Population.” <i>The Astronomical Journal</i>, vol. 131, no. 1, American Astronomical Society, 2006, pp. 49–54, doi:<a href=\"https://doi.org/10.1086/498063\">10.1086/498063</a>.","ieee":"G. T. Richards <i>et al.</i>, “A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. II. Constraints on the 4.0 &#60; z &#60; 5.4 quasar population,” <i>The Astronomical Journal</i>, vol. 131, no. 1. American Astronomical Society, pp. 49–54, 2006.","short":"G.T. Richards, Z. Haiman, B. Pindor, M.A. Strauss, X. Fan, D. Eisenstein, D.P. Schneider, N.A. Bahcall, J. Brinkmann, M. Fukugita, The Astronomical Journal 131 (2006) 49–54.","ista":"Richards GT, Haiman Z, Pindor B, Strauss MA, Fan X, Eisenstein D, Schneider DP, Bahcall NA, Brinkmann J, Fukugita M. 2006. A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. II. Constraints on the 4.0 &#60; z &#60; 5.4 quasar population. The Astronomical Journal. 131(1), 49–54.","ama":"Richards GT, Haiman Z, Pindor B, et al. A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. II. Constraints on the 4.0 &#60; z &#60; 5.4 quasar population. <i>The Astronomical Journal</i>. 2006;131(1):49-54. doi:<a href=\"https://doi.org/10.1086/498063\">10.1086/498063</a>","chicago":"Richards, Gordon T., Zoltán Haiman, Bartosz Pindor, Michael A. Strauss, Xiaohui Fan, Daniel Eisenstein, Donald P. Schneider, Neta A. Bahcall, J. Brinkmann, and Masataka Fukugita. “A Snapshot Survey for Gravitational Lenses among z ≥ 4.0 Quasars. II. Constraints on the 4.0 &#60; z &#60; 5.4 Quasar Population.” <i>The Astronomical Journal</i>. American Astronomical Society, 2006. <a href=\"https://doi.org/10.1086/498063\">https://doi.org/10.1086/498063</a>.","apa":"Richards, G. T., Haiman, Z., Pindor, B., Strauss, M. A., Fan, X., Eisenstein, D., … Fukugita, M. (2006). A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. II. Constraints on the 4.0 &#60; z &#60; 5.4 quasar population. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/498063\">https://doi.org/10.1086/498063</a>"},"title":"A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. II. Constraints on the 4.0 < z < 5.4 quasar population","day":"01","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"1","_id":"17727","scopus_import":"1","date_created":"2024-09-06T09:13:53Z","extern":"1","author":[{"last_name":"Richards","first_name":"Gordon T.","full_name":"Richards, Gordon T."},{"last_name":"Haiman","orcid":"0000-0003-3633-5403","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"first_name":"Bartosz","last_name":"Pindor","full_name":"Pindor, Bartosz"},{"full_name":"Strauss, Michael A.","last_name":"Strauss","first_name":"Michael A."},{"full_name":"Fan, Xiaohui","first_name":"Xiaohui","last_name":"Fan"},{"full_name":"Eisenstein, Daniel","last_name":"Eisenstein","first_name":"Daniel"},{"full_name":"Schneider, Donald P.","last_name":"Schneider","first_name":"Donald P."},{"last_name":"Bahcall","first_name":"Neta A.","full_name":"Bahcall, Neta A."},{"first_name":"J.","last_name":"Brinkmann","full_name":"Brinkmann, J."},{"full_name":"Fukugita, Masataka","first_name":"Masataka","last_name":"Fukugita"}],"publication_status":"published","related_material":{"link":[{"relation":"erratum","url":"https://doi.org/10.1086/506907"}]},"month":"01","type":"journal_article","page":"49-54","status":"public"},{"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/381906"}],"publisher":"American Astronomical Society","abstract":[{"text":"Over the last few years, the Sloan Digital Sky Survey (SDSS) has discovered several hundred quasars with redshift between 4.0 and 6.4. Including the effects of magnification bias, one expects a priori that an appreciable fraction of these objects are gravitationally lensed. We have used the Advanced Camera for Surveys on the Hubble Space Telescope to carry out a snapshot imaging survey of high-redshift SDSS quasars to search for gravitationally split lenses. This paper, the first in a series reporting the results of the survey, describes snapshot observations of four quasars at z = 5.74, 5.82, 5.99, and 6.30, respectively. We find that none of these objects has a lensed companion within 5 mag with a separation larger than 0farcs3; within 2.5 mag we can rule out companions within 0farcs1. Based on the nondetection of strong lensing in these four systems, we constrain the z ∼ 6 luminosity function to a slope of β > -4.63 (3 σ), assuming a break in the quasar luminosity function at M = -24.1. We discuss the implications of this constraint on the ionizing background due to quasars in the early universe. Given that these quasars are not highly magnified, estimates of the masses of their central engines by the Eddington argument must be taken seriously, possibly challenging models of black hole formation.","lang":"eng"}],"language":[{"iso":"eng"}],"article_processing_charge":"No","intvolume":"       127","publication":"The Astronomical Journal","date_published":"2004-03-01T00:00:00Z","volume":127,"year":"2004","article_type":"original","oa_version":"Published Version","publication_identifier":{"issn":["0004-6256","1538-3881"]},"quality_controlled":"1","doi":"10.1086/381906","date_updated":"2024-09-30T13:53:57Z","oa":1,"citation":{"ieee":"G. T. Richards <i>et al.</i>, “A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. I. The z &#62;5.7 sample,” <i>The Astronomical Journal</i>, vol. 127, no. 3. American Astronomical Society, pp. 1305–1312, 2004.","mla":"Richards, Gordon T., et al. “A Snapshot Survey for Gravitational Lenses among z ≥ 4.0 Quasars. I. The z &#62;5.7 Sample.” <i>The Astronomical Journal</i>, vol. 127, no. 3, American Astronomical Society, 2004, pp. 1305–12, doi:<a href=\"https://doi.org/10.1086/381906\">10.1086/381906</a>.","short":"G.T. Richards, M.A. Strauss, B. Pindor, Z. Haiman, X. Fan, D. Eisenstein, D.P. Schneider, N.A. Bahcall, J. Brinkmann, R. Brunner, The Astronomical Journal 127 (2004) 1305–1312.","ista":"Richards GT, Strauss MA, Pindor B, Haiman Z, Fan X, Eisenstein D, Schneider DP, Bahcall NA, Brinkmann J, Brunner R. 2004. A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. I. The z &#62;5.7 sample. The Astronomical Journal. 127(3), 1305–1312.","chicago":"Richards, Gordon T., Michael A. Strauss, Bartosz Pindor, Zoltán Haiman, Xiaohui Fan, Daniel Eisenstein, Donald P. Schneider, Neta A. Bahcall, J. Brinkmann, and Robert Brunner. “A Snapshot Survey for Gravitational Lenses among z ≥ 4.0 Quasars. I. The z &#62;5.7 Sample.” <i>The Astronomical Journal</i>. American Astronomical Society, 2004. <a href=\"https://doi.org/10.1086/381906\">https://doi.org/10.1086/381906</a>.","ama":"Richards GT, Strauss MA, Pindor B, et al. A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. I. The z &#62;5.7 sample. <i>The Astronomical Journal</i>. 2004;127(3):1305-1312. doi:<a href=\"https://doi.org/10.1086/381906\">10.1086/381906</a>","apa":"Richards, G. T., Strauss, M. A., Pindor, B., Haiman, Z., Fan, X., Eisenstein, D., … Brunner, R. (2004). A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. I. The z &#62;5.7 sample. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/381906\">https://doi.org/10.1086/381906</a>"},"title":"A snapshot survey for gravitational lenses among z ≥ 4.0 quasars. I. The z >5.7 sample","day":"01","issue":"3","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","_id":"17790","scopus_import":"1","date_created":"2024-09-06T10:22:30Z","extern":"1","author":[{"full_name":"Richards, Gordon T.","last_name":"Richards","first_name":"Gordon T."},{"first_name":"Michael A.","last_name":"Strauss","full_name":"Strauss, Michael A."},{"full_name":"Pindor, Bartosz","last_name":"Pindor","first_name":"Bartosz"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"},{"first_name":"Xiaohui","last_name":"Fan","full_name":"Fan, Xiaohui"},{"full_name":"Eisenstein, Daniel","last_name":"Eisenstein","first_name":"Daniel"},{"full_name":"Schneider, Donald P.","last_name":"Schneider","first_name":"Donald P."},{"full_name":"Bahcall, Neta A.","last_name":"Bahcall","first_name":"Neta A."},{"full_name":"Brinkmann, J.","last_name":"Brinkmann","first_name":"J."},{"full_name":"Brunner, Robert","first_name":"Robert","last_name":"Brunner"}],"publication_status":"published","page":"1305-1312","month":"03","type":"journal_article","status":"public"},{"day":"01","issue":"4","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","_id":"17750","scopus_import":"1","date_updated":"2024-09-30T07:33:02Z","oa":1,"citation":{"mla":"Fan, Xiaohui, et al. “A Survey of z &#62; 5.7 Quasars in the Sloan Digital Sky Survey. II. Discovery of Three Additional Quasars at z &#62; 6.” <i>The Astronomical Journal</i>, vol. 125, no. 4, American Astronomical Society, 2003, pp. 1649–59, doi:<a href=\"https://doi.org/10.1086/368246\">10.1086/368246</a>.","ieee":"X. Fan <i>et al.</i>, “A survey of z &#62; 5.7 quasars in the Sloan Digital Sky Survey. II. Discovery of three additional quasars at z &#62; 6,” <i>The Astronomical Journal</i>, vol. 125, no. 4. American Astronomical Society, pp. 1649–1659, 2003.","ista":"Fan X, Strauss MA, Schneider DP, Becker RH, White RL, Haiman Z, Gregg M, Pentericci L, Grebel EK, Narayanan VK, Loh Y-S, Richards GT, Gunn JE, Lupton RH, Knapp GR, Ivezić Ž, Brandt WN, Collinge M, Hao L, Harbeck D, Prada F, Schaye J, Strateva I, Zakamska N, Anderson S, Brinkmann J, Bahcall NA, Lamb DQ, Okamura S, Szalay A, York DG. 2003. A survey of z &#62; 5.7 quasars in the Sloan Digital Sky Survey. II. Discovery of three additional quasars at z &#62; 6. The Astronomical Journal. 125(4), 1649–1659.","short":"X. Fan, M.A. Strauss, D.P. Schneider, R.H. Becker, R.L. White, Z. Haiman, M. Gregg, L. Pentericci, E.K. Grebel, V.K. Narayanan, Y.-S. Loh, G.T. Richards, J.E. Gunn, R.H. Lupton, G.R. Knapp, Ž. Ivezić, W.N. Brandt, M. Collinge, L. Hao, D. Harbeck, F. Prada, J. Schaye, I. Strateva, N. Zakamska, S. Anderson, J. Brinkmann, N.A. Bahcall, D.Q. Lamb, S. Okamura, A. Szalay, D.G. York, The Astronomical Journal 125 (2003) 1649–1659.","ama":"Fan X, Strauss MA, Schneider DP, et al. A survey of z &#62; 5.7 quasars in the Sloan Digital Sky Survey. II. Discovery of three additional quasars at z &#62; 6. <i>The Astronomical Journal</i>. 2003;125(4):1649-1659. doi:<a href=\"https://doi.org/10.1086/368246\">10.1086/368246</a>","chicago":"Fan, Xiaohui, Michael A. Strauss, Donald P. Schneider, Robert H. Becker, Richard L. White, Zoltán Haiman, Michael Gregg, et al. “A Survey of z &#62; 5.7 Quasars in the Sloan Digital Sky Survey. II. Discovery of Three Additional Quasars at z &#62; 6.” <i>The Astronomical Journal</i>. American Astronomical Society, 2003. <a href=\"https://doi.org/10.1086/368246\">https://doi.org/10.1086/368246</a>.","apa":"Fan, X., Strauss, M. A., Schneider, D. P., Becker, R. H., White, R. L., Haiman, Z., … York, D. G. (2003). A survey of z &#62; 5.7 quasars in the Sloan Digital Sky Survey. II. Discovery of three additional quasars at z &#62; 6. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/368246\">https://doi.org/10.1086/368246</a>"},"title":"A survey of z > 5.7 quasars in the Sloan Digital Sky Survey. II. Discovery of three additional quasars at z > 6","page":"1649-1659","type":"journal_article","month":"04","status":"public","date_created":"2024-09-06T09:38:08Z","extern":"1","author":[{"last_name":"Fan","first_name":"Xiaohui","full_name":"Fan, Xiaohui"},{"full_name":"Strauss, Michael A.","last_name":"Strauss","first_name":"Michael A."},{"full_name":"Schneider, Donald P.","last_name":"Schneider","first_name":"Donald P."},{"full_name":"Becker, Robert H.","last_name":"Becker","first_name":"Robert H."},{"full_name":"White, Richard L.","last_name":"White","first_name":"Richard L."},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán"},{"last_name":"Gregg","first_name":"Michael","full_name":"Gregg, Michael"},{"full_name":"Pentericci, Laura","last_name":"Pentericci","first_name":"Laura"},{"full_name":"Grebel, Eva K.","first_name":"Eva K.","last_name":"Grebel"},{"full_name":"Narayanan, Vijay K.","last_name":"Narayanan","first_name":"Vijay K."},{"full_name":"Loh, Yeong-Shang","last_name":"Loh","first_name":"Yeong-Shang"},{"full_name":"Richards, Gordon T.","last_name":"Richards","first_name":"Gordon T."},{"full_name":"Gunn, James E.","last_name":"Gunn","first_name":"James E."},{"full_name":"Lupton, Robert H.","last_name":"Lupton","first_name":"Robert H."},{"full_name":"Knapp, Gillian R.","first_name":"Gillian R.","last_name":"Knapp"},{"last_name":"Ivezić","first_name":"Željko","full_name":"Ivezić, Željko"},{"full_name":"Brandt, W. N.","last_name":"Brandt","first_name":"W. N."},{"full_name":"Collinge, Matthew","first_name":"Matthew","last_name":"Collinge"},{"full_name":"Hao, Lei","first_name":"Lei","last_name":"Hao"},{"last_name":"Harbeck","first_name":"Daniel","full_name":"Harbeck, Daniel"},{"full_name":"Prada, Francisco","first_name":"Francisco","last_name":"Prada"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"last_name":"Strateva","first_name":"Iskra","full_name":"Strateva, Iskra"},{"first_name":"Nadia","last_name":"Zakamska","full_name":"Zakamska, Nadia"},{"full_name":"Anderson, Scott","first_name":"Scott","last_name":"Anderson"},{"first_name":"Jon","last_name":"Brinkmann","full_name":"Brinkmann, Jon"},{"full_name":"Bahcall, Neta A.","first_name":"Neta A.","last_name":"Bahcall"},{"full_name":"Lamb, Don Q.","first_name":"Don Q.","last_name":"Lamb"},{"first_name":"Sadanori","last_name":"Okamura","full_name":"Okamura, Sadanori"},{"full_name":"Szalay, Alex","first_name":"Alex","last_name":"Szalay"},{"full_name":"York, Donald G.","first_name":"Donald G.","last_name":"York"}],"publication_status":"published","intvolume":"       125","date_published":"2003-04-01T00:00:00Z","publication":"The Astronomical Journal","volume":125,"main_file_link":[{"url":"https://doi.org/10.1086/368246","open_access":"1"}],"publisher":"American Astronomical Society","abstract":[{"lang":"eng","text":"We present the discovery of three new quasars at z>6 in 1300 deg^2 of SDSS imaging data, J114816.64+525150.3 (z=6.43), J104845.05+463718.3 (z=6.23) and J163033.90+401209.6 (z=6.05). The first two objects have weak Ly alpha emission lines; their redshifts are determined from the positions of the Lyman break. They are only accurate to 0.05 and could be affected by the presence of broad absorption line systems. The last object has a Ly alpha strength more typical of lower redshift quasars. Based on a sample of six quasars at z>5.7 that cover 2870 deg^2 presented in this paper and in Paper I, we estimate the comoving density of luminous quasars at z 6 and M_{1450} < -26.8 to be (8 +/- 3)x10^{-10} Mpc^{-3} (for H_0 = 50 km/s/Mpc, Omega = 1). HST imaging of two z>5.7 quasars and high-resolution ground-based images (seeing 0.4'') of three additional z>5.7 quasars show that none of them is gravitationally lensed. The luminosity distribution of the high-redshfit quasar sample suggests the bright end slope of the quasar luminosity function at z 6 is shallower than Psi L^{-3.5} (2-sigma), consistent with the absence of strongly lensed objects."}],"language":[{"iso":"eng"}],"article_processing_charge":"No","publication_identifier":{"issn":["0004-6256","1538-3881"]},"quality_controlled":"1","doi":"10.1086/368246","year":"2003","article_type":"original","oa_version":"Published Version"},{"citation":{"short":"C. Stoughton, R.H. Lupton, M. Bernardi, M.R. Blanton, S. Burles, F.J. Castander, A.J. Connolly, D.J. Eisenstein, J.A. Frieman, G.S. Hennessy, R.B. Hindsley, Ž. Ivezić, S. Kent, P.Z. Kunszt, B.C. Lee, A. Meiksin, J.A. Munn, H.J. Newberg, R.C. Nichol, T. Nicinski, J.R. Pier, G.T. Richards, M.W. Richmond, D.J. Schlegel, J.A. Smith, M.A. Strauss, M. SubbaRao, A.S. Szalay, A.R. Thakar, D.L. Tucker, D.E. Vanden Berk, B. Yanny, J.K. Adelman, J.E. Anderson, Jr., S.F. Anderson, J. Annis, N.A. Bahcall, J.A. Bakken, M. Bartelmann, S. Bastian, A. Bauer, E. Berman, H. Böhringer, W.N. Boroski, S. Bracker, C. Briegel, J.W. Briggs, J. Brinkmann, R. Brunner, L. Carey, M.A. Carr, B. Chen, D. Christian, P.L. Colestock, J.H. Crocker, I. Csabai, P.C. Czarapata, J. Dalcanton, A.F. Davidsen, J.E. Davis, W. Dehnen, S. Dodelson, M. Doi, T. Dombeck, M. Donahue, N. Ellman, B.R. Elms, M.L. Evans, L. Eyer, X. Fan, G.R. Federwitz, S. Friedman, M. Fukugita, R. Gal, B. Gillespie, K. Glazebrook, J. Gray, E.K. Grebel, B. Greenawalt, G. Greene, J.E. Gunn, E. de Haas, Z. Haiman, M. Haldeman, P.B. Hall, M. Hamabe, B. Hansen, F.H. Harris, H. Harris, M. Harvanek, S.L. Hawley, J.J.E. Hayes, T.M. Heckman, A. Helmi, A. Henden, C.J. Hogan, D.W. Hogg, D.J. Holmgren, J. Holtzman, C.-H. Huang, C. Hull, S.-I. Ichikawa, T. Ichikawa, D.E. Johnston, G. Kauffmann, R.S.J. Kim, T. Kimball, E. Kinney, M. Klaene, S.J. Kleinman, A. Klypin, G.R. Knapp, J. Korienek, J. Krolik, R.G. Kron, J. Krzesiński, D.Q. Lamb, R.F. Leger, S. Limmongkol, C. Lindenmeyer, D.C. Long, C. Loomis, J. Loveday, B. MacKinnon, E.J. Mannery, P.M. Mantsch, B. Margon, P. McGehee, T.A. McKay, B. McLean, K. Menou, A. Merelli, H.J. Mo, D.G. Monet, O. Nakamura, V.K. Narayanan, T. Nash, E.H. Neilsen, Jr., P.R. Newman, A. Nitta, M. Odenkirchen, N. Okada, S. Okamura, J.P. Ostriker, R. Owen, A.G. Pauls, J. Peoples, R.S. Peterson, D. Petravick, A. Pope, R. Pordes, M. Postman, A. Prosapio, T.R. Quinn, R. Rechenmacher, C.H. Rivetta, H.-W. Rix, C.M. Rockosi, R. Rosner, K. Ruthmansdorfer, D. Sandford, D.P. Schneider, R. Scranton, M. Sekiguchi, G. Sergey, R. Sheth, K. Shimasaku, S. Smee, S.A. Snedden, A. Stebbins, C. Stubbs, I. Szapudi, P. Szkody, G.P. Szokoly, S. Tabachnik, Z. Tsvetanov, A. Uomoto, M.S. Vogeley, W. Voges, P. Waddell, R. Walterbos, S. Wang, M. Watanabe, D.H. Weinberg, R.L. White, S.D.M. White, B. Wilhite, D. Wolfe, N. Yasuda, D.G. York, I. Zehavi, W. Zheng, The Astronomical Journal 123 (2002) 485–548.","ista":"Stoughton C et al. 2002. Sloan digital sky survey: Early data release. The Astronomical Journal. 123(1), 485–548.","ieee":"C. Stoughton <i>et al.</i>, “Sloan digital sky survey: Early data release,” <i>The Astronomical Journal</i>, vol. 123, no. 1. American Astronomical Society, pp. 485–548, 2002.","mla":"Stoughton, Chris, et al. “Sloan Digital Sky Survey: Early Data Release.” <i>The Astronomical Journal</i>, vol. 123, no. 1, American Astronomical Society, 2002, pp. 485–548, doi:<a href=\"https://doi.org/10.1086/324741\">10.1086/324741</a>.","apa":"Stoughton, C., Lupton, R. H., Bernardi, M., Blanton, M. R., Burles, S., Castander, F. J., … Zheng, W. (2002). Sloan digital sky survey: Early data release. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/324741\">https://doi.org/10.1086/324741</a>","ama":"Stoughton C, Lupton RH, Bernardi M, et al. Sloan digital sky survey: Early data release. <i>The Astronomical Journal</i>. 2002;123(1):485-548. doi:<a href=\"https://doi.org/10.1086/324741\">10.1086/324741</a>","chicago":"Stoughton, Chris, Robert H. Lupton, Mariangela Bernardi, Michael R. Blanton, Scott Burles, Francisco J. Castander, A. J. Connolly, et al. “Sloan Digital Sky Survey: Early Data Release.” <i>The Astronomical Journal</i>. American Astronomical Society, 2002. <a href=\"https://doi.org/10.1086/324741\">https://doi.org/10.1086/324741</a>."},"date_updated":"2024-11-12T09:51:31Z","title":"Sloan digital sky survey: Early data release","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"1","day":"01","scopus_import":"1","_id":"17799","extern":"1","date_created":"2024-09-06T10:32:06Z","publication_status":"published","related_material":{"link":[{"relation":"erratum","url":"https://doi.org/10.1086/340314"}]},"author":[{"first_name":"Chris","last_name":"Stoughton","full_name":"Stoughton, Chris"},{"full_name":"Lupton, Robert H.","last_name":"Lupton","first_name":"Robert H."},{"last_name":"Bernardi","first_name":"Mariangela","full_name":"Bernardi, Mariangela"},{"full_name":"Blanton, Michael R.","first_name":"Michael R.","last_name":"Blanton"},{"full_name":"Burles, Scott","first_name":"Scott","last_name":"Burles"},{"full_name":"Castander, Francisco J.","last_name":"Castander","first_name":"Francisco J."},{"last_name":"Connolly","first_name":"A. 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French","last_name":"Leger"},{"first_name":"Siriluk","last_name":"Limmongkol","full_name":"Limmongkol, Siriluk"},{"full_name":"Lindenmeyer, Carl","last_name":"Lindenmeyer","first_name":"Carl"},{"full_name":"Long, Daniel C.","last_name":"Long","first_name":"Daniel C."},{"full_name":"Loomis, Craig","first_name":"Craig","last_name":"Loomis"},{"full_name":"Loveday, Jon","first_name":"Jon","last_name":"Loveday"},{"full_name":"MacKinnon, Bryan","first_name":"Bryan","last_name":"MacKinnon"},{"last_name":"Mannery","first_name":"Edward J.","full_name":"Mannery, Edward J."},{"first_name":"P. M.","last_name":"Mantsch","full_name":"Mantsch, P. M."},{"full_name":"Margon, Bruce","last_name":"Margon","first_name":"Bruce"},{"first_name":"Peregrine","last_name":"McGehee","full_name":"McGehee, Peregrine"},{"full_name":"McKay, Timothy A.","first_name":"Timothy A.","last_name":"McKay"},{"last_name":"McLean","first_name":"Brian","full_name":"McLean, Brian"},{"full_name":"Menou, Kristen","first_name":"Kristen","last_name":"Menou"},{"first_name":"Aronne","last_name":"Merelli","full_name":"Merelli, Aronne"},{"first_name":"H. J.","last_name":"Mo","full_name":"Mo, H. J."},{"full_name":"Monet, David G.","first_name":"David G.","last_name":"Monet"},{"full_name":"Nakamura, Osamu","first_name":"Osamu","last_name":"Nakamura"},{"full_name":"Narayanan, Vijay K.","last_name":"Narayanan","first_name":"Vijay K."},{"first_name":"Thomas","last_name":"Nash","full_name":"Nash, Thomas"},{"full_name":"Neilsen, Jr., Eric H.","first_name":"Eric H.","last_name":"Neilsen, Jr."},{"first_name":"Peter R.","last_name":"Newman","full_name":"Newman, Peter R."},{"last_name":"Nitta","first_name":"Atsuko","full_name":"Nitta, Atsuko"},{"first_name":"Michael","last_name":"Odenkirchen","full_name":"Odenkirchen, Michael"},{"full_name":"Okada, Norio","last_name":"Okada","first_name":"Norio"},{"full_name":"Okamura, Sadanori","last_name":"Okamura","first_name":"Sadanori"},{"full_name":"Ostriker, Jeremiah P.","last_name":"Ostriker","first_name":"Jeremiah P."},{"first_name":"Russell","last_name":"Owen","full_name":"Owen, Russell"},{"first_name":"A. George","last_name":"Pauls","full_name":"Pauls, A. George"},{"last_name":"Peoples","first_name":"John","full_name":"Peoples, John"},{"full_name":"Peterson, R. S.","last_name":"Peterson","first_name":"R. S."},{"full_name":"Petravick, Donald","last_name":"Petravick","first_name":"Donald"},{"full_name":"Pope, Adrian","first_name":"Adrian","last_name":"Pope"},{"full_name":"Pordes, Ruth","last_name":"Pordes","first_name":"Ruth"},{"last_name":"Postman","first_name":"Marc","full_name":"Postman, Marc"},{"full_name":"Prosapio, Angela","last_name":"Prosapio","first_name":"Angela"},{"first_name":"Thomas R.","last_name":"Quinn","full_name":"Quinn, Thomas R."},{"last_name":"Rechenmacher","first_name":"Ron","full_name":"Rechenmacher, Ron"},{"first_name":"Claudio H.","last_name":"Rivetta","full_name":"Rivetta, Claudio H."},{"last_name":"Rix","first_name":"Hans-Walter","full_name":"Rix, Hans-Walter"},{"first_name":"Constance M.","last_name":"Rockosi","full_name":"Rockosi, Constance M."},{"last_name":"Rosner","first_name":"Robert","full_name":"Rosner, Robert"},{"full_name":"Ruthmansdorfer, Kurt","last_name":"Ruthmansdorfer","first_name":"Kurt"},{"full_name":"Sandford, Dale","last_name":"Sandford","first_name":"Dale"},{"last_name":"Schneider","first_name":"Donald P.","full_name":"Schneider, Donald P."},{"full_name":"Scranton, Ryan","last_name":"Scranton","first_name":"Ryan"},{"first_name":"Maki","last_name":"Sekiguchi","full_name":"Sekiguchi, Maki"},{"last_name":"Sergey","first_name":"Gary","full_name":"Sergey, Gary"},{"full_name":"Sheth, Ravi","first_name":"Ravi","last_name":"Sheth"},{"first_name":"Kazuhiro","last_name":"Shimasaku","full_name":"Shimasaku, Kazuhiro"},{"first_name":"Stephen","last_name":"Smee","full_name":"Smee, Stephen"},{"full_name":"Snedden, Stephanie A.","last_name":"Snedden","first_name":"Stephanie A."},{"full_name":"Stebbins, Albert","first_name":"Albert","last_name":"Stebbins"},{"first_name":"Christopher","last_name":"Stubbs","full_name":"Stubbs, Christopher"},{"full_name":"Szapudi, István","first_name":"István","last_name":"Szapudi"},{"first_name":"Paula","last_name":"Szkody","full_name":"Szkody, Paula"},{"first_name":"Gyula P.","last_name":"Szokoly","full_name":"Szokoly, Gyula P."},{"first_name":"Serge","last_name":"Tabachnik","full_name":"Tabachnik, Serge"},{"full_name":"Tsvetanov, Zlatan","last_name":"Tsvetanov","first_name":"Zlatan"},{"full_name":"Uomoto, Alan","last_name":"Uomoto","first_name":"Alan"},{"first_name":"Michael S.","last_name":"Vogeley","full_name":"Vogeley, Michael S."},{"full_name":"Voges, Wolfgang","first_name":"Wolfgang","last_name":"Voges"},{"full_name":"Waddell, Patrick","last_name":"Waddell","first_name":"Patrick"},{"first_name":"René","last_name":"Walterbos","full_name":"Walterbos, René"},{"full_name":"Wang, Shu-i","first_name":"Shu-i","last_name":"Wang"},{"full_name":"Watanabe, Masaru","first_name":"Masaru","last_name":"Watanabe"},{"last_name":"Weinberg","first_name":"David H.","full_name":"Weinberg, David H."},{"last_name":"White","first_name":"Richard L.","full_name":"White, Richard L."},{"full_name":"White, Simon D. M.","last_name":"White","first_name":"Simon D. M."},{"last_name":"Wilhite","first_name":"Brian","full_name":"Wilhite, Brian"},{"full_name":"Wolfe, David","last_name":"Wolfe","first_name":"David"},{"first_name":"Naoki","last_name":"Yasuda","full_name":"Yasuda, Naoki"},{"first_name":"Donald G.","last_name":"York","full_name":"York, Donald G."},{"full_name":"Zehavi, Idit","first_name":"Idit","last_name":"Zehavi"},{"first_name":"Wei","last_name":"Zheng","full_name":"Zheng, Wei"}],"type":"journal_article","month":"01","page":"485-548","status":"public","abstract":[{"text":"The Sloan Digital Sky Survey (SDSS) is an imaging and spectroscopic survey that will eventually cover approximately one-quarter of the celestial sphere and collect spectra of ≈106 galaxies, 100,000 quasars, 30,000 stars, and 30,000 serendipity targets. In 2001 June, the SDSS released to the general astronomical community its early data release, roughly 462 deg2 of imaging data including almost 14 million detected objects and 54,008 follow-up spectra. The imaging data were collected in drift-scan mode in five bandpasses (u, g, r, i, and z); our 95% completeness limits for stars are 22.0, 22.2, 22.2, 21.3, and 20.5, respectively. The photometric calibration is reproducible to 5%, 3%, 3%, 3%, and 5%, respectively. The spectra are flux- and wavelength-calibrated, with 4096 pixels from 3800 to 9200 Å at R ≈ 1800. We present the means by which these data are distributed to the astronomical community, descriptions of the hardware used to obtain the data, the software used for processing the data, the measured quantities for each observed object, and an overview of the properties of this data set.","lang":"eng"}],"publisher":"American Astronomical Society","article_processing_charge":"No","language":[{"iso":"eng"}],"volume":123,"publication":"The Astronomical Journal","date_published":"2002-01-01T00:00:00Z","intvolume":"       123","OA_type":"free access","year":"2002","oa_version":"None","article_type":"original","publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"doi":"10.1086/324741","quality_controlled":"1"},{"year":"2001","oa_version":"Preprint","article_type":"original","publication_identifier":{"issn":["0004-6256"]},"quality_controlled":"1","doi":"10.1086/324111","abstract":[{"lang":"eng","text":"We present the results from a survey of i-dropout objects selected from ∼1550 deg^2 of multicolor imaging data from the Sloan Digital Sky Survey to search for luminous quasars at z ≳ 5.8. Objects with i*-z* > 2.2 and z* < 20.2 are selected, and follow-up J-band photometry is used to separate L- and T-type cool dwarfs from high-redshift quasars. We describe the discovery of three new quasars, SDSSp J083643.85+005453.3 (z = 5.82), J130608.26+035626.3 (z = 5.99), and J103027.10+052455.0 (z = 6.28). The quasar SDSSp J083643.85+005453.3 is a radio source with flux of 1.1 mJy at 20 cm. The spectra of all three quasars show strong and broad Lyα + N V emission lines and very strong Lyα forest absorption, with a mean continuum decrement DA > 0.90. The ARC 3.5 m spectrum of SDSSp J103027.10+052455.0 shows that over a range of ∼300 Å immediately blueward of the Lyα emission, the average transmitted flux is only 0.003 ± 0.020 times that of the continuum level, consistent with zero flux over a ∼300 Å range of the Lyα forest region and suggesting a tentative detection of the complete Gunn-Peterson trough. The existence of strong metal lines in the quasar spectra suggests early metal enrichment in the quasar environment. The three new objects, together with the previously published z = 5.8 quasar SDSSp J104433.04-012502.2, form a complete color-selected flux-limited sample at z ≳ 5.8. We estimate the selection function of this sample, taking into account the estimated variations in the quasar spectral energy distribution, as well as observational photometric errors. We find that at z = 6, the comoving density of luminous quasars at M1450 < -26.8 (H0 = 50 km s-1 Mpc-1, Ω = 1) is 1.1 × 10-9 Mpc-3. This is a factor of ∼2 lower than that at z ∼ 5 and is consistent with an extrapolation of the observed quasar evolution at z < 5. Using the current sample, we discuss the constraint on the shape of the quasar luminosity function and the implications for the contribution of quasars to the ionizing background at z ∼ 6. The luminous quasars discussed in the paper have central black hole masses of several times 109 M⊙ by the Eddington argument, with likely dark halo masses on the order of 1013 M⊙. Their observed space density provides a sensitive test of models of quasar and galaxy formation at high redshift."}],"publisher":"American Astronomical Society","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/0108063"}],"language":[{"iso":"eng"}],"article_processing_charge":"No","publication":"The Astronomical Journal","date_published":"2001-12-01T00:00:00Z","volume":122,"OA_type":"green","intvolume":"       122","extern":"1","external_id":{"arxiv":["astro-ph/0108063"]},"date_created":"2024-09-06T11:57:53Z","publication_status":"published","author":[{"first_name":"Xiaohui","last_name":"Fan","full_name":"Fan, Xiaohui"},{"first_name":"Vijay K.","last_name":"Narayanan","full_name":"Narayanan, Vijay K."},{"last_name":"Lupton","first_name":"Robert H.","full_name":"Lupton, Robert H."},{"first_name":"Michael A.","last_name":"Strauss","full_name":"Strauss, Michael A."},{"first_name":"Gillian R.","last_name":"Knapp","full_name":"Knapp, Gillian R."},{"first_name":"Robert H.","last_name":"Becker","full_name":"Becker, Robert H."},{"first_name":"Richard L.","last_name":"White","full_name":"White, Richard L."},{"full_name":"Pentericci, Laura","last_name":"Pentericci","first_name":"Laura"},{"full_name":"Leggett, S. K.","last_name":"Leggett","first_name":"S. K."},{"first_name":"Zoltán","orcid":"0000-0003-3633-5403","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"last_name":"Gunn","first_name":"James E.","full_name":"Gunn, James E."},{"last_name":"Ivezić","first_name":"Željko","full_name":"Ivezić, Željko"},{"last_name":"Schneider","first_name":"Donald P.","full_name":"Schneider, Donald P."},{"last_name":"Anderson","first_name":"Scott F.","full_name":"Anderson, Scott F."},{"last_name":"Brinkmann","first_name":"J.","full_name":"Brinkmann, J."},{"first_name":"Neta A.","last_name":"Bahcall","full_name":"Bahcall, Neta A."},{"full_name":"Connolly, Andrew J.","first_name":"Andrew J.","last_name":"Connolly"},{"full_name":"Csabai, István","last_name":"Csabai","first_name":"István"},{"first_name":"Mamoru","last_name":"Doi","full_name":"Doi, Mamoru"},{"last_name":"Fukugita","first_name":"Masataka","full_name":"Fukugita, Masataka"},{"last_name":"Geballe","first_name":"Tom","full_name":"Geballe, Tom"},{"first_name":"Eva K.","last_name":"Grebel","full_name":"Grebel, Eva K."},{"full_name":"Harbeck, Daniel","first_name":"Daniel","last_name":"Harbeck"},{"first_name":"Gregory","last_name":"Hennessy","full_name":"Hennessy, Gregory"},{"last_name":"Lamb","first_name":"Don Q.","full_name":"Lamb, Don Q."},{"last_name":"Miknaitis","first_name":"Gajus","full_name":"Miknaitis, Gajus"},{"full_name":"Munn, Jeffrey A.","last_name":"Munn","first_name":"Jeffrey A."},{"first_name":"Robert","last_name":"Nichol","full_name":"Nichol, Robert"},{"full_name":"Okamura, Sadanori","first_name":"Sadanori","last_name":"Okamura"},{"first_name":"Jeffrey R.","last_name":"Pier","full_name":"Pier, Jeffrey R."},{"full_name":"Prada, Francisco","first_name":"Francisco","last_name":"Prada"},{"full_name":"Richards, Gordon T.","first_name":"Gordon T.","last_name":"Richards"},{"first_name":"Alex","last_name":"Szalay","full_name":"Szalay, Alex"},{"full_name":"York, Donald G.","last_name":"York","first_name":"Donald G."}],"page":"2833-2849","month":"12","type":"journal_article","status":"public","oa":1,"citation":{"ista":"Fan X, Narayanan VK, Lupton RH, Strauss MA, Knapp GR, Becker RH, White RL, Pentericci L, Leggett SK, Haiman Z, Gunn JE, Ivezić Ž, Schneider DP, Anderson SF, Brinkmann J, Bahcall NA, Connolly AJ, Csabai I, Doi M, Fukugita M, Geballe T, Grebel EK, Harbeck D, Hennessy G, Lamb DQ, Miknaitis G, Munn JA, Nichol R, Okamura S, Pier JR, Prada F, Richards GT, Szalay A, York DG. 2001. A survey of z &#62; 5.8 quasars in the sloan digital sky survey. I. Discovery of three new quasars and the spatial density of luminous quasars at z ∼ 6. The Astronomical Journal. 122(6), 2833–2849.","short":"X. Fan, V.K. Narayanan, R.H. Lupton, M.A. Strauss, G.R. Knapp, R.H. Becker, R.L. White, L. Pentericci, S.K. Leggett, Z. Haiman, J.E. Gunn, Ž. Ivezić, D.P. Schneider, S.F. Anderson, J. Brinkmann, N.A. Bahcall, A.J. Connolly, I. Csabai, M. Doi, M. Fukugita, T. Geballe, E.K. Grebel, D. Harbeck, G. Hennessy, D.Q. Lamb, G. Miknaitis, J.A. Munn, R. Nichol, S. Okamura, J.R. Pier, F. Prada, G.T. Richards, A. Szalay, D.G. York, The Astronomical Journal 122 (2001) 2833–2849.","ieee":"X. Fan <i>et al.</i>, “A survey of z &#62; 5.8 quasars in the sloan digital sky survey. I. Discovery of three new quasars and the spatial density of luminous quasars at z ∼ 6,” <i>The Astronomical Journal</i>, vol. 122, no. 6. American Astronomical Society, pp. 2833–2849, 2001.","mla":"Fan, Xiaohui, et al. “A Survey of z &#62; 5.8 Quasars in the Sloan Digital Sky Survey. I. Discovery of Three New Quasars and the Spatial Density of Luminous Quasars at z ∼ 6.” <i>The Astronomical Journal</i>, vol. 122, no. 6, American Astronomical Society, 2001, pp. 2833–49, doi:<a href=\"https://doi.org/10.1086/324111\">10.1086/324111</a>.","apa":"Fan, X., Narayanan, V. K., Lupton, R. H., Strauss, M. A., Knapp, G. R., Becker, R. H., … York, D. G. (2001). A survey of z &#62; 5.8 quasars in the sloan digital sky survey. I. Discovery of three new quasars and the spatial density of luminous quasars at z ∼ 6. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/324111\">https://doi.org/10.1086/324111</a>","ama":"Fan X, Narayanan VK, Lupton RH, et al. A survey of z &#62; 5.8 quasars in the sloan digital sky survey. I. Discovery of three new quasars and the spatial density of luminous quasars at z ∼ 6. <i>The Astronomical Journal</i>. 2001;122(6):2833-2849. doi:<a href=\"https://doi.org/10.1086/324111\">10.1086/324111</a>","chicago":"Fan, Xiaohui, Vijay K. Narayanan, Robert H. Lupton, Michael A. Strauss, Gillian R. Knapp, Robert H. Becker, Richard L. White, et al. “A Survey of z &#62; 5.8 Quasars in the Sloan Digital Sky Survey. I. Discovery of Three New Quasars and the Spatial Density of Luminous Quasars at z ∼ 6.” <i>The Astronomical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/324111\">https://doi.org/10.1086/324111</a>."},"date_updated":"2024-11-12T12:51:42Z","arxiv":1,"title":"A survey of z > 5.8 quasars in the sloan digital sky survey. I. Discovery of three new quasars and the spatial density of luminous quasars at z ∼ 6","OA_place":"repository","issue":"6","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","scopus_import":"1","_id":"17825"},{"arxiv":1,"title":"The Discovery of a Luminous z = 5.80 Quasar from the Sloan Digital Sky Survey","OA_place":"repository","citation":{"ieee":"X. Fan <i>et al.</i>, “The Discovery of a Luminous z = 5.80 Quasar from the Sloan Digital Sky Survey,” <i>The Astronomical Journal</i>, vol. 120, no. 3. American Astronomical Society, pp. 1167–1174, 2000.","mla":"Fan, Xiaohui, et al. “The Discovery of a Luminous z = 5.80 Quasar from the Sloan Digital Sky Survey.” <i>The Astronomical Journal</i>, vol. 120, no. 3, American Astronomical Society, 2000, pp. 1167–74, doi:<a href=\"https://doi.org/10.1086/301534\">10.1086/301534</a>.","short":"X. Fan, R.L. White, M. Davis, R.H. Becker, M.A. Strauss, Z. Haiman, D.P. Schneider, M.D. Gregg, J.E. Gunn, G.R. Knapp, R.H. Lupton, J.E. Anderson, Jr., S.F. Anderson, J. Annis, N.A. Bahcall, W.N. Boroski, R.J. Brunner, B. Chen, A.J. Connolly, I. Csabai, M. Doi, M. Fukugita, G.S. Hennessy, R.B. Hindsley, T. Ichikawa, Ž. Ivezić, J. Loveday, A. Meiksin, T.A. McKay, J.A. Munn, H.J. Newberg, R. Nichol, S. Okamura, J.R. Pier, M. Sekiguchi, K. Shimasaku, C. Stoughton, A.S. Szalay, G.P. Szokoly, A.R. Thakar, M.S. Vogeley, D.G. York, The Astronomical Journal 120 (2000) 1167–1174.","ista":"Fan X, White RL, Davis M, Becker RH, Strauss MA, Haiman Z, Schneider DP, Gregg MD, Gunn JE, Knapp GR, Lupton RH, Anderson, Jr. JE, Anderson SF, Annis J, Bahcall NA, Boroski WN, Brunner RJ, Chen B, Connolly AJ, Csabai I, Doi M, Fukugita M, Hennessy GS, Hindsley RB, Ichikawa T, Ivezić Ž, Loveday J, Meiksin A, McKay TA, Munn JA, Newberg HJ, Nichol R, Okamura S, Pier JR, Sekiguchi M, Shimasaku K, Stoughton C, Szalay AS, Szokoly GP, Thakar AR, Vogeley MS, York DG. 2000. The Discovery of a Luminous z = 5.80 Quasar from the Sloan Digital Sky Survey. The Astronomical Journal. 120(3), 1167–1174.","chicago":"Fan, Xiaohui, Richard L. White, Marc Davis, Robert H. Becker, Michael A. Strauss, Zoltán Haiman, Donald P. Schneider, et al. “The Discovery of a Luminous z = 5.80 Quasar from the Sloan Digital Sky Survey.” <i>The Astronomical Journal</i>. American Astronomical Society, 2000. <a href=\"https://doi.org/10.1086/301534\">https://doi.org/10.1086/301534</a>.","ama":"Fan X, White RL, Davis M, et al. The Discovery of a Luminous z = 5.80 Quasar from the Sloan Digital Sky Survey. <i>The Astronomical Journal</i>. 2000;120(3):1167-1174. doi:<a href=\"https://doi.org/10.1086/301534\">10.1086/301534</a>","apa":"Fan, X., White, R. L., Davis, M., Becker, R. H., Strauss, M. A., Haiman, Z., … York, D. G. (2000). The Discovery of a Luminous z = 5.80 Quasar from the Sloan Digital Sky Survey. <i>The Astronomical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/301534\">https://doi.org/10.1086/301534</a>"},"oa":1,"date_updated":"2024-11-12T12:45:11Z","scopus_import":"1","_id":"17823","issue":"3","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","publication_status":"published","author":[{"full_name":"Fan, Xiaohui","last_name":"Fan","first_name":"Xiaohui"},{"first_name":"Richard L.","last_name":"White","full_name":"White, Richard L."},{"last_name":"Davis","first_name":"Marc","full_name":"Davis, Marc"},{"first_name":"Robert H.","last_name":"Becker","full_name":"Becker, Robert H."},{"first_name":"Michael A.","last_name":"Strauss","full_name":"Strauss, Michael A."},{"last_name":"Haiman","orcid":"0000-0003-3633-5403","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"first_name":"Donald P.","last_name":"Schneider","full_name":"Schneider, Donald P."},{"first_name":"Michael D.","last_name":"Gregg","full_name":"Gregg, Michael D."},{"last_name":"Gunn","first_name":"James E.","full_name":"Gunn, James E."},{"last_name":"Knapp","first_name":"G. R.","full_name":"Knapp, G. R."},{"full_name":"Lupton, Robert H.","last_name":"Lupton","first_name":"Robert H."},{"full_name":"Anderson, Jr., John E.","last_name":"Anderson, Jr.","first_name":"John E."},{"full_name":"Anderson, Scott F.","last_name":"Anderson","first_name":"Scott F."},{"full_name":"Annis, James","last_name":"Annis","first_name":"James"},{"first_name":"Neta A.","last_name":"Bahcall","full_name":"Bahcall, Neta A."},{"full_name":"Boroski, William N.","first_name":"William N.","last_name":"Boroski"},{"full_name":"Brunner, Robert J.","first_name":"Robert J.","last_name":"Brunner"},{"full_name":"Chen, Bing","last_name":"Chen","first_name":"Bing"},{"last_name":"Connolly","first_name":"Andrew J.","full_name":"Connolly, Andrew J."},{"last_name":"Csabai","first_name":"István","full_name":"Csabai, István"},{"full_name":"Doi, Mamoru","last_name":"Doi","first_name":"Mamoru"},{"first_name":"Masataka","last_name":"Fukugita","full_name":"Fukugita, Masataka"},{"last_name":"Hennessy","first_name":"G. S.","full_name":"Hennessy, G. S."},{"full_name":"Hindsley, Robert B.","last_name":"Hindsley","first_name":"Robert B."},{"first_name":"Takashi","last_name":"Ichikawa","full_name":"Ichikawa, Takashi"},{"full_name":"Ivezić, Željko","last_name":"Ivezić","first_name":"Željko"},{"full_name":"Loveday, Jon","last_name":"Loveday","first_name":"Jon"},{"last_name":"Meiksin","first_name":"Avery","full_name":"Meiksin, Avery"},{"last_name":"McKay","first_name":"Timothy A.","full_name":"McKay, Timothy A."},{"full_name":"Munn, Jeffrey A.","last_name":"Munn","first_name":"Jeffrey A."},{"first_name":"Heidi Jo","last_name":"Newberg","full_name":"Newberg, Heidi Jo"},{"first_name":"Robert","last_name":"Nichol","full_name":"Nichol, Robert"},{"last_name":"Okamura","first_name":"Sadanori","full_name":"Okamura, Sadanori"},{"first_name":"Jeffrey R.","last_name":"Pier","full_name":"Pier, Jeffrey R."},{"full_name":"Sekiguchi, Maki","first_name":"Maki","last_name":"Sekiguchi"},{"first_name":"Kazuhiro","last_name":"Shimasaku","full_name":"Shimasaku, Kazuhiro"},{"full_name":"Stoughton, Chris","last_name":"Stoughton","first_name":"Chris"},{"full_name":"Szalay, Alexander S.","first_name":"Alexander S.","last_name":"Szalay"},{"last_name":"Szokoly","first_name":"Gyula P.","full_name":"Szokoly, Gyula P."},{"first_name":"Aniruddha R.","last_name":"Thakar","full_name":"Thakar, Aniruddha R."},{"full_name":"Vogeley, Michael S.","last_name":"Vogeley","first_name":"Michael S."},{"first_name":"Donald G.","last_name":"York","full_name":"York, Donald G."}],"extern":"1","date_created":"2024-09-06T11:56:06Z","external_id":{"arxiv":["astro-ph/0005414"]},"status":"public","page":"1167-1174","month":"09","type":"journal_article","language":[{"iso":"eng"}],"article_processing_charge":"No","abstract":[{"text":"We present observations of SDSSp J104433.04-012502.2, a luminous quasar at z = 5.80 discovered from Sloan Digital Sky Survey (SDSS) multicolor imaging data. This object was selected as an i'-band dropout object, with i* = 21.8 ± 0.2 and z* = 19.2 ± 0.1. It has an absolute magnitude M1450 = -27.2 (H0 = 50 km s-1 Mpc-1, q0 = 0.5). The spectrum shows a strong and broad Lyα emission line, strong Lyα forest absorption lines with a mean continuum decrement DA = 0.91 and a Lyman limit system at z = 5.72. The spectrum also shows strong O I and Si IV emission lines similar to those of quasars at z ≲ 5, suggesting that these metals were produced at a redshift beyond 6. The lack of a Gunn-Peterson trough in the spectrum indicates that the universe is already highly ionized at z ∼ 5.8. Using a high-resolution spectrum in the Lyα forest region, we place a conservative upper limit on the optical depth because of the Gunn-Peterson effect of τ < 0.5 in regions of minimum absorption. The Lyα forest absorption in this object is much stronger than that in quasars at z ≲ 5. The object is unresolved in a deep image with excellent seeing, implying that it is unlensed. The black hole mass of this quasar is ∼3 × 109 M⊙ if we assume no lensing amplification and that it is radiating at the Eddington luminosity, implying that it resides in a very massive dark matter halo. The discovery of one quasar at M1450 < -27 in a survey area of 600 deg2 is consistent with an extrapolation of the observed luminosity function at lower redshifts. The abundance and evolution of such quasars can provide sensitive tests for models of quasar and galaxy formation.","lang":"eng"}],"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/0005414","open_access":"1"}],"publisher":"American Astronomical Society","date_published":"2000-09-01T00:00:00Z","publication":"The Astronomical Journal","volume":120,"OA_type":"green","intvolume":"       120","oa_version":"Preprint","article_type":"original","year":"2000","quality_controlled":"1","doi":"10.1086/301534","publication_identifier":{"issn":["0004-6256"]}}]