Search

With the volume and availability of astronomical data growing rapidly, astronomers will soon rely on the use of machine learning algorithms in their daily work. This proceeding aims to give an overview of what machine learning is and delve into the many different types of learning algorithms and examine two astronomical use cases. Machine learning has opened a world of possibilities for us astronomers working with large amounts of data, however if not careful, users can trip into common pitfalls. Here we'll focus on solving problems related to time-series light curve data and optical imaging data mainly from the Deeper, Wider, Faster Program (DWF). Alongside the written examples, online notebooks will be provided to demonstrate these different techniques. This guide aims to help you build a small toolkit of knowledge and tools to take back with you for use on your own future machine learning projects., Comment: 12 pages, 5 Figures, International Astronomical Union Proceedings Series 368

Full list of authors: Andreoni, Igor; Coughlin, Michael W.; Perley, Daniel A.; Yao, Yuhan; Lu, Wenbin; Cenko, S. Bradley; Kumar, Harsh; Anand, Shreya; Ho, Anna Y. Q.; Kasliwal, Mansi M.; de Ugarte Postigo, Antonio; Sagués-Carracedo, Ana; Schulze, Steve; Kann, D. Alexander; Kulkarni, S. R.; Sollerman, Jesper; Tanvir, Nial; Rest, Armin; Izzo, Luca; Somalwar, Jean J.; Kaplan, David L.; Ahumada, Tomás; Anupama, G. C.; Auchettl, Katie; Barway, Sudhanshu; Bellm, Eric C.; Bhalerao, Varun; Bloom, Joshua S.; Bremer, Michael; Bulla, Mattia; Burns, Eric; Campana, Sergio; Chandra, Poonam; Charalampopoulos, Panos; Cooke, Jeff; D'Elia, Valerio; Das, Kaustav Kashyap; Dobie, Dougal; Agüí Fernández, José Feliciano; Freeburn, James; Fremling, Cristoffer; Gezari, Suvi; Goode, Simon; Graham, Matthew J. ; Hammerstein, Erica; Karambelkar, Viraj R.; Kilpatrick, Charles D.; Kool, Erik C.; Krips, Melanie; Laher, Russ R.; Leloudas, Giorgos; Levan, Andrew; Lundquist, Michael J.; Mahabal, Ashish A.; Medford, Michael S.; Miller, M. Coleman; Möller, Anais; Mooley, Kunal P.; Nayana, A. J.; Nir, Guy; Pang, Peter T. H.; Paraskeva, Emmy; Perley, Richard A.; Petitpas, Glen; Pursiainen, Miika; Ravi, Vikram; Ridden-Harper, Ryan; Riddle, Reed; Rigault, Mickael; Rodriguez, Antonio C.; Rusholme, Ben; Sharma, Yashvi; Smith, I. A.; Stein, Robert D.; Thöne, Christina; Tohuvavohu, Aaron; Valdes, Frank; van Roestel, Jan; Vergani, Susanna D.; Wang, Qinan; Zhang, Jielai.--Correction to: Nature https://doi.org/10.1038/s41586-022-05465-8 Published online 30 November 2022., Tidal disruption events (TDEs) are bursts of electromagnetic energy that are released when supermassive black holes at the centres of galaxies violently disrupt a star that passes too close1. TDEs provide a window through which to study accretion onto supermassive black holes; in some rare cases, this accretion leads to launching of a relativistic jet2,3,4,5,6,7,8,9, but the necessary conditions are not fully understood. The best-studied jetted TDE so far is Swift J1644+57, which was discovered in γ-rays, but was too obscured by dust to be seen at optical wavelengths. Here we report the optical detection of AT2022cmc, a rapidly fading source at cosmological distance (redshift z = 1.19325) the unique light curve of which transitioned into a luminous plateau within days. Observations of a bright counterpart at other wavelengths, including X-ray, submillimetre and radio, supports the interpretation of AT2022cmc as a jetted TDE containing a synchrotron ‘afterglow’, probably launched by a supermassive black hole with spin greater than approximately 0.3. Using four years of Zwicky Transient Facility10 survey data, we calculate a rate of 0.02+0.04−0.01 Gpc−3 yr−1 for on-axis jetted TDEs on the basis of the luminous, fast-fading red component, thus providing a measurement complementary to the rates derived from X-ray and radio observations11. Correcting for the beaming angle effects, this rate confirms that approximately 1 per cent of TDEs have relativistic jets. Optical surveys can use AT2022cmc as a prototype to unveil a population of jetted TDEs. © 2022. The Author(s), under exclusive licence to Springer Nature Limited., M.W.C. acknowledges support from the National Science Foundation with grant numbers PHY-2010970 and OAC-2117997. E.C.K. acknowledges support from the G.R.E.A.T .research environment and the Wenner-Gren Foundations. M. Bulla acknowledges support from the Swedish Research Council (reg. no. 2020-03330). H.K. and T.A. thank the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant no. 1829740, the Brinson Foundation, and the Moore Foundation; their participation in the programme has benefited this work. W.L. was supported by the Lyman Spitzer, Jr. Fellowship at Princeton University. M.R. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 759194 - USNAC). G.L., P. Charalampopoulos and M.P. were supported by a research grant (19054) from VILLUM FONDEN. P.T.H.P. is supported by the research programme of the Netherlands Organization for Scientific Research (NWO). D.A.K. acknowledges support from Spanish National Research Project RTI2018-098104-J-I00 (GRBPhot). The material is based on work supported by NASA under award no. 80GSFC17M0002. A.J.N. acknowledges DST-INSPIRE Faculty Fellowship (IFA20-PH-259) for supporting this research. I.A. is a Neil Gehrels Fellow. This work has been supported by the research project grant ‘Understanding the Dynamic Universe’ funded by the Knut and Alice Wallenberg Foundation under Dnr KAW 2018.0067. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility (ZTF) project. ZTF is supported by the National Science Foundation under grant no. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington (UW), Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by Caltech Optical Observatories, IPAC, and UW. The work is partly based on the observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. We acknowledge all co-investigators of our GTC proposal. SED Machine is based on work supported by the National Science Foundation under grant no. 1106171. The ZTF forced-photometry service was funded under the Heising–Simons Foundation grant no. 12540303 (PI: M.J.G.). The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2013-2016) under grant agreement no. 312430 (OPTICON). Based on observations collected at the European Southern Observatory under ESO programme 106.21T6.015. This work made use of data from the GROWTH-India Telescope (GIT) set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB). It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia. Based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofísica de Canarias. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias with financial support from the UK Science and Technology Facilities Council. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Partly based on observations collected at Centro Astronómico Hispano en Andalucía (CAHA) at Calar Alto, operated jointly by Instituto de Astrofísica de Andalucía (CSIC) and Junta de Andalucía. The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Research Institute of Thailand and the Center for Astronomical Mega-Science (as well as the National Key R&D Program of China with no. 2017YFA0402700). Additional funding support is provided by the Science and Technology Facilities Council of the UK and participating universities and organizations in the UK and Canada. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. The JCMT data reported here were obtained under project M22AP030 (principal investigator D.A.P.). The Starlink software is currently supported by the East Asian Observatory. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This work is based on observations carried out under project number W21BK with the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Based on observations obtained at the international Gemini Observatory, a programme of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. On behalf of the Gemini Observatory partnership: the National Science Foundation (USA), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work was enabled by observations made from the Gemini North telescope, located within the Maunakea Science Reserve and adjacent to the summit of Maunakea., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.