The La Silla Schmidt Southern Survey
Adam A. Miller, Natasha S. Abrams, G. Aldering, Shreya Anand, C. R. Angus, I. Arcavi, C. Baltay, F. E. Bauer, Daniel Brethauer, J. S. Bloom, Hemanth Bommireddy, M. Catelan, R. Chornock, P. Clark, Thomas E. Collett, G. Dimitriadis, S. M. Faris, F. Förster, A. Franckowiak, C. Frohmaier, L. Galbany, R. B. Galleguillos Silva, A. Goobar, Or Graur, C. P. Gutiérrez, Saarah Hall, Erica Hammerstein, K. Herner, I. Hook, Macy Huston, J. Johansson, C. D. Kilpatrick, Alex Kim, R. A. Knop, M. Kowalski, Lindsey A. Kwok, Natalie LeBaron, Kenneth W. Lin, Chang Liu, Jessica R. Lu, Wenbin Lu, R. Lunnan, K. Maguire, L. Makrygianni, R. Margutti, Dan Maoz, Patrik Milán Veres, T. Moore, A. J. Nayana, M. Nicholl, J. Nordin, S. R. Oates, G. Pignata, Abigail Polin, D. Poznanski, J. L. Prieto, D. Rabinowitz, Nabeel Rehemtulla, M. Rigault, Dan Ryczanowski, Nikhil Sarin, S. Schulze, Ved G. Shah, Xinyue Sheng, Samuel P. R. Shilling, Brooke Simmons, Avinash Singh, G. P. Smith, M. Smith, J. Sollerman, Maayane T. Soumagnac, C. W. Stubbs, M. Sullivan, Aswin Suresh, Benny Trakhtenbrot, Charlotte Ward, Eli Wiston, Helen Xiong, Yuhan Yao, P. Nugent
Abstract
Abstract We present the La Silla Schmidt Southern Survey (LS4), a new wide-field, time-domain survey to be conducted with the 1 m ESO Schmidt telescope. The 268 megapixel LS4 camera mosaics 32 2k × 4k fully depleted CCDs, providing a ∼20 deg 2 field of view with 1 ″ pixel −1 resolution. The LS4 camera will have excellent performance at longer wavelengths: in a standard 45 s exposure the expected 5 σ limiting magnitudes in g , i , z are ∼21.5, ∼20.9, and ∼20.3 mag (AB), respectively. The telescope design requires a novel filter holder that fixes different bandpasses over each quadrant of the detector. Two quadrants will have i band, while the other two will be g and z band with color information obtained by dithering targets across the different quadrants. The majority (90%) of the observing time will be used to conduct a public survey that monitors the extragalactic sky at both moderate (3 days) and high (1 day) cadence, as well as focused observations within the Galactic plane and bulge. Alerts from the public survey will be broadcast to the community via established alert brokers. LS4 will run concurrently with the Vera C. Rubin Observatory’s Legacy Survey of Space and Time (LSST). The combination of LS4+LSST will enable detailed holistic monitoring of many nearby transients: high-cadence LS4 observations will resolve the initial rise and peak of the light curve while less-frequent but deeper observations by LSST will characterize the years before and after explosion. Here, we summarize the primary science objectives of LS4 including microlensing events in the Galaxy, extragalactic transients powered by massive black holes or stellar explosions, the search for electromagnetic counterparts to multi-messenger events, and supernova cosmology.