The Atacama Cosmology Telescope: Summary of DR4 and DR5 Data Products and Data Access

Creators: Mallaby-Kay, Maya; Atkins, Zachary; Aiola, Simone; Amodeo, Stefania; Austermann, Jason E.; Beall, James A.; Becker, Daniel T.; Bond, J. Richard; Calabrese, Erminia; Chesmore, Grace E.; Choi, Steve K.; Crowley, Kevin T.; Darwish, Omar; Denison, Edward V.; Devlin, Mark J.; Duff, Shannon M.; Duivenvoorden, Adriaan J.; Dunkley, Jo; Ferraro, Simone; Fichman, Kyra; Gallardo, Patricio A.; Golec, Joseph E.; Guan, Yilun; Han, Dongwon; Hasselfield, Matthew; Hill, J. Colin; Hilton, Gene C.; Hilton, Matt; Hložek, Renée; Hubmayr, Johannes; Huffenberger, Kevin M.; Hughes, John P.; Koopman, Brian J.; Louis, Thibaut; MacInnis, Amanda; Madhavacheril, Mathew S.; McMahon, Jeff; Moodley, Kavilan; Naess, Sigurd; Namikawa, Toshiya; Nati, Federico; Newburgh, Laura B.; Nibarger, John P.; Niemack, Michael D.; Page, Lyman A.; Salatino, Maria; Schaan, Emmanuel; Schillaci, Alessandro; Sehgal, Neelima; Sherwin, Blake D.; Sifón, Cristóbal; Simon, Sara; Staggs, Suzanne T.; Storer, Emilie R.; Ullom, Joel N.; Van Engelen, Alexander; Van Lanen, Jeff; Vale, Leila R.; Wollack, Edward J.; Xu, Zhilei

Abstract

Two recent large data releases for the Atacama Cosmology Telescope (ACT), called DR4 and DR5, are available for public access. These data include temperature and polarization maps that cover nearly half the sky at arcminute resolution in three frequency bands; lensing maps and component-separated maps covering ~2100 deg² of sky; derived power spectra and cosmological likelihoods; a catalog of over 4000 galaxy clusters; and supporting ancillary products including beam functions and masks. The data and products are described in a suite of ACT papers; here we provide a summary. In order to facilitate ease of access to these data, we present a set of Jupyter IPython notebooks developed to introduce users to DR4, DR5, and the tools needed to analyze these data. The data products (excluding simulations) and the set of notebooks are publicly available on the NASA Legacy Archive for Microwave Background Data Analysis; simulation products are available on the National Energy Research Scientific Computing Center.

Additional Information

© 2021. The American Astronomical Society. Received 2021 March 5; revised 2021 April 15; accepted 2021 April 27; published 2021 July 5. This work was supported by the U.S. National Science Foundation through awards AST-0408698, AST-0965625, and AST-1440226 for the ACT project, as well as awards PHY-0355328, PHY-0855887, and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astrońomico Atacama in northern Chile under the auspices of the Comisi on Nacionalde Investigacíon (CONICYT). The development of multichroic detectors and lenses was supported by NASA grants NNX13AE56G and NNX14AB58G. Detector research at NIST was supported by the NIST Innovations in Measurement Science program. Computations were performed on Cori at NERSC as part of the CMB Community allocation, on the Niagara supercomputer at the SciNet HPC Consortium, and on Feynman and Tiger at Princeton Research Computing. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund-Research Excellence, and the University of Toronto. M.M.K. is supported by the NSF Graduate Research Fellowship under grant No. DGE-1256260. D.H., A.M., and N.S. acknowledge support from NSF grant Nos. AST-1513618 and AST-1907657. E.C. acknowledges support from the STFC Ernest Rutherford Fellowship ST/M004856/2 and STFC Consolidated grant ST/S00033X/1, and from the Horizon 2020 ERC Starting grant (No. 849169). K.M. acknowledges support from the National Research Foundation of South Africa. Z.X. acknowledges support from the Gordon and Betty Moore Foundation. Z.L., E.S., and J.D. are supported through NSF grant AST-1814971. We gratefully acknowledge the publicly available software packages that were instrumental for this work. These packages include HEALPix (Gorski et al. 2005) and the python wrapper for HEALPix, which is healpy (Zonca et al. 2019). We also made use of Astropy, 69 a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013, 2018), libsharp (Reinecke & Seljebotn 2013), and the matplotlib (Hunter 2007) package. We used pixell 70 as well as pyactlike. 71 We also relied on CAMB (Lewis et al. 2000) as well as getdist (Lewis 2019). For power spectra examples, we used NaWrapper 72 , which is a wrapper for NaMaster (Alonso et al. 2019). 73 The packages numpy (Oliphant 2006; van der Walt et al. 2011; Harris et al. 2020), pandas (McKinney 2010; pandas development team 2020), and scipy (Virtanen et al. 2020) were also used throughout this work. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA), part of the High Energy Astrophysics Science Archive Center (HEASARC). HEASARC/LAMBDA is a service of the Astrophysics Science Division at the NASA Goddard Space Flight Center. We also acknowledge the use of the National Energy Research Scientific Computing Center (NERSC) for hosting the ACT data, and the use of GitHub for hosting our repositories.

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