The BUFFALO HST Survey

Creators: Steinhardt, Charles L.; Jauzac, Mathilde; Acebron, Ana; Atek, Hakim; Capak, Peter; Davidzon, Iary; Eckert, Dominique; Harvey, David; Koekemoer, Anton M.; Lagos, Claudia D. P.; Mahler, Guillaume; Montes, Mireia; Niemiec, Anna; Nonino, Mario; Oesch, P. A.; Richard, Johan; Rodney, Steven A.; Schaller, Matthieu; Sharon, Keren; Strolger, Louis-Gregory; Allingham, Joseph; Amara, Adam; Bahé, Yannick; Bœhm, Céline; Bose, Sownak; Bouwens, Rychard J.; Bradley, Larry D.; Brammer, Gabriel; Broadhurst, Tom; Cañas, Rodrigo; Cen, Renyue; Clément, Benjamin; Clowe, Douglas; Coe, Dan; Connor, Thomas; Darvish, Behnam; Diego, Jose M.; Ebeling, Harald; Edge, A. C.; Egami, Eiichi; Ettori, Stefano; Faisst, Andreas L.; Frye, Brenda; Furtak, Lukas J.; Gómez-Guijarro, C.; Remolina González, J. D.; Gonzalez, Anthony; Graur, Or; Gruen, Daniel; Harvey, David; Hensley, Hagan; Hovis-Afflerbach, Beryl; Jablonka, Pascale; Jha, Saurabh W.; Jullo, Eric; Kneib, Jean-Paul; Kokorev, Vasily; Lagattuta, David J.; Limousin, Marceau; von der Linden, Anja; Linzer, Nora B.; Lopez, Adrian; Magdis, Georgios E.; Massey, Richard; Masters, Daniel C.; Maturi, Matteo; McCully, Curtis; McGee, Sean L.; Meneghetti, Massimo; Mobasher, Bahram; Moustakas, Leonidas A.; Murphy, Eric J.; Natarajan, Priyamvada; Neyrinck, Mark; O'Connor, Kyle; Oguri, Masamune; Pagul, Amanda; Rhodes, Jason; Rich, R. Michael; Robertson, Andrew; Sereno, Mauro; Shan, Huanyuan; Smith, Graham P.; Sneppen, Albert; Squires, Gordon K.; Tam, Sut-Ieng; Tchernin, Céline; Toft, Sune; Umetsu, Keiichi; Weaver, John R.; van Weeren, R. J.; Williams, Liliya L. R.; Wilson, Tom J.; Yan, Lin; Zitrin, Adi

Abstract

The Beyond Ultra-deep Frontier Fields and Legacy Observations (BUFFALO) is a 101 orbit + 101 parallel Cycle 25 Hubble Space Telescope (HST) Treasury program taking data from 2018 to 2020. BUFFALO will expand existing coverage of the Hubble Frontier Fields (HFF) in Wide Field Camera 3/IR F105W, F125W, and F160W and Advanced Camera for Surveys/WFC F606W and F814W around each of the six HFF clusters and flanking fields. This additional area has not been observed by HST but is already covered by deep multiwavelength data sets, including Spitzer and Chandra. As with the original HFF program, BUFFALO is designed to take advantage of gravitational lensing from massive clusters to simultaneously find high-redshift galaxies that would otherwise lie below HST detection limits and model foreground clusters to study the properties of dark matter and galaxy assembly. The expanded area will provide the first opportunity to study both cosmic variance at high redshift and galaxy assembly in the outskirts of the large HFF clusters. Five additional orbits are reserved for transient follow-up. BUFFALO data including mosaics, value-added catalogs, and cluster mass distribution models will be released via MAST on a regular basis as the observations and analysis are completed for the six individual clusters.

Additional Information

© 2020. The American Astronomical Society. Received 2019 November 9; revised 2019 December 23; accepted 2019 December 27; published 2020 April 3. C.S. acknowledges support from the ERC Consolidator Grant funding scheme (project ConTExT, grant No. 648179). The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. M.J. is supported by the United Kingdom Research and Innovation (UKRI) Future Leaders Fellowship "Using Cosmic Beasts to uncover the Nature of Dark Matter" (grant No. MR/S017216/1). This project was also supported by the Science and Technology Facilities Council (grant No. ST/L00075X/1). J.A. is supported by the Postgraduate Research Scholarship in Astroparticle Physics/Cosmology at the University of Sydney. A.A. acknowledges the support of the Royal Society through the Wolfson Fellowship program. Y.M.B. acknowledges funding from the EU Horizon 2020 research and innovation program under Marie Skłodowska-Curie grant agreement 747645 (ClusterGal) and the Netherlands Organisation for Scientific Research (NWO) through VENI grant 016.183.011. R.J.B. gratefully acknowledges the support of TOP grant TOP1.16.057. R.C. is supported by the MERAC foundation postdoctoral grant awarded to C.L. and by the Consejo Nacional de Ciencia y Tecnología CONACYT CVU 520137 Scholar 290609 Overseas Scholarship 438594. The work of T.C. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant No. NNX12AE20G, and the National Science Foundation, grant No. 1716907. J.M.D. acknowledges the support of project PGC2018-101814-B-100 (MCIU/AEI/MINECO/FEDER, UE), Ministerio de Ciencia, Investigación y Universidades. A.C.E. acknowledges support from STFC grant ST/P00541/1. S.E. acknowledges a financial contribution from the contracts ASI 2015-046-R.0 and ASI-INAF n.2017-14-H.0 and INAF "Call per interventi aggiuntivi a sostegno della ricerca di main stream di INAF." O.G. is supported by an NSF Astronomy and Astrophysics Fellowship under award AST-1602595. D.H. acknowledges the support by the Delta ITP foundation. E.J. acknowledges AMU, CNRS, and CNES for their support. C.D.P.L. is funded by the ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) through project number CE170100013. M.L. acknowledges CNRS and CNES for support. G.E.M. acknowledges support from the Villum Fonden research grant 13160 "Gas to stars, stars to dust: tracing star formation across cosmic time." The work of L.A.M. took place at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. J.R. was supported by JPL, which is run under a contract for NASA by Caltech. R.M.R. acknowledges support from HST-GO-15117.005. M.S. is supported by the Netherlands Organization for Scientific Research (NWO) VENI grant 639.041.749 H.Y.S. acknowledges support from the NSFC of China under grant 11973070 and the Shanghai Committee of Science and Technology grant No. 19ZR1466600. G.P.S. acknowledges financial support from STFC grant No. ST/N000633/1. C.T. acknowledges the support of the Deutsche Forschungsgemeinschaft under BA 1369/28-1 S.T. acknowledges support from the ERC Consolidator Grant funding scheme (project ConTExT, grant No. 648179). The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. K.U. was supported by the Ministry of Science and Technology of Taiwan (grant MOST 106-2628-M-001-003-MY3) and the Academia Sinica Investigator Award (grant AS-IA-107-M01). R.J.v.W. acknowledges support from the VIDI research program with project No. 639.042.729, which is financed by the Netherlands Organisation for Scientific Research (NWO). This work has made use of the CANDIDE Cluster at the Institut d'Astrophysique de Paris and made possible by grants from the PNCG and the DIM-ACAV.

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