TY - JOUR
T1 - The Atacama Cosmology Telescope
T2 - Detection of Millimeter-wave Transient Sources
AU - Naess, Sigurd
AU - Battaglia, Nick
AU - Richard Bond, J.
AU - Calabrese, Erminia
AU - Choi, Steve K.
AU - Cothard, Nicholas F.
AU - Devlin, Mark
AU - Duell, Cody J.
AU - Duivenvoorden, Adriaan J.
AU - Dunkley, Jo
AU - Dünner, Rolando
AU - Gallardo, Patricio A.
AU - Gralla, Megan
AU - Guan, Yilun
AU - Halpern, Mark
AU - Colin Hill, J.
AU - Hilton, Matt
AU - Huffenberger, Kevin M.
AU - Koopman, Brian J.
AU - Kosowsky, Arthur B.
AU - Madhavacheril, Mathew S.
AU - McMahon, Jeff
AU - Nati, Federico
AU - Niemack, Michael D.
AU - Page, Lyman
AU - Partridge, Bruce
AU - Salatino, Maria
AU - Sehgal, Neelima
AU - Spergel, David
AU - Staggs, Suzanne
AU - Wollack, Edward J.
AU - Xu, Zhilei
N1 - Funding Information:
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 U.B.C. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion (CONICYT). Computations were performed on the Niagara supercomputer at the SciNet HPC Consortium and on the Simons-Popeye cluster of the Flatiron Institute. 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. K.M.H. is supported by NSF through AST 1815887. E.C. acknowledges support from the STFC Ernest Rutherford Fellowship ST/M004856/2 and STFC Consolidated grant ST/S00033X/1, and from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 849169). S.K.C. acknowledges support from NSF award AST-2001866. Z.X. is supported by the Gordon and Betty Moore Foundation. N.S. acknowledges support from NSF grant No. AST-1907657
Publisher Copyright:
© 2021. The American Astronomical Society. All rights reserved.
PY - 2021/7/1
Y1 - 2021/7/1
N2 - We report on the serendipitous discovery of three transient millimeter-wave sources using data from the Atacama Cosmology Telescope. The first, detected at R.A. = 273.8138, decl. = -49.4628 at ∼50σ total, brightened from less than 5 mJy to at least 1100 mJy at 150 GHz with an unknown rise time shorter than 13 days, during which the increase from 250 mJy to 1100 mJy took only 8 minutes. Maximum flux was observed on 2019 November 8. The source's spectral index in flux between 90-150 GHz was positive, α = 1.5 ± 0.2. The second, detected at R.A. = 105.1584, decl. = -11.2434 at ∼20σ total, brightened from less than 20 mJy to at least 300 mJy at 150 GHz with an unknown rise time shorter than 8 days. Maximum flux was observed on 2019 December 15. Its spectral index was also positive, α = 1.8 ± 0.2. The third, detected at R.A. = 301.9952, decl. = 16.1652 at ∼40σ total, brightened from less than 8 mJy to at least 300 mJy at 150 GHz over a day or less but decayed over a few days. Maximum flux was observed on 2018 September 11. Its spectrum was approximately flat, with a spectral index of α = -0.2 ± 0.1. None of the sources were polarized to the limits of these measurements. The two rising-spectrum sources are coincident in position with M and K stars, while the third is coincident with a G star.
AB - We report on the serendipitous discovery of three transient millimeter-wave sources using data from the Atacama Cosmology Telescope. The first, detected at R.A. = 273.8138, decl. = -49.4628 at ∼50σ total, brightened from less than 5 mJy to at least 1100 mJy at 150 GHz with an unknown rise time shorter than 13 days, during which the increase from 250 mJy to 1100 mJy took only 8 minutes. Maximum flux was observed on 2019 November 8. The source's spectral index in flux between 90-150 GHz was positive, α = 1.5 ± 0.2. The second, detected at R.A. = 105.1584, decl. = -11.2434 at ∼20σ total, brightened from less than 20 mJy to at least 300 mJy at 150 GHz with an unknown rise time shorter than 8 days. Maximum flux was observed on 2019 December 15. Its spectral index was also positive, α = 1.8 ± 0.2. The third, detected at R.A. = 301.9952, decl. = 16.1652 at ∼40σ total, brightened from less than 8 mJy to at least 300 mJy at 150 GHz over a day or less but decayed over a few days. Maximum flux was observed on 2018 September 11. Its spectrum was approximately flat, with a spectral index of α = -0.2 ± 0.1. None of the sources were polarized to the limits of these measurements. The two rising-spectrum sources are coincident in position with M and K stars, while the third is coincident with a G star.
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U2 - 10.3847/1538-4357/abfe6d
DO - 10.3847/1538-4357/abfe6d
M3 - Article
AN - SCOPUS:85109850370
SN - 0004-637X
VL - 915
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 14
ER -