摘要
The Event Horizon Telescope (EHT) observed the compact radio source, Sagittarius A* (Sgr A*), in the Galactic Center on 2017 April 5-11 in the 1.3 mm wavelength band. At the same time, interferometric array data from the Atacama Large Millimeter/submillimeter Array and the Submillimeter Array were collected, providing Sgr A* light curves simultaneous with the EHT observations. These data sets, complementing the EHT very long baseline interferometry, are characterized by a cadence and signal-to-noise ratio previously unattainable for Sgr A* at millimeter wavelengths, and they allow for the investigation of source variability on timescales as short as a minute. While most of the light curves correspond to a low variability state of Sgr A*, the April 11 observations follow an X-ray flare and exhibit strongly enhanced variability. All of the light curves are consistent with a red-noise process, with a power spectral density (PSD) slope measured to be between -2 and -3 on timescales between 1 minute and several hours. Our results indicate a steepening of the PSD slope for timescales shorter than 0.3 hr. The spectral energy distribution is flat at 220 GHz, and there are no time lags between the 213 and 229 GHz frequency bands, suggesting low optical depth for the event horizon scale source. We characterize Sgr A*'s variability, highlighting the different behavior observed just after the X-ray flare, and use Gaussian process modeling to extract a decorrelation timescale and a PSD slope. We also investigate the systematic calibration uncertainties by analyzing data from independent data reduction pipelines.
| 原文 | 英語 |
|---|---|
| 文章編號 | L19 |
| 期刊 | Astrophysical Journal Letters |
| 卷 | 930 |
| 發行號 | 2 |
| DOIs | |
| 出版狀態 | 已發佈 - 2022 5月 1 |
ASJC Scopus subject areas
- 天文和天體物理學
- 空間與行星科學
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於: Astrophysical Journal Letters, 卷 930, 編號 2, L19, 01.05.2022.
研究成果: 雜誌貢獻 › 期刊論文 › 同行評審
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TY - JOUR
T1 - Millimeter Light Curves of Sagittarius A* Observed during the 2017 Event Horizon Telescope Campaign
AU - Wielgus, Maciek
AU - Marchili, Nicola
AU - Martí-Vidal, Iván
AU - Keating, Garrett K.
AU - Ramakrishnan, Venkatessh
AU - Tiede, Paul
AU - Fomalont, Ed
AU - Issaoun, Sara
AU - Neilsen, Joey
AU - Nowak, Michael A.
AU - Blackburn, Lindy
AU - Gammie, Charles F.
AU - Goddi, Ciriaco
AU - Haggard, Daryl
AU - Lee, Daeyoung
AU - Moscibrodzka, Monika
AU - Tetarenko, Alexandra J.
AU - Bower, Geoffrey C.
AU - Chan, Chi Kwan
AU - Chatterjee, Koushik
AU - Chesler, Paul M.
AU - Dexter, Jason
AU - Doeleman, Sheperd S.
AU - Georgiev, Boris
AU - Gurwell, Mark
AU - Johnson, Michael D.
AU - Marrone, Daniel P.
AU - Mus, Alejandro
AU - Psaltis, Dimitrios
AU - Ripperda, Bart
AU - Witzel, Gunther
AU - Akiyama, Kazunori
AU - Alberdi, Antxon
AU - Alef, Walter
AU - Algaba, Juan Carlos
AU - Anantua, Richard
AU - Asada, Keiichi
AU - Azulay, Rebecca
AU - Bach, Uwe
AU - Baczko, Anne Kathrin
AU - Ball, David
AU - Baloković, Mislav
AU - Barrett, John
AU - Bauböck, Michi
AU - Benson, Bradford A.
AU - Bintley, Dan
AU - Blundell, Raymond
AU - Boland, Wilfred
AU - Bouman, Katherine L.
AU - Boyce, Hope
AU - Bremer, Michael
AU - Brinkerink, Christiaan D.
AU - Brissenden, Roger
AU - Britzen, Silke
AU - Broderick, Avery E.
AU - Broguiere, Dominique
AU - Bronzwaer, Thomas
AU - Bustamante, Sandra
AU - Byun, Do Young
AU - Carlstrom, John E.
AU - Ceccobello, Chiara
AU - Chael, Andrew
AU - Chatterjee, Shami
AU - Chen, Ming Tang
AU - Chen, Yongjun
AU - Cho, Ilje
AU - Christian, Pierre
AU - Conroy, Nicholas S.
AU - Conway, John E.
AU - Cordes, James M.
AU - Crawford, Thomas M.
AU - Crew, Geoffrey B.
AU - Cruz-Osorio, Alejandro
AU - Cui, Yuzhu
AU - Davelaar, Jordy
AU - De Laurentis, Mariafelicia
AU - Deane, Roger
AU - Dempsey, Jessica
AU - Desvignes, Gregory
AU - Dhruv, Vedant
AU - Dzib, Sergio A.
AU - Eatough, Ralph P.
AU - Emami, Razieh
AU - Falcke, Heino
AU - Farah, Joseph
AU - Fish, Vincent L.
AU - Ford, H. Alyson
AU - Fraga-Encinas, Raquel
AU - Freeman, William T.
AU - Friberg, Per
AU - Fromm, Christian M.
AU - Fuentes, Antonio
AU - Galison, Peter
AU - García, Roberto
AU - Gentaz, Olivier
AU - Gold, Roman
AU - Gómez-Ruiz, Arturo I.
AU - Gómez, José L.
AU - Gu, Minfeng
AU - Hada, Kazuhiro
AU - Haworth, Kari
AU - Hecht, Michael H.
AU - Hesper, Ronald
AU - Ho, Luis C.
AU - Ho, Paul
AU - Honma, Mareki
AU - Huang, Chih Wei L.
AU - Huang, Lei
AU - Hughes, David H.
AU - Ikeda, Shiro
AU - Impellizzeri, C. M.Violette
AU - Inoue, Makoto
AU - James, David J.
AU - Jannuzi, Buell T.
AU - Janssen, Michael
AU - Jeter, Britton
AU - Jiang, Wu
AU - Jiménez-Rosales, Alejandra
AU - Jorstad, Svetlana
AU - Joshi, Abhishek V.
AU - Jung, Taehyun
AU - Karami, Mansour
AU - Karuppusamy, Ramesh
AU - Kawashima, Tomohisa
AU - Kettenis, Mark
AU - Kim, Dong Jin
AU - Kim, Jae Young
AU - Kim, Jongsoo
AU - Kim, Junhan
AU - Kino, Motoki
AU - Koay, Jun Yi
AU - Kocherlakota, Prashant
AU - Kofuji, Yutaro
AU - Koch, Patrick M.
AU - Koyama, Shoko
AU - Kramer, Carsten
AU - Kramer, Michael
AU - Krichbaum, Thomas P.
AU - Kuo, Cheng Yu
AU - La Bella, Noemi
AU - Lauer, Tod R.
AU - Lee, Sang Sung
AU - Leung, Po Kin
AU - Levis, Aviad
AU - Li, Zhiyuan
AU - Lico, Rocco
AU - Lindahl, Greg
AU - Lindqvist, Michael
AU - Lisakov, Mikhail
AU - Liu, Jun
AU - Liu, Kuo
AU - Liuzzo, Elisabetta
AU - Lo, Wen Ping
AU - Lobanov, Andrei P.
AU - Loinard, Laurent
AU - Lonsdale, Colin
AU - Lu, Ru Sen
AU - Mao, Jirong
AU - Markoff, Sera
AU - Marscher, Alan P.
AU - Matsushita, Satoki
AU - Matthews, Lynn D.
AU - Medeiros, Lia
AU - Menten, Karl M.
AU - Michalik, Daniel
AU - Mizuno, Izumi
AU - Mizuno, Yosuke
AU - Moran, James M.
AU - Moriyama, Kotaro
AU - Müller, Cornelia
AU - Musoke, Gibwa
AU - Myserlis, Ioannis
AU - Nadolski, Andrew
AU - Nagai, Hiroshi
AU - Nagar, Neil M.
AU - Nakamura, Masanori
AU - Narayan, Ramesh
AU - Narayanan, Gopal
AU - Natarajan, Iniyan
AU - Nathanail, Antonios
AU - Fuentes, Santiago Navarro
AU - Neri, Roberto
AU - Ni, Chunchong
AU - Noutsos, Aristeidis
AU - Oh, Junghwan
AU - Okino, Hiroki
AU - Olivares, Héctor
AU - Ortiz-León, Gisela N.
AU - Oyama, Tomoaki
AU - Özel, Feryal
AU - Palumbo, Daniel C.M.
AU - Paraschos, Georgios Filippos
AU - Park, Jongho
AU - Parsons, Harriet
AU - Patel, Nimesh
AU - Pen, Ue Li
AU - Pesce, Dominic W.
AU - Piétu, Vincent
AU - Plambeck, Richard
AU - PopStefanija, Aleksandar
AU - Porth, Oliver
AU - Pötzl, Felix M.
AU - Prather, Ben
AU - Preciado-López, Jorge A.
AU - Pu, Hung Yi
AU - Rao, Ramprasad
AU - Rawlings, Mark G.
AU - Raymond, Alexander W.
AU - Rezzolla, Luciano
AU - Ricarte, Angelo
AU - Roelofs, Freek
AU - Rogers, Alan
AU - Ros, Eduardo
AU - Romero-Canizales, Cristina
AU - Roshanineshat, Arash
AU - Rottmann, Helge
AU - Roy, Alan L.
AU - Ruiz, Ignacio
AU - Ruszczyk, Chet
AU - Rygl, Kazi L.J.
AU - Sánchez, Salvador
AU - Sánchez-Argüelles, David
AU - Sánchez-Portal, Miguel
AU - Sasada, Mahito
AU - Satapathy, Kaushik
AU - Savolainen, Tuomas
AU - Schloerb, F. Peter
AU - Schuster, Karl Friedrich
AU - Shao, Lijing
AU - Shen, Zhiqiang
AU - Small, Des
AU - Sohn, Bong Won
AU - SooHoo, Jason
AU - Souccar, Kamal
AU - Sun, He
AU - Tazaki, Fumie
AU - Tilanus, Remo P.J.
AU - Titus, Michael
AU - Torne, Pablo
AU - Traianou, Efthalia
AU - Trent, Tyler
AU - Trippe, Sascha
AU - van Bemmel, Ilse
AU - van Langevelde, Huib Jan
AU - van Rossum, Daniel R.
AU - Vos, Jesse
AU - Wagner, Jan
AU - Ward-Thompson, Derek
AU - Wardle, John
AU - Weintroub, Jonathan
AU - Wex, Norbert
AU - Wharton, Robert
AU - Wiik, Kaj
AU - Wondrak, Michael F.
AU - Wong, George N.
AU - Wu, Qingwen
AU - Yamaguchi, Paul
AU - Yoon, Doosoo
AU - Young, André
AU - Yuan, Feng
AU - Young, Ken
AU - Younsi, Ziri
AU - Yuan, Ye Fei
AU - Zensus, J. Anton
AU - Zhang, Shuo
AU - Zhao, Guang Yao
AU - Zhao, Shan Shan
N1 - Publisher Copyright: © 2022. The Author(s)
PY - 2022/5/1
Y1 - 2022/5/1
N2 - The Event Horizon Telescope (EHT) observed the compact radio source, Sagittarius A* (Sgr A*), in the Galactic Center on 2017 April 5-11 in the 1.3 mm wavelength band. At the same time, interferometric array data from the Atacama Large Millimeter/submillimeter Array and the Submillimeter Array were collected, providing Sgr A* light curves simultaneous with the EHT observations. These data sets, complementing the EHT very long baseline interferometry, are characterized by a cadence and signal-to-noise ratio previously unattainable for Sgr A* at millimeter wavelengths, and they allow for the investigation of source variability on timescales as short as a minute. While most of the light curves correspond to a low variability state of Sgr A*, the April 11 observations follow an X-ray flare and exhibit strongly enhanced variability. All of the light curves are consistent with a red-noise process, with a power spectral density (PSD) slope measured to be between -2 and -3 on timescales between 1 minute and several hours. Our results indicate a steepening of the PSD slope for timescales shorter than 0.3 hr. The spectral energy distribution is flat at 220 GHz, and there are no time lags between the 213 and 229 GHz frequency bands, suggesting low optical depth for the event horizon scale source. We characterize Sgr A*'s variability, highlighting the different behavior observed just after the X-ray flare, and use Gaussian process modeling to extract a decorrelation timescale and a PSD slope. We also investigate the systematic calibration uncertainties by analyzing data from independent data reduction pipelines.
AB - The Event Horizon Telescope (EHT) observed the compact radio source, Sagittarius A* (Sgr A*), in the Galactic Center on 2017 April 5-11 in the 1.3 mm wavelength band. At the same time, interferometric array data from the Atacama Large Millimeter/submillimeter Array and the Submillimeter Array were collected, providing Sgr A* light curves simultaneous with the EHT observations. These data sets, complementing the EHT very long baseline interferometry, are characterized by a cadence and signal-to-noise ratio previously unattainable for Sgr A* at millimeter wavelengths, and they allow for the investigation of source variability on timescales as short as a minute. While most of the light curves correspond to a low variability state of Sgr A*, the April 11 observations follow an X-ray flare and exhibit strongly enhanced variability. All of the light curves are consistent with a red-noise process, with a power spectral density (PSD) slope measured to be between -2 and -3 on timescales between 1 minute and several hours. Our results indicate a steepening of the PSD slope for timescales shorter than 0.3 hr. The spectral energy distribution is flat at 220 GHz, and there are no time lags between the 213 and 229 GHz frequency bands, suggesting low optical depth for the event horizon scale source. We characterize Sgr A*'s variability, highlighting the different behavior observed just after the X-ray flare, and use Gaussian process modeling to extract a decorrelation timescale and a PSD slope. We also investigate the systematic calibration uncertainties by analyzing data from independent data reduction pipelines.
UR - http://www.scopus.com/inward/record.url?scp=85130735318&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85130735318&partnerID=8YFLogxK
U2 - 10.3847/2041-8213/ac6428
DO - 10.3847/2041-8213/ac6428
M3 - Article
AN - SCOPUS:85130735318
SN - 2041-8205
VL - 930
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 2
M1 - L19
ER -