Abstract
In 2017 the Event Horizon Telescope (EHT) observed the supermassive black hole at the center of the Milky Way, Sagittarius A* (Sgr A*), at a frequency of 228.1 GHz (λ = 1.3 mm). The fundamental physics tests that even a single pulsar orbiting Sgr A* would enable motivate searching for pulsars in EHT data sets. The high observing frequency means that pulsars—which typically exhibit steep emission spectra—are expected to be very faint. However, it also negates pulse scattering, an effect that could hinder pulsar detections in the Galactic center. Additionally, magnetars or a secondary inverse Compton emission could be stronger at millimeter wavelengths than at lower frequencies. We present a search for pulsars close to Sgr A* using the data from the three most sensitive stations in the EHT 2017 campaign: the Atacama Large Millimeter/submillimeter Array, the Large Millimeter Telescope, and the IRAM 30 m Telescope. We apply three detection methods based on Fourier-domain analysis, the fast folding algorithm, and single-pulse searches targeting both pulsars and burst-like transient emission. We use the simultaneity of the observations to confirm potential candidates. No new pulsars or significant bursts were found. Being the first pulsar search ever carried out at such high radio frequencies, we detail our analysis methods and give a detailed estimation of the sensitivity of the search. We conclude that the EHT 2017 observations are only sensitive to a small fraction (≲2.2%) of the pulsars that may exist close to Sgr A*, motivating further searches for fainter pulsars in the region.
Original language | English (US) |
---|---|
Article number | 14 |
Journal | Astrophysical Journal |
Volume | 959 |
Issue number | 1 |
DOIs | |
State | Published - Dec 1 2023 |
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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In: Astrophysical Journal, Vol. 959, No. 1, 14, 01.12.2023.
Research output: Contribution to journal › Article › peer-review
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TY - JOUR
T1 - A Search for Pulsars around Sgr A* in the First Event Horizon Telescope Data Set
AU - Torne, Pablo
AU - Liu, Kuo
AU - Eatough, Ralph P.
AU - Wongphechauxsorn, Jompoj
AU - Cordes, James M.
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AU - Jiang, Wu
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AU - Navarro, Santiago
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AU - Johnson, Michael D.
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AU - Bach, Uwe
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AU - Ball, David
AU - Baloković, Mislav
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AU - Bauböck, Michi
AU - Benson, Bradford A.
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AU - Broderick, Avery E.
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AU - Bronzwaer, Thomas
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AU - Kocherlakota, Prashant
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AU - Lauer, Tod R.
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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
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AU - Lo, Wen Ping
AU - Lobanov, Andrei P.
AU - Loinard, Laurent
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AU - Mao, Jirong
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AU - Marrone, Daniel P.
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AU - Menten, Karl M.
AU - Michalik, Daniel
AU - Mizuno, Izumi
AU - Mizuno, Yosuke
AU - Moran, James M.
AU - Moriyama, Kotaro
AU - Moscibrodzka, Monika
AU - Müller, Cornelia
AU - Müller, Hendrik
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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 - Neilsen, Joey
AU - Neri, Roberto
AU - Ni, Chunchong
AU - Noutsos, Aristeidis
AU - Nowak, Michael A.
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 - Pesce, Dominic W.
AU - Piétu, Vincent
AU - Plambeck, Richard
AU - PopStefanija, Aleksandar
AU - Porth, Oliver
AU - Pötzl, Felix M.
AU - Preciado-López, Jorge A.
AU - Psaltis, Dimitrios
AU - Pu, Hung Yi
AU - Prather, Ben
AU - Ramakrishnan, Venkatessh
AU - Rao, Ramprasad
AU - Rawlings, Mark G.
AU - Rezzolla, Luciano
AU - Ripperda, Bart
AU - Ricarte, Angelo
AU - Roelofs, Freek
AU - Rogers, Alan
AU - Ros, Eduardo
AU - Romero-Cañizales, Cristina
AU - Roshanineshat, Arash
AU - Roy, Alan L.
AU - Ruszczyk, Chet
AU - Sánchez-Argüelles, David
AU - Sasada, Mahito
AU - Satapathy, Kaushik
AU - Savolainen, Tuomas
AU - Schloerb, F. Peter
AU - Schonfeld, Jonathan
AU - Small, Des
AU - Sohn, Bong Won
AU - SooHoo, Jason
AU - Souccar, Kamal
AU - Sun, He
AU - Tetarenko, Alexandra J.
AU - Tiede, Paul
AU - Tilanus, Remo P.J.
AU - Titus, Michael
AU - Toscano, Teresa
AU - Traianou, Efthalia
AU - Trent, Tyler
AU - Trippe, Sascha
AU - Turk, Matthew
AU - van Bemmel, Ilse
AU - van Langevelde, Huib Jan
AU - van Rossum, Daniel R.
AU - Vos, Jesse
AU - Ward-Thompson, Derek
AU - Wardle, John
AU - Weintroub, Jonathan
AU - Wex, Norbert
AU - Wielgus, Maciek
AU - Wiik, Kaj
AU - Witzel, Gunther
AU - Wondrak, Michael F.
AU - Wong, George N.
AU - Wu, Qingwen
AU - Yadlapalli, Nitika
AU - Yamaguchi, Paul
AU - Yfantis, Aristomenis
AU - Yoon, Doosoo
AU - Young, André
AU - Young, Ken
AU - Younsi, Ziri
AU - Yu, Wei
AU - Yuan, Feng
AU - Yuan, Ye Fei
AU - Zensus, J. Anton
AU - Zhang, Shuo
AU - Zhao, Guang Yao
AU - Zhao, Shan Shan
N1 - Publisher Copyright: © 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/12/1
Y1 - 2023/12/1
N2 - In 2017 the Event Horizon Telescope (EHT) observed the supermassive black hole at the center of the Milky Way, Sagittarius A* (Sgr A*), at a frequency of 228.1 GHz (λ = 1.3 mm). The fundamental physics tests that even a single pulsar orbiting Sgr A* would enable motivate searching for pulsars in EHT data sets. The high observing frequency means that pulsars—which typically exhibit steep emission spectra—are expected to be very faint. However, it also negates pulse scattering, an effect that could hinder pulsar detections in the Galactic center. Additionally, magnetars or a secondary inverse Compton emission could be stronger at millimeter wavelengths than at lower frequencies. We present a search for pulsars close to Sgr A* using the data from the three most sensitive stations in the EHT 2017 campaign: the Atacama Large Millimeter/submillimeter Array, the Large Millimeter Telescope, and the IRAM 30 m Telescope. We apply three detection methods based on Fourier-domain analysis, the fast folding algorithm, and single-pulse searches targeting both pulsars and burst-like transient emission. We use the simultaneity of the observations to confirm potential candidates. No new pulsars or significant bursts were found. Being the first pulsar search ever carried out at such high radio frequencies, we detail our analysis methods and give a detailed estimation of the sensitivity of the search. We conclude that the EHT 2017 observations are only sensitive to a small fraction (≲2.2%) of the pulsars that may exist close to Sgr A*, motivating further searches for fainter pulsars in the region.
AB - In 2017 the Event Horizon Telescope (EHT) observed the supermassive black hole at the center of the Milky Way, Sagittarius A* (Sgr A*), at a frequency of 228.1 GHz (λ = 1.3 mm). The fundamental physics tests that even a single pulsar orbiting Sgr A* would enable motivate searching for pulsars in EHT data sets. The high observing frequency means that pulsars—which typically exhibit steep emission spectra—are expected to be very faint. However, it also negates pulse scattering, an effect that could hinder pulsar detections in the Galactic center. Additionally, magnetars or a secondary inverse Compton emission could be stronger at millimeter wavelengths than at lower frequencies. We present a search for pulsars close to Sgr A* using the data from the three most sensitive stations in the EHT 2017 campaign: the Atacama Large Millimeter/submillimeter Array, the Large Millimeter Telescope, and the IRAM 30 m Telescope. We apply three detection methods based on Fourier-domain analysis, the fast folding algorithm, and single-pulse searches targeting both pulsars and burst-like transient emission. We use the simultaneity of the observations to confirm potential candidates. No new pulsars or significant bursts were found. Being the first pulsar search ever carried out at such high radio frequencies, we detail our analysis methods and give a detailed estimation of the sensitivity of the search. We conclude that the EHT 2017 observations are only sensitive to a small fraction (≲2.2%) of the pulsars that may exist close to Sgr A*, motivating further searches for fainter pulsars in the region.
UR - http://www.scopus.com/inward/record.url?scp=85179827016&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85179827016&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/acf4f2
DO - 10.3847/1538-4357/acf4f2
M3 - Article
AN - SCOPUS:85179827016
SN - 0004-637X
VL - 959
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 14
ER -