First Sagittarius A* Event Horizon Telescope Results. IV. Variability, Morphology, and Black Hole Mass
Mao JR; Inoue M; Loinard L; Romero-Canizales C; Matthews LD; Young K; Fomalont E; Neilsen J; Levis A; Hesper R; Bremer M; Wong GN; Yuan YF; Sanchez S; Myserlis I; Dhruv V; Gu MF; Blundell R; Rao R; Gammie CF; Blackburn L; Jung T; Traianou E; Marchili N; Nagai H; Nakamura M; Trippe S; Freeman WT; Lee D; Emami R; Karami M; Davelaar J; Kocherlakota P; Noutsos A; Ramakrishnan V; Zensus JA; Preciado-Lopez JA; Kino M; Christian P; Trent T; Britzen S; Porth O; Yoon D; Deane R; Akiyama K; Liu J; Ford HA; Chen YJ; Conroy NS; Nowak MA; Pu HY; Kawashima T; Zhang S; Plambeck R; Broderick AE; Raymond AW; Gurwell M; Mus A; Bach U; Lonsdale CJ; Rezzolla L; Koay JY; Schonfeld J; Ruiz I; Bintley D; Kim JY; Okino H; Lico R; Palumbo DCM; Cho I; Liu K; Turk M; Gomez-Ruiz AI; Nagar NM; Keating GK; Kramer M; Moriyama K; Mizuno I; Narayanan G; Yuan F; Jeter B; Markoff S; Natarajan I; Dzib SA; Gold R; Cheng XP; Liuzzo E; Leung PK; Prather B; Fraga-Encinas R; Krichbaum TP; Sanchez-Arguelles D; De Laurentis M; Oyama T; Mizuno Y; Bower GC; La Bella N; Ni CC; Fuentes SN; Schloerb FP; Wondrak MF; Haworth K; Roshanineshat A; Ripperda B; Moscibrodzka M; Kettenis M; Kim DJ; Musoke G; Johnson MD; Satapathy K; Benson BA; Farah J; Heumann D; Jimenez-Rosales A; Lindqvist M; Zhao SS; Sanchez-Portal M; Chatterjee K; Parsons H; Ward-Thompson D; van Langevelde HJ; Algaba JC; Zhao GY; Sasada M; Patel N; Weintroub J; Small D; Conway JE; Sun H; Impellizzeri CMV; James DJ; Muller C; Potzl FM; Wu QW; Lauer TR; Lu RS; Michalik D; Pesce DW; Neri R; Shen ZQ; Dexter J; Shao LJ; Crawford TM; Carlstrom JE; Roelofs F; Haggard D; Ho P; Lindahl G; PopStefanija A; Cordes JM; Friberg P; Hada K; Ikeda S; Oh J; van Rossum DR; Nadolski A; Lo WP; Crew GB; Paraschos GF; Pen UL; Honma M; Kramer C; Huang L; Janssen M; Garcia R; Marrone DP; Brinkerink CD; Fuentes A; Ricarte A; Ceccobello C; Chatterjee S; Issaoun S; Chan CK; Rottmann H; Ortiz-Leon GN; Narayan R; Ruszczyk C; Doeleman SS; Azulay R; Witzel G; Wiik K; Hecht MH; Ros E; Karuppusamy R; Jiang W; Moran JM; Torne P; Galison P; Eatough RP; Pietu V; Bronzwaer T; Lobanov AP; Baczko AK; Gentaz O; Matsushita S; Young A; Fromm CM; Yamaguchi P; Cui YZ; Tetarenko AJ; Sohn BW; Rygl KLJ; Menten KM; Nathanail A; Schuster KF; Dempsey J; Boyce H; Medeiros L; Wharton R; van Bemmel I; Cruz-Osorio A; Younsi Z; Wardle J; Tazaki F; Bustamante S; Baubock M; Tilanus RPJ; Titus M; Brissenden R; Alberdi A; Wielgus M; Olivares H; Bouman KL; Ho LC; Kofuji Y; Wagner J; Byun DY; Georgiev B; Anantua R; Lisakov M; Desvignes G; Fish VL; Lee SS; Balokovic M; Koch PM; Gomez JL; Broguiere D; Rawlings MG; Dougal S; Roy AL; Vos J; Kuo CY; Koyama S; Kim J; Goddi C; Alef W; Souccar K; Ball D; Tiede P; Li ZY; Huang CWL; Marti-Vidal I; Park J; Chael A; Jorstad S; Chang DO; SooHoo J; Wex N; Jannuzi BT; Joshi AV; Rogers A; Barrett J; Falcke H; Marscher AP; Asada K; Hughes DH; Chen MT; Savolainen T
First Sagittarius A* Event Horizon Telescope Results. IV. Variability, Morphology, and Black Hole Mass
Mao JR
Inoue M
Loinard L
Romero-Canizales C
Matthews LD
Young K
Fomalont E
Neilsen J
Levis A
Hesper R
Bremer M
Wong GN
Yuan YF
Sanchez S
Myserlis I
Dhruv V
Gu MF
Blundell R
Rao R
Gammie CF
Blackburn L
Jung T
Traianou E
Marchili N
Nagai H
Nakamura M
Trippe S
Freeman WT
Lee D
Emami R
Karami M
Davelaar J
Kocherlakota P
Noutsos A
Ramakrishnan V
Zensus JA
Preciado-Lopez JA
Kino M
Christian P
Trent T
Britzen S
Porth O
Yoon D
Deane R
Akiyama K
Liu J
Ford HA
Chen YJ
Conroy NS
Nowak MA
Pu HY
Kawashima T
Zhang S
Plambeck R
Broderick AE
Raymond AW
Gurwell M
Mus A
Bach U
Lonsdale CJ
Rezzolla L
Koay JY
Schonfeld J
Ruiz I
Bintley D
Kim JY
Okino H
Lico R
Palumbo DCM
Cho I
Liu K
Turk M
Gomez-Ruiz AI
Nagar NM
Keating GK
Kramer M
Moriyama K
Mizuno I
Narayanan G
Yuan F
Jeter B
Markoff S
Natarajan I
Dzib SA
Gold R
Cheng XP
Liuzzo E
Leung PK
Prather B
Fraga-Encinas R
Krichbaum TP
Sanchez-Arguelles D
De Laurentis M
Oyama T
Mizuno Y
Bower GC
La Bella N
Ni CC
Fuentes SN
Schloerb FP
Wondrak MF
Haworth K
Roshanineshat A
Ripperda B
Moscibrodzka M
Kettenis M
Kim DJ
Musoke G
Johnson MD
Satapathy K
Benson BA
Farah J
Heumann D
Jimenez-Rosales A
Lindqvist M
Zhao SS
Sanchez-Portal M
Chatterjee K
Parsons H
Ward-Thompson D
van Langevelde HJ
Algaba JC
Zhao GY
Sasada M
Patel N
Weintroub J
Small D
Conway JE
Sun H
Impellizzeri CMV
James DJ
Muller C
Potzl FM
Wu QW
Lauer TR
Lu RS
Michalik D
Pesce DW
Neri R
Shen ZQ
Dexter J
Shao LJ
Crawford TM
Carlstrom JE
Roelofs F
Haggard D
Ho P
Lindahl G
PopStefanija A
Cordes JM
Friberg P
Hada K
Ikeda S
Oh J
van Rossum DR
Nadolski A
Lo WP
Crew GB
Paraschos GF
Pen UL
Honma M
Kramer C
Huang L
Janssen M
Garcia R
Marrone DP
Brinkerink CD
Fuentes A
Ricarte A
Ceccobello C
Chatterjee S
Issaoun S
Chan CK
Rottmann H
Ortiz-Leon GN
Narayan R
Ruszczyk C
Doeleman SS
Azulay R
Witzel G
Wiik K
Hecht MH
Ros E
Karuppusamy R
Jiang W
Moran JM
Torne P
Galison P
Eatough RP
Pietu V
Bronzwaer T
Lobanov AP
Baczko AK
Gentaz O
Matsushita S
Young A
Fromm CM
Yamaguchi P
Cui YZ
Tetarenko AJ
Sohn BW
Rygl KLJ
Menten KM
Nathanail A
Schuster KF
Dempsey J
Boyce H
Medeiros L
Wharton R
van Bemmel I
Cruz-Osorio A
Younsi Z
Wardle J
Tazaki F
Bustamante S
Baubock M
Tilanus RPJ
Titus M
Brissenden R
Alberdi A
Wielgus M
Olivares H
Bouman KL
Ho LC
Kofuji Y
Wagner J
Byun DY
Georgiev B
Anantua R
Lisakov M
Desvignes G
Fish VL
Lee SS
Balokovic M
Koch PM
Gomez JL
Broguiere D
Rawlings MG
Dougal S
Roy AL
Vos J
Kuo CY
Koyama S
Kim J
Goddi C
Alef W
Souccar K
Ball D
Tiede P
Li ZY
Huang CWL
Marti-Vidal I
Park J
Chael A
Jorstad S
Chang DO
SooHoo J
Wex N
Jannuzi BT
Joshi AV
Rogers A
Barrett J
Falcke H
Marscher AP
Asada K
Hughes DH
Chen MT
Savolainen T
IOP Publishing Ltd
Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2022081154903
https://urn.fi/URN:NBN:fi-fe2022081154903
Tiivistelmä
In this paper we quantify the temporal variability and image morphology of the horizon-scale emission from Sgr A*, as observed by the EHT in 2017 April at a wavelength of 1.3 mm. We find that the Sgr A* data exhibit variability that exceeds what can be explained by the uncertainties in the data or by the effects of interstellar scattering. The magnitude of this variability can be a substantial fraction of the correlated flux density, reaching similar to 100% on some baselines. Through an exploration of simple geometric source models, we demonstrate that ring-like morphologies provide better fits to the Sgr A* data than do other morphologies with comparable complexity. We develop two strategies for fitting static geometric ring models to the time-variable Sgr A* data; one strategy fits models to short segments of data over which the source is static and averages these independent fits, while the other fits models to the full data set using a parametric model for the structural variability power spectrum around the average source structure. Both geometric modeling and image-domain feature extraction techniques determine the ring diameter to be 51.8 +/- 2.3 mu as (68% credible intervals), with the ring thickness constrained to have an FWHM between similar to 30% and 50% of the ring diameter. To bring the diameter measurements to a common physical scale, we calibrate them using synthetic data generated from GRMHD simulations. This calibration constrains the angular size of the gravitational radius to be 4.8(-0.7)(+1.4) mu as, which we combine with an independent distance measurement from maser parallaxes to determine the mass of Sgr A* to be 4.0(-0.6)(+1.1) x 10(6) M-circle dot.
Kokoelmat
- Rinnakkaistallenteet [19207]