2022ApJ...930L..15E

Query : 2022ApJ...930L..15E

2022ApJ...930L..15E - Astrophys. J., 930, L15-L15 (2022/May-2)

First Sagittarius A* Event Horizon Telescope Results. IV. Variability, Morphology, and Black Hole Mass.

EHT COLLABORATION, AKIYAMA K., ALBERDI A., ALEF W., ALGABA J.C., ANANTUA R., ASADA K., AZULAY R., BACH U., BACZKO A.-K., BALL D., BALOKOVIC M., BARRETT J., BAUBOCK M., BENSON B.A., BINTLEY D., BLACKBURN L., BLUNDELL R., BOUMAN K.L., BOWER G.C., BOYCE H., BREMER M., BRINKERINK C.D., BRISSENDEN R., BRITZEN S., BRODERICK A.E., BROGUIERE D., BRONZWAER T., BUSTAMANTE S., BYUN D.-Y., CARLSTROM J.E., CECCOBELLO C., CHAEL A., CHAN C.-K., CHATTERJEE K., CHATTERJEE S., CHEN M.-T., CHEN Y., CHENG X., CHO I., CHRISTIAN P., CONROY N.S., CONWAY J.E., CORDES J.M., CRAWFORD T.M., CREW G.B., CRUZ-OSORIO A., CUI Y., DAVELAAR J., DE LAURENTIS M., DEANE R., DEMPSEY J., DESVIGNES G., DEXTER J., DHRUV V., DOELEMAN S.S., DOUGAL S., DZIB S.A., EATOUGH R.P., EMAMI R., FALCKE H., FARAH J., FISH V.L., FOMALONT E., FORD H.A., FRAGA-ENCINAS R., FREEMAN W.T., FRIBERG P., FROMM C.M., FUENTES A., GALISON P., GAMMIE C.F., GARCIA R., GENTAZ O., GEORGIEV B., GODDI C., GOLD R., GOMEZ-RUIZ A.I., GOMEZ J.L., GU M., GURWELL M., HADA K., HAGGARD D., HAWORTH K., HECHT M.H., HESPER R., HEUMANN D., HO L.C., HO P., HONMA M., HUANG C.-W.L., HUANG L., HUGHES D.H., IKEDA S., IMPELLIZZERI C.M.V., INOUE M., ISSAOUN S., JAMES D.J., JANNUZI B.T., JANSSEN M., JETER B., JIANG W., JIMENEZ-ROSALES A., JOHNSON M.D., JORSTAD S., JOSHI A.V., JUNG T., KARAMI M., KARUPPUSAMY R., KAWASHIMA T., KEATING G.K., KETTENIS M., KIM D.-J., KIM J.-Y., KIM J., KIM J., KINO M., KOAY J.Y., KOCHERLAKOTA P., KOFUJI Y., KOCH P.M., KOYAMA S., KRAMER C., KRAMER M., KRICHBAUM T.P., KUO C.-Y., LA BELLA N., LAUER T.R., LEE D., LEE S.-S., LEUNG P.K., LEVIS A., LI Z., LICO R., LINDAHL G., LINDQVIST M., LISAKOV M., LIU J., LIU K., LIUZZO E., LO W.-P., LOBANOV A.P., LOINARD L., LONSDALE C.J., LU R.-S., MAO J., MARCHILI N., MARKOFF S., MARRONE D.P., MARSCHER A.P., MARTI-VIDAL I., MATSUSHITA S., MATTHEWS L.D., MEDEIROS L., MENTEN K.M., MICHALIK D., MIZUNO I., MIZUNO Y., MORAN J.M., MORIYAMA K., MOSCIBRODZKA M., MULLER C., MUS A., MUSOKE G., MYSERLIS I., NADOLSKI A., NAGAI H., NAGAR N.M., NAKAMURA M., NARAYAN R., NARAYANAN G., NATARAJAN I., NATHANAIL A., NAVARRO FUENTES S., NEILSEN J., NERI R., NI C., NOUTSOS A., NOWAK M.A., OH J., OKINO H., OLIVARES H., ORTIZ-LEON G.N., OYAMA T., PALUMBO D.C.M., PARASCHOS G.F., PARK J., PARSONS H., PATEL N., PEN U.-L., PESCE D.W., PIETU V., PLAMBECK R., POPSTEFANIJA A., PORTH O., POTZL F.M., PRATHER B., PRECIADO-LOPEZ J.A., PU H.-Y., RAMAKRISHNAN V., RAO R., RAWLINGS M.G., RAYMOND A.W., REZZOLLA L., RICARTE A., RIPPERDA B., ROELOFS F., ROGERS A., ROS E., ROMERO-CANIZALES C., ROSHANINESHAT A., ROTTMANN H., ROY A.L., RUIZ I., RUSZCZYK C., RYGL K.L.J., SANCHEZ S., SANCHEZ-ARGUELLES D., SANCHEZ-PORTAL M., SASADA M., SATAPATHY K., SAVOLAINEN T., SCHLOERB F.P., SCHONFELD J., SCHUSTER K.-F., SHAO L., SHEN Z., SMALL D., SOHN B.W., SOOHOO J., SOUCCAR K., SUN H., TAZAKI F., TETARENKO A.J., TIEDE P., TILANUS R.P.J., TITUS M., TORNE P., TRAIANOU E., TRENT T., TRIPPE S., TURK M., VAN BEMMEL I., VAN LANGEVELDE H.J., VAN ROSSUM D.R., VOS J., WAGNER J., WARD-THOMPSON D., WARDLE J., WEINTROUB J., WEX N., WHARTON R., WIELGUS M., WIIK K., WITZEL G., WONDRAK M.F., WONG G.N., WU Q., YAMAGUCHI P., YOON D., YOUNG A., YOUNG K., YOUNSI Z., YUAN F., YUAN Y.-F., ZENSUS J.A., ZHANG S., ZHAO G.-Y., ZHAO S.-S. and CHANG D.O.

Abstract (from CDS):

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 ∼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 µas (68% credible intervals), with the ring thickness constrained to have an FWHM between ∼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} µas, 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}\times {10}^{6} M☉.

Abstract Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Black holes

Simbad objects: 5

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Number of rows : 5
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3
2 QSO B1730-130 Bla 17 33 02.70578907 -13 04 49.5482119   18 19.50 18.78 17.39 ~ 1198 1
3 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
4 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 4970 3
5 QSO B1921-293 BLL 19 24 51.05595254 -29 14 30.1210248   18.71 18.21 15.07   ~ 918 1

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