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2023ApJ...959...14T - Astrophys. J., 959, 14 (2023/December-2)

A Search for Pulsars around Sgr A* in the First Event Horizon Telescope Data Set.

TORNE P., LIU K., EATOUGH R.P., WONGPHECHAUXSORN J., CORDES J.M., DESVIGNES G., DE LAURENTIS M., KRAMER M., RANSOM S.M., CHATTERJEE S., WHARTON R., KARUPPUSAMY R., BLACKBURN L., JANSSEN M., CHAN C.-K., CREW G.B., MATTHEWS L.D., GODDI C., ROTTMANN H., WAGNER J., SANCHEZ S., RUIZ I., ABBATE F., BOWER G.C., SALAMANCA J.J., GOMEZ-RUIZ A.I., HERRERA-AGUILAR A., JIANG W., LU R.-S., PEN U.-L., RAYMOND A.W., SHAO L., SHEN Z., PAUBERT G., SANCHEZ-PORTAL M., KRAMER C., CASTILLO M., NAVARRO S., JOHN D., SCHUSTER K.-F., JOHNSON M.D., RYGL K.L.J., 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., BLUNDELL R., BOUMAN K.L., 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., CHANG D.O., CHATTERJEE K., CHEN M.-T., CHEN Y., CHENG X., CHO I., CHRISTIAN P., CONROY N.S., CONWAY J.E., CRAWFORD T.M., CRUZ-OSORIO A., CUI Y., DAHALE R., DAVELAAR J., DEANE R., DEMPSEY J., DEXTER J., DHRUV V., DOELEMAN S.S., DOUGAL S., DZIB S.A., EMAMI R., FALCKE H., FARAH J., FISH V.L., FOMALONT E., FORD H.A., FOSCHI M., FRAGA-ENCINAS R., FREEMAN W.T., FRIBERG P., FROMM C.M., FUENTES A., GALISON P., GAMMIE C.F., GARCIA R., GENTAZ O., GEORGIEV B., GOLD R., 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., JETER B., JIMENEZ-ROSALES A., JORSTAD S., JOSHI A.V., JUNG T., KARAMI M., 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., KOYAMA S., 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., LIUZZO E., LO W.-P., LOBANOV A.P., LOINARD L., LONSDALE C.J., MacDONALD N.R., MAO J., MARCHILI N., MARKOFF S., MARRONE D.P., MARSCHER A.P., MARTI-VIDAL I., MATSUSHITA S., MEDEIROS L., MENTEN K.M., MICHALIK D., MIZUNO I., MIZUNO Y., MORAN J.M., MORIYAMA K., MOSCIBRODZKA M., MULLER C., MULLER H., MUS A., MUSOKE G., MYSERLIS I., NADOLSKI A., NAGAI H., NAGAR N.M., NAKAMURA M., NARAYAN R., NARAYANAN G., NATARAJAN I., NATHANAIL A., NEILSEN J., NERI R., NI C., NOUTSOS A., NOWAK M.A., OH J., OKINO H., OLIVARES H., ORTIZ-LEON G.N., OYAMA T., OZEL F., PALUMBO D.C.M., PARASCHOS G.F., PARK J., PARSONS H., PATEL N., PESCE D.W., PIETU V., PLAMBECK R., POPSTEFANIJA A., PORTH O., POTZL F.M., PRATHER B., PRECIADO-LOPEZ J.A., PSALTIS D., PU H.-Y., RAMAKRISHNAN V., RAO R., RAWLINGS M.G., REZZOLLA L., RICARTE A., RIPPERDA B., ROELOFS F., ROGERS A., ROS E., ROMERO-CANIZALES C., ROSHANINESHAT A., ROY A.L., RUSZCZYK C., SANCHEZ-ARGUELLES D., SASADA M., SATAPATHY K., SAVOLAINEN T., SCHLOERB F.P., SCHONFELD J., SMALL D., SOHN B.W., SOOHOO J., SOUCCAR K., SUN H., TETARENKO A.J., TIEDE P., TILANUS R.P.J., TITUS M., TOSCANO T., TRAIANOU E., TRENT T., TRIPPE S., TURK M., VAN BEMMEL I., VAN LANGEVELDE H.J., VAN ROSSUM D.R., VOS J., WARD-THOMPSON D., WARDLE J., WEINTROUB J., WEX N., WIELGUS M., WIIK K., WITZEL G., WONDRAK M.F., WONG G.N., WU Q., YADLAPALLI N., YAMAGUCHI P., YFANTIS A., YOON D., YOUNG A., YOUNG K., YOUNSI Z., YU W., YUAN F., YUAN Y.-F., ZENSUS J.A., ZHANG S., ZHAO G.-Y. and ZHAO S.-S.

Abstract (from CDS):

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.

Abstract Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Radio pulsars - Pulsars - Magnetars - Neutron stars - Black hole physics - Period search - Surveys - Interstellar scattering - Galactic center - Supermassive black holes - Radio transient sources - Millimeter astronomy

Simbad objects: 8

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