2024AJ....168..130R


Query : 2024AJ....168..130R

2024AJ....168..130R - Astron. J., 168, 130 (2024/September-0)

First Very Long Baseline Interferometry Detections at 870 μm.

RAYMOND A.W., DOELEMAN S.S., ASADA K., BLACKBURN L., BOWER G.C., BREMER M., BROGUIERE D., CHEN M.-T., CREW G.B., DORNBUSCH S., FISH V.L., GARCIA R., GENTAZ O., GODDI C., HAN C.-C., HECHT M.H., HUANG Y.-D., JANSSEN M., KEATING G.K., KOAY J.Y., KRICHBAUM T.P., LO W.-P., MATSUSHITA S., MATTHEWS L.D., MORAN J.M., NORTON T.J., PATEL N., PESCE D.W., RAMAKRISHNAN V., ROTTMANN H., ROY A.L., SANCHEZ S., TILANUS R.P.J., TITUS M., TORNE P., WAGNER J., WEINTROUB J., WIELGUS M., YOUNG A., AKIYAMA K., ALBENTOSA-RUIZ E., ALBERDI A., ALEF W., ALGABA J.C., ANANTUA R., AZULAY R., BACH U., BACZKO A.-K., BALL D., BALOKOVIC M., BANDYOPADHYAY B., BARRETT J., BAUBOCK M., BENSON B.A., BINTLEY D., BLUNDELL R., BOUMAN K.L., BOYCE H., BRISSENDEN R., BRITZEN S., BRODERICK A.E., BRONZWAER T., BUSTAMANTE S., CARLSTROM J.E., CHAEL A., CHAN C.-K., CHANG D.O., CHATTERJEE K., CHATTERJEE S., 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., DE LAURENTIS M., DEANE R., DEMPSEY J., DESVIGNES G., DEXTER J., DHRUV V., DIHINGIA I.K., DZIB S.A., EATOUGH R.P., EMAMI R., FALCKE H., FARAH J., FOMALONT E., FONTANA A.-L., FORD H.A., FOSCHI M., FRAGA-ENCINAS R., FREEMAN W.T., FRIBERG P., FROMM C.M., FUENTES A., GALISON P., GAMMIE C.F., GEORGIEV B., GOLD R., GOMEZ-RUIZ A.I., GOMEZ J.L., GU M., GURWELL M., HADA K., HAGGARD D., 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., JIANG W., JIMENEZ-ROSALES A., JOHNSON M.D., JORSTAD S., JONES A.C., JOSHI A.V., JUNG T., KARUPPUSAMY R., KAWASHIMA T., KETTENIS M., KIM D.-J., KIM J.-Y., KIM J., KIM J., KINO M., KOCHERLAKOTA P., KOFUJI Y., KOCH P.M., KOYAMA S., KRAMER C., KRAMER J.A., KRAMER M., KUBO D., KUO C.-Y., LA BELLA N., LEE S.-S., LEVIS A., LI Z., LICO R., LINDAHL G., LINDQVIST M., LISAKOV M., LIU J., LIU K., LIUZZO E., LOBANOV A.P., LOINARD L., LONSDALE C.J., LOWITZ A.E., LU R.-S., MacDONALD N.R., MAHIEU S., MAIER D., MAO J., MARCHILI N., MARKOFF S., MARRONE D.P., MARSCHER A.P., MARTI-VIDAL I., MEDEIROS L., MENTEN K.M., MIZUNO I., MIZUNO Y., MONTGOMERY J., MORIYAMA K., MOSCIBRODZKA M., MULAUDZI W., MULLER C., MULLER H., MUS A., MUSOKE G., MYSERLIS I., NAGAI H., NAGAR N.M., NAKAMURA M., NARAYANAN G., NATARAJAN I., NATHANAIL A., NAVARRO FUENTES S., NEILSEN J., NI C., NOWAK M.A., OH J., OKINO H., OLIVARES SANCHEZ H.R., OYAMA T., OZEL F., PALUMBO D.C.M., PARASCHOS G.F., PARK J., PARSONS H., PEN U.-L., PIETU V., POPSTEFANIJA A., PORTH O., PRATHER B., PRINCIPE G., PSALTIS D., PU H.-Y., RAFFIN P.A., RAO R., RAWLINGS M.G., RICARTE A., RIPPERDA B., ROELOFS F., ROMERO-CANIZALES C., ROS E., ROSHANINESHAT A., RUIZ I., RUSZCZYK C., RYGL K.L.J., 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., SOSAPANTA SALAS L.D., SOUCCAR K., STANWAY J.S., SUN H., TAZAKI F., TETARENKO A.J., TIEDE P., TOMA K., 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., WASHINGTON J.E., WHARTON R., WIIK K., WITZEL G., WONDRAK M.F., WONG G.N., WU Q., YADLAPALLI N., YAMAGUCHI P., YFANTIS A., YOON D., YOUNSI Z., YU W., YUAN F., YUAN Y.-F., ZENSUS J.A., ZHANG S., ZHAO G.-Y. and ZHAO S.-S.

Abstract (from CDS):

The first very long baseline interferometry (VLBI) detections at 870 μm wavelength (345 GHz frequency) are reported, achieving the highest diffraction-limited angular resolution yet obtained from the surface of the Earth and the highest-frequency example of the VLBI technique to date. These include strong detections for multiple sources observed on intercontinental baselines between telescopes in Chile, Hawaii, and Spain, obtained during observations in 2018 October. The longest-baseline detections approach 11 Gλ, corresponding to an angular resolution, or fringe spacing, of 19 μas. The Allan deviation of the visibility phase at 870 μm is comparable to that at 1.3 mm on the relevant integration timescales between 2 and 100 s. The detections confirm that the sensitivity and signal chain stability of stations in the Event Horizon Telescope (EHT) array are suitable for VLBI observations at 870 μm. Operation at this short wavelength, combined with anticipated enhancements of the EHT, will lead to a unique high angular resolution instrument for black hole studies, capable of resolving the event horizons of supermassive black holes in both space and time.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Very long baseline interferometry - Radio interferometry - Black holes - Supermassive black holes - High angular resolution - Astronomical techniques - Event horizons

Simbad objects: 10

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Number of rows : 10
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 QSO B0420-0127 Bla 04 23 15.80072217 -01 20 33.0656073   17.50 17.00 16.28   ~ 1263 3
2 QSO B0507+179 Bla 05 10 02.36912937 +18 00 41.5815635   20.0 19.0 19.09   ~ 470 1
3 ICRF J052109.8+163822 Sy1 05 21 09.88596258 +16 38 22.0515459   19.37 18.84 18.480   ~ 910 1
4 ESO 362-21 BLL 05 22 57.98464178 -36 27 30.8512953   15.26 14.62 14.48   ~ 873 2
5 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3
6 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
7 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 4970 3
8 NAME BL Lac BLL 22 02 43.2913536816 +42 16 39.979416792   15.66 14.72     ~ 2397 1
9 4C 11.69 Bla 22 32 36.40890093 +11 43 50.9040592   17.75 17.33     ~ 1205 2
10 3C 454.3 Bla 22 53 57.7480438728 +16 08 53.561508864   16.57 16.10 15.22   ~ 3004 2

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