2021ApJ...916...98G

Query : 2021ApJ...916...98G

2021ApJ...916...98G - Astrophys. J., 916, 98-98 (2021/August-1)

Detection of galactic and extragalactic millimeter-wavelength transient sources with SPT-3G.

GUNS S., FOSTER A., DALEY C., RAHLIN A., WHITEHORN N., ADE P.A.R., AHMED Z., ANDERES E., ANDERSON A.J., ARCHIPLEY M., AVVA J.S., AYLOR K., BALKENHOL L., BARRY P.S., BASU THAKUR R., BENABED K., BENDER A.N., BENSON B.A., BIANCHINI F., BLEEM L.E., BOUCHET F.R., BRYANT L., BYRUM K., CARLSTROM J.E., CARTER F.W., CECIL T.W., CHANG C.L., CHAUBAL P., CHEN G., CHO H.-M., CHOU T.-L., CLICHE J.-F., CRAWFORD T.M., CUKIERMAN A., DE HAAN T., DENISON E.V., DIBERT K., DING J., DOBBS M.A., DUTCHER D., EVERETT W., FENG C., FERGUSON K.R., FU J., GALLI S., GAMBREL A.E., GARDNER R.W., GOECKNER-WALD N., GUALTIERI R., GUPTA N., GUYSER R., HALVERSON N.W., HARKE-HOSEMANN A.H., HARRINGTON N.L., HENNING J.W., HILTON G.C., HIVON E., HOLDER G.P., HOLZAPFEL W.L., HOOD J.C., HOWE D., HUANG N., IRWIN K.D., JEONG O.B., JONAS M., JONES A., KHAIRE T.S., KNOX L., KOFMAN A.M., KORMAN M., KUBIK D.L., KUHLMANN S., KUO C.-L., LEE A.T., LEITCH E.M., LOWITZ A.E., LU C., MARRONE D.P., MEYER S.S., MICHALIK D., MILLEA M., MONTGOMERY J., NADOLSKI A., NATOLI T., NGUYEN H., NOBLE G.I., NOVOSAD V., OMORI Y., PADIN S., PAN Z., PASCHOS P., PEARSON J., PHADKE K.A., POSADA C.M., PRABHU K., QUAN W., REICHARDT C.L., RIEBEL D., RIEDEL B., ROUBLE M., RUHL J.E., SAYRE J.T., SCHIAPPUCCI E., SHIROKOFF E., SMECHER G., SOBRIN J.A., STARK A.A., STEPHEN J., STORY K.T., SUZUKI A., THOMPSON K.L., THORNE B., TUCKER C., UMILTA C., VALE L.R., VIEIRA J.D., WANG G., WU W.L.K., YEFREMENKO V., YOON K.W., YOUNG M.R. and ZHANG L.

Abstract (from CDS):

High angular resolution cosmic microwave background experiments provide a unique opportunity to conduct a survey of time-variable sources at millimeter wavelengths, a population that has primarily been understood through follow-up measurements of detections in other bands. Here we report the first results of an astronomical transient survey with the South Pole Telescope (SPT) using the SPT-3G camera to observe 1500 deg2 of the southern sky. The observations took place from 2020 March to November in three bands centered at 95, 150, and 220 GHz. This survey yielded the detection of 15 transient events from sources not previously detected by the SPT. The majority are associated with variable stars of different types, expanding the number of such detected flares by more than a factor of two. The stellar flares are unpolarized and bright, in some cases exceeding 1 Jy, and have durations from a few minutes to several hours. Another population of detected events last for 2-3 weeks and appear to be extragalactic in origin. Though data availability at other wavelengths is limited, we find evidence for concurrent optical activity for two of the stellar flares. Future data from SPT-3G and forthcoming instruments will provide real-time detection of millimeter-wave transients on timescales of minutes to months.

Abstract Copyright: © 2021. The American Astronomical Society. All rights reserved.

Journal keyword(s): Stellar flares - Active galactic nuclei - High energy astrophysics - Transient detection - Transient sources - Millimeter astronomy - Surveys

Simbad objects: 20

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Number of rows : 20
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 UCAC3 53-724 TT* 00 21 27.7146373416 -63 51 08.188664904       15.06 13.19 M5.5V 16 0
2 V* CC Eri BY* 02 34 22.5661889568 -43 47 46.869120096 11.305 10.201 8.865 7.926 6.992 K7V 285 0
3 UCAC4 165-002704 PM* 02 55 31.7837348088 -57 02 52.330155360   17.883 16.108 15.737   M4.3 18 0
4 SPT-SV J030016.1-571921 ev 03 00 16.1 -57 19 21           ~ 1 0
5 WISEA J030116.15-571917.7 IR 03 01 16.15 -57 19 17.7           ~ 1 0
6 JW 566 Y*O 05 35 17.990 -05 16 13.63   14.9 18.7   15.757 K7+M1.5 44 0
7 ACT-T J061647-402140 ev 06 16 47.00 -40 21 40.5           ~ 2 0
8 WISE J061647.01-402142.8 Bla 06 17.1 -40 26           ~ 5 0
9 NAME Proxima Centauri PM* 14 29 42.9461331854 -62 40 46.164680672 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1483 0
10 SN 2018cow SN* 16 16 00.254 +22 16 05.10           SNIb 305 0
11 HD 197481 BY* 20 45 09.5324974119 -31 20 27.237889841   10.05 8.627 9.078 6.593 M1VeBa1 1344 0
12 CD-50 13207 BY* 21 01 21.2058398736 -49 33 07.339961016     11.051   9.724 K7 11 0
13 CD-55 8799 Ro* 21 20 44.0932507872 -54 37 59.278211976   11.76 10.73   9.391 K0III 13 0
14 V* Z Ind Ro* 21 54 24.3642932040 -49 56 41.256982068   11.76 10.61   9.340 K2IIIe 17 0
15 2RXS J224112.8-540103 X 22 41 12.8 -54 01 03           ~ 1 0
16 WISEA J224115.38-540102.3 IR 22 41 15.38 -54 01 02.3           ~ 1 0
17 SPT-SV J224116.7-540107 ev 22 41 16.7 -54 01 07           ~ 1 0
18 WISEA J224117.10-540105.2 IR 22 41 17.10 -54 01 05.2           ~ 1 0
19 V* BI Ind RS* 23 13 52.7842528944 -68 17 28.814107128   8.89 7.67     K2IIIp 50 0
20 UCAC4 114-133248 ** 23 20 47.046072 -67 23 21.49404   15.75 14.17 14.09 11.33 M5 15 0

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