J/A+A/633/A98 Gaia16aye microlensing event photometry (Wyrzykowski+, 2020) ================================================================================ Full orbital solution for the binary system in the northern Galactic disk microlensing event Gaia16aye. Wyrzykowski L., Mroz P., Rybicki K. A., Gromadzki M., Kolaczkowski Z., Zielinski M., Zielinski P., Britavskiy N., Gomboc A., Sokolovsky K., Hodgkin S. T., Abe L., Aldi G. F., AlMannaei A., Altavilla G., Al Qasim A., Anupama G.C., Awiphan S., Bachelet E., Bakis V. Baker S., Bartlett S., Bendjoya P., Benson K., Bikmaev I. F., Birenbaum G., Blagorodnova N., Blanco-Cuaresma S., Boeva S., Bonanos A. Z., Bozza V., Bramich D.M., Bruni I., Burenin R.A., Burgaz U., Butterley T., Caines H.E., Caton D.B., Calchi Novati S., Carrasco J.M., Cassan A., Cepas V., Cropper M., Chruslinska M., Clementini G., Clerici A., Conti D., Conti M., Cross S., Cusano F., Damljanovic G., Dapergolas A., D'Ago G., de Bruijne J.H.J., Dennefeld M., Dhillon V.S., Dominik M., Dziedzic J., Erece O., Eselevich M.V., Esenoglu H., Eyer L., Figuera Jaimes R., Fossey S.J., Galeev A. I., Grebenev S. A., Gupta A.C., Gutaev A. G., Hallakoun N., Hamanowicz A., Han C., Handzlik B., Haislip J.B., Hardy L.K., Harrison D.L., Hoette V.L., Horne K., Hudec R., Hundertmark M., Ihanec N., Irtuganov E.N., Itoh R., Iwanek P., Jovanovic M.D., Janulis R., Jelinek M., Jensen E., Kaczmarek Z., Katz D., Khamitov I.M., Kilic Y., Klencki J., Kolb U., Kouprianov V.V., Kruszynska K., Kurowski S., Latev G., Lee C-H., Leonini S., Leto G., Lewis F., Li Z., Liakos A., Littlefair S.P., Lu J., Manser C.J., Mao S., Maoz D., Maskoliunas M., Maund J.R., Melnikov S. S., Ment K., Mikolajczyk P., Morrell M., Mowlavi N., Mozdzierski D., Nazarov S., Netzel H., Nesci R., Ngeow C. -C., Norton A.J., Ofek E. O., Pakstiene E., Palaversa L., Pandey A., Paraskeva E., Pawlak M., Penny M.T., Penprase B.E., Piascik A., Prieto J.L., Qvam J.K.T., Ranc C., Rebassa-Mansergas A., Reichart D.E., Reig P., Rhodes L., Rivet J.-P., Rixon G., Roberts D., Rosi P., Russell D.M., Zanmar Sanchez R., Scarpetta G., Seabroke G., Shappee B.J., Schmidt R., Shvartzvald Y., Sitek M., Skowron J., Sniegowska M., Snodgrass C., Soares P.S., Spetsieri Z.T., Stankeviciute A., Steele I.A., Street R.A., Strobl J., Tinjaca Ramirez L.M., Tomasella L., Tsapras Y., Villanueva S.Jr., Vince O., Wambsganss J., Wiersema K., Wilson R.W., Yoldas A., Zhuchkov R.Ya., Zhukov D.G., Zdanavicius J., Zola S., Zubareva A. =2020A&A...633A..98W (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Gravitational lensing ; Photometry Keywords: gravitational lensing: micro - techniques: photometric - binaries: general stars: individual: Gaia16aye Abstract: Gaia16aye was a binary microlensing event, the first such event ever discovered in the direction towards the Northern Galactic Disk and one of the first microlensing events detected and alerted by the Gaia space mission. Its light curve exhibited five distinct brightening episodes, reaching up to 11mag, and was covered in great detail with almost 25000 data points gathered by a network of telescopes. We present the photometric and spectroscopic follow-up covering 500 days of the event evolution and search for a possible microlensing model in order to derive the parameters of the lensing binary system. For Gaia16aye event we employed a full Keplerian binary orbit microlensing model combined with the Earth and Gaia motion around the Sun, to reproduce the complex light curve. The photometric data allowed us to solve the microlensing events entirely and to derive the complete and unique set of orbital parameters of the binary lensing system. We also report on the detection of the first ever microlensing space-parallax between the Earth and Gaia located at L2. The binary system properties were derived from microlensing parameters and we found that the system is composed of two main-sequence stars with masses 0.570.05 M and 0.36+/-0.03M_{sun}_ at 780pc, with an orbital period of 2.88 years and eccentricity of 0.30. We also predict the astrometric microlensing signal for this binary lens as it will be seen by Gaia as well as the radial velocity curve. Events like Gaia16aye indicate the potential for the microlensing method to probe the mass function of dark objects, including black holes, in other directions than the Galactic bulge. This case also emphasises the importance of long-term time-domain coordinated observations which can be done with a network of heterogeneous telescopes. Description: Photometric data for the microlensing event Gaia16aye. We present three separate tables with the follow-up data, Gaia data and the set of data used in the modelling process. Objects: --------------------------------------------------------------------- RA (ICRS) DE Designation(s) --------------------------------------------------------------------- 19 40 01.13 +30 07 53.4 Gaia DR2 2032454944878107008 = Gaia 16aye --------------------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file model.dat 30 590 Photometry of data used in modelling followup.dat 58 24513 Photometry of all follow-up data gaia.dat 37 84 Photometric measurements from Gaia -------------------------------------------------------------------------------- See also: I/345 : Gaia DR2 (Gaia Collaboration, 2018) Byte-by-byte Description of file: model.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 13 F13.5 d HJD Heliocentric Julian Date 15- 20 F6.3 mag mag Apparent magnitude in filter 22- 26 F5.3 mag e_mag Uncertainty in mag 28 A1 --- Filter [GVIi] Filter 30 I1 --- Obs [1/8] Observatory code (1) -------------------------------------------------------------------------------- Note (1): Observatory codes as follows: 1 = Gaia (G) 2 = Bialkow (I) 3 = APT2 (I) 4 = LT (i) 5 = DEMONEXT (I) 6 = Swarthmore (I) 7 = UBT60 (I) 8 = ASAS-SN (V) -------------------------------------------------------------------------------- Byte-by-byte Description of file: followup.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 I6 --- ID Unique ID of the data point 8- 18 F11.5 d MJD Modified Julian Date 20- 25 F6.3 mag mag Apparent magnitude in Filter 27- 31 F5.3 mag e_mag Uncertainty in mag 33 A1 --- Filter [BGVgriz] Name of the photometric band 35- 58 A24 --- Tel ID of the telescope in the format TelescopeCode_Observer or ObservatoryLabel -------------------------------------------------------------------------------- Byte-by-byte Description of file: gaia.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 19 A19 "datime" TCB TCB date in the format yyyy-mm-ddThh:mm:ss 21- 31 F11.3 d JD Julian Date 33- 37 F5.2 mag Gmag Apparent Gaia G magnitude -------------------------------------------------------------------------------- Acknowledgements: Lukasz Wyrzykowski, wyrzykow(at)astrouw.edu.pl, Astronomical Observatory, University of Warsaw ================================================================================ (End) L. Wyrzykowski [Astron. Obs., Warsaw Univ.], P. Vannier [CDS] 21-Oct-2019