J/ApJ/899/130 BVRI light curves of Gaia 18dvy (Szegedi-Elek+, 2020)
Gaia 18dvy: a new FUor in the Cygnus OB3 association.
Szegedi-Elek E., Abraham P., Wyrzykowski L., Kun M., Kospal A., Chen L.,
Marton G., Moor A., Kiss C., Pal A., Szabados L., Varga J.,
Varga-Verebelyi E., Andreas C., Bachelet E., Bischoff R., Bodi A.,
Breedt E., Burgaz U., Butterley T., Carrasco J.M., Cepas V.,
Damljanovic G., Gezer I., Godunova V., Gromadzki M., Gurgul A., Hardy L.,
Hildebrandt F., Hoffmann S., Hundertmark M., Ihanec N., Janulis R.,
Kalup C., Kaczmarek Z., Konyves-Toth R., Krezinger M., Kruszynska K.,
Littlefair S., Maskoliunas M., Meszaros L., Mikolajczyk P., Mugrauer M.,
Netzel H., Ordasi A., Pakstiene E., Rybicki K.A., Sarneczky K., Seli B.,
Simon A., Siskauskaite K., Sodor A., Sokolovsky K.V., Stenglein W.,
Street R., Szakats R., Tomasella L., Tsapras Y., Vida K., Zdanavicius J.,
Zielinski M., Zielinski P., Ziolkowska O.
<Astrophys. J., 899, 130 (2020)>
=2020ApJ...899..130S 2020ApJ...899..130S
ADC_Keywords: Stars, variable; Photometry, VRI
Keywords: Star formation ; Accretion ; Protoplanetary disks ;
Eruptive variable stars
Abstract:
We present optical-infrared photometric and spectroscopic observations
of Gaia 18dvy, located in the Cygnus OB3 association at a distance of
1.88kpc. Gaia 18dvy was noted by the Gaia alerts system when its light
curve exhibited a ∼4mag rise in 2018-2019. The brightening was also
observable at mid-infared wavelengths. The infrared colors of Gaia
18dvy became bluer as the outburst progressed. Its optical and
near-infrared spectroscopic characteristics in the outburst phase are
consistent with those of bona fide FU Orionis-type young eruptive
stars. The progenitor of the outburst is probably a low-mass K-type
star with an optical extinction of ∼3mag. A radiative transfer
modeling of the circumstellar structure, based on the quiescent
spectral energy distribution, indicates a disk with a mass of
4x10-3M☉. Our simple accretion disk modeling implies that the
accretion rate had been exponentially increasing for more than 3yr
until mid-2019, when it reached a peak value of 6.9x10-6M☉/yr.
In many respects, Gaia 18dvy is similar to the FU Ori-type object HBC722.
Description:
We observed Gaia 18dvy in the BVRCIC bands between 2019 June and
December using the 60/90/180cm Schmidt telescope at the Konkoly
Observatory (Hungary).
We monitored Gaia 18dvy at optical wavelengths using the Optical
Infrared Coordination Network for Astronomy (OPTICON) Time-Domain
Follow-up Network (including the following telescopes: pt5m telescope
at the Roque de los Muchachos Observatory on La Palma; 0.8m Telescopi
Joan Oro (TJO) at l'Observatori Astronomic del Montsec in Spain; 1.4m
telescope at the Astronomical Station Vidojevica (ASV), near
Prokuplje, Serbia; 0.6m Bialkow Observatory, operated by the
Astronomical Institute of the University of Wroclaw, Poland; 0.35m
Cassegrain and 1.65m Ritchey-Chretien telescopes of Moletai
Astronomical Observatory in Moletai, Kulionys, Lithuania; 2.3m
Aristarchos Telescope at Helmos Observatory, Peloponnese, Greece; 2m
Ritchey-Chretien and 0.6m Cassegrain telescopes at the Terskol
Observatory (the North Caucasus, Russia) operated by ICAMER of NAS of
Ukraine; 0.6m Ritchey-Chretien telescope of the Michigan State
University Observatory (MPC code 766), USA) since 2019 February.
Gaia 18dvy was also observed with the Schmidt-Teleskop-Kamera of
University Observatory Jena in the Bessell V, R, and I bands. Each
night, two frames (60s) were taken in each filter.
Gaia 18dvy was also monitored with the Las Cumbres Observatory (LCO)
network of robotic telescopes. About 200 images have been obtained in
V and IC.
We obtained an optical spectrum of Gaia 18dvy with the Isaac Newton
Telescope (La Palma, Spain) on 2019 February 20, using the
Intermediate Dispersion Spectrograph. We took an optical spectrum on
2019 February 28 at the Copernico 1.82m telescope operated by
INAF-Osservatorio Astronomico di Padova (Asiago, Italy), using the
Asiago Faint Object Spectrograph (AFOSC). And we obtained a
near-infrared (NIR) spectrum of Gaia 18dvy on 2019 May 21 with NOTCam.
See Section 2.2.
Objects:
---------------------------------------------------------------
RA (2000) DE Designation(s)
---------------------------------------------------------------
20 05 06.03 +36 29 13.6 Gaia 18dvy = 2MASS J20050603+3629135
---------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 56 951 Follow-up photometry
--------------------------------------------------------------------------------
See also:
II/319 : UKIDSS-DR9 LAS, GCS and DXS Surveys (Lawrence+ 2012)
II/314 : UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/ApJ/454/151 : OB Associations of the Northern Milky Way (Massey+ 1995)
J/ApJ/733/L8 : Optical and IR photometry of [KOS94] HA11 (Kun+, 2011)
J/ApJ/750/99 : The Pan-STARRS1 photometric system (Tonry+, 2012)
J/ApJS/208/9 : Intrinsic colors and temperatures of PMS stars (Pecaut+, 2013)
http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia18dvy/ : Gaia alerts for Gaia18dvy
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.3 d MJD [8541/8830] Modified Julian Date (JD-2400000.5)
10- 12 A3 --- Band Photometry band (B, V, R_C, I_C, i and r)
14- 18 F5.2 mag mag [5.7/18] Magnitude measured in the band
20- 23 F4.2 mag e_mag [0/0.5] Uncertainty for magnitude
25- 56 A32 --- Inst Telescope used for measuring the magnitude
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 20-Oct-2021