VizieR Online Data Catalog: ~30yr of opt. spectroscopy & Vmag obs. of GW Ori (Czekala+, 2017)

GW Ori was observed with the ALMA interferometer on 2015 May 14 (program ID 2012.1.00496.S), with 37 of the 12m main array antennas configured to span baselines of 23-558m. The ALMA correlator was set up to process data in four spectral windows: 220.426 and 230.450GHz to observe the ¹³CO and ¹²CO J=2-1 transitions, around 219.763GHz to observe the C¹⁸O J=2-1 transition and the continuum in a 1.875GHz range around 231.956GHz. The observations cycled between GW Ori and the quasar J0510+1800 with a 7-minute cadence. See section 2.1 for further details.

GW Ori was monitored spectroscopically at the Harvard-Smithsonian Center for Astrophysics for more than 35yr, beginning in 1981 November. A total of 203 usable spectra were gathered through 2009 April using three nearly identical echelle spectrographs with a resolving power of R~35000 mounted on three different telescopes: the 1.5m Tillinghast reflector at the Fred L. Whipple Observatory (Mount Hopkins, AZ), the 4.5m equivalent Multiple Mirror Telescope (also on Mount Hopkins) before conversion to a monolithic mirror, and occasionally on the 1.5m Wyeth reflector at the Oak Ridge Observatory (in the town of Harvard, MA). See section 2.2 for further explanations.

We have assembled a high-cadence light curve of GW Ori covering a ~30yr time span by drawing from several ongoing photometric surveys and archival observations. Photoelectric UBVR observations of GW Ori were obtained at Mount Maidanak Observatory in Uzbekistan from 1987 to 2003. See section 2.3.1. Both telescopes of the Kilodegree Extremely Little Telescope (KELT) project use a broad R-band filter. GW Ori was located in KELT-South field 05 and was observed 2889 times from UT 2010 February 28 until UT 2015 April 09, with a median uncertainty of 0.005 mag. See section 2.3.2. The two observatory (Las Campanas, Chile, and Haleakala, Maui) of All-sky Automated Survey (ASAS) observed GW Ori in the V band from UT 2001 March 11 until UT 2009 November 29, obtaining 480 observations with a median per-point uncertainty of 0.036mag. See section 2.3.3. ASAS-SN surveys the entire sky down to V~17mag every ~2days. Hosted by the Las Cumbres Observatory at Mount Haleakala, Hawaii, and the Cerro Tololo Inter-American Observatory in Chile. ASAS-SN obtained 799 observations of GW Ori from UT 2014 December 16 until UT 2017 March 15, with a typical per-point error of 0.01mag. See section 2.3.4.

(2 data files).