| Ref | Type | Facility | Instrum. | Npt | Comments |
| Crouzet et al. 2012 | spec | Hubble Space Telescope satellite | Near Infrared Camera and Multi-Object Spectrometer | 15 | CROUZET ET AL 2012 Three transits of XO-2b were observed in spectrophotometry by HST NICMOS, on 2007 November 2, 2007 December 11, and 2008 February 12. Each visit is divided into 5 HST orbits, containing 68 images of 32 s each. In total, 1006 images were acquired. We used the G141 grism, covering a spectral range from 1.1 to 1.9μm. The length of the spectral trace is∼110 pixels, and the PSF (Point Spread Function) was defocused to a FWHM (Full Width Half Maximum) of 5 pixels to minimize the effect of inter- and intra-pixel variations. The resulting spectral resolution R=λ/∆λ= 37. The detector is read out in MULTIACCUM mode with NSAMP = 10,i.e.each image is composed of 10 successive readouts. When necessary, we will designate XO-2 as XO-2 N, and the companion star as XO-2 S (XO-2 N is located 30” north of XO-2 S). |
| Pearson et al. 2019 | spec | Association of Universities for Research in Astronomy (AURA) 8.1m Frederick C. Gillett Gemini North Telescope at Mauna Kea Observatory | GMOS | 60 | PEARSON ET AL 2019 Spectroscopic measurements of XO-2b were recorded with GMOS-N on 2016 January 05 at the Gemini 8.1 m Observatory on Mauna Kea in Hawaii (Allington-Smithet al. 2002). The spectrograph is equipped with a e2vdeep-depletion (DD) array of three CCDs which make a 6144×4608 pixel sensor with a plate scale of 0.0727′′per pixel. The three CCDs are stitched together to cre-ate a large detector with a∼20 pixel gap between each channels (lower pixel columns) exhibit a -0.5 pixel shift inposition relative to the first image, while the blue chan-nels (larger pixel columns) exhibit a 3 pixel shift relativeto the first image. XO-2S and XO-2N both exhibit a rotation but to varying extents. This rotation is negligible over our spectral extraction aperture because it produces at most a 0.12 pixel difference along the dispersion axis. |
| Pearson et al. 2019 | spec | National Optical Astronomy Observatory (NOAO) 4m Nicholas U. Mayall Telescope at Kitt Peak National Observatory (KPNO) | KOSMOS | 86 | PEARSON ET AL 2019 We obtained one transit observation of XO-2b with the 4 m Mayall Telescope on Kitt Peak in Arizona equipped with the multiobject visible-band spectrograph KOS-MOS on 2015 February 07. The spectrograph is equipped with a 2k x 4k e2v Deep Depletion CCD with a binned plate scale of 0.292′′/pixel (Martini et al. 2014). To reduce the read-out time to 19 seconds the CCD wasbinned 2x2. We used the Blue VPH grism, which has a wavelength range of 370–620 nm and R=2100 with peak transmission∼0.4 near 500 nm. |
| Sing et al. 2011 | spec | Gran Telescopio CANARIAS 10.4m telescope | OSIRIS | 4 | SING ET AL 2011 We observed with the GTC 10.4 meter telescope i using the Optical System for Imaging and low Resolution Integrated Spectroscopy (OSIRIS) instrument during three separate nights in service mode. We used the tunable filter (TF), which allows fornarrow-band imaging capable of specifying the wave-length(s) of our target and reference stars. The TF consists of a Fabry-Perot etalon, whose cavity separation can be adjusted, giving rise to a wide range of resolving powers, with OSIRIS capable of R=300 to 1000. |
| Zellem et al. 2015 | phot | Steward Observatorys 1.5 meter Kuiper Telescope | Mont4k CCD | 13 | ZELLEM ET AL 2015 Photometric measurements were conducted at the University of Arizona’s 61” (1.55 m) Kuiper Telescope,equipped with the Mont4k CCD, a 4096×4096 pixel sensor with a 9.7’×9.7’ field of view. Bessel U-band measurements alone were obtained on 2012 January 5, 2013 January 21, and 2013 February 24 (UT). Harris B-band measurements alone were obtained on 2012 October 29and 2014 January 30 (UT). Simultaneous U and B-bandmeasurements were taken on 2012 December 10, 2014February 12, 2015 January 18, and 2015 February 8(UT). Typical seeing was∼1.5” |
