| Ref | Type | Facility | Instrum. | Npt | Comments |
| Bean et al. 2013 | spec | Magellan II Landon Clay Telescope | MMIRS | 9 | BEAN ET AL 2013. e present ground-based measurements of the transmission and emission spectra of the hot-Jupiter WASP-19b in nine spectroscopic channels from 1.25 to 2.35 μm |
| Huitson et al. 2013 | spec | Hubble Space Telescope satellite | Space Telescope Imaging Spectrograph | 4 | HUITSON ET AL 2013 We measure the transmission spectrum of WASP-19b from three transits usinglow-resolution optical spectroscopy from the Hubble Space Telescope (HST) SpaceTelescope Imaging Spectrograph (STIS). The STIS spectra cover a wavelength rangeof 0.29-1.03μm, with resolving powerR= 500. |
| Huitson et al. 2013 | spec | Hubble Space Telescope satellite | Wide Field Camera 3 | 6 | HUITSON ET AL 2013 The optical data are combined witharchival near-infrared data from the HST Wide Field Camera 3 (WFC3) G141 grism,covering the wavelength range from 1.087 to 1.687μm, with resolving powerR= 130.HUITSON ET AL 2013 |
| Lendl et al. 2013 | phot | La Silla Observatorys 60-cm TRAPPIST Telescope | TRAPPISTCam | 1 | LENDL ET AL 2013 Nine transits and four occultations of WASP-19b were observedwith the robotic 60 cm TRAPPIST |
| Lendl et al. 2013 | phot | The Swiss Euler 1.2m Telescope | EulerCam | 3 | LENDL ET AL 2013 Five transit and six occultation lightcurves have been obtained with EulerCam, the imager of the Euler-Swiss telescope at LaSilla. |
| Mancini et al. 2013 | phot | 0.3-m Perth Exoplanet Survey Telescope | | 1 | MANCINI ET AL 2013 One partial transit and seven full transits of WASP 19 were observed using the DFOSC imager mounted on the 1.54 m Danish Telescope at La Silla during the MindStep campaigns in 2010 and 2011. The instrument has a field of view of 13.7 x 13.7 and a plate scale of 0.39 '' pixel. All observations were performed through a Gunn i filter and using the defocussing method. |
| Mancini et al. 2013 | phot | Danish 1.54m telescope at European Southern Observatory | DFOSC imager | 1 | MANCINI ET AL 2013. One transit was observed on 2012 April 15 with the GROND instrument mounted on the MPG/ESO 2.2m telescope at ESO La Silla, Chile. GROND is an imaging system, capable of simultaneous photometric observations in four optical (similar to Sloan g', r', i', z') and three NIR (J, H, K) passbands. |
| Mancini et al. 2013 | phot | Max Planck Gesellschaft 2.2 meter Telescope at European Southern Observatory | GROND | 4 | MANDELL ET AL 2013 Observations of WASP-19 b using the Wide Field Camera 3 on the HST were conducted between June and July 2011. The observations were taken with the G141 grism on WFC's infrared channel providing slitless spectra covering the wavelenght range 1.1 to 1.7 microns at aa maximun resolving powerof 130 at 1.4 microns |
| Mandell et al. 2013 | spec | Hubble Space Telescope satellite | Wide Field Camera 3 | 19 | MANDELL ET AL 2013 Observations of WASP-19 b using the Wide Field Camera 3 on the HST were conducted between June and July 2011. The observations were taken with the G141 grism on WFC's infrared channel providing slitless spectra covering the wavelenght range 1.1 to 1.7 microns at aa maximun resolving powerof 130 at 1.4 microns |
| Sedaghati et al. 2015 | spec | Very Large Telescope (Antu) | FORS2 | 27 | We observed WASP-19 between 2014 November 16 05:16 UTand 08:49 UT with FORS2, under thin cirrus, in multi-object spectroscopic mode (MXU), using a mask with slits 30′′ long and 10′′wide placed on WASP-19, as well as on six reference stars. Data were binned (2×2), yielding a scale of 0.25′′perpixel. Grism 600RI (with the order sorter filter GG435) was used, leading to a wavelength coverage1of about 550 to 830 nm.Our observations covered a full transit, while the object moved from airmass 2.5 to 1.2, with the seeing varying between 0.8′′ and 2.2′′. The high airmass at the start, in combination with thecirrus, is most likely the cause of the larger scatter in the lightcurve prior to ingress (Fig. 1). Using the MIT CCD, time se-ries of the target and reference stars were obtained using 30sexposures until 08:18 UT2. The LADC was left in park positionduring the whole observing sequence, with the two prisms fixedat their minimal separation (30 mm). In total, we had 155 usefulexposures, 85 of which were taken in transit. The typical signal-to-noise ratio of WASP-19 on one spectrum was about 300 at thecentral wavelength. |
| Tregloan-Reed et al. 2013 | phot | New Technology Telescope | EFOSC2 | 3 | TREGLOAN REED ET AL 2013. New Technology Telescope (NTT) operated at ESO LaSilla, Chile. The instrument used was EFOSC2, operated in imagingmode and with a Gunnrfilter (ESO filter #786).
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| Wong et al. 2016 | phot | Spitzer Space Telescope satellite | Infrared Array Camera (IRAC) | 2 | WONG ET AL 2016. We analyze full-orbit phase curve observations of the transiting hot Jupiters WASP-19b and HAT-P-7b at 3.6 and 4.5 μm, obtained using the Spitzer Space Telescope. For WASP-19b, we measure secondary eclipse depths of 0.485% +/- 0.024% and 0.584% +/- 0.029% at 3.6 and 4.5 microns, which are consistent with a single blackbody with effective temperature 2372 +/- 60 K |
| Zhou et al. 2013 | spec | Faulkes Telescope South | Merope 2Kx2K | 1 | ZHOU ET AL 2013. We monitored an eclipse of WASP-19b using the 2 mFaulkes Telescope South (FTS), located at Siding Spring Observatory, Australia, on 2012 December 29. Observations were performed in the Pan-STARRS z-band centred at 0.866 μm |
| Exoplanets-A (CASCADe) | spec | HST | WFC3 | 25 | Exoplanets-A reduction
CASCADE v. 1.0.0
Created:2021_2_27:12_23_37
Obs.Type:transit |
| Exoplanets-A (CASCADe) | spec | HST | WFC3 | 25 | Exoplanets-A reduction
CASCADE v. 1.0.0
Created:2021_2_27:12_31_14
Obs.Type:eclipse |
