![]() 2008) operating in the H band with the H23 filter pair (wavelength H2 = 1.587 μm wavelength H3 = 1.667 μm: Vigan et al. 2008) operating at a spectral resolution R = 50 in the wavelength range between 0.95 and 1.35 μm, with a field of view (FOV) of 1.7 × 1.7 arcsec 2 corresponding to a maximum projected separation from the star of ∼1 au and InfraRed Dual-band Imager and Spectrograph (IRDIS) (Dohlen et al. All the observations were performed in the IRDIFS mode, with the Integral Field Spectrograph (IFS) (Claudi et al. Proxima Cen was observed during six different nights as part of the Guaranteed Time Observations (GTO) programme of the SPHERE consortium. However, the same data can be exploited to put some constraints on the mass of possible objects around Proxima, after calculating the contrast obtained from these observations. This will give us a unique opportunity to measure the star mass directly (Zurlo et al., in preparation). This star is clearly visible even when it is not undergoing the microlensing effect. We have observed Proxima repeatedly with SPHERE in the past months, with the aim of obtaining precise astrometry of a background star that is undergoing a microlensing event caused by the approach of Proxima (Sahu et al. 2014), but never exploiting direct imaging techniques. 2014) and astrometric measurements (Lurie et al. Similar work has been done in the past, exploiting both the radial velocity (RV) technique (Endl & Kürster 2008 Zechmeister, Kürster & Endl 2009 Barnes et al. Exploiting direct imaging observations, it is possible to put some constraints on the mass and radius of other objects in the Proxima system. 2008), it would, however, be interesting to have information about further possible objects at larger separations to characterize the system fully. 2006) and Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) (Beuzit et al. Gemini Planet Imager (GPI) (Macintosh et al. While this planet, which has a separation of just 0.05 au with a period of 11.2 d and a minimum mass of 1.3 M ⊕, cannot be imaged with the current instrumentation aimed at detecting the emitted light from extrasolar planets, e.g. 2016), new interest arose in the nearest star system to the Sun. Instrumentation: spectrographs, methods: data analysis, techniques: imaging spectroscopy, stars: individual: Proxima Centauri, planetary systems 1 INTRODUCTIONĪfter the recent discovery of a terrestrial planet around the star Proxima Centauri (Anglada-Escudé et al. Since the residual noise for the observations is dominated by photon noise and thermal background, longer exposures in good observing conditions could improve the achievable contrast limit further. ![]() We also made an attempt to estimate the radius of possible planets around Proxima using the reflected light. We obtained mass limits of the order of 4 M Jup at separations of 2 au or larger, representing the most stringent mass limits at separations larger than 5 au available at the moment. The dual-band imaging camera IRDIS also enables us to probe larger separations than other techniques such as radial velocity or astrometry. Our IFS observations reveal that no planet more massive than ∼6–7 M Jup can be present within 1 au. No planet was detected directly, but we set upper limits on the mass up to 7 au by exploiting the AMES-COND models. We performed a series of observations of Proxima Centauri using Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE), the planet-finder instrument installed at the European Southern Observatory (ESO) Very Large Telescope (VLT) UT3, using its near-infrared modules, InfraRed Dual-band Imager and Spectrograph (IRDIS) and IFS. Writing 24 rows (of 1000 field and 35 index objects) to correspondence file.The recent discovery of an earth-like planet around Proxima Centauri has drawn much attention to this star and its environment. I would really like to be able to rely on ASTAP.įound tag-along columns from field: FLUX BACKGROUNDįield 1: solved with index index-4109.fits.įield 1: tried 3821 quads, matched 27977 codes. I even did the 180 degree search, which is supposed to do a blind solve, and even that fails. Can someone help with ASTAP settings for solving the attached image? is easily able to solve it but no matter what settings I try in ASTAP it fails to solve.
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