{"paper":{"title":"Internal calibration of Gaia BP/RP low-resolution spectra","arxiv_id":"2106.01752","primary_cat":"astro-ph.IM","submitted_at":"2021-06-03T11:04:28+00:00","version_compiled":"v2"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v2","sentences":[{"i":0,"p":0.97,"id":"s0","own":false,"role":"background","text":"The full third Gaia data release will provide the calibrated spectra obtained with the blue and red Gaia slit-less spectrophotometers.","hedge":{"p":0.93,"label":"asserted"},"own_p":0.12,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.24,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.97,"limitation":0.0,"future_work":0.01,"contribution":0.01,"interpretation":0.0}},{"i":1,"p":0.87,"id":"s1","own":false,"role":"background","text":"The main challenge when facing Gaia spectral calibration is that no lamp spectra or flat fields are available during the mission.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.14,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.13,"role_probabilities":{"gap":0.12,"method":0.0,"result":0.0,"background":0.87,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.99,"id":"s2","own":false,"role":"background","text":"Also, the significant size of the line spread function with respect to the dispersion of the prisms produces alien photons contaminating neighbouring positions of the spectra.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.2,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.69,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.99,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.86,"id":"s3","own":false,"role":"background","text":"This makes the calibration special and different from standard approaches.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.11,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.12,"role_probabilities":{"gap":0.01,"method":0.0,"result":0.0,"background":0.86,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.12}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"contribution","text":"This work gives a detailed description of the internal calibration model to obtain the spectrophotometric data in the Gaia catalogue.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.84,"main_claim_p":0.11,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":1.0,"interpretation":0.0}},{"i":5,"p":0.5,"id":"s5","own":false,"role":"method","text":"The main purpose of the internal calibration is to bring all the epoch spectra onto a common flux and pixel (pseudo-wavelength) scale, taking into account variations over the focal plane and with time, producing a mean spectrum from all the observations of the same source.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.49,"main_claim_p":0.23,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.5,"result":0.0,"background":0.02,"limitation":0.0,"future_work":0.0,"contribution":0.48,"interpretation":0.0}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"method","text":"In order to describe all observations in a common mean flux and pseudo-wavelength scale, we construct a suitable representation of the internally calibrated mean spectra via basis functions and we describe the transformation between non calibrated epoch spectra and calibrated mean spectra via a discrete convolution, parametrising the convolution kernel to recover the relevant coefficients.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.13,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":1.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":7,"p":0.55,"id":"s7","own":true,"role":"contribution","text":"The model proposed here is able to combine all observations into a mean instrument to allow the comparison of different sources and observations obtained with different instrumental conditions along the mission and the generation of mean spectra from a number of observations of the same source.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.82,"main_claim_p":0.32,"quantitative":false,"quantitative_p":0.14,"role_probabilities":{"gap":0.0,"method":0.23,"result":0.1,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.55,"interpretation":0.12}},{"i":8,"p":0.52,"id":"s8","own":true,"role":"method","text":"The output of this model provides the internal mean spectra, not as a sampled function (flux and wavelength), but as a linear combination of basis functions, although sampled spectra can easily be derived from them.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.87,"main_claim_p":0.22,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":0.52,"result":0.33,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.13,"interpretation":0.02}}]},"compiled":{"main_claim":{"p":0.97,"text":"The model proposed here is able to combine all observations into a mean instrument to allow the comparison of different sources and observations obtained with different instrumental conditions along the mission and the generation of mean spectra from a number of observations of the same source.","location":"abstract s7","hedge_strength":{"p":0.98,"label":"asserted"}},"provenance":{"route":{"via":"TypeSafe 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