2020A&A...640A..42C


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.24CEST09:54:32

2020A&A...640A..42C - Astronomy and Astrophysics, volume 640A, 42-42 (2020/8-1)

RASSINE: Interactive tool for normalising stellar spectra. I. Description and performance of the code.

CRETIGNIER M., FRANCFORT J., DUMUSQUE X., ALLART R. and PEPE F.

Abstract (from CDS):


Aims. We provide an open-source code allowing an easy, intuitive, and robust normalisation of spectra.
Methods. We developed RASSINE, a Python code for normalising merged 1D spectra through the concepts of convex hulls. The code uses six parameters that can be easily fine-tuned. The code also provides a complete user-friendly interactive interface, including graphical feedback, that helps the user to choose the parameters as easily as possible. To facilitate the normalisation even further, RASSINE can provide a first guess for the parameters that are derived directly from the merged 1D spectrum based on previously performed calibrations.
Results. For HARPS spectra of the Sun that were obtained with the HELIOS solar telescope, a continuum accuracy of 0.20% on line depth can be reached after normalisation with RASSINE. This is three times better than with the commonly used method of polynomial fitting. For HARPS spectra of α Cen B, a continuum accuracy of 2.0% is reached. This rather poor accuracy is mainly due to molecular band absorption and the high density of spectral lines in the bluest part of the merged 1D spectrum. When wavelengths shorter than 4500Å are excluded, the continuum accuracy improves by up to 1.2%. The line-depth precision on individual spectrum normalisation is estimated to be ∼0.15%, which can be reduced to the photon-noise limit (0.10%) when a time series of spectra is given as input for RASSINE.
Conclusions. With a continuum accuracy higher than the polynomial fitting method and a line-depth precision compatible with photon noise, RASSINE is a tool that can find applications in numerous cases, for example stellar parameter determination, transmission spectroscopy of exoplanet atmospheres, or activity-sensitive line detection.

Abstract Copyright: © ESO 2020

Journal keyword(s): techniques: spectroscopic - methods: numerical - methods: data analysis

Simbad objects: 8

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Number of rows : 8

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 142 PM* 00 06 19.17544 -49 04 30.6817   6.30 5.76     F7V 212 1
2 * q01 Eri PM* 01 42 29.3148822519 -53 44 26.991165270   6.05 5.52     F9V 270 1
3 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1101 1
4 * e Eri PM* 03 19 55.6509352 -43 04 11.217495 5.20 4.98 4.27 3.65 3.25 G6V 399 1
5 * alf Hor PM* 04 14 00.1144482 -42 17 39.723208 5.97 4.96 3.86 3.00 2.41 K2III 132 0
6 CD-38 3220 * 07 10 24.0606039387 -39 05 50.570553937   11.00 10.51     F6V 33 0
7 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 901 1
8 * 61 Cyg A BY* 21 06 53.9396100677 +38 44 57.897024357 7.50 6.39 5.21 4.19 3.54 K5V 950 0

    Equat.    Gal    SGal    Ecl

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2020.10.24-09:54:32

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