2010A&A...515A.106F


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.18CEST12:21:14

2010A&A...515A.106F - Astronomy and Astrophysics, volume 515, A106-106 (2010/6-1)

Evaluating the stability of atmospheric lines with HARPS.

FIGUEIRA P., PEPE F., LOVIS C. and MAYOR M.

Abstract (from CDS):

When searching for extrasolar systems using the radial velocity technique, the need for high-precision measurements implies that a precise wavelength calibration is required. The choice of the calibrator is a particularly important open question in the infra-red domain, where precision and achievements remain inferior to those in the optical. We investigate the long-term stability of atmospheric lines as a precise wavelength reference and analyze their sensitivity to different atmospheric and observing conditions.We use HARPS archival data for three bright stars, tau Ceti, µ Arae, and e Eri, which span 6 years and include high-cadence measurements performed over several nights. We cross-correlate this data with an O2 mask and evaluate both radial velocity and bisector variations to a photon noise level of 1m/s.We find that the telluric lines in the three data-sets are stable down to 10m/s (rms) over the 6 years. We also show that the radial velocity variations can be modeled by simple atmospheric models, yielding a final precision of 1-2m/s.The long-term stability of atmospheric lines was 10m/s over six years, in spite of atmospheric phenomena. Atmospheric lines can be used as a wavelength reference for short timescale programs, yielding a precision of 5m/s without any correction. A higher precision, of 2m/s, can be reached if the atmospheric phenomena are corrected for using the simple atmospheric model described, making it a very competitive method even on long timescales.

Abstract Copyright:

Journal keyword(s): atmospheric effects - instrumentation: spectrographs - methods: observational - techniques: radial velocities - planetary systems

Simbad objects: 7

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Number of rows : 7

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1064 1
2 * e Eri PM* 03 19 55.6509352 -43 04 11.217495 5.20 4.98 4.27 3.65 3.25 G6V 392 1
3 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1658 1
4 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1740 0
5 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2090 0
6 * mu. Ara PM* 17 44 08.7036342277 -51 50 02.591049123   5.85 5.15     G3IV-V 455 2
7 * 51 Peg ** 22 57 27.9804167474 +20 46 07.782240714 6.39 6.16 5.46 4.97 4.61 G2IV 1058 1

    Equat.    Gal    SGal    Ecl

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2019.10.18-12:21:14

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