2006A&A...453..309N


Query : 2006A&A...453..309N

2006A&A...453..309N - Astronomy and Astrophysics, volume 453, 309-319 (2006/7-1)

High resolution spectroscopy for Cepheids distance determination. I. Line asymmetry.

NARDETTO N., MOURARD D., KERVELLA P., MATHIAS P., MERAND A. and BERSIER D.

Abstract (from CDS):

The ratio of pulsation to radial velocity (the projection factor) is currently limiting the accuracy of the Baade-Wesselink method, and in particular of its interferometric version recently applied to several nearby Cepheids. This work aims at establishing a link between the line asymmetry evolution over the Cepheids' pulsation cycles and their projection factor, with the final objective to improve the accuracy of the Baade-Wesselink method for distance determinations. We present HARPS high spectral resolution observations (R=120000) of nine galactic Cepheids: R Tra, S Cru, Y Sgr, {beta} Dor, {zeta} Gem, Y Oph, RZ Vel, l Car and RS Pup, having a good period sampling (P=3.39d to P=41.52d). We fit spectral line profiles by an asymmetric bi-Gaussian to derive radial velocity, Full-Width at Half-Maximum in the line (FWHM) and line asymmetry for all stars. We then extract correlations curves between radial velocity and asymmetry. A geometric model providing synthetic spectral lines, including limb-darkening, a constant FWHM (hereafter σC) and the rotation velocity is used to interpret these correlations curves. For all stars, comparison between observations and modelling is satisfactory, and we were able to determine the projected rotation velocities and σC for all stars. We also find a correlation between the rotation velocity (Vrotsini) and the period of the star: Vrotsini=(-11.5±0.9)log(P)+(19.8±1.0)[km/s]. Moreover, we observe a systematic shift in observational asymmetry curves (noted γO), related to the period of the star, which is not explained by our static model: γO=(-10.7±0.1)log(P)+(9.7±0.2)[in %]. For long-period Cepheids, in which velocity gradients, compression or shock waves seem to be large compared to short- or medium-period Cepheids we observe indeed a greater systematic shift in asymmetry curves. This new way of studying line asymmetry seems to be very promising for a better understanding of Cepheids atmosphere and to determine, for each star, a dynamic projection factor.

Abstract Copyright:

Journal keyword(s): techniques: spectroscopic - stars: atmospheres - stars: oscillations - stars: variables: Cepheids - stars: distances

VizieR on-line data: <Available at CDS (J/A+A/453/309): table1.dat table345.dat>

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 * bet Dor cC* 05 33 37.5159729864 -62 29 23.376457680 5.13 4.58 3.76 3.55 3.12 F8/G0Ib 365 0
2 * zet Gem cC* 07 04 06.5312384690 +20 34 13.074474962 5.20 4.58 3.79   3.082 G1Ib 553 0
3 V* RS Pup cC* 08 13 04.2157111224 -34 34 42.696447852 8.89 8.51 7.04   5.453 F8Iab 337 0
4 V* RZ Vel cC* 08 37 01.3028699904 -44 06 52.846248456   8.507 7.260     G1Ib 216 0
5 * l Car cC* 09 45 14.8117044917 -62 30 28.450312664   5.09 3.75     G5Iab/b 309 0
6 * L Car * 10 22 58.1460612 -66 54 05.390302 4.35 4.86 4.99     B8V 105 0
7 V* S Cru cC* 12 54 21.9975732000 -58 25 50.215759464 7.94 7.34 6.58   5.730 F7Ib/II 183 0
8 V* R TrA cC* 15 19 45.7128267840 -66 29 45.743160624 7.29 6.96 6.39   5.844 F7Ib/II 182 0
9 V* Y Oph cC* 17 52 38.7019050072 -06 08 36.874071816 8.62 7.61 6.21     G3Ia 357 0
10 V* Y Sgr cC* 18 21 22.9862401944 -18 51 36.006450458 7.31 6.69 5.75   4.810 F8II 283 0

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2022.11.28-08:56:29

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