2017A&A...600A.127K


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.19CET17:20:33

2017A&A...600A.127K - Astronomy and Astrophysics, volume 600A, 127-127 (2017/4-1)

Observational calibration of the projection factor of Cepheids. III. The long-period Galactic Cepheid RS Puppis.

KERVELLA P., TRAHIN B., BOND H.E., GALLENNE A., SZABADOS L., MERAND A., BREITFELDER J., DAILLOUX J., ANDERSON R.I., FOUQUE P., GIEREN W., NARDETTO N. and PIETRZYNSKI G.

Abstract (from CDS):

The projection factor (p-factor) is an essential component of the classical Baade-Wesselink (BW) technique, which is commonly used to determine the distances to pulsating stars. It is a multiplicative parameter used to convert radial velocities into pulsational velocities. As the BW distances are linearly proportional to the p-factor, its accurate calibration for Cepheids is of critical importance for the reliability of their distance scale. We focus on the observational determination of the p-factor of the long-period Cepheid RS Pup (P=41.5-days). This star is particularly important as this is one of the brightest Cepheids in the Galaxy and an analog of the Cepheids used to determine extragalactic distances. An accurate distance of 1910±80pc (±4.2%) has recently been determined for RS Pup using the light echoes propagating in its circumstellar nebula. We combine this distance with new VLTI/PIONIER interferometric angular diameters, photometry, and radial velocities to derive the p-factor of RS Pup using the code Spectro-Photo-Interferometry of Pulsating Stars (SPIPS). We obtain p=1.250±0.064 (±5.1%), defined for cross-correlation radial velocities. Together with measurements from the literature, the p-factor of RS Pup confirms the good agreement of a constant p{bar}=1.293±0.039(±3.0%) model with the observations. We conclude that the p-factor of Cepheids is constant or mildly variable over a broad range of periods (3.7 to 41.5-days).

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: individual: RS Pup - stars: variables: Cepheids - techniques: interferometric - techniques: photometric - stars: distances - distance scale - distance scale

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 OGLE LMC-CEP-227 cC* 04 52 15.6982549282 -70 14 31.242341027     15.317   14.438 ~ 47 0
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15113 1
3 * bet Dor cC* 05 33 37.5125319201 -62 29 23.323100433 5.13 4.58 3.76 3.55 3.12 F8/G0Ib 350 0
4 * zet Gem cC* 07 04 06.5307903 +20 34 13.073871 5.20 4.58 3.79   3.082 G1Ib 539 0
5 HD 67977 * 08 09 10.1888320527 -35 27 18.060190001   7.100 6.209     G8III 17 0
6 V* RS Pup cC* 08 13 04.2157137938 -34 34 42.691837063 8.89 8.00 6.70   5.453 F8Iab 323 0
7 HD 68978 PM* 08 13 34.4987340538 -31 44 07.381417481   7.36 6.75     G0.5V 74 0
8 HD 69002 * 08 13 41.0751948827 -33 34 10.297478683   7.537 6.377     K2III 14 0
9 HD 73947 * 08 39 50.1206584753 -34 00 35.318350023   8.46 7.08     K2III 9 0
10 * l Car cC* 09 45 14.8112246 -62 30 28.451894   4.33 3.40     G5Iab/b 293 1
11 [MMN2007] A1 gLS 14 17 35.9 +52 26 46     21.53   19.69 ~ 77 0
12 V* X Sgr cC* 17 47 33.6241002643 -27 49 50.848981593 5.84 5.34 4.54 6.03 3.661 F7II 312 0
13 * gam01 Sgr cC* 18 05 01.2265190154 -29 34 48.303215344 5.99 5.47 4.69   3.869 G0Ib/II 329 0
14 * kap Pav WV* 18 56 57.0309200480 -67 14 00.566631622   5.08 4.40     G5Iab/b 120 0
15 V* FF Aql cC* 18 58 14.7482217777 +17 21 39.295590199 6.61 6.18 5.38     F6Ib 346 0
16 V* V1154 Cyg cC* 19 48 15.4663192383 +43 07 36.959329251   9.92 9.14   8.120 G0 83 0
17 * del Cep cC* 22 29 10.2650184 +58 24 54.713856 4.71 4.35 3.75   3.219 F5Iab:+B7-8 685 0

    Equat.    Gal    SGal    Ecl

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