2011A&A...534A..95S


Query : 2011A&A...534A..95S

2011A&A...534A..95S - Astronomy and Astrophysics, volume 534A, 95-95 (2011/10-1)

Calibrating the Cepheid period-luminosity relation from the infrared surface brightness technique. II. The effect of metallicity and the distance to the LMC'.

STORM J., GIEREN W., FOUQUE P., BARNES T.G., SOSZYNSKI I., PIETRZYNSKI G., NARDETTO N. and QUELOZ D.

Abstract (from CDS):

The extragalactic distance scale builds directly on the Cepheid period-luminosity (PL) relation as delineated by the sample of Cepheids in the Large Magellanic Cloud (LMC). However, the LMC is a dwarf irregular galaxy, quite different from the massive spiral galaxies used for calibrating the extragalactic distance scale. Recent investigations suggest that not only the zero-point but also the slope of the Milky Way PL relation differ significantly from that of the LMC, casting doubts on the universality of the Cepheid PL relation. We want to make a differential comparison of the PL relations in the two galaxies by delineating the PL relations using the same method, the infrared surface brightness method (IRSB), and the same precepts. We furthermore extend the metallicity baseline for investigating the zero-point dependence, by applying the method to five SMC Cepheids as well. The IRSB method is a Baade-Wesselink type method to determine individual distances to Cepheids. We apply a newly revised calibration of the method as described in an accompanying paper (Storm et al., 2011A&A...534A..94S, Paper I) to 36 LMC and five SMC Cepheids and delineate new PL relations in the V,I,J, & K bands as well as in the Wesenheit indices in the optical and near-IR. We present 509 new and accurate radial velocity measurements for a sample of 22 LMC Cepheids, enlarging our earlier sample of 14 stars to include 36 LMC Cepheids. The new calibration of the IRSB method is directly tied to the recent HST parallax measurements to ten Milky Way Cepheids, and we find a LMC barycenter distance modulus of 18.45±0.04 (random error only) from the 36 individual LMC Cepheid distances. In the J,K bands we find identical slopes for the LMC and Milky Way PL relations and only a weak letallicity effect on the zero points (consistent with a zero effect), metal poor stars being fainter. In the optical we find the Milky Way slopes are slightly shallower than the LMC slopes (but again consistent with no difference in the slopes) and small effects on the zero points. However, the important Wesenheit index in V,(V-I) shows a metallicity effect on the slope and on the zero point which is likely to be significant. We find a significant metallicity effect on the WVIindex γ(WVI)=-0.23±0.10mag/dex as well as an effect on the slope. The K-band PL relation on the other hand is found to be an excellent extragalactic standard candle being metallicity insensitive in both slope and zero-point and at the same time being reddening insensitive and showing the least internal dispersion.

Abstract Copyright:

Journal keyword(s): stars: variables: Cepheids - stars: fundamental parameters - stars: distances - Magellanic Clouds - distance scale

VizieR on-line data: <Available at CDS (J/A+A/534/A95): table3.dat table2.dat>

Simbad objects: 43

goto Full paper

goto View the references in ADS

Number of rows : 43
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 SV* HV 1328 cC* 00 32 54.9172871016 -73 49 19.085722104   14.17 14.116   13.431 ~ 31 0
2 SV* HV 1333 cC* 00 36 03.4615743240 -73 55 58.867078620   15.87 14.702   13.820 ~ 24 0
3 SV* HV 1335 cC* 00 36 55.6921565160 -73 56 28.053638520   15.399 14.746   13.983 ~ 32 0
4 SV* HV 1345 cC* 00 40 38.5969623096 -73 13 14.311161660   15.428 14.779   13.957 ~ 24 0
5 SV* HV 822 cC* 00 41 55.4776238040 -73 32 23.608342176   14.39 14.524   13.618 ~ 27 0
6 IC 1613 GiC 01 04 54.2 +02 08 00   10.42 10.01 9.77   ~ 1179 2
7 SV* HV 12717 cC* 04 43 20.8471430712 -69 13 47.809980552   15.48 14.733 14.20 13.950 ~ 28 0
8 OGLE LMC-CEP-79 cC* 04 47 06.8785090776 -69 17 39.488964900   15.02 14.116 13.62 13.114 ~ 13 1
9 SV* HV 12452 cC* 04 48 51.3419874096 -69 21 22.760929404   15.53 14.755 14.40 13.941 ~ 30 0
10 SV* HV 873 cC* 04 54 23.7765040872 -70 54 05.735484684   12.97 12.44 12.58 12.178 F8I 48 0
11 SV* HV 877 cC* 04 57 01.7944309968 -67 59 42.589297284   14.10 13.363   12.232 ~ 50 0
12 SV* HV 876 cC* 04 57 12.3631684656 -67 22 57.291144672   14.29 13.666 13.32 12.711 ~ 24 0
13 SV* HV 878 cC* 04 57 51.0483921048 -69 57 29.683493100   13.40 13.623 13.62 12.693 ~ 42 0
14 SV* HV 12505 cC* 04 57 56.7393106608 -68 48 57.612161700   16.99 14.847 14.75 13.808 ~ 20 0
15 SV* HV 879 cC* 04 58 05.5960382376 -69 27 15.480133020   14.72 13.457 13.01 12.299 ~ 56 0
16 HD 268878 cC* 04 58 10.7956592640 -69 56 58.781211396   13.83 13.134 12.96 12.005 K5 71 0
17 SV* HV 881 cC* 04 58 32.8016229936 -70 20 45.716108784   13.26 13.175 12.61 12.156 ~ 38 0
18 SV* HV 2282 cC* 05 01 24.9394462656 -70 04 18.287395644   15.10 14.446 13.95 13.350 ~ 26 0
19 SV* HV 2338 cC* 05 06 08.8555282080 -71 15 26.118906300   12.83 12.26   11.858 ~ 60 0
20 HD 269075 cC* 05 06 47.9715275784 -70 02 13.295472684   13.30 12.944 12.77 11.861 M 65 0
21 SV* HV 899 cC* 05 07 07.8256721256 -68 53 19.448617524   13.50 13.471 12.83 12.403 ~ 53 0
22 SV* HV 909 cC* 05 09 20.1372980832 -70 27 27.043469748   13.32 12.67 12.11 11.949 ~ 62 0
23 SV* HV 5655 cC* 05 11 05.4172344768 -70 30 34.412745888   15.46 14.563 14.06 13.578 ~ 28 0
24 SV* HV 914 cC* 05 12 47.0346290592 -69 06 08.881150860     14.926   14.197 ~ 26 0
25 SV* HV 12197 Ce* 05 13 13 -65 30.8   16.741 16.102     ~ 28 0
26 SV* HV 12199 Ce* 05 13 19 -65 29.5   16.916 16.289     ~ 30 0
27 SV* HV 12198 cC* 05 13 26.6692125288 -65 27 04.932684468   16.627 15.970   15.230 ~ 40 0
28 NGC 1866 GlC 05 13 38.920 -65 27 52.75           ~ 406 0
29 SV* HV 12202 Ce* 05 13 39 -65 29.0   16.756 16.080     ~ 28 0
30 SV* HV 12203 Ce* 05 13 40 -65 29.6   16.811 16.140     ~ 29 0
31 SV* HV 2369 cC* 05 13 53.6706712704 -67 03 48.446510436 14.7 12.88 12.21   11.648 F5?I? 64 0
32 SV* HV 12204 cC* 05 13 57.8740222848 -65 28 39.333037188   16.18 15.715   15.076 ~ 32 0
33 SV* HV 2405 cC* 05 14 41.5551364872 -70 42 32.084016804   15.88 15.151 14.70 14.355 ~ 28 0
34 SV* HV 2527 cC* 05 25 39.1090655328 -71 06 39.848203476   15.49 14.615 14.16 13.670 ~ 35 0
35 SV* HV 2549 cC* 05 27 00.5741329320 -71 38 35.749371876   14.34 13.796 13.36 12.890 ~ 40 0
36 SV* HV 2538 cC* 05 27 07.7611991376 -68 29 42.907715952   15.32 14.475 14.05 13.468 ~ 21 0
37 SV* HV 12816 cC* 05 29 58.4215444680 -65 54 20.308873644   15.09 14.49 14.13 13.846 ~ 40 0
38 SV* HV 12815 cC* 05 30 02.4652768272 -65 56 01.783841568   14.39 14.04 13.48 12.551 ~ 44 0
39 SV* HV 1005 cC* 05 36 06.7990326216 -68 49 13.370391588   14.92 14.70 14.12 13.222 ~ 33 0
40 SV* HV 1006 cC* 05 37 22.4442138216 -69 28 59.373425928   15.23 14.398 13.91 13.478 ~ 23 0
41 SV* HV 2827 cC* 05 43 47.3076015504 -66 35 08.943397872   13.37 12.02   11.220 M 57 0
42 SV* HV 1023 cC* 05 46 36.1848254832 -68 11 03.439255668   14.66 14.06 13.52 12.775 ~ 43 0
43 SV* HV 6093 cC* 05 57 46.8445419408 -68 41 04.285724352   15.96 15.304 15.02 14.628 ~ 29 0

To bookmark this query, right click on this link: simbad:objects in 2011A&A...534A..95S and select 'bookmark this link' or equivalent in the popup menu


2022.12.01-01:40:42

© Université de Strasbourg/CNRS

    • Contact