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


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.17CEST03:52:57

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 reference 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 - 2019
#notes
1 SV* HV 1328 cC* 00 32 54.9174261947 -73 49 19.086114742   14.17 14.116   13.431 ~ 28 0
2 SV* HV 1333 cC* 00 36 03.4614162922 -73 55 58.866210528   15.87 14.702   13.820 ~ 21 0
3 SV* HV 1335 cC* 00 36 55.6923398590 -73 56 28.055695177   15.399 14.746   13.983 ~ 29 0
4 SV* HV 1345 cC* 00 40 38.5968646914 -73 13 14.312423788   15.428 14.779   13.957 ~ 23 0
5 SV* HV 822 cC* 00 41 55.4775921384 -73 32 23.609186717   14.39 14.524   13.618 ~ 25 0
6 IC 1613 GiC 01 04 54.2 +02 08 00   10.42 10.01 9.77   ~ 1079 2
7 SV* HV 12717 cC* 04 43 20.8472580242 -69 13 47.811181001   15.48 14.733 14.20 13.950 ~ 25 0
8 OGLE LMC-CEP-79 cC* 04 47 06.8782178918 -69 17 39.491131004   15.02 14.116 13.62 13.114 ~ 13 1
9 SV* HV 12452 cC* 04 48 51.3419131055 -69 21 22.760708546   15.53 14.755 14.40 13.941 ~ 27 0
10 SV* HV 873 cC* 04 54 23.7766671988 -70 54 05.736569775   12.97 12.44 12.58 12.178 F8I 45 0
11 SV* HV 877 cC* 04 57 01.7945303401 -67 59 42.590749460   14.10 13.363   12.232 ~ 48 0
12 SV* HV 876 cC* 04 57 12.3634768644 -67 22 57.294407958   14.29 13.666 13.32 12.711 ~ 23 0
13 SV* HV 878 cC* 04 57 51.0484622567 -69 57 29.682156385   13.40 13.564 13.62 12.722 ~ 40 0
14 SV* HV 12505 cC* 04 57 56.7395086983 -68 48 57.612570508   16.99 14.847 14.75 13.808 ~ 18 0
15 SV* HV 879 cC* 04 58 05.5960529644 -69 27 15.481012522   14.72 13.356 13.01 12.341 ~ 51 0
16 HD 268878 cC* 04 58 10.7957486662 -69 56 58.783004889   13.83 13.02 12.96 12.071 K5 67 0
17 SV* HV 881 cC* 04 58 32.8021199081 -70 20 45.717120470   13.26 13.064 12.61 12.19 ~ 35 0
18 SV* HV 2282 cC* 05 01 24.9394908748 -70 04 18.288809757   15.10 14.332 13.95 13.427 ~ 22 0
19 SV* HV 2338 cC* 05 06 08.8557525637 -71 15 26.119435535   12.83 12.26   11.858 ~ 60 0
20 HD 269075 cC* 05 06 47.9723051964 -70 02 13.297259550   13.30 12.48 12.77 11.842 M 63 0
21 SV* HV 899 cC* 05 07 07.8253500672 -68 53 19.453088959   13.50 13.343 12.83 12.449 ~ 51 0
22 SV* HV 909 cC* 05 09 20.1376380251 -70 27 27.043906162   13.32 12.67 12.11 11.949 ~ 61 0
23 SV* HV 5655 cC* 05 11 05.4172717803 -70 30 34.412175091   15.46 14.563 14.06 13.578 ~ 26 0
24 SV* HV 914 cC* 05 12 47.0348475429 -69 06 08.881909422     14.926   14.197 ~ 25 0
25 SV* HV 12197 Ce* 05 13 13 -65 30.8   16.741 16.102     ~ 27 0
26 SV* HV 12199 Ce* 05 13 19 -65 29.5   16.916 16.289     ~ 29 0
27 SV* HV 12198 cC* 05 13 26.6694544251 -65 27 04.933284395   16.627 15.970   15.230 ~ 38 0
28 NGC 1866 GlC 05 13 38.920 -65 27 52.75   9.98 9.73     ~ 385 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 53.6708479354 -67 03 48.447940301 14.7 12.88 12.21   11.648 F5?I? 62 0
32 SV* HV 12204 cC* 05 13 57.8780755 -65 28 39.329725   16.18 15.715   15.076 ~ 31 0
33 SV* HV 2405 cC* 05 14 41.5552104934 -70 42 32.084769065   15.88 15.151 14.70 14.355 ~ 26 0
34 SV* HV 2527 cC* 05 25 39.1089344552 -71 06 39.848335076   15.49 14.615 14.16 13.670 ~ 32 0
35 SV* HV 2549 cC* 05 27 00.5741196389 -71 38 35.749590862   14.34 13.796 13.36 12.890 ~ 38 0
36 SV* HV 2538 cC* 05 27 07.7609332305 -68 29 42.908268981   15.32 14.475 14.05 13.468 ~ 20 0
37 SV* HV 12816 cC* 05 29 58.4215724392 -65 54 20.309760307   15.09 14.49 14.13 13.846 ~ 38 0
38 SV* HV 12815 cC* 05 30 02.4652196559 -65 56 01.785181166   14.39 14.04 13.48 12.551 ~ 44 0
39 SV* HV 1005 cC* 05 36 06.7992237500 -68 49 13.369825110   14.92 14.70 14.12 13.222 ~ 30 0
40 SV* HV 1006 cC* 05 37 22.4444907013 -69 28 59.372408599   15.23 14.398 13.91 13.478 ~ 20 0
41 SV* HV 2827 cC* 05 43 47.3080229900 -66 35 08.943172884   13.37 12.02   11.220 M 54 0
42 SV* HV 1023 cC* 05 46 36.1850662920 -68 11 03.440243508   14.66 14.06 13.52 12.775 ~ 39 0
43 SV* HV 6093 cC* 05 57 46.8444050721 -68 41 04.284451547   15.96 15.304 15.02 14.628 ~ 26 0

    Equat.    Gal    SGal    Ecl

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


2019.10.17-03:52:57

© Université de Strasbourg/CNRS

    • Contact