2005ApJ...627..224G


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.16CEST20:21:39

2005ApJ...627..224G - Astrophys. J., 627, 224-237 (2005/July-1)

Direct distances to Cepheids in the Large Magellanic Cloud: evidence for a universal slope of the period-luminosity relation up to solar abundance.

GIEREN W., STORM J., BARNES III T.G., FOUQUE P., PIETRZYNSKI G. and KIENZLE F.

Abstract (from CDS):

We have applied the infrared surface brightness (ISB) technique to derive distances to 13 Cepheid variables in the LMC that span a period range from 3 to 42 days. From the absolute magnitudes of the variables calculated from these distances, we find that the LMC Cepheids define tight period-luminosity (PL) relations in the V, I, W, J, and K bands that agree exceedingly well with the corresponding Galactic PL relations derived from the same technique and are significantly steeper than the LMC PL relations in these bands observed by the OGLE-II Project in V, I, and W and by Persson and coworkers in J and K. We find that the LMC Cepheid distance moduli we derive, after correcting them for the tilt of the LMC bar, depend significantly on the period of the stars, in the sense that the shortest period Cepheids have distance moduli near 18.3, whereas the longest period Cepheids are found to lie near 18.6. Since such a period dependence of the tilt-corrected LMC distance moduli should not exist, there must be a systematic, period-dependent error in the ISB technique not discovered in previous work. We identify as the most likely culprit the p-factor, which is used to convert the observed Cepheid radial velocities into their pulsational velocities. By demanding (1) a zero slope on the distance modulus versus period diagram and (2) a zero mean difference between the ISB and ZAMS fitting distance moduli of a sample of well-established Galactic cluster Cepheids, we find that p=1.58(±0.02)-0.15(±0.05)logP, with the p-factor depending more strongly on Cepheid period (and thus luminosity) than indicated by past theoretical calculations. When we recalculate the distances of the LMC Cepheids with the revised p-factor law suggested by our data, we not only obtain consistent distance moduli for all stars but also decrease the slopes in the various LMC PL relations (and particularly in the reddening-independent K and W bands) to values that are consistent with the values observed by OGLE-II and Persson and coworkers. From our 13 Cepheids, we determine the LMC distance modulus to be 18.56±0.04 mag, with an additional estimated systematic uncertainty of ∼0.1 mag. Using the same corrected p-factor law to redetermine the distances of the Galactic Cepheids, the new Galactic PL relations are also found consistent with the observed optical and near-infrared PL relations in the LMC. Our main conclusion from the ISB analysis of the LMC Cepheid sample is that, within current uncertainties, there seems to be no significant difference between the slopes of the PL relations in the Milky Way and LMC. With literature data on more metal-poor systems, it seems now possible to conclude that the slope of the Cepheid PL relation is independent of metallicity in the broad range in [Fe/H] from -1.0 dex to solar abundance, within a small uncertainty. The new evidence from the first ISB analysis of a sizable sample of LMC Cepheids suggests that the previous, steeper Galactic PL relations obtained from this technique were caused by an underestimation of the period dependence in the model-based p-factor law used in the previous work. We emphasize, however, that our current results must be substantiated by new theoretical models capable of explaining the steeper period dependence of the p-factor law, and we will also need data on more LMC field Cepheids to rule out remaining concerns about the validity of our current interpretation.

Abstract Copyright:

Journal keyword(s): Stars: Variables: Cepheids - Cosmology: Distance Scale - Galaxies: Distances and Redshifts - Galaxies: Magellanic Clouds - Stars: Oscillations

Simbad objects: 58

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Number of rows : 58

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 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9793 1
2 NGC 300 GiG 00 54 53.4460065856 -37 41 03.182962667 8.83 8.69 8.13 7.46   ~ 1356 2
3 IC 1613 GiC 01 04 54.2 +02 08 00   10.42 10.01 9.77   ~ 1132 2
4 V* SU Cas cC* 02 51 58.7508894403 +68 53 18.601570075 6.92 6.44 5.80     F5.5III+ 412 1
5 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 3078 0
6 V* V1229 Tau EB* 03 47 29.4535999265 +24 17 18.016988974   6.87 6.81   6.74 A0VpSi+Am 182 0
7 SV* HV 879 cC* 04 58 05.5960529644 -69 27 15.481012522   14.72 13.356 13.01 12.341 ~ 53 0
8 HD 268878 cC* 04 58 10.7957486662 -69 56 58.783004889   13.83 13.02 12.96 12.071 K5 68 0
9 SV* HV 2338 cC* 05 06 08.8557525637 -71 15 26.119435535   12.83 12.26   11.858 ~ 60 0
10 SV* HV 899 cC* 05 07 07.8253500672 -68 53 19.453088959   13.50 13.343 12.83 12.449 ~ 51 0
11 SV* HV 909 cC* 05 09 20.1376380251 -70 27 27.043906162   13.32 12.67 12.11 11.949 ~ 61 0
12 SV* HV 12197 Ce* 05 13 13 -65 30.8   16.741 16.102     ~ 28 0
13 SV* HV 12199 Ce* 05 13 19 -65 29.5   16.916 16.289     ~ 30 0
14 SV* HV 12198 cC* 05 13 26.6694544251 -65 27 04.933284395   16.627 15.970   15.230 ~ 40 0
15 NGC 1866 GlC 05 13 38.920 -65 27 52.75           ~ 396 0
16 SV* HV 12202 Ce* 05 13 39 -65 29.0   16.756 16.080     ~ 28 0
17 SV* HV 12203 Ce* 05 13 40 -65 29.6   16.811 16.140     ~ 29 0
18 SV* HV 12204 cC* 05 13 57.8739395146 -65 28 39.329976067   16.18 15.715   15.076 ~ 32 0
19 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15356 1
20 SV* HV 12816 cC* 05 29 58.4215724392 -65 54 20.309760307   15.09 14.49 14.13 13.846 ~ 39 0
21 SV* HV 12815 cC* 05 30 02.4652196559 -65 56 01.785181166   14.39 14.04 13.48 12.551 ~ 44 0
22 V* T Mon cC* 06 25 12.9997562821 +07 05 08.561189768 8.24 7.20 5.98   4.996 G3Iabv+A0p 450 1
23 V* CV Mon cC* 06 37 04.8448658715 +03 03 50.276498200   11.32 9.90   8.631 ~ 217 0
24 V* VZ Pup cC* 07 38 35.2380584126 -28 29 58.597876520   11.469 10.154 9.583   F7.5 133 1
25 V* AQ Pup cC* 07 58 22.0887170720 -29 07 48.335325928   9.70 8.54   7.175 F5-G2Ib 182 0
26 V* LS Pup cC* 07 58 59.2197671330 -29 18 28.357057956   11.75 10.59 9.88 8.933 ~ 78 0
27 V* BN Pup cC* 08 06 21.4748690781 -30 05 48.768197196   10.99 9.75 8.97 8.981 G4 109 0
28 V* RS Pup cC* 08 13 04.2157137938 -34 34 42.691837063 8.89 8.00 6.70   5.453 F8Iab 325 0
29 V* RZ Vel cC* 08 37 01.3029337589 -44 06 52.844429407   8.507 7.260     G1Ib 203 0
30 V* T Vel cC* 08 37 40.8268486937 -47 21 43.082343785   8.92 7.68   6.970 G0II 154 0
31 V* SW Vel cC* 08 43 38.6904013543 -47 24 11.196771088   9.58 8.32     F8/G0Ib 171 0
32 V* CS Vel cC* 09 41 10.2609558071 -53 48 57.782655270   12.46 11.24   10.078 ~ 94 0
33 * l Car cC* 09 45 14.8112246 -62 30 28.451894   4.33 3.40     G5Iab/b 296 1
34 V* RY Vel cC* 10 20 41.0317627466 -55 19 17.035924264   9.71 7.86   6.840 F5Ib/II 134 0
35 V* VY Car cC* 10 44 32.6908129391 -57 33 55.326019898 8.12 7.70 6.87   6.299 F7Iab/b 200 0
36 V* WZ Car cC* 10 55 18.7272542108 -60 56 23.951208594   10.40 9.37     F8 135 0
37 V* U Car cC* 10 57 48.1866898409 -59 43 55.880151632 8.31 7.21 6.11   5.073 G5/8Iab 216 0
38 V* UU Mus cC* 11 52 17.7225421742 -65 24 15.060675590   10.5 9.54     F7/G0p 120 0
39 V* VW Cen cC* 13 33 59.0299132697 -64 03 19.999430004   11.60 10.36   8.785 ~ 108 0
40 V* KN Cen cC* 13 36 36.8945451169 -64 33 29.916343439   11.22 9.86     G8Iab+B6.0V 128 0
41 V* XX Cen cC* 13 40 18.6446943543 -57 36 47.444003198   8.72 7.30   6.747 F7/8II 174 0
42 V* V Cen cC* 14 32 33.0828020969 -56 53 15.774776152 8.44 7.84 6.93   5.798 F5Ib/II 247 0
43 V* V340 Nor cC* 16 13 17.3998357878 -54 14 05.588347830   9.61 8.47 8.83   G2Iab 138 0
44 V* S Nor cC* 16 18 51.8313333962 -57 53 59.253617873 8.15 7.49 6.49   5.427 F8/G0Ib 348 1
45 V* BF Oph cC* 17 06 05.4979763004 -26 34 50.031704299 8.00 7.61 6.93   6.377 G0II 206 0
46 V* RY Sco cC* 17 50 52.3454231474 -33 42 20.410667234 9.77 8.79 7.51   6.256 F6Ib 172 0
47 V* Y Oph cC* 17 52 38.7021149511 -06 08 36.875163136 8.62 7.61 6.21     G3Ia 347 0
48 V* WZ Sgr cC* 18 16 59.7158915244 -19 04 32.989119557   9.10 7.45     F7(III) 233 0
49 V* U Sgr cC* 18 31 53.3321808602 -19 07 30.262730218 8.50 7.81 6.68   5.413 G1Ib 439 0
50 V* EV Sct cC* 18 36 39.6017832876 -08 11 05.360422056   10.99 9.90     G0II 234 0
51 V* BB Sgr cC* 18 50 59.8730479535 -20 17 42.828317888 8.07 7.53 6.69   5.824 G0Ib 237 0
52 NGC 6822 G 19 44 56.199 -14 47 51.29   18 8.1     ~ 1460 0
53 V* SV Vul cC* 19 51 30.9059608126 +27 27 36.835645654 8.65 7.86 6.74   5.703 F8Ia 404 0
54 * eta Aql cC* 19 52 28.3677478 +01 00 20.369619 5.12 4.61 3.80   3.030 F6Iab+B9.8V 642 0
55 * 10 Sge cC* 19 56 01.2614273274 +16 38 05.236276391 6.45 6.03 5.36 6.81 4.789 F7Ib 332 0
56 V* X Cyg cC* 20 43 24.1918662954 +35 35 16.075732392 8.69 7.70 6.47   5.241 F7Ib 444 0
57 * del Cep cC* 22 29 10.2650184 +58 24 54.713856 4.71 4.35 3.75   3.219 F5Iab:+B7-8 689 0
58 V* Z Lac cC* 22 40 52.1456104219 +56 49 46.083960286   9.71 8.57   7.164 F6Ib 214 0

    Equat.    Gal    SGal    Ecl

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2021.05.16-20:21:39

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