1998ApJ...508..844G


Query : 1998ApJ...508..844G

1998ApJ...508..844G - Astrophys. J., 508, 844-853 (1998/December-1)

Systematics of RR Lyrae statistical parallax. III. Apparent magnitudes and extinctions.

GOULD A. and POPOWSKI P.

Abstract (from CDS):

We sing the praises of the central limit theorem. Having previously removed all other possible causes of significant systematic error in the statistical-parallax determination of RR Lyrae absolute magnitudes, we investigate systematic errors from two final sources of input data: apparent magnitudes and extinctions. We find corrections due to each of about 0.05 mag, i.e., about half the statistical error. However, these are of opposite sign and so approximately cancel out. The apparent-magnitude system that we previously adopted from Layden et al. was calibrated to the photoelectric photometry of Clube & Dawe. Using Hipparcos photometry and archival modern ground-based photometry, we show that the Clube & Dawe system is about 0.06 mag too bright. Extinctions were previously based on the map of Burstein & Heiles, which was constructed from H I maps. We argue that extinctions should rather be estimated using the new map of Schlegel, Finkbeiner, & Davis based on COBE and IRAS measurements of dust emission. This substitution increases the mean estimated extinction by about 0.05 mag, primarily because of a difference in the zero point of the two maps. Our final estimate for the absolute magnitude is MV = 0.77±0.13 at [Fe/H] = -1.60 for a pure sample of 147 halo RR Lyrae stars, or MV = 0.80±0.11 at [Fe/H] = -1.71 if we incorporate kinematic information from 716 nonkinematically selected non-RR Lyrae stars from Beers & Sommer-Larsen. These are 2 and 3 σ fainter than recent determinations of MV based on main-sequence fitting of clusters using Hipparcos measurements of subdwarfs by Reid and Gratton et al. Since statistical parallax is being cleared of systematic errors and since the probability of a more than 2 σ statistical fluctuation is less than 1/20, we conclude that these brighter determinations may be in error. In the course of these three papers, we have corrected six systematic errors whose absolute values total 0.20 mag. Had these, contrary to the expectation of the central limit theorem, all lined up one way, they could have resolved the conflict in favor of the brighter determinations. In fact, the net change was only 0.06 mag.

Abstract Copyright: ∼

Journal keyword(s): ISM: Dust, Extinction - Methods: Statistical - Stars: Distances - Stars: Kinematics - Stars: Variables: Other: (RR Lyrae)

Simbad objects: 28

goto Full paper

goto View the references in ADS

Number of rows : 28
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 V* VX Scl RR* 01 35 23.6616795216 -35 07 42.603497976   12.22 12.01     A2 57 0
2 V* SX For RR* 03 30 22.3499972497 -36 03 13.503234127   11.313 10.975     kA1hF5 83 0
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
4 V* RX Col RR* 06 13 14.7399958536 -37 15 00.566702568           ~ 58 0
5 V* HH Pup RR* 07 20 35.5562195569 -46 42 30.091727783   11.52 11.31 11.49   A3II/III 94 0
6 V* TU UMa RR* 11 29 48.4893885624 +30 04 02.379416844 9.56 9.41 9.26     kA2hA9.5 246 0
7 V* RV Oct RR* 13 46 31.7442284943 -84 24 06.384454864   11.39 10.94     ~ 105 0
8 V* TY Aps RR* 14 48 50.0092910856 -71 19 41.895022044   12.03 11.65     kA5hF0 74 0
9 V* XZ Aps RR* 14 52 05.4231924775 -79 40 46.572766688           ~ 72 0
10 V* AR Ser RR* 15 33 30.8124184584 +02 46 37.888313880   11.92 11.85     A9V 74 0
11 V* V413 Oph RR* 16 25 11.1042342168 -10 31 25.501414332     12.12     kF3hF6 51 0
12 V* RW TrA RR* 17 00 46.6887966960 -66 39 49.950083772   11.96 11.95     kF0hF5 71 0
13 M 92 GlC 17 17 07.39 +43 08 09.4     6.52     ~ 2240 0
14 NGC 6411 AG? 17 35 32.8446342384 +60 48 48.236693796   13.2       ~ 119 0
15 NGC 6388 GlC 17 36 17.461 -44 44 08.34           ~ 988 1
16 V* V494 Sco RR* 17 40 48.4775333904 -31 32 31.778481840   12.02 11.62 11.39 10.830 A0 93 0
17 V* WY Pav RR* 17 56 12.3623256744 -57 09 43.423375320   12.54 13.07     ~ 46 0
18 V* MS Ara RR* 18 03 04.2887091600 -52 43 20.583643332   12.42 12.23     ~ 50 0
19 V* IN Ara RR* 18 07 40.2050405280 -54 36 28.751288256   11.10 15.10     ~ 32 0
20 V* V455 Oph RR* 18 15 18.5275718352 +12 21 08.486845992           kA2hA7 64 0
21 V* V413 CrA RR* 18 47 57.6196241592 -37 44 22.531389180   11.00 10.6     kA7hF1 75 0
22 V* BK Dra RR* 19 18 20.6701513824 +66 24 47.965359924   11.44 10.99     kA0hF0.5 89 0
23 V* BN Pav RR* 19 38 03.3819133536 -60 36 39.589772436           ~ 45 0
24 V* BP Pav RR* 19 58 00.1364749488 -65 44 09.970660788           ~ 46 0
25 V* CP Aqr RR* 21 10 12.8490024720 -01 43 16.138701372   12.19 11.70     kF1.5hF7.5 70 0
26 V* Z Mic RR* 21 16 22.7047906743 -30 17 03.065542503   11.58 11.37     kF3hF8 83 0
27 V* RY Oct RR* 21 36 09.3510357528 -77 18 13.536240948   12.46 12.14     ~ 44 0
28 V* SS Oct RR* 21 53 35.3533002696 -82 46 43.756880124           ~ 56 0

To bookmark this query, right click on this link: simbad:objects in 1998ApJ...508..844G and select 'bookmark this link' or equivalent in the popup menu