2011ApJ...730..119R


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.02CET13:21:42

2011ApJ...730..119R - Astrophys. J., 730, 119 (2011/April-1)

A 3% solution: determination of the Hubble constant with the Hubble Space Telescope and Wide Field Camera 3.

RIESS A.G., MACRI L., CASERTANO S., LAMPEITL H., FERGUSON H.C., FILIPPENKO A.V., JHA S.W., LI W., CHORNOCK R. and SILVERMAN J.M.

Abstract (from CDS):

We use the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST) to determine the Hubble constant from optical and infrared observations of over 600 Cepheid variables in the host galaxies of eight recent Type Ia supernovae (SNe Ia), providing the calibration for a magnitude-redshift relation based on 253 SNe Ia. Increased precision over past measurements of the Hubble constant comes from five improvements: (1) more than doubling the number of infrared observations of Cepheids in the nearby SN hosts; (2) increasing the sample size of ideal SN Ia calibrators from six to eight; (3) increasing by 20% the number of Cepheids with infrared observations in the megamaser host NGC 4258; (4) reducing the difference in the mean metallicity of the Cepheid comparison samples between NGC 4258 and the SN hosts from Δlog [O/H] = 0.08 to 0.05; and (5) calibrating all optical Cepheid colors with a single camera, WFC3, to remove cross-instrument zero-point errors. The result is a reduction in the uncertainty in H0 due to steps beyond the first rung of the distance ladder from 3.5% to 2.3%. The measurement of H 0 via the geometric distance to NGC 4258 is 74.8±3.1 km/s/Mpc, a 4.1% measurement including systematic uncertainties. Better precision independent of the distance to NGC 4258 comes from the use of two alternative Cepheid absolute calibrations: (1) 13 Milky Way Cepheids with trigonometric parallaxes measured with HST/fine guidance sensor and Hipparcos and (2) 92 Cepheids in the Large Magellanic Cloud for which multiple accurate and precise eclipsing binary distances are available, yielding 74.4±2.5 km/s/Mpc, a 3.4% uncertainty including systematics. Our best estimate uses all three calibrations but a larger uncertainty afforded from any two: H0= 73.8±2.4 km/s/Mpc including systematic errors, corresponding to a 3.3% uncertainty. The improved measurement of H0, when combined with the Wilkinson Microwave Anisotropy Probe (WMAP) 7 year data, results in a tighter constraint on the equation-of-state parameter of dark energy of w = -1.08±0.10. It also rules out the best-fitting gigaparsec-scale void models, posited as an alternative to dark energy. The combined H0+ WMAP results yield Neff= 4.2±0.7 for the number of relativistic particle species in the early universe, a low-significance excess for the value expected from the three known neutrino flavors.

Abstract Copyright:

Journal keyword(s): cosmological parameters - dark energy - distance scale - galaxies: distances and redshifts - stars: variables: Cepheids - supernovae: general

VizieR on-line data: <Available at CDS (J/ApJ/730/119): table2.dat>

Errata: errata vol. 732, art. 129 (2011) and vol. 752, art. 76 (2012)

Status at CDS : All or part of tables of objects will not be ingested in SIMBAD.

Simbad objects: 27

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Number of rows : 27

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 NGC 12 G 00 08 44.752 +04 36 45.12   14.5       ~ 38 0
2 * alf UMi cC* 02 31 49.09456 +89 15 50.7923 3.00 2.62 2.02 1.53 1.22 F8Ib 617 2
3 SN 2002fk SN* 03 22 05.71 -15 24 03.2     15.7     SNIa 80 1
4 NGC 1309 GiG 03 22 06.5558186281 -15 23 59.793798444   12.08   12.5 11.7 ~ 187 0
5 SV* HV 2274 EB* 05 02 40.7806907576 -68 24 21.497024742 13.298 13.984 14.127 14.192 14.390 ~ 75 0
6 OGLE J051019.64-685812.3 EB* 05 10 19.65 -68 58 12.0     16.673   15.715 ~ 29 0
7 SV* HV 12012 EB* 05 19 11.7873771387 -69 42 24.840934999 14.404 15.396 15.135   15.699 ~ 25 0
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15064 1
9 SV* HV 982 EB* 05 29 52.31 -69 09 22.6   14.76 14.648 14.99 14.761 ~ 45 0
10 SV* HV 5936 EB* 05 33 38.82 -66 37 40.0   15.01 14.741 15.25 14.911 ~ 32 0
11 SN 1995al SN* 09 50 55.97 +33 33 09.4   13.36 13.22     SNIa 89 1
12 NGC 3021 GiG 09 50 57.1458788689 +33 33 12.942434723   12.6       ~ 164 0
13 SN 1994ae SN* 10 47 01.94 +17 16 30.8   13.20 12.99     SNIa 152 1
14 NGC 3370 GiG 10 47 04.039 +17 16 25.31   12.4       ~ 210 0
15 SN 1998aq SN* 11 56 25.87 +55 07 43.2   12.31 14.9     SNIa 168 1
16 NGC 3982 Sy1 11 56 28.169 +55 07 31.30   12.20 11.70 11.18   ~ 494 1
17 SN 2007sr SN* 12 01 52.80 -18 58 21.7     12.79     SNIa 72 1
18 NGC 4038 GiP 12 01 53.002 -18 52 03.32   10.91   9.74 11.0 ~ 1281 1
19 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1566 0
20 M 106 Sy2 12 18 57.620 +47 18 13.39   9.14 8.41 8.11   ~ 2138 3
21 NGC 4536 GiP 12 34 27.129 +02 11 16.37 11.14 11.16 10.55 17.393   ~ 758 3
22 SN 1981B SN* 12 34 29.57 +02 11 59.3   11.74       SNIa 386 1
23 NGC 4639 GiP 12 42 52.3781396179 +13 15 26.712929286   13.62 12.72     ~ 563 0
24 SN 1990N SN* 12 42 56.68 +13 15 23.4   12.69 12.62     SNIa 374 1
25 SN 2007af SN* 14 22 21.03 -00 23 37.6     15.4     SNIa 130 1
26 NGC 5584 EmG 14 22 23.811 -00 23 14.82   12.80   12.0 11.8 ~ 219 0
27 GSC 02581-02323 * 16 31 33.8125078770 +30 08 46.398483547 13.576 12.972 12.917 12.564 12.212 G2V 62 0

    Equat.    Gal    SGal    Ecl

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2020.12.02-13:21:42

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