2021ApJ...922..259M

Query : 2021ApJ...922..259M

2021ApJ...922..259M - Astrophys. J., 922, 259-259 (2021/December-1)

Optimal cosmic microwave background lensing reconstruction and parameter estimation with SPTpol data.

MILLEA M., DALEY C.M., CHOU T.-L., ANDERES E., ADE P.A.R., ANDERSON A.J., AUSTERMANN J.E., AVVA J.S., BEALL J.A., BENDER A.N., BENSON B.A., BIANCHINI F., BLEEM L.E., CARLSTROM J.E., CHANG C.L., CHAUBAL P., CHIANG H.C., CITRON R., CORBETT MORAN C., CRAWFORD T.M., CRITES A.T., DE HAAN T., DOBBS M.A., EVERETT W., GALLICCHIO J., GEORGE E.M., GOECKNER-WALD N., GUNS S., GUPTA N., HALVERSON N.W., HENNING J.W., HILTON G.C., HOLDER G.P., HOLZAPFEL W.L., HRUBES J.D., HUANG N., HUBMAYR J., IRWIN K.D., KNOX L., LEE A.T., LI D., LOWITZ A., McMAHON J.J., MEYER S.S., MOCANU L.M., MONTGOMERY J., NATOLI T., NIBARGER J.P., NOBLE G., NOVOSAD V., OMORI Y., PADIN S., PATIL S., PRYKE C., REICHARDT C.L., RUHL J.E., SALIWANCHIK B.R., SCHAFFER K.K., SIEVERS C., SMECHER G., STARK A.A., THORNE B., TUCKER C., VEACH T., VIEIRA J.D., WANG G., WHITEHORN N., WU W.L.K. and YEFREMENKO V.

Abstract (from CDS):

We perform the first simultaneous Bayesian parameter inference and optimal reconstruction of the gravitational lensing of the cosmic microwave background (CMB), using 100 deg2 of polarization observations from the SPTpol receiver on the South Pole Telescope. These data reach noise levels as low as 5.8 µK arcmin in polarization, which are low enough that the typically used quadratic estimator (QE) technique for analyzing CMB lensing is significantly suboptimal. Conversely, the Bayesian procedure extracts all lensing information from the data and is optimal at any noise level. We infer the amplitude of the gravitational lensing potential to be Aφ=0.949±0.122 using the Bayesian pipeline, consistent with our QE pipeline result, but with 17% smaller error bars. The Bayesian analysis also provides a simple way to account for systematic uncertainties, performing a similar job as frequentist "bias hardening" or linear bias correction, and reducing the systematic uncertainty on Aph due to polarization calibration from almost half of the statistical error to effectively zero. Finally, we jointly constrain Aph along with AL, the amplitude of lensing-like effects on the CMB power spectra, demonstrating that the Bayesian method can be used to easily infer parameters both from an optimal lensing reconstruction and from the delensed CMB, while exactly accounting for the correlation between the two. These results demonstrate the feasibility of the Bayesian approach on real data, and pave the way for future analysis of deep CMB polarization measurements with SPT-3G, Simons Observatory, and CMB-S4, where improvements relative to the QE can reach 1.5 times tighter constraints on Aph and seven times lower effective lensing reconstruction noise.

Abstract Copyright: © 2021. The American Astronomical Society. All rights reserved.

Journal keyword(s): Cosmology - Cosmic microwave background radiation - Gravitational lensing - Weak gravitational lensing - Bayesian statistics

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 RCW 38 SFR 08 59 05.50 -47 30 39.4           ~ 306 2

Query : 2021ApJ...922..259M

Basic data :
RCW 38 -- Star Forming Region
Origin of the objects types :

(Ref) Object type as listed in the reference "Ref"
(acronym) Object type linked to the acronym according to the original reference
() Anterior to 2007, before we can link the objet type to a reference, or given by the CDS team in some particular cases

Other object types: 		SFR (), Rad (GRS,Kes,...), HII (RCW,[HBB99],...), * (MHR)
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
ICRS coord. (ep=J2000) : 		08 59 05.50 -47 30 39.4 [ ] D ~
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
FK4 coord. (ep=B1950 eq=1950) : 		08 57 23.57 -47 18 56.1 [ ]
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
Gal coord. (ep=J2000) : 		267.94067 -01.05770 [ ]
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', {sourceSize:12, color:'#30a090'})); aladin.on('objectClicked', function(object) { var objName=object.data.MAIN_ID; aladin.showPopup(object.ra,object.dec,'',''+ objName+''); });" title="Show Simbad objects"> Overlay Simbad points in this preview
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GAL 268.0-01.1 Kes 5 [GS70] 268.0-01.0 [WMG70] 268.0-01.1
GRS G267.94 -01.03 MHR 5 [HBB99] 268.034-0.984
GRS G267.94 -01.06 MSH 08-4-07 [KC97c] G268.0-01.0
GRS G268.00 -01.10 RCW 38 [SG70] 268.0-1.1

References (306 between 1850 and 2024) (Total 306)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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distance : 1   

   

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Data at NED - NASA/IPAC Extragalactic Database : RCW 38

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