constraints on material, size and abundance of interplanetary dust from the wmap data valeri dikarev...
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Constraints on Constraints on Material, Size and Material, Size and
Abundance of Abundance of Interplanetary Dust Interplanetary Dust
from the WMAP Datafrom the WMAP DataValeri DikarevValeri Dikarev1,2,41,2,4, Oliver Preuß, Oliver Preuß11
Sami SolankiSami Solanki11
Harald KrügerHarald Krüger1,21,2, Alexander Krivov, Alexander Krivov33
11Max Planck Institute for Solar System Research, GermanyMax Planck Institute for Solar System Research, Germany22Max Planck Institute for Nuclear Physics, GermanyMax Planck Institute for Nuclear Physics, Germany
33Astrophysical Institute of Friedrich Schiller University in Astrophysical Institute of Friedrich Schiller University in Jena, GermanyJena, Germany
44Astronomical Institute of St. Petersburg University, RussiaAstronomical Institute of St. Petersburg University, Russia
The CMB FluctuationsThe CMB FluctuationsThe CMB FluctuationsThe CMB Fluctuations
http://map.gsfc.nasa.gov/
WMAP is the most recent and WMAP is the most recent and accurate CMB mapping missionaccurate CMB mapping mission
Analysis of the CMB Analysis of the CMB FluctuationsFluctuations
E.g. expansions into multipole seriesE.g. expansions into multipole series The multipoles: Gaussian random The multipoles: Gaussian random
with predicted power (standard with predicted power (standard inflationary cosmology)inflationary cosmology)
Analysis of the CMB Analysis of the CMB FluctuationsFluctuations
E.g. expansions into multipole seriesE.g. expansions into multipole series The multipoles: Gaussian random The multipoles: Gaussian random
with predicted power (standard with predicted power (standard inflationary cosmology)inflationary cosmology)
Some Bias Unaccounted?Some Bias Unaccounted?
Although potentially pointing to unknown Although potentially pointing to unknown physics of the early Universe, the anomalies physics of the early Universe, the anomalies may also be due to an unknown may also be due to an unknown measurement biasmeasurement bias
A dark dust cloud in the vicinity of the Solar A dark dust cloud in the vicinity of the Solar system was proposed (e.g. Schwarz et al., system was proposed (e.g. Schwarz et al., Frisch)Frisch)
We have investigated the properties of We have investigated the properties of the hypothetical cloud using constraints the hypothetical cloud using constraints from WMAP as well as from non-from WMAP as well as from non-detection in IRdetection in IR
The Cloud in the The Cloud in the MicrowavesMicrowaves
WMAP was equipped with five radiometers WMAP was equipped with five radiometers operating at the wavelengths from 3 to 14 operating at the wavelengths from 3 to 14 mmmm
Several independent methods were Several independent methods were developed to remove foreground emissiondeveloped to remove foreground emission The WMAP team (Bennett et al.) uses maps of The WMAP team (Bennett et al.) uses maps of
foregrounds obtained also by other instruments, foregrounds obtained also by other instruments, e.g. Galactic dust template (Finkbeiner et al.) e.g. Galactic dust template (Finkbeiner et al.)
ILC techniques (e.g. Tegmark et al.) are adaptive ILC techniques (e.g. Tegmark et al.) are adaptive and do not use a-priori information about and do not use a-priori information about foregrounds, aim to remove everything with non-foregrounds, aim to remove everything with non-CMB spectrumCMB spectrum
Their results are highly compatibleTheir results are highly compatible If there is an unknown cloud in the Solar If there is an unknown cloud in the Solar
system it has to have a CMB spectrumsystem it has to have a CMB spectrum
The Cloud in the The Cloud in the Microwaves 2Microwaves 2
SILICATE >~10 mmCARBON >~1 mmNO IRONNO ICE
Above ~5 Above ~5 mm, both mm, both CMB and CMB and dust are dust are blackbodies blackbodies in Rayleigh-in Rayleigh-Jeans regime. Jeans regime. We only need We only need the emissivity the emissivity of dust to be of dust to be flat.flat.
The Cloud in the Infrared The Cloud in the Infrared LightLight
IPD: Interplanetary Dust (Gruen et al . 1985; 10-100 IPD: Interplanetary Dust (Gruen et al . 1985; 10-100 μμm)m) Cloud: Macroscopic particles, i.e. flat emissivity throughout Cloud: Macroscopic particles, i.e. flat emissivity throughout λλ
rangerange
Why Do We Have to Why Do We Have to Worry?Worry?
The 1997 night sky reference extrapolates The 1997 night sky reference extrapolates emission by interplanetary dust roughly in emission by interplanetary dust roughly in accord with the Gruen et al. (1985) model based accord with the Gruen et al. (1985) model based mostly on the data from the vicinity of Earthmostly on the data from the vicinity of Earth
Most Meteor Streams are Most Meteor Streams are Outside 1AUOutside 1AU
Hughes & McBride (1990): there is a lot more Hughes & McBride (1990): there is a lot more big dust grains outside 1 AU than we see near big dust grains outside 1 AU than we see near EarthEarth
Comet 1P/Halley
All Short-Period Comets
So This Cloud Can BeSo This Cloud Can Be More likely distant than nearbyMore likely distant than nearby More likely carbonaceous than silicate, iron or More likely carbonaceous than silicate, iron or
iceice The extra temperature no more than ~30 The extra temperature no more than ~30 μμKK Meteoroid streams may provide ~7.5 Meteoroid streams may provide ~7.5 μμK (K (ττ~3 ~3
1010-7-7)) This is below WMAP’s pixel sensitivity of 20 This is below WMAP’s pixel sensitivity of 20 μμKK However, if the cloud is extended it may have However, if the cloud is extended it may have
affected some multipoles in a detectable wayaffected some multipoles in a detectable way Unlikely the reason of the WMAP anomalies Unlikely the reason of the WMAP anomalies
that had triggered this studythat had triggered this study Worthwhile to look for, for both dust and Worthwhile to look for, for both dust and
cosmology communitiescosmology communities