Constraints on Material, Size and Abundance of Interplanetary Dust from the WMAP Data Valeri Dikarev 1,2,4, Oliver Preuß 1 Sami Solanki 1 Harald Krüger 1,2, Alexander Krivov 3 1 Max Planck Institute for Solar System Research, Germany 2 Max Planck Institute for Nuclear Physics, Germany 3 Astrophysical Institute of Friedrich Schiller University in Jena, Germany 4 Astronomical Institute of St. Petersburg University, Russia

The CMB Fluctuations WMAP is the most recent and accurate CMB mapping mission WMAP is the most recent and accurate CMB mapping mission

Analysis of the CMB Fluctuations E.g. expansions into multipole series E.g. expansions into multipole series The multipoles: Gaussian random with predicted power (standard inflationary cosmology) The multipoles: Gaussian random with predicted power (standard inflationary cosmology)

Analysis of the CMB Fluctuations E.g. expansions into multipole series E.g. expansions into multipole series The multipoles: Gaussian random with predicted power (standard inflationary cosmology) The multipoles: Gaussian random with predicted power (standard inflationary cosmology)

The Quadrupole (Ecliptic Coordinates)

The Octopole (Ecliptic Coordinates)

Some Bias Unaccounted? Although potentially pointing to unknown physics of the early Universe, the anomalies may also be due to an unknown measurement bias Although potentially pointing to unknown physics of the early Universe, the anomalies may also be due to an unknown measurement bias A dark dust cloud in the vicinity of the Solar system was proposed (e.g. Schwarz et al., Frisch) A dark dust cloud in the vicinity of the Solar system was proposed (e.g. Schwarz et al., Frisch) We have investigated the properties of the hypothetical cloud using constraints from WMAP as well as from non-detection in IR We have investigated the properties of the hypothetical cloud using constraints from WMAP as well as from non-detection in IR

The Cloud in the Microwaves WMAP was equipped with five radiometers operating at the wavelengths from 3 to 14 mm WMAP was equipped with five radiometers operating at the wavelengths from 3 to 14 mm Several independent methods were developed to remove foreground emission Several independent methods were developed to remove foreground emission The WMAP team (Bennett et al.) uses maps of foregrounds obtained also by other instruments, e.g. Galactic dust template (Finkbeiner et al.) The WMAP team (Bennett et al.) uses maps of foregrounds obtained also by other instruments, e.g. Galactic dust template (Finkbeiner et al.) ILC techniques (e.g. Tegmark et al.) are adaptive and do not use a-priori information about foregrounds, aim to remove everything with non-CMB spectrum ILC techniques (e.g. Tegmark et al.) are adaptive and do not use a-priori information about foregrounds, aim to remove everything with non-CMB spectrum Their results are highly compatible Their results are highly compatible If there is an unknown cloud in the Solar system it has to have a CMB spectrum If there is an unknown cloud in the Solar system it has to have a CMB spectrum

The Cloud in the Microwaves 2 SILICATE >~10 mm CARBON >~1 mm NO IRON NO ICE Above ~5 mm, both CMB and dust are blackbodies in Rayleigh-Jeans regime. We only need the emissivity of dust to be flat. Above ~5 mm, both CMB and dust are blackbodies in Rayleigh-Jeans regime. We only need the emissivity of dust to be flat.

Diffuse Night Sky 1997

The Cloud in the Infrared Light IPD: Interplanetary Dust (Gruen et al. 1985; μm) IPD: Interplanetary Dust (Gruen et al. 1985; μm) Cloud: Macroscopic particles, i.e. flat emissivity throughout λ range Cloud: Macroscopic particles, i.e. flat emissivity throughout λ range

Why Do We Have to Worry? The 1997 night sky reference extrapolates emission by interplanetary dust roughly in accord with the Gruen et al. (1985) model based mostly on the data from the vicinity of Earth The 1997 night sky reference extrapolates emission by interplanetary dust roughly in accord with the Gruen et al. (1985) model based mostly on the data from the vicinity of Earth

Most Meteor Streams are Outside 1AU Hughes & McBride (1990): there is a lot more big dust grains outside 1 AU than we see near Earth Hughes & McBride (1990): there is a lot more big dust grains outside 1 AU than we see near Earth Comet 1P/Halley All Short- Period Comets

So This Cloud Can Be More likely distant than nearby More likely distant than nearby More likely carbonaceous than silicate, iron or ice More likely carbonaceous than silicate, iron or ice The extra temperature no more than ~30 μK The extra temperature no more than ~30 μK Meteoroid streams may provide ~7.5 μK (τ~ ) Meteoroid streams may provide ~7.5 μK (τ~ ) This is below WMAP’s pixel sensitivity of 20 μK This is below WMAP’s pixel sensitivity of 20 μK However, if the cloud is extended it may have affected some multipoles in a detectable way However, if the cloud is extended it may have affected some multipoles in a detectable way Unlikely the reason of the WMAP anomalies that had triggered this study Unlikely the reason of the WMAP anomalies that had triggered this study Worthwhile to look for, for both dust and cosmology communities Worthwhile to look for, for both dust and cosmology communities

What the Cloud Can Look Like μKμKμKμK Meteoroid streams from short-period comets through WMAP’s sky-scanning pattern Meteoroid streams from short-period comets through WMAP’s sky-scanning pattern