The Low-Order Multipoles and Dust in the Vicinity of the Solar System 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 Cosmic Microwave Background Radiation Released 10,000 years after the Big Bang, 13 Gyr ago Released 10,000 years after the Big Bang, 13 Gyr ago Modulated by matter clumps and gravitational potential at that time Modulated by matter clumps and gravitational potential at that time Average temperature K Average temperature K Fluctuations ~100 μK (cosmological) Fluctuations ~100 μK (cosmological) Discovered in 1960s Discovered in 1960s Most recently surveyed by WMAP Most recently surveyed by WMAP

The WMAP Orbit

The WMAP Scanning Pattern The WMAP measured the difference of the sky temperatures in its two beams separated by 140° The WMAP measured the difference of the sky temperatures in its two beams separated by 140°

The CMB Fluctuations

The CMB Fluctuations Analysis Expansion into series of spherical harmonic functions Expansion into series of spherical harmonic functions

The Quadrupole (Galactic Coordinates)

The Octopole (Galactic Coordinates)

The Quadrupole & Octopole (Galactic Coordinates)

The Quadrupole (Ecliptic Coordinates)

The Octopole (Ecliptic Coordinates)

The Quadrupole & Octopole (Ecliptic Coordinates)

A Bias Unaccounted? Unknown dust cloud? Unknown dust cloud? Bound to the Solar system? Bound to the Solar system? Constraints that we have: Constraints that we have: PhotometricPhotometric SpectrometricSpectrometric  Geometric This talk’s primary subject: expanding maps of various dust clouds into multipoles This talk’s primary subject: expanding maps of various dust clouds into multipoles

The Zodiacal Cloud The smooth background zodiacal cloud of Kelsall et al. (1998) as it would look through the WMAP scanning pattern The smooth background zodiacal cloud of Kelsall et al. (1998) as it would look through the WMAP scanning pattern 1 mm, 5 mm 1 mm, 5 mm

The Zodiacal Cloud The smooth background zodiacal cloud of Kelsall et al. (1998) as it would look through the WMAP scanning pattern The smooth background zodiacal cloud of Kelsall et al. (1998) as it would look through the WMAP scanning pattern The quadrupole moment of multipole expansion The quadrupole moment of multipole expansion 1 mm, 5 mm 1 mm, 5 mm

The Zodiacal Cloud The smooth background zodiacal cloud of Kelsall et al. (1998) as it would look through the WMAP scanning pattern The smooth background zodiacal cloud of Kelsall et al. (1998) as it would look through the WMAP scanning pattern The octopole moment of multipole expansion The octopole moment of multipole expansion 1 mm, 5 mm 1 mm, 5 mm

The Kelsall Model Components

The Asteroid Dust Bands The asteroid dust bands of Kelsall et al. (1998) as they would look through the WMAP scanning 1 mm The asteroid dust bands of Kelsall et al. (1998) as they would look through the WMAP scanning 1 mm Left: Eos family, right: Themis&Koronis family Left: Eos family, right: Themis&Koronis family

The Asteroid Dust Bands The asteroid dust bands of Kelsall et al. (1998) as they would look through the WMAP scanning 1 mm The asteroid dust bands of Kelsall et al. (1998) as they would look through the WMAP scanning 1 mm The quadrupole moment of the multipole expansion The quadrupole moment of the multipole expansion Left: Eos family, right: Themis&Koronis family Left: Eos family, right: Themis&Koronis family

The Asteroid Dust Bands The asteroid dust bands of Kelsall et al. (1998) as they would look through the WMAP scanning 1 mm The asteroid dust bands of Kelsall et al. (1998) as they would look through the WMAP scanning 1 mm The octopole moment of the multipole expansion The octopole moment of the multipole expansion Left: Eos family, right: Themis&Koronis family Left: Eos family, right: Themis&Koronis family

The Taurid Meteor Complex A meteor stream on a highly eccentric orbit A meteor stream on a highly eccentric orbit Semi-major axis 2.2 AU, eccentricity 0.8, inclination 3.6º Semi-major axis 2.2 AU, eccentricity 0.8, inclination 3.6º A direct view from the Sun, no WMAP motion/scanning A direct view from the Sun, no WMAP motion/scanning

The Taurid Meteor Complex A meteor stream on a highly eccentric orbit A meteor stream on a highly eccentric orbit Semi-major axis 2.2 AU, eccentricity 0.8, inclination 3.6º Semi-major axis 2.2 AU, eccentricity 0.8, inclination 3.6º WMAP motion/scanning simulated WMAP motion/scanning simulated

The Taurid Meteor Complex A meteor stream on a highly eccentric orbit A meteor stream on a highly eccentric orbit Semi-major axis 2.2 AU, eccentricity 0.8, inclination 3.6º Semi-major axis 2.2 AU, eccentricity 0.8, inclination 3.6º WMAP motion/scanning simulated, the quadrupole WMAP motion/scanning simulated, the quadrupole

The Taurid Meteor Complex A meteor stream on a highly eccentric orbit A meteor stream on a highly eccentric orbit Semi-major axis 2.2 AU, eccentricity 0.8, inclination 3.6º Semi-major axis 2.2 AU, eccentricity 0.8, inclination 3.6º WMAP motion/scanning simulated, the octopole WMAP motion/scanning simulated, the octopole

Interstellar Dust: “Fessenkov Flow” Number density in an unconstrained mono- directional flow of dust focused by the Solar gravity. V ∞ =30 km/s Number density in an unconstrained mono- directional flow of dust focused by the Solar gravity. V ∞ =30 km/s

Interstellar Dust Flow The focused flow of interstellar dust as it would look through the WMAP scanning pattern The focused flow of interstellar dust as it would look through the WMAP scanning pattern Left: the vertex is in the ecliptic, right: the vertex latitude is 45 degrees Left: the vertex is in the ecliptic, right: the vertex latitude is 45 degrees The total emission map The total emission map

Interstellar Dust Flow The focused flow of interstellar dust as it would look through the WMAP scanning pattern The focused flow of interstellar dust as it would look through the WMAP scanning pattern Left: the vertex is in the ecliptic, right: the vertex latitude is 45 degrees Left: the vertex is in the ecliptic, right: the vertex latitude is 45 degrees The quadrupole The quadrupole

Interstellar Dust Flow The focused flow of interstellar dust as it would look through the WMAP scanning pattern The focused flow of interstellar dust as it would look through the WMAP scanning pattern Left: the vertex is in the ecliptic, right: the vertex latitude is 45 degrees Left: the vertex is in the ecliptic, right: the vertex latitude is 45 degrees The octopole The octopole

More Dust Clouds Tested Long-period comet trail Long-period comet trail All short-period comets All short-period comets The Oort cloud dust The Oort cloud dust The Edgeworth-Kuiper belt dust The Edgeworth-Kuiper belt dust The beta-Pic dust The beta-Pic dust Photometry, geometry and/or spectrometry allows one to reject hypotheses Photometry, geometry and/or spectrometry allows one to reject hypotheses

Galactic Templete Removes thermal emission from galactic dust (Schlegel et al. 1998) Removes thermal emission from galactic dust (Schlegel et al. 1998) Made by using the IRAS and COBE sky maps at >100 micron wavelength, where the galactic dust is dominant Made by using the IRAS and COBE sky maps at >100 micron wavelength, where the galactic dust is dominant Polluted by the zodiacal dust emission Polluted by the zodiacal dust emission The zodiacal emission is removed by using a simple model based on 12 micron COBE maps The zodiacal emission is removed by using a simple model based on 12 micron COBE maps The residuals left after removal non-negligible The residuals left after removal non-negligible Can account for a ~microKelvin, not the full magnitude of quadrupole/octopole Can account for a ~microKelvin, not the full magnitude of quadrupole/octopole

Summary The CMB map made by WMAP contain anomalous fluctuation aligned with the solar-system geometry The CMB map made by WMAP contain anomalous fluctuation aligned with the solar-system geometry An unknown dust cloud was proposed as a reason An unknown dust cloud was proposed as a reason In this talk, the thermal emission by several candidate clouds was simulated and compared with the CMB maps In this talk, the thermal emission by several candidate clouds was simulated and compared with the CMB maps No cloud has explained the anomalies so far No cloud has explained the anomalies so far The inversion approach is suggested, i.e. the reconstruction of the cloud based on the data rather than testing known clouds against the data The inversion approach is suggested, i.e. the reconstruction of the cloud based on the data rather than testing known clouds against the data