BICEP2 Science Images

BICEP2 B-mode Signal Gravitational waves from inflation generate a faint but distinctive twisting pattern in the polarization of the CMB, known as a "curl" or B-mode pattern. For the density fluctuations that generate most of the polarization of the CMB, this part of the primordial pattern is exactly zero. Shown here is the actual B-mode pattern observed with the BICEP2 telescope, with the line segments showing the polarization from different spots on the sky. The red and blue shading shows the degree of clockwise and anti-clockwise twisting of this B-mode pattern.

 Gravitational waves from inflation generate a faint but distinctive twisting pattern in the polarization of the CMB, known as a "curl" or B-mode pattern. For the density fluctuations that generate most of the polarization of the CMB, this part of the primordial pattern is exactly zero. Shown here is the actual B-mode pattern observed with the BICEP2 telescope, with the line segments showing the polarization from different spots on the sky. The red and blue shading shows the degree of clockwise and anti-clockwise twisting of this B-mode pattern. (BICEP2 Collaboration)

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History of the Universe The bottom part of this illustration shows the scale of the universe versus time. Specific events are shown such as the formation of neutral Hydrogen at 380 000 years after the big bang. Prior to this time, the constant interaction between matter (electrons) and light (photons) made the universe opaque. After this time, the photons we now call the CMB started streaming freely. The fluctuations (differences from place to place) in the matter distribution left their imprint on the CMB photons. The density waves appear as temperature and The bottom part of this illustration shows the scale of the universe versus time. Specific events are shown such as the formation of neutral Hydrogen at 380 000 years after the big bang. Prior to this time, the constant interaction between matter (electrons) and light (photons) made the universe opaque. After this time, the photons we now call the CMB started streaming freely. The fluctuations (differences from place to place) in the matter distribution left their imprint on the CMB photons. The density waves appear as temperature and "E-mode" polarization. The gravitational waves leave a characteristic signature in the CMB polarization: the "B-modes". Both density and gravitational waves come from quantum fluctuations which have been magnified by inflation to be present at the time when the CMB photons were emitted. (BICEP2 Collaboration)

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Polarization Diagram This illustration displays the mechanism by which density and gravitational waves produce E- and B-mode patterns in the polarization of the CMB. For a single density wave propagating in the direction of the arrow, an electron will always see hotter and colder photons in a direction parallel or perpendicular to the plane of this single wave (a plane at right angles to the arrow). Regardless of the direction of the density wave, this can thus only produce E-mode polarization patterns (upper right). A single gravitational wave is more complex. Although it propagates in the same direction as the density wave, it stretches and squeezes space in a direction perpendicular from it. Depending on the orientation of this stretch/squeeze motion, the gravitational wave is capable of producing either E- or B-mode polarization patterns (lower right). The structure of the universe at the moment the CMB was emitted is a large combinations of these density and gravitational waves.

 This illustration displays the mechanism by which density and gravitational waves produce E- and B-mode patterns in the polarization of the CMB. For a single density wave propagating in the direction of the arrow, an electron will always see hotter and colder photons in a direction parallel or perpendicular to the plane of this single wave (a plane at right angles to the arrow). Regardless of the direction of the density wave, this can thus only produce E-mode polarization patterns (upper right). A single gravitational wave is more complex. Although it propagates in the same direction as the density wave, it stretches and squeezes space in a direction perpendicular from it. Depending on the orientation of this stretch/squeeze motion, the gravitational wave is capable of producing either E- or B-mode polarization patterns (lower right). The structure of the universe at the moment the CMB was emitted is a large combinations of these density and gravitational waves. (BICEP2 Collaboration)

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BICEP2 Photo Gallery

BICEP2 Twilight The BICEP2 telescope at twilight, which occurs only twice a year at the South Pole. The MAPO observatory (home of the Keck Array telescope) and the South Pole station can be seen in the background. (<i>Steffen Richter, Harvard University</i>) The BICEP2 telescope at twilight, which occurs only twice a year at the South Pole. The MAPO observatory (home of the Keck Array telescope) and the South Pole station can be seen in the background. (Steffen Richter, Harvard University)

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South Pole Dark Sector A LC-130 aircraft is passing the NSF South Pole station Dark Sector during take off. CMB telescopes visible in the background include (left to right) the South Pole Telescope, the BICEP2 telescope, and the Keck Array telescope. (<i>Steffen Richter, Harvard University</i>) A LC-130 aircraft is passing the NSF South Pole station Dark Sector during take off. CMB telescopes visible in the background include (left to right) the South Pole Telescope, the BICEP2 telescope, and the Keck Array telescope. (Steffen Richter, Harvard University)

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Dark Sector Lab The Dark Sector Lab (DSL), located 3/4 of a mile from the Geographic South Pole, houses the BICEP2 telescope (left) and the South Pole Telescope (right). (<i>Steffen Richter, Harvard University</i>) The Dark Sector Lab (DSL), located 3/4 of a mile from the Geographic South Pole, houses the BICEP2 telescope (left) and the South Pole Telescope (right). (Steffen Richter, Harvard University)

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Dark Sector Sunrise The sun rises behind the CMB telescopes at the National Science Foundation’s South Pole Station. (<i>Steffen Richter, Harvard University</i>) The sun rises behind the CMB telescopes at the National Science Foundation’s South Pole Station. (Steffen Richter, Harvard University)

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BICEP2 sunset The sun sets behind BICEP2 (in the foreground) and the South Pole Telescope (in the background). (<i>Steffen Richter, Harvard University</i>) The sun sets behind BICEP2 (in the foreground) and the South Pole Telescope (in the background). (Steffen Richter, Harvard University)

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BICEP2 Electronics Testing Graduate student Justus Brevik tests the BICEP2 readout electronics from the warm environment of the Dark Sector Lab. (<i>Steffen Richter, Harvard University</i>) Graduate student Justus Brevik tests the BICEP2 readout electronics from the warm environment of the Dark Sector Lab. (Steffen Richter, Harvard University)

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BICEP2 Focal Plane The BICEP2 telescope's focal plane consisting of an array of 512 superconducting bolometers, designed to operate at 0.25 K (0.25 degrees Celsius above absolute zero) in order to reduce thermal noise in the detectors. The focal plane was developed and produced at NASA's Jet Propulsion Laboratory. (<i>Anthony Turner, JPL</i>) The BICEP2 telescope's focal plane consisting of an array of 512 superconducting bolometers, designed to operate at 0.25 K (0.25 degrees Celsius above absolute zero) in order to reduce thermal noise in the detectors. The focal plane was developed and produced at NASA's Jet Propulsion Laboratory. (Anthony Turner, JPL)

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BICEP2 Focal Plane under the Microscope The BICEP2 telescope's focal plane uses novel technology, developed at NASA's Jet Propulsion Laboratory, to build an array of devices that use superconductivity to gather, filter, detect, and amplify polarized radiation from the cosmic microwave background. Each pixel is made from a printed antenna sensitive to polarized millimeter-wave radiation, with a filter that determines the spectral response at 150 GHz, and a sensitive detector fabricated on a thin micro-machined membrane. The antennas and filters are made from superconducting and dielectric materials with extremely low propagation loss. The detector uses a superconducting transition-edge film as a sensitive thermometer to detect the heat from millimeter-wave radiation that was collected by the antenna and dissipated at the detector. Finally a tiny electrical current from the sensor is measured with amplifiers on the focal plane called SQUIDs (Superconducting QUantum Interference Devices). The focal planes are manufactured using optical lithography techniques, similar to those used in the industrial production of integrated circuits for computers. (<i>Anthony Turner, JPL</i>) The BICEP2 telescope's focal plane uses novel technology, developed at NASA's Jet Propulsion Laboratory, to build an array of devices that use superconductivity to gather, filter, detect, and amplify polarized radiation from the cosmic microwave background. Each pixel is made from a printed antenna sensitive to polarized millimeter-wave radiation, with a filter that determines the spectral response at 150 GHz, and a sensitive detector fabricated on a thin micro-machined membrane. The antennas and filters are made from superconducting and dielectric materials with extremely low propagation loss. The detector uses a superconducting transition-edge film as a sensitive thermometer to detect the heat from millimeter-wave radiation that was collected by the antenna and dissipated at the detector. Finally a tiny electrical current from the sensor is measured with amplifiers on the focal plane called SQUIDs (Superconducting QUantum Interference Devices). The focal planes are manufactured using optical lithography techniques, similar to those used in the industrial production of integrated circuits for computers. (Anthony Turner, JPL)

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BICEP2 Detector The detector shown in this electron-beam micrograph works by converting the light from the cosmic microwave background into heat in a meandered resistor. A Titanium film tuned on its transition to a superconducting state makes a sensitive thermometer to measure this heat. The resistor and thermometer are located on an island of material, suspended in free space on tiny fibers made by a process called micro-machining. The sensors are cooled to just 0.25 degrees above absolute zero to minimize thermal noise. (<i>Anthony Turner, JPL</i>) The detector shown in this electron-beam micrograph works by converting the light from the cosmic microwave background into heat in a meandered resistor. A Titanium film tuned on its transition to a superconducting state makes a sensitive thermometer to measure this heat. The resistor and thermometer are located on an island of material, suspended in free space on tiny fibers made by a process called micro-machining. The sensors are cooled to just 0.25 degrees above absolute zero to minimize thermal noise. (Anthony Turner, JPL)

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Arrival Cryogenics technicians Kathleen Dewahl and Flint Hamblin arrive at the South Pole after a three hour flight from McMurdo Station on the coast of Antarctica. (<i>Steffen Richter, Harvard University</i>) Cryogenics technicians Kathleen Dewahl and Flint Hamblin arrive at the South Pole after a three hour flight from McMurdo Station on the coast of Antarctica. (Steffen Richter, Harvard University)

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Liquid Helium Offload Liquid Helium for use in BICEP2 (in the background to the right), is being unloaded from a LC-130 aircraft at the Geographic South Pole. (<i>Steffen Richter, Harvard University</i>) Liquid Helium for use in BICEP2 (in the background to the right), is being unloaded from a LC-130 aircraft at the Geographic South Pole. (Steffen Richter, Harvard University)

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Liquid Helium Delivery Liquid Helium is being delivered by snowmobile to BICEP2. (<i>Robert Schwarz, University of Minnesota</i>) Liquid Helium is being delivered by snowmobile to BICEP2. (Robert Schwarz, University of Minnesota)

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BICEP2 Immersive, interactive, 360° Panorama The Dark Sector Lab (DSL) houses the BICEP2 telescope (surrounded by a ground shield) and the South Pole Telescope. Peeking over the BICEP2 ground shield one can make out the Keck Array CMB telescope and the National Science Foundation's Amundsen-Scott South Pole Station.<p>The 360° panorama was photographed from a Kite on a balmy spring day at a temperature of -81.4°F / -63°C (windchill -117.4°F / -83°C) <i>(Steffen Richter, Harvard University)</i><p><small>Use your mouse to move around; SHIFT and CTRL keys to zoom.</small> The Dark Sector Lab (DSL) houses the BICEP2 telescope (surrounded by a ground shield) and the South Pole Telescope. Peeking over the BICEP2 ground shield one can make out the Keck Array CMB telescope and the National Science Foundation's Amundsen-Scott South Pole Station.

The 360° panorama was photographed from a Kite on a balmy spring day at a temperature of -81.4°F / -63°C (windchill -117.4°F / -83°C) (Steffen Richter, Harvard University)
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Google Streetview of the Dark Sector Lab Google Streetview of the Dark Sector Lab roof. The Keck Array CMB telescope and Amundsen-Scott South Pole Station can be seen behind the BICEP2 ground shield (<i>Google</i>) Google Streetview of the Dark Sector Lab roof. The Keck Array CMB telescope and Amundsen-Scott South Pole Station can be seen behind the BICEP2 ground shield (Google).
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