The Green Bank Telescope Ronald Maddalena National Radio Astronomy Observatory
National Radio Astronomy Observatory National Laboratory Founded in 1954 Funded by the National Science Foundation
Telescope Structure and Optics
Large 100-m Diameter: High Sensitivity High Angular Resolution – wavelength / Diameter
GBT Telescope Optics 110 m x 100 m of a 208 m parent paraboloid Effective diameter: 100 m Off axis - Clear/Unblocked Aperture
Telescope Optics High Dynamic Range High Fidelity Images
Telescope Optics
Prime Focus: Retractable boom Gregorian Focus: 8-m subreflector - 6-degrees of freedom
Telescope Optics Rotating Turret with 8 receiver bays
Telescope Structure Fully Steerable Elevation Limit: 5º Can observe 85% of the entire Celestial Sphere Slew Rates: Azimuth - 40º/min; Elevation - 20º/min
Telescope Structure Blind Pointing: (1 point/focus) Offset Pointing: (90 min) Continuous Tracking: (30 min)
Telescope Structure
Active Surface Surface Deformations from Finite Element Model
Active Surface
Main Reflector: 2209 actuated panels with 68 μm rms. Total surface: rms 400 μm
Receivers ReceiverOperating RangeStatus Prime Focus 10.29—0.92 GHzCommissioned Prime Focus —1.23 GHzCommissioned L Band1.15—1.73 GHzCommissioned S Band1.73—2.60 GHzCommissioned C Band3.95—5.85 GHzCommissioned X Band8.2—10.0 GHzCommissioned Ku Band12.4—15.4 GHzCommissioned K Band18—26.5 GHzCommissioned Ka Band26—40 GHzPartially Commissioned Q Band40—50 GHzCommissioned W Band68—92 GHzUnder Construction Penn Array86—94 GHzUnder Construction
Backends
National Radio Quiet Zone
Science with the GBT
Current Science Projects
Milky Way Our Home Galaxy Projected image on the night sky is the Milky Way Dust in the Interstellar Medium obstructs our optical view. Need Radio observations to peer through the dust Our perspective is from a star in the outer Milky Way. Serves as a nearby example of the 100 billion other galaxies
Interstellar Medium The Material Between the Stars Constituents Gases Hydrogen (92% by number) Helium (8%) Oxygen, Carbon, etc. (0.1 %) Dust Particles 1% of the mass of the ISM Average Density: 1 H atom / cm 3 Place where stars & planets form The byproduct of the death of stars
Interstellar Medium Properties State of Hydrogen TemperatureDensities (H/cm 3 ) Percent Volume HII Regions & Planetary Nebulae Ionized5000 K0.5< 1% Diffuse ISMIonized1,000,000 K0.0150% Warm ISMAtomic3000 K0.330% Cold ISMAtomic300 K3010% Molecular Clouds Molecular< 30 K> 30010%
HII Regions Isolated regions where H is ionized. UV from hot (20,000 – 50,000 K), blue stars produces ionization. HII Regions Formed around young, massive, & short- lived (< few x 10 6 years) stars. Near regions where they formed
Scientific Results - Imaging
Diffuse ISM – Galactic Center
Atomic Hydrogen Spectral-Line Radiation Discovered by Ewen and Purcell in Found in regions where H is atomic. 300 K, 30 H/cm 3 Spin-flip (hyperfine) transition Electron & protons have “spin” In a H atoms, spins of proton and electron may be aligned or anti-aligned. Aligned state has more energy. Difference in Energy = h v v = 1420 MHz An aligned H atom will take 11 million years to flip the spin of the electron. But, atoms in Milky Way so H atoms per second emit at 1420 MHz
Spectral-Line Radiation- What do they tell us? Width of line Motion of gas within the region Height of the line Maybe temperature of the gas Area under the line Maybe number of atoms in that direction.
Doppler Affect Frequency Observed = Frequency Emitted / (1 + V/c)
Spectral-Line Radiation Milky Way Rotation and Mass For any cloud Observed velocity = difference between projected Sun’s motion and projected cloud motion. For cloud B The highest observed velocity along the line of site V Rotation = V observed + V sun *sin(L) R = R Sun * sin(L) Repeat for a different angle L and cloud B Determine V Rotation (R) From Newton’s law, derive M(R) from V(R)
Scientific Results – Milky Way Gas
Scientific Results – Milky Way
Interstellar Molecules Hydroxyl (OH) first molecule found with radio telescopes (1964). Molecule Formation: Need high densities Lots of dust needed to protect molecules for stellar UV But, optically obscured – need radio telescopes Low temperatures (< 100 K) Some molecules (e.g., H2) form on dust grains Most form via ion-molecular gas-phase reactions
Interstellar Molecules Ion-molecular gas-phase reactions Starts with a cosmic ray that ionizes a H atom All exothermic reactions Charge transfer Two-body interactions
Interstellar Molecules About 90% of the over 129 interstellar molecules discovered with radio telescopes. Rotational (electric dipole) Transitions Up to thirteen atoms Many carbon-based (organic) Many cannot exist in normal laboratories (e.g., OH) H 2 most common molecule: No dipole moment so no rotational transition at radio wavelengths. Only observable in UV (rotational) or Infrared (vibrational) transitions from space. Use CO, the second most common molecule, as a tracer for H 2
A few molecules (OH, H 2 O, …) maser Interstellar Molecules
Scientific Results - Molecules
Molecular Clouds Discovered 1970 by Penzias, Jefferts, & Wilson and others. Coldest (5-30 K), densest (100 –10 6 H atoms/cm 3 ) parts of the ISM. Where stars are formed 50% of the ISM mass A few percent of the Galaxy’s volume. Concentrated in spiral arms Dust Clouds = Molecular Clouds
Molecular Clouds Discovered 1970 by Penzias, Jefferts, & Wilson and others. Coldest (5-30 K), densest (100 –10 6 H atoms/cm 3 ) parts of the ISM. Where stars are formed 50% of the ISM mass A few percent of the Galaxy’s volume. Concentrated in spiral arms Dust Clouds = Molecular Clouds
Scientific Results – Lunar Radar
Scientific Results – Galaxy Formation
Scientific Results - Pulsars
Fastest Pulsar