Science Highlights from The Green Bank Telescope. Felix Jay Lockman NRAO, Green Bank WV
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1 Science Highlights from The Green Bank Telescope Felix Jay Lockman NRAO, Green Bank WV
2 The Green Bank Telescope (GBT) Sensitivity Radio Quiet Zone 100 meters
3 Receivers cover 0.1 to 100 GHz >85% of total sky covered δ -46 National Radio Quiet Zone Competitively Scheduled
4 National Radio Quiet Zone
5 The Green Bank Telescope (GBT)
6
7 The Active Surface RMS < 240μ at night the goal is 210μ University of Georgia, Sept 2011
8 6220 h in 2014 ~⅓ at ν 18 GHz Point source sensitivity of a ~120m telescope Point source sensitivity 2 better than VLA at 2 GHz University of Georgia, Sept 2011
9
10
11 Research areas of most-cited GBT publications (November 2014) Pulsars and compact objects Gravity and General Relativity Galactic Hydrogen surveys Interstellar Chemistry The internal structure of Mercury Evolution of spiral galaxies Star formation & pre-stellar objects Studies of a binary black hole Hydrogen content of galaxies Molecules in highly redshifted galaxies Anisotropies in the cosmic Infrared background
12 A digression on the sensitivity of radio telescopes angular resolution λ/diam
13 A digression on the sensitivity of radio telescopes angular resolution λ/diam point source signal strength πr a 2
14 A digression on the sensitivity of radio telescopes angular resolution λ/diam point source signal strength πr a 2 time to detect (signal strength) - 2
15 A digression on the sensitivity of radio telescopes angular resolution λ/diam point source signal strength πr a 2 time to detect (signal strength) - 2 t ra - 4 (point source)
16 A digression on the sensitivity of radio telescopes point source t / 1 A 2 e
17 A digression on the sensitivity of radio telescopes point source t / 1 A 2 e extended source t / f 2 / Diam4 A 2 e
18 A digression on the sensitivity of radio telescopes Diam = 1000 m Diam = 100 m
19 A digression on the sensitivity of radio telescopes Instrument f 2 21cm HPBW GBT Arecibo VLA-D VLA-C VLA-B ASKAP 10 6
20 A digression on the sensitivity of radio telescopes Instrument f 2 21cm HPBW GBT Arecibo VLA-D VLA-C VLA-B ASKAP 10 6 For a given collecting area, the brightness sensitivity is always greatest for a filled aperture
21 A digression on the sensitivity of radio telescopes Instrument f 2 21cm HPBW GBT Arecibo VLA-D VLA-C VLA-B ASKAP 10 6 For a given collecting area, the brightness sensitivity is always greatest for a filled aperture This is not related to the issue of missing short spacings
22 VLBA Limited to T>10 5 K
23 Bi-static radar studies with Arecibo GBT receiving
24 VENUS RADAR B. Campbell
25 A radar return is speckled
26 A radar return is speckled
27 The radar return is speckled
28
29
30 Large Longitude Libration of Mercury Reveals a Molten Core Margot et al Science
31
32 Europa
33 Chelyabinsk, Russia -- Feb. 15, 2013
34 Goldstone-GBT 27 Jan 2015 Asteroid 2004BL86
35 The Pulsar Renaissance Fastest Pulsar Most Massive Pulsar Pulsars in Globular Clusters Tests of General Relativity Relativistic Spin Precession Pulsar in a three-body system Coolest white dwarf star (a diamond as big as the Ritz)
36 A Solid Carbon Diamond Star Orbiting a Pulsar 1.05 M Kaplan et al. (2014) Teff < K
37 A Pulsar in a Triple System ARECIBO+ GBT Ransom et al. Nature (2014) Testing the Equivalence Principle
38 Gravitational Delay
39 GBT measurements of the radio pulsar J Residual delay µs Demorest et al. (2010)
40 Residual delay µs
41 Residual delay µs
42 DETECTING GRAVITATIONAL RADIATION
43 Predicted Power in Gravitational Radiation Pulsar timing
44 VLBI Resolution of the Pleiades distance controversy Melis et al. (2014)
45 The Chemistry of Interstellar Space Some (of the 17+) New GBT Molecule Detections C6 H+
46 The Chemistry of Interstellar Space propenal propanal cyanoformaldehyde ketenimine Some (of the 17+) New GBT Molecule Detections C6 H+
47 HC7N: A Chemical Clock in a Molecular Cloud? Friesen et al. (2013) [NH3]/[HC7N]
48 Star Formation in a Filament in Taurus Dust GBT NH3 Young Min Seo et al ApJ 805, 185
49 Star Formation in a Filament in Taurus Dust GBT NH3 Young Min Seo et al ApJ 805, 185
50 Star Formation in a Filament in Taurus Young Min Seo et al ApJ 805, 185
51 GBT W-band Spectral Survey Frayer et al. (2015)
52 GBT detection of mm-cm sized dust in star-forming clouds 5 Schnee et al. (2014) MUSTANG Bolometer Array 3.3mm GHz
53 GBT High-Resolution SZE in a Galaxy Cluster X-ray: ne 2 SZE: ne VLA non-thermal
54 HI Intensity Mapping Ui- Le Pen, Jeffrey B. Peterson et al.
55 Masui et al. (2013)
56 The Local Group of Galaxies
57 No Hydrogen in the Milky Way s Dwarf Galaxies Galaxy L (L ) MHI (M ) Segue I 340 <11 UMa II 41,000 <74 Bootes II 1,000 <38 Coma Ber 3,700 <62 Ursa Mi 280,000 <63 Draco 280,000 <133 GBT results from Spekkens et al Spitzer Cloud 400
58 Spekkens et al. 2014
59 Optical + VLA + GBT Chynoweth et al
60 GBT HI study of Andromeda M Thilker et al 2004
61 Andromeda is devouring its smaller neighbors
62 M33 M31
63 M33 M31
64 GBT detection of Local Group Gas Clouds Wolfe et al x10 17 Wolfe, Lockman, & Pisano 2015
65 GBT detection of Local Group Gas Clouds No stars in any of these! Not self-gravitating 5x10 17 Wolfe et al Wolfe, Lockman, & Pisano 2015
66
67 The GBT in 2016+
68 The GBT in VEGAS (NSF grant to UC Berkeley) 16 spectrometers Up to 8 spectral windows per spectrometer Up to1.25 GHz per spectrometer
69 ARGUS -- 8 GBT spectroscopy at 3mm 16 element scalable GHz FPA Stanford/CIT- JPL/UMd/ Miami/NRAO (NSF grant to Stanford)
70 GBT MUSTANG - 2 (NSF grant to Univ Penn) 223 pixels >4 FOV 35x faster than MUSTANG
71 ARGUS 3mm 16-pixel camera footprint 4% complete sampling
72 FLAG 21cm
73 UMass Scalable GHz PAF
74 The wave of the future UMass Scalable GHz PAF
75 The wave of the future UMass Scalable GHz PAF
76
77 How do I get to use the GBT?
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