Alanna Connors, for the AstroStatistics Alanna Connors, for the AstroStatistics Working Group at Harvard Smithsonian Working Group at Harvard Smithsonian

Center for AstrophysicsCenter for Astrophysics

““Processing of some sophistication is needed, Processing of some sophistication is needed, rather than being just a fixup at the end.” rather than being just a fixup at the end.”

Tim CornwellTim Cornwell

Astronomy Instruments from Astronomy Instruments from the Quantum Age:the Quantum Age:

Do New Instruments, or Do New Instruments, or New Ideas, Drive New Science?New Ideas, Drive New Science?

OUTLINEOUTLINE All Optical:

Eye and Hand Telescope and Hand Photography

New Science: Equations for fun! Mathematics of Invariance: Relativity+ QM Bohr Atom

New Instruments: Seeing the Invisible Below the Visible: Radio, Infrared (skip) ** Above the visible: Ionizing Radiation Background or signal: Cosmic rays

Old Instruments, New Instruments: Chandra has it easy, but illustrates main principles Tougher Instruments; still, “Do It Right”

Early Observations: Eye, Early Observations: Eye, HandHand

Crab Supernova July 1054 Crab Supernova July 1054 ADAD Anasazi Anasazi

JapanJapan Chinese Chinese

guest guest star star “seen “seen in the in the day like day like Venus”Venus”

Armillary SphereArmillary Sphere

Grand Sweep of Stars and Grand Sweep of Stars and Planets:Planets:

How to Infer 3D from How to Infer 3D from meticulous 2D:meticulous 2D:

Ptolemy, Hypatia, … Ptolemy, Hypatia, …

Telescope: Galileo and Telescope: Galileo and onwardsonwards

Allows more meticulous Allows more meticulous precisionprecision

Planetary Motions: 3D from Planetary Motions: 3D from 2D: Kepler, Brahe, Hooke, 2D: Kepler, Brahe, Hooke,

Newton…Newton…

Statistics:Statistics:

Least-Squares Fitting (LaPlace)Least-Squares Fitting (LaPlace)

Periodic Motion (Fourier)Periodic Motion (Fourier)

SKIPPING many interesting math SKIPPING many interesting math techniques for orbits, etc.techniques for orbits, etc.

Quantum Mechanics & Quantum Mechanics & Relativity: Relativity:

Oh, Equations! Fun!Oh, Equations! Fun! QUANTUM MECHANICSQUANTUM MECHANICS

E = h E = h ( Energy = Planck constant * frequency ) ( Energy = Planck constant * frequency ) = c / = c / (frequency = light-speed / wavelength)(frequency = light-speed / wavelength) Wave properties for light AND matter!Wave properties for light AND matter!

Comes in lumps:Comes in lumps: Particle properties for matter AND light!Particle properties for matter AND light!

RELATIVITY:RELATIVITY: E = m c^2E = m c^2 Electron ~ 0.5 MeV, Proton and neutron ~ 1 GeVElectron ~ 0.5 MeV, Proton and neutron ~ 1 GeV

Potential Potential Energy Energy balanced by balanced by angular angular momentummomentum* Angular * Angular momentum momentum quantizedquantized = = nhnh

* Result: * Result: ConstructivConstructive e interferenceinterference: Integer : Integer ’s ’s in each in each orbit orbit Energy Energy levels ~ levels ~ 1/n^2 1/n^2

Stellar Spectra: Annie Jump Stellar Spectra: Annie Jump Cannon Cannon

Women of Harvard College Women of Harvard College ObservatoryObservatory

Cecelia Payne-Gaposchkin: Cecelia Payne-Gaposchkin: Old Astronomy + New QM for 1st Old Astronomy + New QM for 1st

TimeTime

Huge amount of careful observations of spectra

QM tells ionization balance

Startling thesis result: Most of the visible universe made of Hydrogen!

New Instruments: New Instruments: Seeing the InvisibleSeeing the Invisible

Jumping Over Whole Story of Jumping Over Whole Story of Radio:Radio:

G. Reber, 1932 backyard; G. Reber, 1932 backyard; Present VLAPresent VLA

(But Interferometry - very intersting!)(But Interferometry - very intersting!)

Ionizing Radiation from the Ionizing Radiation from the SkySky

Victor Hess flies with a gold-leaf electroscope like one at left; Measures decreasing discharge time as altitude increases

Radio-Chemistry Skill of Curie Radio-Chemistry Skill of Curie Family:Family:

Supply Standards of Radioactive Supply Standards of Radioactive MaterialsMaterials

Radium, purified

New InstrumentsNew Instruments

•Scintillators (right; also reading) •Cloud chamber DEMO(tracing tracks by hand from photographs!)•Geiger Counter DEMO•Photographic / emulsion•Basics same as many modern ones

Take a minute to think Take a minute to think about Statistics, Iabout Statistics, I

Historical notes on watching for Historical notes on watching for scintillations in a dark roomscintillations in a dark room

Tracks: tracing by hand (!) until very Tracks: tracing by hand (!) until very recently (some HEP still do!)recently (some HEP still do!) Historical note: for some reason, most technicians Historical note: for some reason, most technicians

who do this are women -- Claudia Brevard and CGRO who do this are women -- Claudia Brevard and CGRO EGRETEGRET

Any thoughts on statistics?Any thoughts on statistics?

Take a minute to think Take a minute to think about Statistics, IIabout Statistics, II

Optical “culture”: What can I see?Optical “culture”: What can I see?

Invisible light “culture”:Invisible light “culture”:

= = RR ii + + bb

<counts>=Eff. Area<counts>=Eff. AreaInst.Redist.Inst.Redist.Source intensity +Sky+Inst. Source intensity +Sky+Inst. BkgBkg

Measured counts = Y ~ Poisson (Measured counts = Y ~ Poisson ())

Poisson(Poisson() ~ Normal() ~ Normal(,sqrt(,sqrt())))

Least-squares, Least-squares, ^2 minimization, CC w/ ^2 minimization, CC w/ RR

Pre-1975: Early X-Ray Pre-1975: Early X-Ray Telescopes: Telescopes:

Bin size>PSF; Many counts/bin; NO Bin size>PSF; Many counts/bin; NO processingprocessing SKYLAB: Solar – very large bright sourceSKYLAB: Solar – very large bright source

Copernicus, ANS; sky, but only point Copernicus, ANS; sky, but only point sourcessources

Pre-1975: Early G-Ray Pre-1975: Early G-Ray “Telescopes”“Telescopes”

Bin size>PSF; fewer counts; “Bin them Bin size>PSF; fewer counts; “Bin them up”up” > 100 MeV G-ray > 100 MeV G-ray

profile of Galactic profile of Galactic planeplane

SAS-2 satellite: charged particle shield covers spark chamberS

1975-1990's: COS-B Gamma-Ray 1975-1990's: COS-B Gamma-Ray SatelliteSatellite

Preliminary imaging; Simple Gauss-Preliminary imaging; Simple Gauss-Normal Normal

“fix it up at the end”“fix it up at the end” Galactic Anti-center Galactic Anti-center region: Crab and region: Crab and Geminga pulsars + Geminga pulsars + Diffuse emissionDiffuse emission

COS-B satellite (Aug '75 - Apr '82; 2 keV – 5GeV) Cutaway of spark-chambers, shielding

1975-1990s: Einstein X-Ray Observatory (HEAO2)

First medium energy X-ray point sources+diffuse imaging; G-N approximation;

“fix it up at the end”Tycho Supernova Remnant (1572)

Einstein Observatory (Nov. '78-April '81; 0.15-3 keV) Mirror assembly

1990's and Beyond: Great 1990's and Beyond: Great ObservatoriesObservatories

need to do it right; no longer can “fix it up need to do it right; no longer can “fix it up at the end”at the end”

SvOutPlaceObject

Compton Gamma-Ray Observatory (Apr '91 – Jun '00; COMPTEL: 0.8-30 MeV; EGRET 20 MeV-100 GeV)

Chandra X-Ray Observatory Jul 1999 and beyond; 0.1-10 keV)

CGRO/EGRET All-Sky Map CGRO/EGRET All-Sky Map diffuse glow; significantly non-diffuse glow; significantly non-

Gaussian statisticsGaussian statistics

SvOutPlaceObject

Log Counts per time per 05 degree pixel: Four years of data

(ranges from zero to thousands per pixel)

CGRO/EGRET All-Sky Map CGRO/EGRET All-Sky Map Log Inferred flux per 0.5 degree pixel: Four years

of data(known point and diffuse sources modelled out)

Haar wavelet basis: Dixon, Hartman, Kolaczyk et al

CGRO/COMPTEL All-Sky CGRO/COMPTEL All-Sky 1.8MeV1.8MeV

(Knödelseder, Dixon, Diehl, Strong, et al 1998)(Knödelseder, Dixon, Diehl, Strong, et al 1998)very non-diagonal instrument response; horrid very non-diagonal instrument response; horrid

backgroundbackground

Mkn 501 at TeV: Whipple Mkn 501 at TeV: Whipple Observatory Observatory

(Quinn et al. for Whipple collaboration, 1996, (Quinn et al. for Whipple collaboration, 1996, ApJL, 456, p83)ApJL, 456, p83)

1st AGN DISCOVERED at TeV; horrid background, 1st AGN DISCOVERED at TeV; horrid background, responseresponse

Chandra has it “easy” …Chandra has it “easy” …BUT illustrates main BUT illustrates main

principlesprinciples

CHANDRA Image of Tycho Supernova

CHANDRA PSF on-axis: varies with energy

CHANDRAPSF: spreads off-axis

5 arcmin off-axis

CHANDRAPSF off- axis10 arcmin

CHANDRA ACIS BACKGROUND

Effect of a Charged Particle Event

FI CCD BI CCD

Higher Energy: More Extreme!Higher Energy: More Extreme! Dim, BKG, Rate… Dim, BKG, Rate…

Hurley et al GRB940210:“The diffuse background in this direction results in about one photon above 30 MeV detected by EGRET in 7 minutes. On the subsequent Compton Observatory orbit, 1.5 hours later, EGRET had 20 minutes of livetime, and 10 gamma rays were detected from the region around the annulus, one with energy 26 GeV.”* ABOUT 2 DOZEN PAPERS on 1!

Pathway for Future:Pathway for Future: Other instruments: Ground-based TeVOther instruments: Ground-based TeV

GLAST, Swift, …GLAST, Swift, …

CON-X, etcCON-X, etc

““Doing it right” in one area Doing it right” in one area helps many overlapping helps many overlapping

areasareas