Документ взят из кэша поисковой машины. Адрес оригинального документа : http://hea-www.harvard.edu/AstroStat/Stat310MM_VI_VII/jcm_20061212.pdf Дата изменения: Tue Dec 12 16:52:58 2006 Дата индексирования: Tue Oct 2 05:48:26 2012 Кодировка: Поисковые слова: apollo 13

Astrophysics for Mathematicians

Jonathan McDowell Smithsonian Astrophysical Observatory






Source and Background


Key concept in astronomy: distinction between source and background Like signal and noise, but... sometimes the background is interesting ('signal') in itself








Deep Field
Faintest sources have only a few photons (get 1 per 4 days per source) Background from sky (varies with position slowly; varies with energy) and from detector (varies with time and position) - both source and backgrounds are Poisson Is this a source or a background fluctuation? What are the confidence intervals on the number of photons from this source? I know there is a star here; what is the upper limit on its flux?






Crowded Field
Problem here is overlapping sources and extended emission What is the error on the individual fluxes of source 1 and source 2 when they both overlap with source 3? What is the total flux of the diffuse purple stuff, ignoring the stars on top of it? What are the fluxes of the stars? How does my confidence in the reality (i.e. flux >0) of a source change if it's on this varying background? How can I automatically detect linear features like this? (Scene parsing problem)






Cosmology: The Hubble Redshift
Spectral lines give fingerprint of compositio, temperature, etc. Hubble's Law: more distant objects are shifted to the red - 'redshift', expanding universe - How do you separate continuum from lines? Model-dependent Measure peak in presence of noise Measure integral under curve in presence of noise and model assumptions






Cosmology: Thinking Big
Map galaxies out to 500 million light years Real velocities (e.g. clusters) superimposed on Hubble flow: distorts radial coordinate Distance is NOT EUCLIDEAN! Volume sampled is no longer 4/3 pi r cubed due to curved space-time Want to derive population properties brightness, size, etc - as function of distance (therefore, cosmic time) But - biases in sample






Biases
NUMBER OF STARS VS MASS Eddington Bias: in astronomy, there are always more little faint things than big bright things. This is true for asteroids, stars, galaxies, .... Suppose there are 10 stars of mass 0.5 and 100 stars of mass 0.4, and you have a 20 percent error on measuring the mass. Then you'll put 2 of the 10 big stars in the smaller 0.4 bin, and you'll put 20 of the 100 small stars in the bigger 0.5 bin, ending up with a measurement of 28 for mass 0.5 and 82 for mass 0.4 - a big problem especially if you truncate your dataset at 0.5.


This is Eddington bias.

HOW BIG --->


Biases
Malmquist Bias: Distant objects are fainter Your telescope can't see the faintest objects Comparing subsamples of near and far objects, you get a different distribution of true luminosities






Quasars






Quasars: V/Vmax
Suppose you observe 1000 quasars with different brightnesses but you don't know their true distances. Each observation has a different limiting brightness. Define Smin is the faintest that to still have seen it. If its actual and Euclidean geometry apply Vmax is the volume the quasar have seen it. a given quasar could have been for you brightness is S, then if the inverse square law V/Vmax = (S/Smin)**(-1.5) where could have been in and you would still

If the population is uniformly distributed in space, you expect for the population to be 0.5; typically half the objects will be in the inner half of the volume and half will be in the outer half. If the answer turns out to be not 0.5, then your population is evolving... You can do the same thing evenwhen the geometry isn't Euclidean (exercise :-))



Censored statistics
These are energy distributions (brightness versus wavelength) of quasars. What is the best estimate of the total brightness of each object? (join the dots) What is the best estimate of the typical energy distribution of the population? You need to take the upper limits into account. (e.g. using the Kaplan-Meier bound) What are the differences between the objects? (PCA)






Binary stars



IM Peg: little yellow star like our Sun, plus big red star with strong magnetic field



Light Curves - Nice and Nasty

Poor sampling; gaps on similar timescale to periodic components Search for periodicities and quasi-periodicities in the presence of noise and complicated window (gap) functions




We're all going to die



Is this rock going to hit the Earth? Can we reliably propagate the orbit 20 years in the future and understand the errors? " There is a 1 in 200 chance that this will hit the Earth in 2028..' - but next week's data point reduces the chance to zero. Can we give the public a better way of expressing the risk than this simple minded conditional probability?