Extrasolar planet detection: a view from the trenches Alex Wolszczan (Penn State) 01/23/06 Collaborators: A. Niedzielski (TCfA) M. Konacki (Caltech)

Ways to find them…

Methods that actually work … Radial velocity Pulse timing Microlensing Transit photometry

Some examples… Neptune-mass planet The transit classic: HD209458 Microlensing planet A “super-comet” around PSR B1257+12?

Orbits from Vr measurements Observations are given in the form of a time series, Vr(i), at epochs t(i), i = 1,…,n A transition from t(i) to (i) is accomplished in two steps: Equation for eccentric anomaly, E From the fit (least squares, etc.), one determines parameters K, e, , T, P

…and from pulsar timing In phase-connected timing, one models pulse phase in terms of spin frequency and its derivatives and tries to keep pulse count starting at t0 A predicted time-of-arrival (TOA) of a pulse at the Solar System barycenter depends on a number of factors:

Determining binary orbits… Collect data: measure Vr’s, TOA’s, P’s Estimate orbital period, Pb (see below) Use Vr’s to estimate a1sini, e, T0, Pb,  (use P’s to obtain an “incoherent orbital solution”) Use TOA’s to derive a “phase-connected” orbital solution

Figuring out the orbital period… Go Lomb-Scargle! If in doubt, try this procedure (borrowed from Joe Taylor): Get the best and most complete time series of your observable (the hardest part) Define the shortest reasonable Pb for your data set Compute orbital phases, I = mod(ti/Pb,1.0) Sort (Pi, ti, I) in order of increasing  Compute s2 = ∑(Pj-Pj-1)2 ignoring terms for which j- j-1> 0.1 Increment Pb = [1/Pb-0.1/(tmax-tmin)]-1 Repeat these steps until an “acceptable” Pb has been reached Choose Pb for the smallest value of s2

The pulsar planet story…

… and the latest puzzle to play with Timing (TOA) residuals at 430 MHz show a 3.7-yr periodicity with a ~10 µs amplitude At 1400 MHz, this periodicity has become evident in late 2003, with a ~2 µs amplitude Two-frequency timing can be used to calculate line-of-sight electron column density (DM) variations, using the cold plasma dispersion law. The data show a typical long-term, interstellar trend in DM, with the superimposed low-amplitude variations By definition, these variations perfectly correlate with the timing residual variations in (a) Because a dispersive delay scales as 2, the observed periodic TOA variations are most likely a superposition of a variable propagation delay and the effect of a Keplerian motion of a very low-mass body

Examples of Vr time series “under construction”

One of the promising candidates… Periods from time domain search: 118, 355 days Periods from periodogram: 120, 400 days Periods from simplex search: 118, 340, also 450 days

…and the best orbital solutions P~340 (e~0.35) appears to be best (lowest rms residual, 2 ~ 1) This case will probably be resolved in the next 2 months, after >2 years of observations

Summary… Given: a time series of your observable Sought: a stable orbital solution to get orbital parameters and planet characteristics Question: astrophysical viability of the model (e.g. stellar activity, neutron star seismology, fake transit events by background stars) Future: new challenges with the advent of high-precision astrometry from ground and space and planet imaging in more distant future