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Mark Huber

Publications and source records attributed to Mark Huber.

38 records · Page 3Linked to original sources

Exact Sampling from Perfect Matchings of Dense Nearly Regular Bipartite Graphs

We present the first algorithm for generating random variates exactly uniformly from the set of perfect matchings of a bipartite graph with a polynomial expected running time over a nontrivial set of graphs. Previous Markov chain approaches obtain approximately uniform variates for arbitrary graphs in polynomial time, but their general running time is $Θ(n^{26} (\ln n)^2).$ Our algorithm employs acceptance/rejection together with a new upper limit on the permanent of a form similar to Bregman's Theorem. For a graph with $2n$ nodes where the degree of every node is nearly $γn$ for a constant $γ$, the expected running time is $O(n^{1.5 + .5/γ})$. Under these conditions, Jerrum and Sinclair showed that a Markov chain of Broder can generate approximately uniform variates in $Θ(n^{4.5 + .5/γ} \ln n)$ time, making our algorithm significantly faster on this class of graph. With our approach, approximately counting the number of perfect matchings (equivalent to finding the permanent of a 0-1 matrix and so $\sharp P$ complete) can be done without use of selfreducibility.

math.PR↗

The Pulsar-White Dwarf-Planet System in Messier 4: Improved Astrometry

A young and undermassive white dwarf has been identified as the possible companion to the millisecond pulsar PSR B1620-26 in Messier 4. This association is important as it then helps constrain the mass of the third body in the system to be of order a few times that of Jupiter. The presence of this planet in M4 has critical implications for planetary formation mechanisms in metal-poor environments such as globular clusters and the early Universe. The identification of the white dwarf is purely via the agreement in position between it and the pulsar and was limited by the accuracy of the pointing of HST which is +/-0.7 arcsec. We have redetermined the position of the white dwarf using ground-based data tied to USNOB-1.0 and find that the pulsar and white dwarf are now coincident to within 0.12 +/- 0.13 arcsec further strengthening the case for association between the two. We have also attempted to improve the proper motion measurement of the white dwarf by a maximum likelihood analysis of the stellar positions measured over a baseline of 5 years. While the errors are reduced by almost a factor of 6 from our previous work, we still have not resolved the cluster's intrinsic dispersion in proper motion. Thus the proper motion of the white dwarf with respect to the cluster itself is still not known although it is very small and is within 2-sigma of that of the cluster internal dispersion.

astro-ph↗