Responses of Private and Public Schools to Voucher Funding: The Czech and Hungarian Experience

A state monopoly in schooling followed the collapse of communism in Central Europe. The centrally planned system was abandoned. Systems comparable with educational voucher scheme, also known as school choice system, were introduced in the Czech Republic and Hungary in the early 1990s. The newly established system of school financing allocates public funds according to the number of students enrolled in a school. Accredited non-state schools, private and religious, are also eligible for public subsidies. The scope and the form of these reforms represent a unique opportunity to test conflicting hypotheses of proponents and opponents of the voucher scheme. In this empirical analysis, we test fundamental theoretical predictions of the voucher model. Specifically, we test: i) whether non-state schools are established at locations where the supply of educational opportunities provided by state schools is low or of low quality, ii) whether state and non-state schools in such a system respond to changes in demand for education, and iii) whether state schools respond to competition from non-state schools. We use detailed school level data on the whole population of schools and data on regional conditions. In our econometric model we estimate education value added, instead of relying on absolute quality of school graduates. We find that non-state schools emerge at locations with excess demand and lower quality state schools. We also find that greater competition from non-state schools creates incentives for state schools with the result that state schools slightly improve the quality of educational inputs used and significantly improve their output, quality of graduates. As concerns the technical schools, we find that non-state schools react to regional labor market conditions in terms of technical branch premium and unemployment rate. We do not find such reactions to market signals by state schools. We introduce this analysis with a review of non-state schools' development in the Czech Republic and Hungary during the 1990s.http://deepblue.lib.umich.edu/bitstream/2027.42/39744/3/wp360.pd

Responses of Private and Public Schools to Voucher Funding:The Czech and Hungarian Experience

A state monopoly in schooling followed the collapse of communism in Central Europe. The centrally planned system was abandoned. Systems comparable with educational voucher scheme, also known as school choice system, were introduced in the Czech Republic and Hungary in the early 1990s. The newly established system of school financing allocates public funds according to the number of students enrolled in a school. Accredited non-state schools, private and religious, are also eligible for public subsidies. The scope and the form of these reforms represent a unique opportunity to test conflicting hypotheses of proponents and opponents of the voucher scheme. In this empirical analysis, we test fundamental theoretical predictions of the voucher model. Specifically, we test: i) whether non-state schools are established at locations where the supply of educational opportunities provided by state schools is low or of low quality, ii) whether state and non-state schools in such a system respond to changes in demand for education, and iii) whether state schools respond to competition from non-state schools. We use detailed school level data on the whole population of schools and data on regional conditions. In our econometric model we estimate education value added, instead of relying on absolute quality of school graduates. We find that non-state school emerge at locations with excess demand and lower quality state schools. We also find that greater competition from non-state schools creates incentives for state schools with the result that state schools slightly improve the quality of educational inputs used and significantly improve their output, quality of graduates. As concerns the technical schools, we find that non-state schools react to regional labor market conditions in terms of technical branch premium and unemployment rate. We do not find such reactions to market signals by state schools. We introduce this analysis with a review of non-state schools' development in the Czech Republic and Hungary during the 1990s.Educational Finance, Government Expenditures and Education, Occupational Choice, Labor Productivity

Cosmic Neutrino Bound on the Dark Matter Annihilation Rate in the Late Universe

How large can the dark matter self-annihilation rate in the late universe be? This rate depends on (rho_DM/m_chi)^2 , where rho_DM/m_chi is the number density of dark matter, and the annihilation cross section is averaged over the velocity distribution. Since the clustering of dark matter is known, this amounts to asking how large the annihilation cross section can be. Kaplinghat, Knox, and Turner proposed that a very large annihilation cross section could turn a halo cusp into a core, improving agreement between simulations and observations; Hui showed that unitarity prohibits this for large dark matter masses. We show that if the annihilation products are Standard Model particles, even just neutrinos, the consequent fluxes are ruled out by orders of magnitude, even at small masses. Equivalently, to invoke such large annihilation cross sections, one must now require that essentially no Standard Model particles are produced.Comment: 4 pages, 2 figures; to appear in the proceedings of the TeV Particle Astrophysics II Workshop, Madison, Wisconsin, 28-31 Aug 200

Status of neutrino astronomy

Astrophysical neutrinos can be produced in proton interactions of charged cosmic rays with ambient photon or baryonic fields. Cosmic rays are observed in balloon, satellite and air shower experiments every day, from below 1e9 eV up to macroscopic energies of 1e21 eV. The observation of different photon fields has been done ever since, today with detections ranging from radio wavelengths up to very high-energy photons in the TeV range. The leading question for neutrino astronomers is now which sources provide a combination of efficient proton acceleration with sufficiently high photon fields or baryonic targets at the same time in order to produce a neutrino flux that is high enough to exceed the background of atmospheric neutrinos. There are only two confirmed astrophysical neutrino sources up to today: the sun and SuperNova 1987A emit and emitted neutrinos at MeV energies. The aim of large underground Cherenkov telescopes like IceCube and KM3NeT is the detection of neutrinos at energies above 100 GeV. In this paper, recent developments of neutrino flux modeling for the most promising extragalactic sources, gamma ray bursts and active galactic nuclei, are presented.Comment: Talk given at Neutrino 2008, Christchurch (New Zealand) 6 pages, 4 figures, 1 tabl

Status of neutrino astronomy

Astrophysical neutrinos can be produced in proton interactions of charged cosmic rays with ambient photon or baryonic fields. Cosmic rays are observed in balloon, satellite and air shower experiments every day, from below 1e9 eV up to macroscopic energies of 1e21 eV. The observation of different photon fields has been done ever since, today with detections ranging from radio wavelengths up to very high-energy photons in the TeV range. The leading question for neutrino astronomers is now which sources provide a combination of efficient proton acceleration with sufficiently high photon fields or baryonic targets at the same time in order to produce a neutrino flux that is high enough to exceed the background of atmospheric neutrinos. There are only two confirmed astrophysical neutrino sources up to today: the sun and SuperNova 1987A emit and emitted neutrinos at MeV energies. The aim of large underground Cherenkov telescopes like IceCube and KM3NeT is the detection of neutrinos at energies above 100 GeV. In this paper, recent developments of neutrino flux modeling for the most promising extragalactic sources, gamma ray bursts and active galactic nuclei, are presented.Comment: Talk given at Neutrino 2008, Christchurch (New Zealand) 6 pages, 4 figures, 1 tabl

Status of neutrino astronomy

Astrophysical neutrinos can be produced in proton interactions of charged cosmic rays with ambient photon or baryonic fields. Cosmic rays are observed in balloon, satellite and air shower experiments every day, from below 1e9 eV up to macroscopic energies of 1e21 eV. The observation of different photon fields has been done ever since, today with detections ranging from radio wavelengths up to very high-energy photons in the TeV range. The leading question for neutrino astronomers is now which sources provide a combination of efficient proton acceleration with sufficiently high photon fields or baryonic targets at the same time in order to produce a neutrino flux that is high enough to exceed the background of atmospheric neutrinos. There are only two confirmed astrophysical neutrino sources up to today: the sun and SuperNova 1987A emit and emitted neutrinos at MeV energies. The aim of large underground Cherenkov telescopes like IceCube and KM3NeT is the detection of neutrinos at energies above 100 GeV. In this paper, recent developments of neutrino flux modeling for the most promising extragalactic sources, gamma ray bursts and active galactic nuclei, are presented.Comment: Talk given at Neutrino 2008, Christchurch (New Zealand) 6 pages, 4 figures, 1 tabl

Muon Track Reconstruction and Data Selection Techniques in AMANDA

The Antarctic Muon And Neutrino Detector Array (AMANDA) is a high-energy neutrino telescope operating at the geographic South Pole. It is a lattice of photo-multiplier tubes buried deep in the polar ice between 1500m and 2000m. The primary goal of this detector is to discover astrophysical sources of high energy neutrinos. A high-energy muon neutrino coming through the earth from the Northern Hemisphere can be identified by the secondary muon moving upward through the detector. The muon tracks are reconstructed with a maximum likelihood method. It models the arrival times and amplitudes of Cherenkov photons registered by the photo-multipliers. This paper describes the different methods of reconstruction, which have been successfully implemented within AMANDA. Strategies for optimizing the reconstruction performance and rejecting background are presented. For a typical analysis procedure the direction of tracks are reconstructed with about 2 degree accuracy.Comment: 40 pages, 16 Postscript figures, uses elsart.st

On the selection of AGN neutrino source candidates for a source stacking analysis with neutrino telescopes

The sensitivity of a search for sources of TeV neutrinos can be improved by grouping potential sources together into generic classes in a procedure that is known as source stacking. In this paper, we define catalogs of Active Galactic Nuclei (AGN) and use them to perform a source stacking analysis. The grouping of AGN into classes is done in two steps: first, AGN classes are defined, then, sources to be stacked are selected assuming that a potential neutrino flux is linearly correlated with the photon luminosity in a certain energy band (radio, IR, optical, keV, GeV, TeV). Lacking any secure detailed knowledge on neutrino production in AGN, this correlation is motivated by hadronic AGN models, as briefly reviewed in this paper. The source stacking search for neutrinos from generic AGN classes is illustrated using the data collected by the AMANDA-II high energy neutrino detector during the year 2000. No significant excess for any of the suggested groups was found.Comment: 43 pages, 12 figures, accepted by Astroparticle Physic

Detection of Atmospheric Muon Neutrinos with the IceCube 9-String Detector

The IceCube neutrino detector is a cubic kilometer TeV to PeV neutrino detector under construction at the geographic South Pole. The dominant population of neutrinos detected in IceCube is due to meson decay in cosmic-ray air showers. These atmospheric neutrinos are relatively well-understood and serve as a calibration and verification tool for the new detector. In 2006, the detector was approximately 10% completed, and we report on data acquired from the detector in this configuration. We observe an atmospheric neutrino signal consistent with expectations, demonstrating that the IceCube detector is capable of identifying neutrino events. In the first 137.4 days of livetime, 234 neutrino candidates were selected with an expectation of 211 +/- 76.1(syst.) +/- 14.5(stat.) events from atmospheric neutrinos