”En ole vielä tavannut lasta, jolle musiikki ei olisi tavalla tai toisella, eri muodoissaan ollut hyödyksi ja avuksi”:erityisluokanopettajien kokemuksia musiikin terapeuttisesta käytöstä erityiskasvatuksessa

Tiivistelmä. Tässä kasvatustieteen pro gradu -tutkielmassa käsitellään erityisluokanopettajien kokemuksia musiikin terapeuttisesta käytöstä erityiskasvatuksessa. Musiikin terapeuttinen vaikutus ihmismieleen on tiedetty jo vuosituhansien ajan. Ihmiset hyödyntävät musiikin terapeuttisuutta arjessaan jopa huomaamattaan. Vauvoille lauletaan kehtolauluja, koska ne rauhoittavat mieltä. Ennen tärkeää urheilusuoritusta urheilijat saattavat kuunnella energisoivaa musiikkia, koska he saavat siitä lisäenergiaa. Surun keskellä musiikki auttaa piristymään ja käsittelemään tunteita. Musiikin avulla voi siis virittäytyä moniin erilaisiin mielentiloihin. Tutkimuksen viitekehyksessä tarkastellaan erityiskasvatuksen kenttää ja musiikin terapeuttisuutta. Erityiskasvatuksen kentän tarkastelussa keskityttiin sen asemaan laissa ja peruskoulussa. Jokaisella oppilaalla on oikeus erityisopetukseen, joka tänä päivänä toteutuu peruskouluissa kolmiportaisena tukea. Tuki on jaettu yleiseen, tehostettuun ja erityiseen tukeen. Musiikin terapeuttisuutta tarkasteltiin musiikkiterapian näkökulmasta: mitä eri menetelmiä musiikkiterapiassa käytetään ja miten ne voivat auttaa etenkin diagnoosin omaavaa lasta. Tutkielma toteutettiin kvalitatiivisena tutkimuksena ja fenomenologisella tutkimusotteella. Tutkielmalla pyrittiin etsimään vastauksia kahteen tutkimuskysymykseen: Miten musiikkia käytetään terapeuttisesti erityiskasvatuksessa? ja Millaisena erityisluokanopettajat ovat kokeneet musiikin terapeuttisen käytön erityiskasvatuksessa? Tutkimuksen aineisto kerättiin sähköisen kyselylomakkeen muodossa ja siihen vastasi 12 erityisluokanopettajaa eri puolilta Suomea. Aineiston analysointiin hyödynnettiin aineistolähtöisen sisällönanalyysin menetelmiä. Tuloksista saatiin selville, että erityisluokanopettajat käyttävät musiikin terapeuttisuutta työssään hyvin monipuolisesti. Eniten musiikin terapeuttisuutta hyödynnettiin oppilaiden rentoutumisessa ja rauhoittumisessa sekä itseilmaisussa. Vastaajat mainitsivat myös diagnoosin omaavien lasten hyötyvän musiikin terapeuttisuudesta. Ylivilkkaat lapset hyötyvät sekä musiikin rauhoittavasta vaikutuksesta että energiaa purkavasta vaikutuksesta. Autistiset lapset reagoivat hyvin usein musiikkiin. Heitä voi musiikin avulla kannustaa sosiaaliseen kanssakäymiseen ja katsekontaktiin. Mutistit voivat ilmaista tunteitaan esimerkiksi musiikkimaalauksen avulla. Kaikki vastaajat kokivat musiikin terapeuttisuuden hyödylliseksi: 7/12 vastaajaa koki sen melko hyödylliseksi ja 5/12 vastaajaa todella hyödylliseksi. Musiikin terapeuttisella käytöllä koettiin olevan oppilaisiin suurimmaksi osaksi positiivinen vaikutus. Musiikin koettiin rauhoittavan ja rentouttavan oppilaita sekä sillä koettiin olevan oppimista tukevia vaikutuksia

Search algorithm for a gravitational wave signal in association with Gamma Ray Burst GRB030329 using the LIGO detectors

One of the brightest Gamma Ray Burst ever recorded, GRB030329, occurred during the second science run of the LIGO detectors. At that time, both interferometers at the Hanford, WA LIGO site were in lock and acquiring data. The data collected from the two Hanford detectors was analyzed for the presence of a gravitational wave signal associated with this GRB. This paper presents a detailed description of the search algorithm implemented in the current analysis.Comment: To appear in the Proceedings of 8th Gravitational Wave Data Analysis Workshop (Milwaukee, WI) (Class. Quantum Grav.

Setting upper limits on the strength of periodic gravitational waves from PSR J1939+2134 using the first science data from the GEO 600 and LIGO detectors

Data collected by the GEO 600 and LIGO interferometric gravitational wave detectors during their first observational science run were searched for continuous gravitational waves from the pulsar J1939+2134 at twice its rotation frequency. Two independent analysis methods were used and are demonstrated in this paper: a frequency domain method and a time domain method. Both achieve consistent null results, placing new upper limits on the strength of the pulsar's gravitational wave emission. A model emission mechanism is used to interpret the limits as a constraint on the pulsar's equatorial ellipticity

Searching for gravitational waves from known pulsars

We present upper limits on the amplitude of gravitational waves from 28 isolated pulsars using data from the second science run of LIGO. The results are also expressed as a constraint on the pulsars' equatorial ellipticities. We discuss a new way of presenting such ellipticity upper limits that takes account of the uncertainties of the pulsar moment of inertia. We also extend our previous method to search for known pulsars in binary systems, of which there are about 80 in the sensitive frequency range of LIGO and GEO 600.Comment: Accepted by CQG for the proceeding of GWDAW9, 7 pages, 2 figure

Upper limits on the strength of periodic gravitational waves from PSR J1939+2134

The first science run of the LIGO and GEO gravitational wave detectors presented the opportunity to test methods of searching for gravitational waves from known pulsars. Here we present new direct upper limits on the strength of waves from the pulsar PSR J1939+2134 using two independent analysis methods, one in the frequency domain using frequentist statistics and one in the time domain using Bayesian inference. Both methods show that the strain amplitude at Earth from this pulsar is less than a few times $10^{-22}$.Comment: 7 pages, 1 figure, to appear in the Proceedings of the 5th Edoardo Amaldi Conference on Gravitational Waves, Tirrenia, Pisa, Italy, 6-11 July 200

First upper limits from LIGO on gravitational wave bursts

We report on a search for gravitational wave bursts using data from the first science run of the LIGO detectors. Our search focuses on bursts with durations ranging from 4 ms to 100 ms, and with significant power in the LIGO sensitivity band of 150 to 3000 Hz. We bound the rate for such detected bursts at less than 1.6 events per day at 90% confidence level. This result is interpreted in terms of the detection efficiency for ad hoc waveforms (Gaussians and sine-Gaussians) as a function of their root-sum-square strain h_{rss}; typical sensitivities lie in the range h_{rss} ~ 10^{-19} - 10^{-17} strain/rtHz, depending on waveform. We discuss improvements in the search method that will be applied to future science data from LIGO and other gravitational wave detectors.Comment: 21 pages, 15 figures, accepted by Phys Rev D. Fixed a few small typos and updated a few reference

Improving the sensitivity to gravitational-wave sources by modifying the input-output optics of advanced interferometers

We study frequency dependent (FD) input-output schemes for signal-recycling interferometers, the baseline design of Advanced LIGO and the current configuration of GEO 600. Complementary to a recent proposal by Harms et al. to use FD input squeezing and ordinary homodyne detection, we explore a scheme which uses ordinary squeezed vacuum, but FD readout. Both schemes, which are sub-optimal among all possible input-output schemes, provide a global noise suppression by the power squeeze factor, while being realizable by using detuned Fabry-Perot cavities as input/output filters. At high frequencies, the two schemes are shown to be equivalent, while at low frequencies our scheme gives better performance than that of Harms et al., and is nearly fully optimal. We then study the sensitivity improvement achievable by these schemes in Advanced LIGO era (with 30-m filter cavities and current estimates of filter-mirror losses and thermal noise), for neutron star binary inspirals, and for narrowband GW sources such as low-mass X-ray binaries and known radio pulsars. Optical losses are shown to be a major obstacle for the actual implementation of these techniques in Advanced LIGO. On time scales of third-generation interferometers, like EURO/LIGO-III (~2012), with kilometer-scale filter cavities, a signal-recycling interferometer with the FD readout scheme explored in this paper can have performances comparable to existing proposals. [abridged]Comment: Figs. 9 and 12 corrected; Appendix added for narrowband data analysi

Analysis of LIGO data for gravitational waves from binary neutron stars

We report on a search for gravitational waves from coalescing compact binary systems in the Milky Way and the Magellanic Clouds. The analysis uses data taken by two of the three LIGO interferometers during the first LIGO science run and illustrates a method of setting upper limits on inspiral event rates using interferometer data. The analysis pipeline is described with particular attention to data selection and coincidence between the two interferometers. We establish an observational upper limit of $\mathcal{R}<$1.7 \times 10^{2}$per year per Milky Way Equivalent Galaxy (MWEG), with 90coalescence rate of binary systems in which each component has a mass in the range 1--3$M_\odot$.Comment: 17 pages, 9 figure

Detector Description and Performance for the First Coincidence Observations between LIGO and GEO

For 17 days in August and September 2002, the LIGO and GEO interferometer gravitational wave detectors were operated in coincidence to produce their first data for scientific analysis. Although the detectors were still far from their design sensitivity levels, the data can be used to place better upper limits on the flux of gravitational waves incident on the earth than previous direct measurements. This paper describes the instruments and the data in some detail, as a companion to analysis papers based on the first data.Comment: 41 pages, 9 figures 17 Sept 03: author list amended, minor editorial change

All-sky search for periodic gravitational waves in LIGO S4 data

We report on an all-sky search with the LIGO detectors for periodic gravitational waves in the frequency range 50-1000 Hz and with the frequency's time derivative in the range -1.0E-8 Hz/s to zero. Data from the fourth LIGO science run (S4) have been used in this search. Three different semi-coherent methods of transforming and summing strain power from Short Fourier Transforms (SFTs) of the calibrated data have been used. The first, known as "StackSlide", averages normalized power from each SFT. A "weighted Hough" scheme is also developed and used, and which also allows for a multi-interferometer search. The third method, known as "PowerFlux", is a variant of the StackSlide method in which the power is weighted before summing. In both the weighted Hough and PowerFlux methods, the weights are chosen according to the noise and detector antenna-pattern to maximize the signal-to-noise ratio. The respective advantages and disadvantages of these methods are discussed. Observing no evidence of periodic gravitational radiation, we report upper limits; we interpret these as limits on this radiation from isolated rotating neutron stars. The best population-based upper limit with 95% confidence on the gravitational-wave strain amplitude, found for simulated sources distributed isotropically across the sky and with isotropically distributed spin-axes, is 4.28E-24 (near 140 Hz). Strict upper limits are also obtained for small patches on the sky for best-case and worst-case inclinations of the spin axes.Comment: 39 pages, 41 figures An error was found in the computation of the C parameter defined in equation 44 which led to its overestimate by 2^(1/4). The correct values for the multi-interferometer, H1 and L1 analyses are 9.2, 9.7, and 9.3, respectively. Figure 32 has been updated accordingly. None of the upper limits presented in the paper were affecte