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Hidden Markov model tracking of continuous gravitational waves
Hidden Markov model tracking of continuous gravitational waves

... Hidden Markov model (HMM) methods offer one powerful strategy for detecting and tracking a wandering frequency [45]. The essential idea is to model f? (t) probabilistically as a Markov chain of transitions between unobservable (“hidden”) frequency states and relate the hidden states to the observed ...
fourier transform and noise
fourier transform and noise

... • Noise Figure • Noise Figure F is designed as the ratio of the signal-to-noise power at the input to the signal to noise power at the output. • The device under consideration can be the entire receiver or a single amplifier stage. The noise figure F also called the noise factor can be computed wit ...
CameraFilters
CameraFilters

... 2. The log, base 10, of 2 is approximately 0.3, which is the nominal density value. The benefit of using density values is that they can be added when combined. Thus two ND .3 filters have a density value of 0.6. However, their combined transmittance would be found by multiplying 0.5 x 0.5 = 0.25, o ...
Y L A  6/ 3
Y L A 6/ 3

... ond part, we consider the frequency-compressive feedback case. In order to analyze an FM system, we shall use an idealized mathematical model. The model (Fig. 1) consists of a symmetrical narrow-bandpass filter, an ideal broadband limiter with zonal filter, and an ideal frequency detector that opera ...
The Technology of Auto-Wahs / Envelope
The Technology of Auto-Wahs / Envelope

... voltage) and appropriate polarity to drive the control element. Not much problem there. In most cases, this simply means providing appropriate gain within the envelope follower itself, or feeding it with an already boosted (or attenuated) signal. Gain setting can usually be adjusted by a single, eas ...
Chapter 1 (Part 2.1) - Noise
Chapter 1 (Part 2.1) - Noise

... • Since it is dependent on temperature, it is also referred to as thermal noise. ...
Exposure Time Calculator for LUCI - USER MANUAL
Exposure Time Calculator for LUCI - USER MANUAL

... The exposure time calculator (ETC) roughly calculates the exposure time of LUCI at the Large Binocular Telescope (LBT). There is a wide choice of different model spectra available (e.g. different main sequence stars). It is also possible to select a blackbody spectrum or a single-line spectrum as an ...
Detection of Point Sources in Maps of the
Detection of Point Sources in Maps of the

... Figure 1.2 CMB frequency spectrum obtained with the FIRAS instrument on COBE in 1996. This spectrum corresponds to that of a black-body with temperature T = 2.725 ± 0.001 K. The error bars have been multiplied by 400. tribution of matter and Rashid Sunyaev realized that they would have an imprint i ...
chapter 5 part 1
chapter 5 part 1

... • Since it is dependent on temperature, it is also referred to as thermal noise. ...
WP3 group report (including roadmap text)
WP3 group report (including roadmap text)

... the power circulating in the Power Recycling cavity will be started in 2010. 2.1.1.1.a Currently all gravitational-wave detectors are using so called Schnupp modulation or frontal modulation together with a slight asymmetry in the arm length. This technique has a very similar effect as modulating th ...
A Bayesian method for the detection of planetary transits
A Bayesian method for the detection of planetary transits

... (some 50 pixels in COROT’s case) and some specific noises whose main contribution is the read out noise of the order of 15 e− /30 s/pix. It also depends on the presence of other sources of photon such as stray light from the Earth and the Zodiacal light. This last one gives a dominant contribution w ...
The Impact of Standing Waves in the LO path of a
The Impact of Standing Waves in the LO path of a

... Our observations have confirmed that a major portion of baseline ripple in the spectra of heterodyne receivers can be attributed to standing waves in the mixer/LO cavity. The amplitude of the ripple structures depends directly on the coupling efficiency of the LO into the signal path. If one can aff ...
How astronomers measure brightness and colours – the magnitude
How astronomers measure brightness and colours – the magnitude

... The magnitudes can be subtracted from each other to form colour indices (e.g. B − V ), note that this is equivalent to division of the fluxes in the two filters. A non-zero colour index means that the apparent flux from the object is stronger in one filter than in the other. The colour indices are u ...
Evaluation of a PtSi Schottky infrared CCD for
Evaluation of a PtSi Schottky infrared CCD for

... tape. Each pixel of this array is the average of the corresponding pixel in the data sequence of several frames. Using this technique, an average object-plus-background frame of data was computed and stored using up to 100 frames of raw data with the telescope pointed at an object. An average backgr ...
G000175-00 - DCC
G000175-00 - DCC

... » burst signals in coincidence with signals in electromagnetic radiation » prompt alarm (~ one hour) with neutrino detectors ...
134-Notes-a
134-Notes-a

... of 1 parsec has a parallax angle of one arsecond (hence the name “par”-“sec”). Figure 1 shows schematically how the parsec is defined. Finally we should mention the astronomical unit (AU), which is the average distance between the earth and the sun. It is very useful when speaking of distances withi ...
PPTX - Miami University
PPTX - Miami University

... Suppose you put some input into a system and get some output. If you put in the same input at a later time, if the system is time invariant, the output will be the same as the original output except it will occur at that later time – In other words, for a time-invariant system S, If y(t) = S{ x(t) } ...
G030627-00 - DCC
G030627-00 - DCC

... looking for. Once statistic is chosen we need to optimise that statistic (if it has some parameters to optimise for) and set up the veto threshold. Consider optimisation of 2 with respect to the number of bins. The main idea is to use software injections of the chirps into the playground data and c ...
NIRCam - STScI
NIRCam - STScI

... • NIRCam images the 0.6 to 5mm (1.7 - 5mm prime) range ...
Stellar Temperatures
Stellar Temperatures

... Stellar temperatures range from ~3000 K to ~100,000 K (although there are exceptions). To zeroth order, they can be considered blackbodies, with stellar absorption lines on top. There is a great variety of stellar absorption lines; the strength of any individual line is determine by the star’s •  Te ...
Recovering Injections Poster
Recovering Injections Poster

... The work presented in this poster was carried out within the LIGO Scientific Collaboration (LSC). The methods and results presented here are under review and are potentially subject to change. The opinions expressed here are those of the author and not necessarily those of the LSC. The author gratef ...
Preparation of Papers in Two-Column Format
Preparation of Papers in Two-Column Format

... information on the transmitted signal [9]. In some eigenvalue based schemes, the information of noise variance is not needed either. In eigenvalue spectrum sensing the test statistic is calculated from the eigenvalues of the received signal covariance matrix. In this paper we focus on the co-operati ...
Improving CoRoT planets parameters with transit reconstruction in
Improving CoRoT planets parameters with transit reconstruction in

... Exo-4 are not significantly different!from those obtained with the NIF and from the published values, implying that traditional variability filtering method are appropriate for the levels of stellar variability in those light curves.!For Exo-1, we obtain a tentative detection of a secondary!eclipse ...
Stellar Temperatures
Stellar Temperatures

... Stellar temperatures range from ~3000 K to ~100,000 K (although there are exceptions). To zeroth order, they can be considered blackbodies, with stellar absorption lines on top. There is a great variety of stellar absorption lines; the strength of any individual line is determined by the star’s •  T ...
The Synthesizer
The Synthesizer

... notice that the device used to do this has an individually decoupled and filtered supply line. The same is true for many of the other logic devices used. This is because an AC logic gate, as used here, is not just a logic gate – it is a very effective non linear mixer/modulator and stray noise on ei ...
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Matched filter

In signal processing, a matched filter (originally known as a North filter) is obtained by correlating a known signal, or template, with an unknown signal to detect the presence of the template in the unknown signal. This is equivalent to convolving the unknown signal with a conjugated time-reversed version of the template. The matched filter is the optimal linear filter for maximizing the signal to noise ratio (SNR) in the presence of additive stochastic noise. Matched filters are commonly used in radar, in which a known signal is sent out, and the reflected signal is examined for common elements of the out-going signal. Pulse compression is an example of matched filtering. It is so called because impulse response is matched to input pulse signals. Two-dimensional matched filters are commonly used in image processing, e.g., to improve SNR for X-ray.Matched filtering is a demodulation technique with LTI (Linear Time Invariant) filters to maximize SNR.
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