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  • https://arxiv.org/abs/1007.0007
    Towards relativistic orbit fitting of Galactic center stars and pulsars
    The S stars orbiting the Galactic center black hole reach speeds of up to a few percent the speed of light during pericenter passage. This makes, for example, S2 at pericenter much more relativistic than known binary pulsars, and opens up new possibilities for testing general relativity. This paper develops a technique for fitting nearly-Keplerian orbits with perturbations from Schwarzschild curvature, frame dragging, and spin-induced torque, to redshift measurements distributed along the orbit but concentrated around pericenter. Both orbital and light-path effects are taken into account. It turns out that absolute calibration of rest-frame frequency is not required. Hence, if pulsars on orbits similar to the S stars are discovered, the technique described here can be applied without change, allowing the much greater accuracies of pulsar timing to be taken advantage of. For example, pulse timing of 3 microsec over one hour amounts to an effective redshift precision of 30 cm/s, enough to measure frame dragging and the quadrupole moment from an S2-like orbit, provided problems like the Newtonian "foreground" due to other masses can be overcome. On the other hand, if stars with orbital periods of order a month are discovered, the same could be accomplished with stellar spectroscopy from the E-ELT at the level of 1 km/s.
    ARXIV.ORG
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    https://arxiv.org/abs/1007.0007
    Towards relativistic orbit fitting of Galactic center stars and pulsars
    The S stars orbiting the Galactic center black hole reach speeds of up to a few percent the speed of light during pericenter passage. This makes, for example, S2 at pericenter much more relativistic than known binary pulsars, and opens up new possibilities for testing general relativity. This paper develops a technique for fitting nearly-Keplerian orbits with perturbations from Schwarzschild curvature, frame dragging, and spin-induced torque, to redshift measurements distributed along the orbit but concentrated around pericenter. Both orbital and light-path effects are taken into account. It turns out that absolute calibration of rest-frame frequency is not required. Hence, if pulsars on orbits similar to the S stars are discovered, the technique described here can be applied without change, allowing the much greater accuracies of pulsar timing to be taken advantage of. For example, pulse timing of 3 microsec over one hour amounts to an effective redshift precision of 30 cm/s, enough to measure frame dragging and the quadrupole moment from an S2-like orbit, provided problems like the Newtonian "foreground" due to other masses can be overcome. On the other hand, if stars with orbital periods of order a month are discovered, the same could be accomplished with stellar spectroscopy from the E-ELT at the level of 1 km/s.
    ARXIV.ORG
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  • https://arxiv.org/abs/astro-ph/0003380
    Photometric Redshifts based on standard SED fitting procedures
    In this paper we study the accuracy of photometric redshifts computed through a standard SED fitting procedure, where SEDs are obtained from broad-band photometry. We present our public code hyperz, which is presently available on the web. We introduce the method and we discuss the expected influence of the different observational conditions and theoretical assumptions. In particular, the set of templates used in the minimization procedure (age, metallicity, reddening, absorption in the Lyman forest, ...) is studied in detail, through both real and simulated data. The expected accuracy of photometric redshifts, as well as the fraction of catastrophic identifications and wrong detections, is given as a function of the redshift range, the set of filters considered, and the photometric accuracy. Special attention is paid to the results expected from real data.
    ARXIV.ORG
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  • https://www.theguardian.com/sport/2013/apr/29/nba-playoffs-lakers-eliminated-howard-ejected
    A nightmare season for the Lakers comes to a fitting end
    Hunter Felt: Dwight Howard's disappointing season ends with an ejection as the San Antonio Spurs sweep the Los Angeles Lakers
    WWW.THEGUARDIAN.COM
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  • https://www.citizen.co.za/entertainment/black-panther-wakanda-forever-emotional/
    'Black Panther: Wakanda Forever' carries the story forward in an emotional, fitting way | The Citizen
    In 'Black Panther: Wakanda Forever,' we follow the women of Wakanda on a journey of love, loss and legacy as they chart a way forward.
    WWW.CITIZEN.CO.ZA
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    https://www.citizen.co.za/entertainment/black-panther-wakanda-forever-emotional/
    'Black Panther: Wakanda Forever' carries the story forward in an emotional, fitting way | The Citizen
    In 'Black Panther: Wakanda Forever,' we follow the women of Wakanda on a journey of love, loss and legacy as they chart a way forward.
    WWW.CITIZEN.CO.ZA
    https://www.citizen.co.za/entertainment/black-panther-wakanda-forever-emotional/
    'Black Panther: Wakanda Forever' carries the story forward in an emotional, fitting way | The Citizen
    In 'Black Panther: Wakanda Forever,' we follow the women of Wakanda on a journey of love, loss and legacy as they chart a way forward.
    WWW.CITIZEN.CO.ZA
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  • https://arxiv.org/abs/1502.01852
    Delving Deep into Rectifiers: Surpassing Human-Level Performance on ImageNet Classification
    Rectified activation units (rectifiers) are essential for state-of-the-art neural networks. In this work, we study rectifier neural networks for image classification from two aspects. First, we propose a Parametric Rectified Linear Unit (PReLU) that generalizes the traditional rectified unit. PReLU improves model fitting with nearly zero extra computational cost and little overfitting risk. Second, we derive a robust initialization method that particularly considers the rectifier nonlinearities. This method enables us to train extremely deep rectified models directly from scratch and to investigate deeper or wider network architectures. Based on our PReLU networks (PReLU-nets), we achieve 4.94% top-5 test error on the ImageNet 2012 classification dataset. This is a 26% relative improvement over the ILSVRC 2014 winner (GoogLeNet, 6.66%). To our knowledge, our result is the first to surpass human-level performance (5.1%, Russakovsky et al.) on this visual recognition challenge.
    ARXIV.ORG
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  • https://arxiv.org/abs/astro-ph/0605678
    An Observational Determination of the Bolometric Quasar Luminosity Function
    We combine a large set of quasar luminosity function (QLF) measurements from the rest-frame optical, soft and hard X-ray, and near- and mid-infrared bands to determine the bolometric QLF in the redshift interval z=0-6. Accounting for the observed distributions of quasar column densities and variation of spectral energy distribution (SED) shapes, and their dependence on luminosity, makes it possible to integrate the observations in a reliable manner and provides a baseline in redshift and luminosity larger than that of any individual survey. We infer the QLF break luminosity and faint-end slope out to z~4.5 and confirm at high significance (>10sigma) previous claims of a flattening in both the faint- and bright-end slopes with redshift. With the best-fit estimates of the column density distribution and quasar SED, which both depend on luminosity, a single bolometric QLF self-consistently reproduces the observed QLFs in all bands and at all redshifts for which we compile measurements. Ignoring this luminosity dependence does not yield a self-consistent bolometric QLF and there is no evidence for any additional dependence on redshift. We calculate the expected relic black hole mass function and mass density, cosmic X-ray background, and ionization rate as a function of redshift and find they are consistent with existing measurements. The peak in the total quasar luminosity density is well-constrained at z=2.15+/-0.05. We provide a number of fitting functions to the bolometric QLF and its manifestations in various bands, and a script to return the QLF at arbitrary frequency and redshift from these fits, as the most simple inferences from the QLF measured in a single band can be misleading.
    ARXIV.ORG
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  • § Code

    #importing libraries
    import pandas as pd
    import numpy as np
    import matplotlib.pyplot as plt
    %matplotlib inline
    #loading dataset
    dataset = pd.read_csv('Position_Salaries.csv')
    X = dataset.iloc[:,1:2].values #making sure X is a matrix and not a vector
    y = dataset.iloc[:,2].values #dependent variable vector


    § Markdown

    **No need to split the data into training and test set because the dataset is too small**

    **Fitting Linear Regression to the dataset**





    § Code

    from sklearn.linear_model import LinearRegression #importing linear regression class from sklearn library
    lin_reg = LinearRegression() #creating an object of the linear regression class
    lin_reg.fit(X,y) #fitting linear regression model to the dataset



    § Output

    > ['LinearRegression(copy_X=True, fit_intercept=True, n_jobs=None, normalize=False)']


    § Markdown

    **Fitting Polynomial Regression to the Dataset**



    § Code

    from sklearn.preprocessing import PolynomialFeatures #importing polynomial features class from sklearn library
    poly_reg = PolynomialFeatures(degree=4) #creating an object of polynomial features class and setting degree to 4 (degree is number of polynomials we want to create) , this will create all polynomials with degree less than or equal to 4 (1,x,x^2,x^3,x^4) , it will also add a column of 1s for constant b0 in equation y=b0+b1x+b2x^2+....+bnx^n (this is done by setting include_bias parameter in constructor to true which is default value ) , so now we have 6 columns in matrix X' now instead of 1 column in matrix X before . This new matrix X' will be used for fitting polynomial regression model . So basically what this class does is it takes one feature and transforms it into multiple features by creating all possible polynomials with degree less than or equal to specified degree . Now we have 6 columns in matrix X' which can be used for fitting polynomial regression model . We can also specify include bias parameter in constructor as false if we don't want that extra column of 1s . Now we have created an object of PolynomialFeatures class with degree set to 4 , now we will fit this object into our independent variable X i.e transform our independent variable X into new matrix X' with 6 columns using fit method on poly_reg object which was created using PolynomialFeatures class . We can use transform method on poly_reg object for transforming independent variable X into new matrix X' but since fit method also does this job so better use fit method only . So basically what fit method does is it takes one feature and transforms it into multiple features by creating all possible polynomials with degree less than or equal to specified degree and then stores these new transformed features in poly_reg object itself which can be accessed using transformed attribute on poly_reg object i.e poly_reg.transformed attribute returns us the new transformed matrix X' which has 6 columns instead of 1 column before transformation . Now after transforming our independent variable into new matrix X' , now we need to fit this new transformed matrix into linear regression model so that we get our polynomial regression model , so for that purpose first create an instance of linear regression class i.e lin reg 2 and then call fit method on this instance passing transformed attribute on poly reg object i.e poly reg dot transformed as first argument and dependent variable y as second argument . Now lin reg 2 object has fitted our transformed independent variable i.e poly reg dot transformed and dependent variable y into linear regression model thus giving us our polynomial regression model which can be accessed using predict method on lin reg 2 object passing some value as argument whose prediction you want . So basically what predict method does is it takes some value x passed as argument and then passes it through equation y = b0 + b1x + b2x^2 + ... + bnx^n where coefficients b0 , b1 ,...bn are stored inside lin reg 2 object itself which were calculated when fitting was done using fit method passing transformed attribute on poly reg object as first argument and dependent variable y as second argument while calling fit method on lin reg 2 instance . Thus predict method returns us predicted value corresponding to x passed as argument after passing x through equation y = b0 + b1x + b2x^2 + ... + bnx^n where coefficients are stored inside lin reg 2 instance itself calculated during fitting process when calling fit method on lin reg 2 instance passing transformed attribute on poly reg instance as first argument and dependent variable y as second argument while calling fit method on lin reg 2 instance . Thus finally after fitting process when calling predict method on lin reg 2 instance passing some value x whose prediction you want , predict method returns us predicted value corresponding to x passed as argument after passing x through equation y = b0 + b1x + b2x^2 + ... + bnx^n where coefficients are stored inside lin reg 2 instance itself calculated during fitting process when calling fit method on lin reg 2 instance passing transformed attribute on poly reg instance as first argument and dependent variable y as second argument while calling fit method on lin

    By: ChatGPT AI
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  • _parameters_file, "r")
    fitting_parameters = json.load(f)
    f.close()

    # Read in the initial guess parameters
    initial_guess_file = os.path.join(data_directory, "initial_guess.json")
    f = open(initial_guess_file, "r")
    initial_guess = json.load(f)
    f.close()

    # Read in the data files
    datafiles = []
    for filename in os.listdir(data_directory):
    if filename[-4:] == ".csv":
    datafiles.append(os.path.join(data_directory, filename))

    # Read in the data from each file and store it as a list of dictionaries with keys 'x' and 'y'
    data = [] # List of dictionaries with keys 'x' and 'y' for each dataset to be fitted

    for file in datafiles:

    print("Loading", file)

    x, y = np.genfromtxt(file, delimiter=",").T # Transpose makes it easier to work with

    dic = {'x': x, 'y': y} # Create a dictionary entry for this dataset

    data.append(dic) # Add it to the list of datasets

    print("Loaded", len(x), "points")

    print("Loaded", len(data), "datasets\n")

    # Fit the model to all of the datasets simultaneously using lmfit's Parameters class and minimize function
    fitparams = lmfit.Parameters() # Create an empty Parameters object to store the fit parameters

    for key in fitting_parameters: # Loop through all of the parameters that need to be fitted and add them to fitparams

    param = fitting_parameters[key] # Get a dictionary containing information about this parameter from fitting_parameters dictionary

    fitparams.add(key, value=initial_guess[key], vary=param['vary'], min=param['min'], max=param['max']) # Add this parameter to fitparams using information from param and initial guess values from initial guess dictionary (which should have been read in earlier)

    By: ChatGPT AI
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