PHYS 134L Spring 2022 Lab 3
" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "Part 1: Astronomical Magnitudes
" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "Throughout this lab we will use three image files: ```cluster1.fits```, ```cluster2.fits```, and ```cluster3.fits```, and three catalogs of extracted stars: ```cluster1.cat```, ```cluster2.cat```, and ```cluster3.cat```. We will begin with the pair ```cluster1.fits``` and ```cluster1.cat```." ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "**We'll begin by making a two-dimensional plot of ```cluster1.fits``` and overplotting the locations of the stars given in ```cluster1.cat.```** Refer to the first lab if you have forgotten how to do this. As in that lab, please use a scale that shows the full dynamic range of the image and that looks nice: no garish color schemes, and few (if any) pixels beyond the limits of your color scale. The $x$ and $y$ pixel locations might be in different locations than they were in ```object.cat``` from Lab 1, so please check and make sure that you are reading the correct column. You may open ```cluster1.cat``` in a text editor (like notepad) or on JupyterHub to double-check the contents of each column.\n" ] }, { "cell_type": "code", "execution_count": null, "metadata": {}, "outputs": [], "source": [ "#Your code here" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "The file ```cluster1.cat``` has many columns besides the $x$ and $y$ positions. We will now look at the information in the columns ```MAG_ISOCOR``` and ```MAGERR_ISOCOR```. **First, make a scatter plot showing ```MAG_ISOCOR``` as a function of ```NUMBER```, i.e., simply plot the magnitudes as a function of the order in which they appear in the catalog. Overplot the error bars given by ```MAGERR_ISOCOR```.** Check the documentation for ```pyplot.errorbar``` if you are unsure of how to get started." ] }, { "cell_type": "code", "execution_count": null, "metadata": {}, "outputs": [], "source": [ "#Your code here" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "It's hard to interpret that previous plot; it looks like a bit of a mess. To make it easier to see what is going on, let's sort the stars by magnitude. You'll want to sort the magnitudes and their uncertainties in the same way. In other words, you want the same uncertainty to remain associated with each measured magnitude. " ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "Assume that you have read in the catalog file and set an array called ```mags``` equal to the column ```MAG_ISOCOR``` and an array called ```mag_errs``` equal to the column ```MAGERR_ISOCOR```. Explain why the following code will produce nonsense if you use the array ```mag_errs_sorted``` for the error bars of ```mags_sorted```:\n", "```\n", "mags_sorted = np.sort(mags)\n", "mag_errs_sorted = np.sort(mag_errs)\n", "```" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "To sort the arrays in the same way, try ```np.argsort```. Experiment yourself a bit to get it working, and read the documentation page. \n" ] }, { "cell_type": "code", "execution_count": null, "metadata": {}, "outputs": [], "source": [ "#Your code here" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "**Now remake your plot of magnitudes with error bars, but sorted by magnitude on the horizontal axis.**" ] }, { "cell_type": "code", "execution_count": null, "metadata": {}, "outputs": [], "source": [ "#Your code here" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "Do the estimated errors varay with magnitude in a systematic way? Explain" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "So far we have used catalogs output by Source Extractor to obtain only the most minimal information about the objects in the detector field of view--the positions and fluxes from each detected object. We will now look at Source Extractor output files for which we have asked the program to do a more thorough job. Typically we want more kinds of information about each object for one of three reasons: to represent the data in a more convenient way, to display the result of a different way to estimate a number (such as the flux) for which we already have a value, or to give information about the reliability of the results displayed in other columns.\n" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "We will continue to work with the catalog given by ```cluster1.cat```, but now will load the columns corresponding to ```FLUX_ISOCOR``` and ```FLUXERR_ISOCOR```. Open the catalog file in a text editor like notepad if you cannot find them. As usual, remember that Source Extractor counts from 1, while python indexes from 0. " ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "Now we will check the relationship between flux and magnitude, if you need a reminder, check out Section 3.2 of the Burns. **Make a scatter plot with ```MAG_ISOCOR``` on the $x$-axis and ```FLUX_ISOCOR``` on the $y$-axis. Once you have done this, adjust the vertical axis to have a logarithmic scaling (check ```pyplot.yscale```).** " ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "Once you have this scatter plot, try fitting a line by eye. The mechanics of how to actually do this properly are beyond the scope of this class. For now, please define a variable $x$ by\n", "```\n", "x = np.linspace(np.amin(mags,np.amax(mags)),10)\n", "```\n", "and a variable $y$ by\n", "```\n", "y = a*x + b\n", "```\n", "where you determine the best-fit ceofficients ```a``` and ```b``` by eye. Depending on how you have implemented your logarithmic vertical scale you may need to plot either \n", "```\n", "y = np.exp(a*x+b)\n", "```\n", "or \n", "```\n", "y = 10**(a*x+b)\n", "```\n", "for it to appear as a line on your plot. **Please overplot your best-fit line on the scatter plot of magnitudes against logarithmic flux.**" ] }, { "cell_type": "code", "execution_count": null, "metadata": {}, "outputs": [], "source": [ "#You code here" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "**Write down the definition of astronomical magnitudes in the space below.**\n" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "**How closely does your fitted constant ```a``` match expectations?**" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "**Approximately what magnitude would yield a flux of 1 given your values of ```a``` and ```b```? Please show your work.**" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "\n", "##Part 2: The Sizes of (Images of) Stars
" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "The catalog file has a column entitled ```FWHM_IMAGE``` (meaning Full Width at Half Maximum of the star image). This parameter is a measure of the width of the star images in units of pixels -- smaller numbers mean sharper images. You can also estimate these values yourself by looking at the image in ds9. " ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "**Open the image in ds9, set the “scale” option to “zscale,” and estimate the size of the images\n", "of stars (in pixels). How do these sizes compare with the FWHM IMAGE values in the catalog\n", "file?**" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "**Now try setting the ds9 ``scale'' to ``min/max'' and ``linear'' and estimate the sizes of a few of the star images (necessarily the brightest ones, since those are all you can see this way). Use the cursor to read the pixel values. How do the sizes you estimate in this way compare to the FWHM_IMAGE values in the catalog file?**" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "**Set the ``Horizontal Graph'' option in the ``View'' tab, and estimate the FWHM of a bright star from this graph. How does this estimate compare with the other two estimates you gave above?**" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "Last lab, you estimated the angular sizes of a few stars; the largest size you should have computed was around 2~mas. You also computed the pixel scale in these images; you should have gotten a scale of around $0.\\!\\!^{\\prime \\prime}58$ arcsec/pixel. **Use these two numbers to estimate the angular size of a star in units of pixels. Please show your work for the unit conversion.**" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "The angular size of a star (in units of pixels) divided by the image FWHM gives a dimensionless number. If this number is larger than 1, the star is said to be resolved: a larger star makes a larger image. If this number is much less than 1, the star is said to be unresolved, because the size of the star on the image is set almost entirely by something other than its physical size. **What is this dimensionless number, angular size/FWHM, for the current image? Roughly how small would the FWHM have to be for any of the stars to be resolved at all?**\n" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your anwer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "**To see if all stars have the same size on the image, make a plot of FWHM ($y$-axis) against stellar magnitude ($x$-axis). As usual, please label your axes and make the plot look nice. Do you see evidence for a dependence of FWHM on magnitude?**" ] }, { "cell_type": "code", "execution_count": null, "metadata": {}, "outputs": [], "source": [ "#Your code here" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "*Your answer here*" ] }, { "cell_type": "markdown", "metadata": {}, "source": [ "For telescopes on the ground, the FWHM is usually set by atmospheric turbulence and is called ``seeing.'' A better site gives a shaper image. \n" ] }, { "cell_type": "markdown", "metadata": {}, "source": [] } ], "metadata": { "kernelspec": { "display_name": "Python 3", "language": "python", "name": "python3" }, "language_info": { "codemirror_mode": { "name": "ipython", "version": 3 }, "file_extension": ".py", "mimetype": "text/x-python", "name": "python", "nbconvert_exporter": "python", "pygments_lexer": "ipython3", "version": "3.8.8" } }, "nbformat": 4, "nbformat_minor": 2 }