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The project uses Python for interactive command use, help access, and plotting. Students interpret observations of star clusters and dwarf galaxies by constructing colour-magnitude diagrams from Padova isochrones and a Salpeter initial mass function, explaining tracks, isochrones, and conversion between theoretical and observational quantities.",{"@graph":69,"@context":122},[70,84,105],{"@type":71,"itemListElement":72},"BreadcrumbList",[73,77,79,82],{"item":74,"name":75,"@type":76,"position":8},"https://docshare.wps.com","Home","ListItem",{"item":78,"name":9,"@type":76,"position":14},"https://docshare.wps.com/document/",{"item":80,"name":30,"@type":76,"position":81},"https://docshare.wps.com/document/technology/",3,{"item":83,"name":65,"@type":76,"position":19},"https://docshare.wps.com/document/sterrenstelsels-computer-project-colour-magnitude-diagrams-and-star-formation-histories/657602/",{"url":83,"name":65,"@type":85,"image":86,"author":91,"headline":65,"publisher":94,"fileFormat":97,"inLanguage":63,"description":67,"dateModified":98,"datePublished":99,"encodingFormat":97,"isAccessibleForFree":100,"interactionStatistic":101},"DigitalDocument",{"url":87,"@type":88,"width":89,"height":90},"https://docshare.wps.com/thumbnails/sterrenstelsels-computer-project-colour-magnitude-diagrams-and-star-formation-histories/657602.png","ImageObject",300,407,{"name":92,"@type":93},"noah","Person",{"url":74,"name":95,"@type":96},"DocShare","Organization","application/pdf","2026-10-29","2026-10-26",true,{"@type":102,"interactionType":103,"userInteractionCount":14},"InteractionCounter",{"@type":104},"ViewAction",{"@type":106,"mainEntity":107},"FAQPage",[108,114,118],{"name":109,"@type":110,"acceptedAnswer":111},"What is the purpose of the Sterrenstelsels computer project?","Question",{"text":112,"@type":113},"The project trains students to interpret observations of star clusters and dwarf galaxies by comparing them with theoretical stellar model calculations using colour-magnitude diagrams.","Answer",{"name":115,"@type":110,"acceptedAnswer":116},"Which programming language is required for the exercises, and why?",{"text":117,"@type":113},"Students use Python because it supports interactive use, built-in help, and convenient creation of plots and saved outputs for later use.",{"name":119,"@type":110,"acceptedAnswer":120},"How do Padova isochrones and the Salpeter IMF relate to the colour-magnitude diagram?",{"text":121,"@type":113},"Students simulate a CMD using Padova isochrones combined with a Salpeter initial mass function, then compare model-derived colours with values tabulated in isochrone tables.","https://schema.org",{"og:url":83,"og:type":124,"og:title":65,"og:site_name":95,"og:description":67},"article",{"robots":126,"canonical":83},"index,follow",{"doc_id":128,"site_id":62},657602,1792984593,{"code":4,"msg":5,"data":131},{"doc_id":128,"user_id":132,"nickname":92,"user_avatar":133,"doc_module":4,"category_id":29,"category_name":30,"doc_title":65,"doc_description":67,"doc_content":134,"file_id":135,"file_url":136,"file_type":137,"file_size":138,"view_count":14,"is_deleted":4,"is_public":8,"is_downloadable":8,"audit_status":8,"page_count":139,"language":140,"language_code":63,"site_id":62,"html_lang":63,"table_of_contents":141,"faqs":142,"seo_title":143,"seo_description":67,"update_tm":129,"read_time":144},1099529839121,"https://ap-avatar.wpscdn.com/davatar_994ba38a5ba835b3df7d355c54d3ed8d","Sterrenstelsels Computer Project: Colour-magnitude diagrams and star formation  \nhistories  \nSøren S. Larsen  \nMay 1, 2014  \nIntroduction  \nThis is the computer project for the course Sterrenstelses (“Galaxies”), a second-year course given at the Radboud University Nijmegen as part of the astrophysics curriculum. The original version of these notes was written by R. Scheepmaker, E. Helder and S. Larsen for a master course on Galaxies taught at Utrecht University during the years 2007–2011. The current version has been modified for this course to fit within a 3 ECT course load, and for use of the Python programming language (instead of IDL) .  \nAt the end of the project, it is mandatory to hand in a short report (􀀔 5 pages) which will be graded and forms part of your final grade for the course. You are allowed to work together with other students on the project, but each student must hand in a separate report, written by yourself. It is not allowed to copy the report (or parts of it) from others.  \nPython  \nFor these exercises you will use the Python programming language. Python is rapidly gaining popularity for astronomical data analysis and a large number of specialized libraries are already available. An attractive feature of Python is that it can be used interactively, [i.e. you](i.e. you) can type commands directly at the prompt and immediately see what happens before using the commands in your programmes. It is easy to make nicelooking plots and save them in a format that can be imported into documents.  \nPython has a built-in help system that provides information on how to call the various functions. This can be accessed from the Python prompt as in the following example:  \n>>> help(numpy.loadtxt)  \nPython will then display the help associated with the numpy .loadtxt function. A large amount of documentation is also available on-line, see e.g. [http://docs.python.org/2/tutorial/index.html](http://docs.python.org/2/tutorial/index.html) for a general tutorial and [http://matplotlib.org/users/pyplot](http://matplotlib.org/users/pyplot) tutorial.html for a tutorial describing the matplotlib plotting package. A good introduction to Python can also be found  \n2  \non the Dutch Wikipedia page,  \n[http://nl.wikipedia.org/wiki/Python](http://nl.wikipedia.org/wiki/Python)   (programmeertaal)  \nFor the purpose of this exercise you can use the standard Python installation on the workstations in the computer rooms ofthe FNWI. You will need to boot the workstation in Linux mode. Then Python can be called simply by typing python at the Unix prompt in a terminal window.  \nColour-Magnitude Diagram  \nIn this exercise you are going to interpret observations of star clusters and dwarf galaxies by comparing them with theoretical stellar model calculations. The aim is to show how ages, distances and other properties can be derived from observational data.  \nYou are going to simulate a Colour-Magnitude Diagram (CMD) using Padova isochrones and a Salpeter Initial Mass Function (IMF) . Padova isochrones and stellar tracks can be found at [http://pleiadi.pd.astro.it/](http://pleiadi.pd.astro.it/), but you can also find all the necessary files for this exercise via links at  \n[http://www.astro.ru.nl/](http://www.astro.ru.nl/) ~slarsen/teaching/Galaxies/  \n1.1 Tracks and Isochrones  \nThe output of stellar model calculations is typically a number of evolutionary tracks which tabulate the evolution of various properties (e􀀋ective temperature, luminosity, etc.) for stars of a given set of (initial) masses as a function of time. Such tracks are computed by starting out with a given chemical composition and following the star through its various stages of evolution as it uses up its nuclear fuel. However, for practical applications it is often more useful to interpolate in these tracks to get the stellar properties as a function of mass for a given age. When presented in this form we talk about stellar isochrones, from Greek isos (=same, equal) and chronos (=","cbCaiogEjsuwkjPj","https://ap.wps.com/l/cbCaiogEjsuwkjPj","pdf",2399318,14,"English","# Introduction\n## Python\n## Colour-Magnitude Diagram\n### Tracks and Isochrones\n### Padova isochrones","[{\"question\":\"What is the purpose of the Sterrenstelsels computer project?\",\"answer\":\"The project trains students to interpret observations of star clusters and dwarf galaxies by comparing them with theoretical stellar model calculations using colour-magnitude diagrams.\"},{\"question\":\"Which programming language is required for the exercises, and why?\",\"answer\":\"Students use Python because it supports interactive use, built-in help, and convenient creation of plots and saved outputs for later use.\"},{\"question\":\"How do Padova isochrones and the Salpeter IMF relate to the colour-magnitude diagram?\",\"answer\":\"Students simulate a CMD using Padova isochrones combined with a Salpeter initial mass function, then compare model-derived colours with values tabulated in isochrone tables.\"}]","Sterrenstelsels Computer Project - Colour-magnitude diagrams and star formation histories | PDF",35]