Blog
Standard Photometric Stars
Photometric-standard stars are stars that have had their light output in various passbands of photometric system measured very carefully. They provide a means to not only calibrate your photometric system, but give a common “yardstick” from which all measurements can be compared.
Extinction
Extinction is the removal of light through dust, gas, or atmosphere, or the overall dimming of starlight by interstellar matter. Extinction comes in two types: Interstellar and Atmospheric.
Counts
Counts focuses on all measured values within an aperture as opposed to focusing on data contained within a single pixel.
Photometry Projects
Some photometry projects are variable stars, supernova study, asteroids and comets, UBVRI, and exoplanets.
Comparison Stars
Comparison stars provide a baseline from which to compare with, and it is important that comp stars are stable and un-variable. Software such as AstroImageJ can help locate comparison stars.
Variable Stars and their Relation to Stellar Evolution
This video covers a high level view of the stellar life cycle as relating to variable stars, discussing pre-main sequence, the main sequence, after the main sequence, and after the AGB
Variable Star Overview
Variable stars have a varying light output as seen from our vantage point; their light output can be affected by extrinsic and intrinsic variables.
Difference Between Nova and Supernova
Stars can go nova multiple times, and is an accretion-explosion cycle; while supernovas only occur once in a star's lifetime and are caused by a high mass star core collapse, releasing great amounts of energy
WCS Coordinates Using MaximDL
This tutorial will show you how to access your star images on BARC, opening them in MaximDL, applying WCS coordinates, and saving the files.
WCS Coordinates
The World Coordinate System (WCS) is the RA and Dec embedded in a FITS image. Multiple tools, such as astrometry.net and MaximDL can insert WCS coordinates into the image
UBVRI & JC filters
The UBVRI system covers all of the visual spectrum and some on the shorter and longer sides, and is the most commonly used system with a large network of standard stars.
Binning
Binning is a method of combining pixels on a CCD chip into one “super” pixel. This provides some advantages and disadvantages.
SNR
The signal-to-noise ratio (SNR) characterizes the quality of a measurement and determines the ultimate performance of the system. The three primary sources of noise in a CCD imaging system are photon noise, dark noise, and read noise, all of which must be considered in the SNR calculation.
FITS Files
FITS files are the end product of a CCD image of an astronomical object, and are designed to store data sets consisting of multi-dimensional arrays and 2-dimensional tables.
CCD Filters Overview
To get information from a target and make color pictures, filters are used. Filters block certain EM wavelengths.
How to Give Good Talks Part III
Practice your presentation before you present, acknowledge your audience, don't have unnecessary body language, use active voice, and don't use too many acronyms.
How to Give Good Talks Part I
To give a good talk, you should first plan. The planning phase includes finding a hook, knowing your takeaway, knowing your audience, and know your time limit.
Common Proper Motion
Common proper-motion pairs are a subset of binaries where the stars share similar proper motions
Theta and Rho
Theta & Rho are the position angle, measured from North, and separation of two objects.
Group Intrinsic
The group of Intrinsic variable stars is classified based on internal stellar structure causing the changes to the star, and thus the variability to their flux. It covers most of the variable star classes: Eruptive, Cataclysmic, and Pulsation.