Analysis Work Space
WISE data in the public release for BRC 27 and additional WISE data to be released in March 2012 for BRC 34 and 38 will be the main focus of our research. We will augment this with data from the Spitzer archival data from the Infrared Array Camera (IRAC) and the Multiband Imaging Photometer for Spitzer (MIPS), Two-Micron All-Sky Survey (2MASS), the Midcourse Space Experiment(MSX), AKARI (literally "light" in Japanese, also known as Astro-F), and we will include IPHAS data for BRC 34 and 38 (IPHAS data will be added for BRC 27 if available in 2012). We will re-reduce and use serendipitous data available in only 2 Spitzer bands around Spitzer footprint areas previously studied, and we will re-reduce Spitzer data for BRC 38 if necessary. We will also obtain new ground based optical photometry in the Sloan bands i and r using the 2-m Las Cumbres Observatory Global Telescope (LCOGT) on Haleakala.
We will use newly released WISE catalog data to investigate point sources, performing manual photometric spot checks to assure validity of the data. We will perfrom photometry for Spitzer areas that are outside of existing analyzed Spitzer data. New photometry will be obtained using MOPEX (Makovoz & Marleau 2005) and the Aperature Photometry Tool (APT) (Laher et al 2012). Ground based data will flush out data set on the shorter wavelength end and help us identify star producing galaxies masquerading as YSOs.
Combining newly obtained data with all existing data and what is known in the literature, we will use infrared excess to look for candidate Young Stellar Objects (YSO) and to describe the properties of known YSO. We will use a method similar to Gutermuth and Koenig color selection method to winnow down YSO candidates exhibiting infrared excess. Photometry data will be collected in spreadsheet form where we perform necessary calculations, such as flux density/magnitude conversions, and produce color-color and colormagnitude diagrams as well as spectral energy diagrams (SEDs).
To classify our sources, we will use the Koenig et al adaptation (2012 ApJ, 744, 130) for WISE data of the Gutermuth et al (2008, 2009). Using this method we will examine color-color diagrams, color magnitude diagrams and spectral energy diagrams to allow us to cut non YSO candidates. First we will remove objects outside our galaxy such as external galaxies with elevated star forming regions and active galacitic nuclei (AGN). Next we will removed shock emmision blobs and resolved structures based on established color restraints. We will then identify YSOs candidates by their class using color criteria.
