Difference between revisions of "Analysis Work Space"
| Line 1: | Line 1: | ||
| − | |||
| − | WISE data in the public release for BRC 27 and additional 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) | + | 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) 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 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, 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. Combining this 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 newly released WISE catalog data, 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 and the Aperature Photometry Tool (APT). Combining this 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 | + | 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). |
Revision as of 20:27, 9 February 2012
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) 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 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, 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 and the Aperature Photometry Tool (APT). Combining this 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).
