Difference between revisions of "Analysis Work Space"
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| − | WISE data in the public release for BRC 27 and additional data to be released in March 2012 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) and the Midcourse Space Experiment (MSX). We will re reduce Spitzer data for BRC 38 if necessary. We will also obtain ground based optical photometry in the Sloan bands was gathered using the 2-m Las Cumbres Observatory Global Telescope (LCOGT) on Haleakala. | + | WISE data in the public release for BRC 27 and additional data to be released in March 2012 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) and the Midcourse Space Experiment (MSX) and we will include IPHAS data for at least brc 34 and 38 (additional data will be added if available in 2012). We will re reduce Spitzer data for BRC 38 if necessary. We will also obtain ground based optical photometry in the Sloan bands was gathered 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. 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 version of the Gutermuth and Koenig color selection method to winnow down YSO candidates. | We will use a version of the Gutermuth and Koenig color selection method to winnow down YSO candidates. | ||
Revision as of 20:54, 1 February 2012
just starting to put down some words here, don't look too hard yet:)
WISE data in the public release for BRC 27 and additional data to be released in March 2012 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) and the Midcourse Space Experiment (MSX) and we will include IPHAS data for at least brc 34 and 38 (additional data will be added if available in 2012). We will re reduce Spitzer data for BRC 38 if necessary. We will also obtain ground based optical photometry in the Sloan bands was gathered 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 a version of the Gutermuth and Koenig color selection method to winnow down YSO candidates.
