The Extension of HOPS Out to 500 ParSecs (eHOPS) project used archival data to survey all the major star forming molecular clouds within 500 pc of the Sun, except Orion (which was surveyed by HOPS). The first eHOPS data release covers the Aquila molecular clouds (d ~ 436 pc). For every source detected in the Herschel/PACS bands, the eHOPS-Aquila catalog contains 1-850 micron SEDs assembled from 2MASS, Spitzer, Herschel, WISE, and JCMT/SCUBA-2 data. A total of 172 protostars are found in Aquila, tightly concentrated in the molecular filaments that thread the clouds. Of these, 72 (42%) are Class 0 protostars, 53 (31%) Class I protostars, 43 (25%) are flat-spectrum protostars, and 4 (2%) are Class II sources. Ten of the Class 0 protostars are young PACS Bright Red Sources similar to those discovered in Orion. eHOPS compares the SEDs to a grid of radiative transfer models to constrain the luminosities, envelope densities, and envelope masses of the protostars.
The Extension of HOPS Out to 500 ParSecs (eHOPS) project used archival data to survey all the major star forming molecular clouds within 500 pc of the Sun, except Orion (which was surveyed by HOPS). The first eHOPS data release covers the Aquila molecular clouds (d ~ 436 pc). For every source detected in the Herschel/PACS bands, the eHOPS-Aquila catalog contains 1-850 micron SEDs assembled from 2MASS, Spitzer, Herschel, WISE, and JCMT/SCUBA-2 data. A total of 172 protostars are found in Aquila, tightly concentrated in the molecular filaments that thread the clouds. Of these, 72 (42%) are Class 0 protostars, 53 (31%) Class I protostars, 43 (25%) are flat-spectrum protostars, and 4 (2%) are Class II sources. Ten of the Class 0 protostars are young PACS Bright Red Sources similar to those discovered in Orion. eHOPS compares the SEDs to a grid of radiative transfer models to constrain the luminosities, envelope densities, and envelope masses of the protostars.
The Spitzer Matching Survey of the Ultra-VISTA Deep Stripes (SMUVS) consists of deep 3.6 and 4.5 imaging of three Ultra-VISTA near-infrared survey stripes in the COSMOS field. SMUVS reaches point-source sensitivities of about 25.0 AB mag at both 3.6 and 4.5 microns with a significance of 4 sigma, accounting for both survey sensitivity and source confusion. To this limit, the SMUVS catalogs contain a total of ~350,000 sources, each of which is detected significantly in at least one IRAC band. Because of its uniform and high sensitivity, relatively large area coverage, and the wide array of ancillary data available in COSMOS, the SMUVS survey will be useful for a large number of cosmological investigations.
