This database is a collection of maps created from the 28 SAS-2 observation files. The original observation files can be accessed within BROWSE by changing to the SAS2RAW database. For each of the SAS-2 observation files, the analysis package FADMAP was run and the resulting maps, plus GIF images created from these maps, were collected into this database. Each map is a 60 x 60 pixel FITS format image with 1 degree pixels. The user may reconstruct any of these maps within the captive account by running FADMAP from the command line after extracting a file from within the SAS2RAW database. The parameters used for selecting data for these product map files are embedded keywords in the FITS maps themselves. These parameters are set in FADMAP, and for the maps in this database are set as 'wide open' as possible. That is, except for selecting on each of 3 energy ranges, all other FADMAP parameters were set using broad criteria. To find more information about how to run FADMAP on the raw event's file, the user can access help files within the SAS2RAW database or can use the 'fhelp' facility from the command line to gain information about FADMAP. This is a service provided by NASA HEASARC .

SONEX_Other_Data_1 is the supplementary datasets for the SONEx suborbital campaign. Included in this product are images from the National Lightning Data Network (NLDN) and Optical Transient Detector (OTD).The SASS (Subsonics Assessment) Ozone and NOx Experiment (SONEX) was an international, multi-organizational mission that took place in October-November 1997. NASA was the US sponsor of SONEX that partnered with POLINAT-2 (Pollution from Aircraft Emissions in the North Atlantic Flight Corridor) funded by the German DLR (Deutsches Zentrum für Luft- und Raumfahrt) or German Aerospace Agency. NASA flew the DC-8 aircraft out of NASA/Ames Research Center. DLR operated an instrumented Falcon 20 aircraft. The staging locations for NAFC sampling were primarily Bangor, Maine (US), and Shannon, Ireland. Subsonic aircraft emissions impact several aspects of atmospheric composition: nitrogen oxides (NOx), CO, and hydrocarbons from emissions can perturb upper tropospheric/lower stratospheric (UT/LS) ozone; water vapor, soot, and sulfur oxides (SOx) emitted by aircraft may perturb clouds and aerosols, changing UT/LS radiative forcing and global temperature.In SONEX and POLINAT, flights were conducted in the vicinity of the North Atlantic Flight Coordinator (NAFC) to observe the impact of aircraft emissions on NOx and ozone (O3). The DC-8 aircraft payload (Singh et al., 1999) primarily measured in-situ CO, CO2, hydrocarbons/halocarbons, O3, aerosols (Dibb et al., 2000), OH/HO2, water vapor, nitric acid (Talbot et al., 1999), photolysis rates, temperature, pressure, winds, NOx, and NOy.Three sampling approaches were implemented during SONEX. First, special meteorological (Fuelberg et al., 2000) were developed to allow targeted sampling for air parcels affected by aircraft emissions and various meteorological events, e.g., convection, lightning (Jeker et al., 2000), stratospheric intrusions (Cho et al., 2000). Second, because the NAFC had not been extensively sampled in the past, it was important for SONEX to characterize the climatology of trace species like CN (Wang et al., 2000), NOx and NOy (Koike et al., 2000). Third, tracers (Simpson et al., 2000; Thompson et al., 1999) and model sensitivity studies (Meijer et al., 2000) were employed for Air Mass Identification. This sampling strategy answered the following questions: Where and when are air masses found with the greatest aircraft influence? When and where was stratospheric air sampled? SONEX showed a substantial impact of aircraft emissions on UT/LS NOx and CN in the vicinity of fresh aircraft emissions. However, during October-November 1997 over the NAFC, UT/LS NOx was dominated by surface emissions redistributed by convection and augmented by lightning.

The Herschel Orion Protostar Survey (HOPS, KPOT_tmegeath_2) is a sample of 410 young stellar objects (YSOs) in the Orion molecular clouds, selected from Spitzer data. Most objects have near-infrared photometry from 2MASS, mid- and far-infrared data from Spitzer and Herschel, and submillimeter photometry from APEX; thus, the SEDs cover 1.2 - 870 microns and are used to classify the sample into protostellar classes. Of the 410 YSOs, 330 have Spitzer and Herschel data and are mostly protostars; the remaining objects include likely extragalactic contaminants and faint YSOs. Using mid-IR spectral indices and bolometric temperatures, the sample of 330 YSOs is classified into 92 Class 0 protostars, 125 Class I protostars, 102 flat-spectrum sources, and 11 Class II re-main-sequence stars. HOPS also implements a simple protostellar model (including a disk in an infalling envelope with outflow cavities) to generate a grid of 30,400 model SEDs and uses it to determine the best-fit model parameters for each protostar.This table contains the 2MASS, Spitzer, Herschel, and APEX source fluxes, as well as the rebinned IRS fluxes, of the 410 HOPS sources. Note that not every source has data at all of these wavelengths.

This table contains a catalog of galaxy clusters selected via their Sunyaev-Zel'dovich (SZ) effect signature from 2500 deg² of South Pole Telescope (SPT) data. This work represents the complete sample of clusters detected at high significance in the 2500 deg² SPT-SZ survey, which was completed in 2011. A total of 677 (409) cluster candidates are identified above a signal-to-noise threshold xi of 4.5 (5.0). Ground- and space-based optical and near-infrared (NIR) imaging confirms overdensities of similarly colored galaxies in the direction of 516 (or 76%) of the xi > 4.5 candidates and 387 (or 95%) of the xi > 5 candidates; the measured purity is consistent with expectations from simulations. Of these confirmed clusters, 415 were first identified in SPT data, including 251 new discoveries reported in this work. The authors estimate photometric redshifts for all candidates with identified optical and/or NIR counterparts; they additionally report redshifts derived from spectroscopic observations for 141 of these systems. The mass threshold of the catalog is roughly independent of redshift above z ~ 0.25 leading to a sample of massive clusters that extends to high redshift. The median mass of the sample is M_500c(rho_crit) ~ 3.5x10¹⁴ M_sun h₇₀^-1, the median redshift is z_med = 0.55, and the highest-redshift systems are at z > 1.4. The combination of large redshift extent, clean selection, and high typical mass makes this cluster sample of particular interest for cosmological analyses and studies of cluster formation and evolution. The South Pole Telescope (SPT) is a 10m diameter telescope located at the National Science Foundation Amundsen-Scott South Pole station in Antarctica. From 2008 to 2011 the telescope was used to conduct the SPT-SZ survey, a survey of ~ 2500 deg² of the southern sky at 95, 150, and 220 GHz. The survey covers a contiguous region from 20h to 7h in Right Ascension and -65 to -40 degrees in Declination (see, e.g., Figure 1 in Story et al. 2013, ApJ, 779, 86) and was mapped to depths of approximately 40, 18, and 70 microK-arcmin at 95, 150, and 220 GHz, respectively. The authors use optical and in some cases NIR imaging (Blanco Telescope, Magellan/Baade, Magellan/Clay, Swope, MPG/ESO, New Technology Telescope, Spitzer, WISE) to confirm candidates as clusters and to obtain redshifts for confirmed systems (see section 4 of the reference paper for more details). They have also used a variety of facilities to obtain spectroscopic observations of the SPT clusters (including VLT/FORS2 & Gemini/GMOS-S). This HEASARC table contains the total of 677 cluster candidates which were identified above a signal-to-noise threshold of xi = 4.5 in the 2500 deg² SPT-SZ survey. This table was created by the HEASARC in March 2015 based on an electronic version of Table 4 from the reference paper which was obtained from the CDS as their catalog J/ApJS/216/27 file table4.dat. This is a service provided by NASA HEASARC .

The Herschel Orion Protostar Survey (HOPS, KPOT_tmegeath_2) is a sample of 410 young stellar objects (YSOs) in the Orion molecular clouds, selected from Spitzer data. Most objects have near-infrared photometry from 2MASS, mid- and far-infrared data from Spitzer and Herschel, and submillimeter photometry from APEX; thus, the SEDs cover 1.2 - 870 microns and are used to classify the sample into protostellar classes. Of the 410 YSOs, 330 have Spitzer and Herschel data and are mostly protostars; the remaining objects include likely extragalactic contaminants and faint YSOs. Using mid-IR spectral indices and bolometric temperatures, the sample of 330 YSOs is classified into 92 Class 0 protostars, 125 Class I protostars, 102 flat-spectrum sources, and 11 Class II re-main-sequence stars. HOPS also implements a simple protostellar model (including a disk in an infalling envelope with outflow cavities) to generate a grid of 30,400 model SEDs and uses it to determine the best-fit model parameters for each protostar.This table contains the SED class, bolometric luminosity and temperature, mid-IR spectral index, and best-fit model parameters for the 330 YSOs with Spitzer and Herschel data.