This dataset contains atmospheric measurements of CO2, CH4, and CO mixing ratios made with a Picarro G2401 spectrometer during the four ATom campaigns. Picarro G2401 uses Wavelength-Scanned Cavity Ring Down Spectroscopy (WS-CRDS), a time-based measurement utilizing a near-infrared laser to measure a spectral signature of the molecule. For the ATom mission, the Picarro instrument was modified in the laboratory to operate across the full pressure altitude range of flight campaigns. The instrument was also modified to have a shorter measurement interval.

NIST X-ray Photoelectron Spectroscopy Database XPS contains over 33,000 data records that can be used for the identification of unknown lines, retrieval of data for selected elements (binding energy, Auger kinetic energy, chemical shift, and surface or interface core-level shift), retrieval of data for selected compounds (according to chemical name, selected groups of elements, or chemical classes), display of Wagner plots, and retrieval of data by scientific citation. For the newer data records, additional information is provided on the specimen material, the conditions of measurement, and the analysis of the data. Version 5.0 includes the addition of Digital Object Identifiers (DOI) to each of the citations. Additionally, Version 5.0 has new features including chemical shift plots, custom-built components for displaying both formatted molecular formulas and formatted spectral lines, and spectral sorting functions of photoelectron lines and Auger Parameters.

The CSI 2264 project performed photometric monitoring of young NGC 2264 cluster members using the Spitzer Infrared Array Camera (IRAC; Fazio et al. 2004) and the Convection, Rotation and Planetary Transits satellite (CoRoT; Baglin et al. 2006) simultaneously. Thirteen other telescopes monitored the region at different times concurrently with (or closely in time to) the primary Spitzer and CoRoT joint campaign. The CSI 2264 project is described in detail in Cody et al. (2014).This table contains CoRoT light curves for objects that are very likely NGC 2264 members (using the criteria described in Cody et al. 2014). There are many rows for each object, because each object has many epochs of data. There are 9 columns in this table, as follows. Columns 7, 8, and 9 (the IRAC excess flag and the light curve types) are duplications of information found in the Object Table, but are repeated here to make it easy for users to, e.g., pull out all of the light curves of a specific type.

Photometric observations of Uranus and Neptune (1972-2016) in the b (472 nm) and y (551 nm) filters of the Strömgren photometric system at Lowell Observatory. Observations recorded mainly seasonal variations of disk-integrated albedos of these objects. This bundle includes 360 observations of Uranus and 433 observations of Neptune from 1972-2016.

The COR1 telescope is the inner coronagraph of the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) instrument suite aboard the twin Solar Terrestrial Relations Observatory (STEREO) spacecraft. Like all coronagraphs, COR1 is designed to measure the weak light from the solar corona in the presence of scattered light from the much brighter solar photosphere. It designed to observe the white light corona from 1.4 to 4 solar radii.

The NIST Database for the Simulation of Electron Spectra for Surface Analysis (SESSA) can be used to simulate Auger-electron spectra and X-ray photoelectron spectra of nanostructures such as islands, lines, spheres, and layered spheres on surfaces. As for earlier versions, such simulations can be performed for multilayer films. Users can specify the compositions and dimensions of each material in the sample structure as well as the measurement configuration. The database contains extensive physical data needed for quantitative interpretations of observed spectra. A more detailed description of SESSA has been published [W. Smekal, W. S. M. Werner, and C. J. Powell Surf. Interface Anal. 37, 1059 (2005)].

The NIST Database for the Simulation of Electron Spectra for Surface Analysis (SESSA) can be used to simulate Auger-electron spectra and X-ray photoelectron spectra of nanostructures such as islands, lines, spheres, and layered spheres on surfaces. As for earlier versions, such simulations can be performed for multilayer films. Users can specify the compositions and dimensions of each material in the sample structure as well as the measurement configuration. The database contains extensive physical data needed for quantitative interpretations of observed spectra. A more detailed description of SESSA has been published [W. Smekal, W. S. M. Werner, and C. J. Powell Surf. Interface Anal. 37, 1059 (2005)].

The CSI 2264 project performed photometric monitoring of young NGC 2264 cluster members using the Spitzer Infrared Array Camera (IRAC; Fazio et al. 2004) and the Convection, Rotation and Planetary Transits satellite (CoRoT; Baglin et al. 2006) simultaneously. Thirteen other telescopes monitored the region at different times concurrently with (or closely in time to) the primary Spitzer and CoRoT joint campaign. The CSI 2264 project is described in detail in Cody et al. (2014).The Object Table contains one line per object, and covers all of the objects in the greater NGC 2264 region, not just those that have light curves or are members.

Wavenumber Calibration Tables from Heterodyne Frequency Measurements contains tables of gas-phase infrared transition wavenumbers and their spectroscopic assignments that are appropriate for calibrating high-spectral-resolution infrared spectrometers. The calibration lines for carbonyl sulfide (OCS), nitrous oxide (N2O), nitric oxide (NO), carbonyl sulfide (CS2), and carbon monoxide (CO) collectively extend from approximately 486 wavenumber (cm-1) to 4355 wavenumbers (cm-1) in the infrared. The bibliography and spectral atlas are current through November 1994. The bibliography covers a range of high-resolution spectroscopic studies on the calibration molecules listed above, including pressure broadening studies.

Cor2 is one of the coronagraphs aboard the STEREO-A spacecraft. It is part of the SECCHI instrument suite. It observes the off-limb corona between 2.5-15 solar radii in visible light. It acquires both total and polarized brightness images.