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.

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.

GLIMPSE360 is a Warm Mission Spitzer Cycle 6 Exploration Science Program (PIDs 60020, 61070, 61071, 61072, 61073, 70072) that mapped 187 degrees of longitude of the Galactic plane that have not been mapped by previous Spitzer Galactic Plane surveys (GLIMPSE, GLIMPSEII, GALCEN, GLIMPSE3D, Vela Carina, SMOG and Cygnus-X). The specific Galactic longitudes covered by GLIMPSE360 are l=65◦-76◦, 82◦-102◦, and 109◦-265◦. The latitude range is about 2.8◦. The latitude center follows the Galactic warp. GLIMPSE360 completes the full circle of the Galactic plane.The GLIMPSE360 Archive (GLM360A or the “Archive”) consists of point sources with less stringent selection critera than the Catalog. The information provided is in the same format as the Catalog. The Catalog is a subset of the Archive, but the entries for a particular source might not be the same due to additional nulling of magnitudes in the Catalog because of the more stringent requirements.

GLIMPSE360 is a Warm Mission Spitzer Cycle 6 Exploration Science Program (PIDs 60020, 61070, 61071, 61072, 61073, 70072) that mapped 187 degrees of longitude of the Galactic plane that have not been mapped by previous Spitzer Galactic Plane surveys (GLIMPSE, GLIMPSEII, GALCEN, GLIMPSE3D, Vela Carina, SMOG and Cygnus-X). The specific Galactic longitudes covered by GLIMPSE360 are l=65◦-76◦, 82◦-102◦, and 109◦-265◦. The latitude range is about 2.8◦. The latitude center follows the Galactic warp. GLIMPSE360 completes the full circle of the Galactic plane.The GLIMPSE360 Catalog (GLM360C, or the “Catalog”) consists of the highest reliability point sources. For each IRAC band the Catalog provides fluxes (with uncertainties), positions (with uncertainties), the areal density of local point sources, the local sky brightness, and a flag that provides information on source quality and known anomalies present in the data.

The Cores to Disks (C2D) Spitzer Legacy Program used all three Spitzer instruments (IRAC, MIPS, and IRS) to observe sources that span the evolutionary sequence from molecular cores to protoplanetary disks, encompassing a wide range of cloud masses, stellar masses, and star-forming environments. In addition to targeting about 150 known compact cores, it surveyed with IRAC and MIPS (3.6-70 mum) the entire areas of five of the nearest large molecular clouds for new candidate protostars and substellar objects as faint as 0.001 solar luminosities. C2D observed with IRAC and MIPS about 190 systems likely to be in the early stages of planetary system formation (ages up to about 10 Myr), probing the evolution of the circumstellar dust, the raw material for planetary cores.The High Reliability CLOUDS Catalog provides the most reliable list of sources in the C2D CLOUDS fields (ChamaeleonII (CHA_II), Lupus (LUP), Ophiuchus (OPH), Perseus (PER) and Serpens (SER)). It is derived from the Full Catalog but requires good signal-to-noise detection in some bands.

The Cores to Disks (C2D) Spitzer Legacy Program used all three Spitzer instruments (IRAC, MIPS, and IRS) to observe sources that span the evolutionary sequence from molecular cores to protoplanetary disks, encompassing a wide range of cloud masses, stellar masses, and star-forming environments. In addition to targeting about 150 known compact cores, it surveyed with IRAC and MIPS (3.6-70 mum) the entire areas of five of the nearest large molecular clouds for new candidate protostars and substellar objects as faint as 0.001 solar luminosities. C2D observed with IRAC and MIPS about 190 systems likely to be in the early stages of planetary system formation (ages up to about 10 Myr), probing the evolution of the circumstellar dust, the raw material for planetary cores.The Millimeter Sources Catalog lists the sources in the ancillary Bolocam data toward the Ophiuchus (OPH), Perseus (PER) and Serpens (SER) clouds.

This table contains some of the results from a study of the structure of the high-mass star-forming region RCW 38 and the spatial distribution of its young stellar population. Spitzer Infrared Array Camera (IRAC) photometry (3-8 micron) is combined with Two Micron All Sky Survey (2MASS) near-IR data to identify young stellar objects (YSOs) by IR-excess emission from their circumstellar material. Chandra X-ray data are used to identify class III pre-main-sequence stars lacking circumstellar material. The authors identify 624 YSOs: 23 class 0/I and 90 flat spectrum (FS) protostars, 437 class II stars, and 74 class III stars. They also identify 29 (27 new) O star candidates over the IRAC field. Seventy-two stars exhibit IR-variability, including 7 class 0/I and 12 flat spectrum YSOs. A further 177 tentative candidates are identified by their location in the IRAC [3.6] versus [3.6]-[5.8] color-magnitude diagram. The authors find strong evidence of subclustering in the region. Three subclusters were identified surrounding the central cluster, with massive and variable stars in each subcluster. The central region shows evidence of distinct spatial distributions of the protostars and pre-main-sequence stars. A previously detected IR cluster, DB2001_Obj36, has been established as a subcluster of RCW 38. This suggests that star formation in RCW 38 occurs over a more extended area than previously thought. The gas-to-dust ratio is examined using the X-ray derived hydrogen column density, NH and the K-band extinction, and found to be consistent with the diffuse interstellar medium, in contrast with Serpens and NGC 1333. The authors posit that the high photoionizing flux of massive stars in RCW 38 affects the agglomeration of the dust grains. This table contains the list of 536 X-ray sources found in the Chandra data using a three-pass method with the CIAO 3.4 Wavdetect tool. This table was created by the HEASARC in January 2012 based on an electronic version of Table 2 from the reference paper which was obtained from the ApJ website. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .

The Cores to Disks (C2D) Spitzer Legacy Program used all three Spitzer instruments (IRAC, MIPS, and IRS) to observe sources that span the evolutionary sequence from molecular cores to protoplanetary disks, encompassing a wide range of cloud masses, stellar masses, and star-forming environments. In addition to targeting about 150 known compact cores, it surveyed with IRAC and MIPS (3.6-70 mum) the entire areas of five of the nearest large molecular clouds for new candidate protostars and substellar objects as faint as 0.001 solar luminosities. C2D observed with IRAC and MIPS about 190 systems likely to be in the early stages of planetary system formation (ages up to about 10 Myr), probing the evolution of the circumstellar dust, the raw material for planetary cores.The High Reliability STARS Catalog provides the most reliable list of sources in the C2D STARS fields (160 targeted stars). It is derived from the Full Catalog but requires good signal-to-noise detection in some bands.

The Cores to Disks (C2D) Spitzer Legacy Program used all three Spitzer instruments (IRAC, MIPS, and IRS) to observe sources that span the evolutionary sequence from molecular cores to protoplanetary disks, encompassing a wide range of cloud masses, stellar masses, and star-forming environments. In addition to targeting about 150 known compact cores, it surveyed with IRAC and MIPS (3.6-70 mum) the entire areas of five of the nearest large molecular clouds for new candidate protostars and substellar objects as faint as 0.001 solar luminosities. C2D observed with IRAC and MIPS about 190 systems likely to be in the early stages of planetary system formation (ages up to about 10 Myr), probing the evolution of the circumstellar dust, the raw material for planetary cores.The Full CORES Catalog provides the most complete but least reliable list of sources in the C2D CORES fields (82 small cloud cores).

The Extragalactic First Look Survey is composed of 4 square degrees of imaging with MIPS and IRAC centered at J1718+5930, with extensive ancillary data from ground-based optical and radio telescopes. As one of the first observations made with Spitzer after the completion of Science Verification at the end of 2003 November, the aim of this 67 hr survey was to characterize the extragalactic source populations observed with Spitzer down to sub-millijansky levels in the mid-infrared.