GLIMPSE3D is the third in a series of large area projects to map selected regions of the Galactic plane using the Spitzer Space Telescope Infrared Array Camera (IRAC). GLIMPSEI1 covered the Galactic plane from |l| = 10◦ to 65◦ and |b| < 1◦; GLIMPSEII filled in the inner 20 degrees of the Galactic plane, |l| < 10◦, with vertical extensions up to ±1.5◦ for |l| =5◦to 2◦, and up to ±2◦ from |l| =2◦to 0◦. GLIMPSE3D adds vertical extensions, generally up to |b| < 3◦, but up to |b| < 4.2◦ in the center of the Galaxy. The goal of this coverage is to provide data to study the vertical stellar and interstellar
The GLIMPSE3D Archive (GLM3DA or the “Archive”) consists of point sources with a signal- to-noise > 5 in at least one band and less stringent selection critera than the Catalog. The photometric uncertainty is typically < 0.3 mag. The GLIMPSE3D Catalog is a subset of the Archive, but note that 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.
GLIMPSE3D is the third in a series of large area projects to map selected regions of the Galactic plane using the Spitzer Space Telescope Infrared Array Camera (IRAC). GLIMPSEI1 covered the Galactic plane from |l| = 10◦ to 65◦ and |b| < 1◦; GLIMPSEII filled in the inner 20 degrees of the Galactic plane, |l| < 10◦, with vertical extensions up to ±1.5◦ for |l| =5◦to 2◦, and up to ±2◦ from |l| =2◦to 0◦. GLIMPSE3D adds vertical extensions, generally up to |b| < 3◦, but up to |b| < 4.2◦ in the center of the Galaxy. The goal of this coverage is to provide data to study the vertical stellar and interstellar
The GLIMPSE3D Archive (GLM3DA or the “Archive”) consists of point sources with a signal- to-noise > 5 in at least one band and less stringent selection critera than the Catalog. The photometric uncertainty is typically < 0.3 mag. The GLIMPSE3D Catalog is a subset of the Archive, but note that 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.
GLIMPSE3D is the third in a series of large area projects to map selected regions of the Galactic plane using the Spitzer Space Telescope Infrared Array Camera (IRAC). GLIMPSEI1 covered the Galactic plane from |l| = 10◦ to 65◦ and |b| < 1◦; GLIMPSEII filled in the inner 20 degrees of the Galactic plane, |l| < 10◦, with vertical extensions up to ±1.5◦ for |l| =5◦to 2◦, and up to ±2◦ from |l| =2◦to 0◦. GLIMPSE3D adds vertical extensions, generally up to |b| < 3◦, but up to |b| < 4.2◦ in the center of the Galaxy. The goal of this coverage is to provide data to study the vertical stellar and interstellar
The GLIMPSE3D Archive (GLM3DA or the “Archive”) consists of point sources with a signal- to-noise > 5 in at least one band and less stringent selection critera than the Catalog. The photometric uncertainty is typically < 0.3 mag. The GLIMPSE3D Catalog is a subset of the Archive, but note that 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.
GLIMPSE3D is the third in a series of large area projects to map selected regions of the Galactic plane using the Spitzer Space Telescope Infrared Array Camera (IRAC). GLIMPSEI1 covered the Galactic plane from |l| = 10◦ to 65◦ and |b| < 1◦; GLIMPSEII filled in the inner 20 degrees of the Galactic plane, |l| < 10◦, with vertical extensions up to ±1.5◦ for |l| =5◦to 2◦, and up to ±2◦ from |l| =2◦to 0◦. GLIMPSE3D adds vertical extensions, generally up to |b| < 3◦, but up to |b| < 4.2◦ in the center of the Galaxy. The goal of this coverage is to provide data to study the vertical stellar and interstellar
The GLIMPSE3D Archive (GLM3DA or the “Archive”) consists of point sources with a signal- to-noise > 5 in at least one band and less stringent selection critera than the Catalog. The photometric uncertainty is typically < 0.3 mag. The GLIMPSE3D Catalog is a subset of the Archive, but note that 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.
GLIMPSE3D is the third in a series of large area projects to map selected regions of the Galactic plane using the Spitzer Space Telescope Infrared Array Camera (IRAC). GLIMPSEI1 covered the Galactic plane from |l| = 10◦ to 65◦ and |b| < 1◦; GLIMPSEII filled in the inner 20 degrees of the Galactic plane, |l| < 10◦, with vertical extensions up to ±1.5◦ for |l| =5◦to 2◦, and up to ±2◦ from |l| =2◦to 0◦. GLIMPSE3D adds vertical extensions, generally up to |b| < 3◦, but up to |b| < 4.2◦ in the center of the Galaxy. The goal of this coverage is to provide data to study the vertical stellar and interstellar
The GLIMPSE3D More Reliable Archive (GLM3DMRA) consists of the higher reliability point sources than the Archive. It was produced for the single visit epoch 2 only source lists to provide a higher reliability source list than the Archive. No highly reliable Catalog is produced for this dataset since it requires a source be detected twice in one band. The sources in the More Reliable Archive have the same stringent criteria as the Catalog except two detections are not required in a single band. Two detections in adjacent bands are required (the “1” can include the 2MASS Ks band); for example one detection in band 1 and one detection in band 2.
Using images from the Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE), we have identified more than 300 extended 4.5um sources (Extended Green Objects (EGOs), for the common coding of the [4.5] band as green in three-color composite InfraRed Array Camera images). We present a catalog of these EGOs, including integrated flux density measurements at 3.6, 4.5, 5.8, 8.0, and 24um from GLIMPSE and the Multiband Imaging Photometer for Spitzer Galactic Plane Survey.
The University of Tasmania Mt Pleasant 26-m and Ceduna 30-m radio telescopes have been used to search for 6.7-GHz class II methanol masers towards 200 GLIMPSE (The Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) sources. The target regions were selected on the basis of their mid-infrared colours as being likely to be young high-mass star formation regions and are either bright at 8.0{mu}m, or have extreme [3.6]-[4.5] colour. Methanol masers were detected towards 38 sites, nine of these being new detections. The prediction was that approximately 20 new 6.7-GHz methanol masers would be detected within 3.5-arcmin of the target GLIMPSE sources, but this is the case for only six of the new detections. A number of possible reasons for the discrepancy between the predicted and actual number of new detections have been investigated. It was not possible to draw any firm conclusions as to the cause, but it may be because many of the target sources are at an evolutionary phase prior to that associated with 6.7-GHz methanol masers. Through comparison of the spectra collected as part of this search with those in the literature, the average lifetime of individual 6.7-GHz methanol maser spectral features is estimated to be around 150yr, much longer than is observed for 22-GHz water masers.
The Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSEI), using the Spitzer Space Telescope Infrared Array Camera (IRAC) surveyed approximately 220 square degrees of the Galactic plane, covering a latitude range of ±1◦, and a longitude range of |l| =10◦−65◦, plus the Observation Strategy Validation (OSV) region at l=284◦. The observations consisted of two 1.2 second integrations at each position, for a total of over 77,000 pointings and ∼310,000 IRAC frames in 400 hours total survey time. The survey consists of a point source Catalog, a point source Archive, and mosaicked images.
The GLIMPSEI Archive (GLMIA or the “Archive”) consists of point sources with a signal- to-noise > 5 in at least one band and less stringent selection critera than the Catalog. The photometric uncertainty is typically < 0.3 mag. The GLIMPSEI Catalog is a subset of the Archive, but note that 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.
The Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSEI), using the Spitzer Space Telescope Infrared Array Camera (IRAC) surveyed approximately 220 square degrees of the Galactic plane, covering a latitude range of ±1◦, and a longitude range of |l| =10◦−65◦, plus the Observation Strategy Validation (OSV) region at l=284◦. The observations consisted of two 1.2 second integrations at each position, for a total of over 77,000 pointings and ∼310,000 IRAC frames in 400 hours total survey time. The survey consists of a point source Catalog, a point source Archive, and mosaicked images.
The GLIMPSEI Catalog (GLMIC, or the “Catalog”) consists of point sources whose selection criteria are determined by the requirement that the reliability be ≥99.5%. There is a range of limiting magnitudes depending on whether the source is in a sparsely populated or low background region or in a region of high diffuse background or high source density. The photometric uncertainty is typically < 0.2 mag.
The Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSEII) imaged longitudes ±10◦ of the central region of the Galaxy. The latitude coverage is ±1◦ from |l| =10◦to 5◦, ±1.5◦ from |l| =5◦to 2◦, and ±2◦ from |l| =2◦to 0◦. GLIMPSEII coverage excludes the Galactic center region l=±1◦, b=±0.75◦ observed by the GALCEN GO program (PID=3677). GLIMPSEII had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006).
The GLIMPSEII Archive (GLMIIA or the “Archive”) consists of point sources with a signal- to-noise > 5 in at least one band and less stringent selection critera than the Catalog. The photometric uncertainty is typically < 0.3 mag. The GLIMPSEII Catalog is a subset of the Archive, but note that 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.