The Spitzer Wide-area InfraRed Extragalactic Survey
Short Name:
SWIRE
Date:
27 Oct 2022 19:00:00
Publisher:
NASA/IPAC Infrared Science Archive
Description:
* A wide-area, high galactic latitude imaging survey conducted using the Spitzer MIPS far-infrared and IRAC mid-infrared cameras. The satellite data will be complemented by an extensive program of ground-based optical, near-infrared and radio observations.
The The VO @ ASTRON's sitewide SIAP version 2 service
publishes all the images published through the site. For more advanced
queries including uploads, all this data is also available through
ObsTAP.
The VSOP (the VLBI Space Observatory Programme) 5 GHz AGN (Active Galactic Nuclei) Survey Program Analysis Data
Short Name:
HALCA_AGN
Date:
19 Oct 2021 06:40:34
Publisher:
JVO
Description:
A significant fraction of the mission time of VSOP was to be dedicated to the VSOP Survey Programme of bright compact Active Galactic Nuclei (AGN) at 5 GHz, which was lead by ISAS. The VSOP Survey Sources are an unbiased dataset of 294 targets, of which 82% were successfully observed.
z0MGS is an archival project combining WISE and GALEX images of nearby galaxies. The main sample consists of ~11,000 galaxies that are deemed to have >10% probability of being within D %lt; 50 Mpc and of having MB %lt; -18. In addition, in the course of iterating on distance estimates when creating the atlas, the z0MGS team generated images for ~5, 000 additional galaxies. These are also included in the delivery, although they do not meet the formal selection criteria. All galaxies included in the atlas have WISE W1 coverage, at minimum. In total, out of the 15,748 galaxies in DR1, 15,716 have coverage in all WISE bands, 11,687 have GALEX NUV and 10,754 have GALEX FUV. If you use z0MGS data, please cite Leroy et al. (2019)
The Archive is formed with all files measured with ARcetri Near Infrared CAmera ( ARNICA). Each files contains (in FITS format) or a single exposure or the mean of single exposures taken at the same telescope position. The filer used can be either a Johnson broad band infrared filter (J, H, K), or a narrow band filter (see ARNICA) page for details). Most measures was acquired at the TIRGO telescope, while a smaller sample cames from the few telescopes Arnica was ported to (WHT, NOT, VATT and TNG). All frame are in FITS format and are 256x256 pixels in size. The archive contains more than 250.000 frames. Most files belongs to a compound measure (we call them "a mosaic").
DOLORES (Device Optimized for the LOw RESolution) is a focal reducer instrument installed at the Nasmyth B focus of the TNG. The detector is a 2048 x 2048 E2V 4240 Thinned back-illuminated, deep-depleted, Astro-BB coated CCD with a pixel size of 13.5 µ. The scale is 0.252 arcsec/px which yields a field of view of about 8.6 x 8.6 arcmin. The instrument allows imaging through broad and narrow band filters as well as spectroscopic observations with resolving powers between RS=~500 and RS=~6000. A multi-slit mode, based on custom masks manufactured by a dedicate cutting machine, is also available. Please note that MOS programs are bound to strict constraints on the number of masks and on the time necessary to design and manufacture them. In particular, each program can request up to a maximum of 5 masks per night and 10 masks per observing run.
NICS (Near Infrared Camera Spectrometer) is the TNG infrared (0.9-2.5 µm) multimode instrument which is based on a HgCdTe Hawaii 1024x1024 array. Its observing capabilities include imaging (4.2' x 4.2' f.o.v.), high-throughput low resolution spectroscopy (RS=50-500), medium resolution spectoscopy (max-R=2500), imaging polarimetry, spectropolarimetry and, when coupled to the adaptive optics module, nearly diffraction limited imaging.
OIG is a CCD camera for direct imaging at optical wavelengths (between 0.32 nd 1.1 microns) for the TNG. It is mounted on the Nasmyth A Adapter interface. OIG is designed to host a variety of CCD chips or mosaics for a field of view up to 10 arcmin. At the moment it is equipped with a mosaic of two thinned and back-illuminated EEV 42-80 CCDs with 2048 x 4096 pixels each (pixel size of 13.5 microns). The resulting pixel scale is 0.072 arcsec/pix for a total field of view of about 4.9 x 4.9 arcmin.
2MASS data were collected by uniformly scanning the entire sky in three
near-infrared bands to detect and characterize point sources brighter than
about 1 mJy in each band, with signal-to-noise ratio (SNR) greater than 10,
using a pixel size of 2.0". This achieves an 80,000-fold improvement in
sensitivity relative to earlier surveys.
2MASS used two new, highly-automated 1.3-m telescopes, one at Mt. Hopkins,
AZ, and one at CTIO, Chile. Each telescope is equipped with a three-channel
camera, each channel consisting of a 256 by 256 array of HgCdTe detectors,
capable of observing the sky simultaneously at J (1.25 microns),
H (1.65 microns), and K<sub>s</sub> (2.17 microns).
<p>2MASS images and other data products can be obtained at the <a href="https://irsa.ipac.caltech.edu/applications/2MASS/QL/">NASA/IPAC Infrared Science Archive</a> Provenance: The Two Micron All Sky Survey is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center, funded by
the National Aeronautics and Space Administration and the National
Science Foundation.. This is a service of NASA HEASARC.
