The MAXIMASTER database table records high-level information of the Monitor of All-sky X-ray Image (MAXI) observations and provides access to the data archive. MAXI is a Japanese experiment located at the International Space Station (ISS), designed to continuously monitor, through a systematic survey, X-ray sources as the ISS orbits Earth. MAXI was launched by the space shuttle Endeavour on 2009 July 16, then mounted on port No. 1 on JEM-EF on July 24. After the electric power was turned on, MAXI started nominal observations on 2009 August 3. The MAXI data are a copy of the MAXI data processing; the output of which is hosted at the DARTS archive located at ISAS (<a href="https://darts.isas.jaxa.jp/astro/maxi/">https://darts.isas.jaxa.jp/astro/maxi/</a>). This catalog is then generated at the HEASARC by collecting high-level information from the data and is updated regularly during operation. This is a service provided by NASA HEASARC .
This all sky mosaic was created by Axel Mellinger and is used
in <i>SkyView</i> with his permission. A fuller description
is available at the
<a href="https://www.milkywaysky.com/">survey website</a>.
<p>
Between October 2007 and August 2009 a digital all-sky mosaic
was assembled from more than 3000 individual CCD frames.
Using an SBIG STL-11000 camera, 70 fields (each covering 40x27 degrees)
were imaged from dark-sky locations in South Africa, Texas and Michigan.
In order to increase the dynamic range beyond the 16 bits of the camera's
analog-to-digital converter (of which approximately 12 bits provide data
above the noise leve) three different exposure times (240s, 15s and 0.5 s)
were used. Five frames were taken for each exposure time and
filter setting. The frames were photometrically calibrated using
standard catalog stars and sky background data
from the Pioneer 10 and 11 space probes. the panorama has an
image scale of 36"/pixel and a limiting magnitude of approximately 14. The
survey has an 18 bit dynamic range.
<p>
The processing of these data used a custom data pipeline built using
IRAF, Source Extractor and SWarp.
<p>
The data used here were converted to three independent RGB color planes
of 8 bits each and provided to SkyView as a single 36000x18000x3 Cartesian
projection cube.
To allow users to efficiently sample data in a region of the sky,
this cube was broken up into 2100x2100 pixel regions with a 50 pixel overlap
between adjacent images. Tiles at the poles were 2100x2050.
<p>
In <i>SkyView</i> each color plane comprises a survey. The individual planes may be
sampled as surveys independently as Mellinger-R, Mellinger-G and Mellinger-B.
The color mosaics can be regenerated by creating an RGB image of all three
surveys. Since <i>SkyView</i> may stretch the intensity values within
each color, linear scaling and a minimum of 0 and maximum of 255 should
be specified to keep the original intensity scalings.
<p>
The full spatial resolution data is used for images of less than
30 degrees on a side. If a user requests a larger region, data are sampled
from a lower resolution 3600x1800x3 data cube. Please contact the survey
author if you need to use the higher resolution data for larger regions.
The Mellinger survey is only available in
<i>SkyView</i> through the website. SkyView-in-a-Jar cannot access
the underlying data. Provenance: Axel Mellinger. This is a service of NASA HEASARC.
The 4850MHz data is a
combination of data from three different surveys: Parkes-MIT-NRAO (PMN)
Southern (-88&#176;; to -37&#176;; declination) and tropical surveys (-29&#176;;
to -9&#176;; declination, and (86+87) Green Bank survey (0&#176;; to +75&#176;;
declination). The data contains gaps between -27&#176;; to -39&#176;;,
-9&#176;; to 0&#176;;, and
+77&#176;; to +90&#176;; declination.
The 4850MHz survey data were obtained by tape from J.J. Condon and are comprised
of 576 images and are used by permission. Full information pertaining to
these surveys are found in the references.<P> Provenance: NRAO, generated by J.J. Condon, J.J. Broderick and G.A. Seielstad, Douglas, K., and Gregory, P.C.. This is a service of NASA HEASARC.
The MIPS Local Galaxies program compiles the Spitzer MIPS observations of all available galaxies in several Herschel-SPIRE Local Galaxies Guaranteed Time Programs, including the Very Nearby Galaxies Survey (VNGS), Dwarf Galaxy Survey (DGS), Herschel Reference Survey (HRS), and Herschel Virgo Cluster Survey (HeViCS).
<P>
The native projection of these data is described as a high-order polynomial
distortion of a gnomonic projection using the same terms as the DSS. Provenance: Data taken by ROE, AAO, and CalTech, Compression
and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
The NEAT/SkyMorph survey provides access to the archives
of the Near Earth Asteroid Tracking (NEAT) project. NEAT is
designed to look for potentially hazardous asteroids, i.e., those
whose orbits cross the Earth's. Over 200,000 images are available
in the NEAT archive.
<a href=https://skyview.gsfc.nasa.gov/skymorph/skymorph.html>SkyMorph</a>
provides a Web interface to the NEAT
images and allows users to select all images in which a given fixed
or moving object is found.
<p>
Unlike most <i>SkyView</i> surveys, the NEAT data are extremely irregular in their
spatial distribution. <i>SkyView</i>'s algorithms for mosaicking images
together to form large images are not adequate for the NEAT data, so
mosaicking is surpressed. Only data within a single NEAT image will
be displayed. The system attempts to find the most recent image within
which has a offset in both RA and Dec of less than 0.8 degrees. If no
such image is found, then an image with the minimum offset is returned, or
the search may fail altogether if there are no nearby plates.
The NEAT telescope uses an array of 4 CCDs. The backgrounds of the
CCDs may differ significantly.
<p>
The NEAT survey covers approximately 30% of the sky. Extreme southern
and low-Galactic latitude regions are unsurveyed. Coverage is otherwise
particularly dense in the ecliptic plane.
<p>
NEAT data consists primarily of groups of three images taken with separations
of 20 minutes and almost identical positions. <i> SkyView </i> will normally
return the last of a 'triplet'. The SkyMorph site can be used to display
an overlay of triplets to look for targets which moved during the interval
between images.
<p>
A catalog of objects detected in the NEAT/SkyMorph pages is accessible
through the SkyMorph pages. 'Light-curves' from all images during which
an object was in the NEAT field of view can also be generated.
<P>
The NEAT data values are in arbitrary density units. To enhance the display
data are transformed such that all pixels below the median values
are scaled linearly to values 0-20, while all pixels above the median
are shifted (but not scaled) to values greater than 20.
Near Infrared Camera and Multi Object Spectrograph
Short Name:
HST.NICMOS
Date:
23 Jul 2020 19:50:23
Publisher:
Space Telescope Science Institute Archive
Description:
The HST Near Infrared Camera and Multi-Object Spectrometer (NICMOS) provides imaging capabilities in broad, medium, and narrow band filters, broad-band imaging polarimetry, coronographic imaging, and slitless grism spectroscopy, in the wavelength range 0.8-2.5 microns. NICMOS has three adjacent but not contiguous cameras, designed to operate independently, each with a dedicated array at a different magnification scale.
![the Fornax VST Survey is licensed under the `Creative Commons Attribution 4.0 License <http://creativecommons.org/licenses/by/4.0/>`_ .. image:: /static/img/ccby.png :alt: [CC-BY]](/registry-search/?f%5Brights_facet%5D%5B%5D=the+Fornax+VST+Survey+is+licensed+under+the+%60Creative+Commons+Attribution+4.0+License+%3Chttp%3A%2F%2Fcreativecommons.org%2Flicenses%2Fby%2F4.0%2F%3E%60_%0A%0A..+image%3A%3A+%2Fstatic%2Fimg%2Fccby.png%0A+++%3Aalt%3A+%5BCC-BY%5D%0A%0A&f%5Btype_facet%5D%5B%5D=Archive&f%5BvalidationLevel_facet%5D%5B%5D=2){kind=link}