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What is SkyServer?
SkyServer is the education and outreach web site of the Sloan Digital Sky
Survey (SDSS). SkyServer makes the entire survey available, free of charge, to
the public. With SkyServer, you can study exactly the same stars and galaxies
that professional astronomers are studying right now.
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What is the Sloan Digital Sky Survey?
The SDSS is one of the most ambitious scientific projects of all time. Its
goal is to make a high-quality three-dimensional map of the universe. The survey
uses a specially-built 2.5-meter telescope in New Mexico, a CCD camera, and
sophisticated software to store and analyze its data.
The SDSS began in June 1998. By the time it ends, the SDSS will have mapped
25% of the night sky, taking images of over 100 million objects. The survey has
already completed a preliminary map of the universe: you can see the map in our First
Discoveries section.
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How do I get around the site?
The main menu bar near the top of the screen (from Home to Help) is always available to
navigate the site. In addition, when you browse using the menubar, a side menu comes up to
help you navigate different parts of the site.
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What can I see on SkyServer?
SkyServer offers two types of data: images and
spectra. Images are pictures of the night sky
taken by our digital camera. Spectra are measurements of the amount of
light a star or galaxy gives off at different wavelengths. SkyServer has
images of more than 80 million stars and galaxies, and spectra for
more than 180,000. For more on our data, see the
Getting Started pages.
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Which query interface or tool should I use?
There are several levels of query interface available in SkyServer, and it can be quite
confusing to choose the one that is appropriate for you. Your choice should depend on what
exactly you want to do, and how comfortable you are with SQL (Structured Query Language) - the
standard language used to query relational databases.
If you are new to SQL and would rather not use it, you should restrict yourself to the
form-based interfaces available on the SkyServer Search page. Use the
radial search to do a simple radial (cone) search, and the rectangular
search to search a rectangular area of the sky. For more sophisticated searches but still without using SQL,
you should use the Imaging Query form and the
Spectro Query form. These will let you build quite complex SQL
queries by filling out a query form. Each of these form-based interfaces will help you learn SQL, since they display the
actual SQL that is sent to the CAS DB server when you hit the Submit button. You
should also look at the Introduction to SQL page for help on SQL.
Once you become more familiar and comfortable with SQL, you should take a look at the sample SQL
queries to see examples of real SDSS science queries. Then you can use the SQL-based interfaces and tools. To run
short, not too complex SQL queries, you can use the SkyServer SQL Search
page. You may also use the Emacs interface or the
command-line sqlCl interface.
To submit longer, more complex SQL queries that may take more than a few minutes to complete, you should use
either the CasJobs batch query workbench (recommended), or the downloadable
sdssQA Java client. However, note that the sdssQA query tool has not been
actively supported beyond DR4.
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Where in the sky do these images come from?
The SDSS takes data in long, narrow "stripes." The current data includes several stripes
near the celestial equator (the Earth's equator projected into the sky), and several in a
C-shaped band of the northern sky. See the DR1 Sky Coverage page for maps and tables of our sky coverage. To see
if a specific area is part of the SDSS, enter its coordinates into the
Finding Chart.
Over the next few years, we will add more data to SkyServer until we have
about one-quarter of the sky covered.
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How can I get all this information?
Use one of SkyServer's tools. Each tool
is designed to access a single type of information - see the
Getting Started pages for more details.
Here is a quick summary of what the most commonly-used tools do.
Famous Places is a gallery of beautiful
SDSS images. The Navigation tool lets you
point and click through the sky. The Object
Explorer gives you access to complete data on a single star, galaxy, or quasar.
The Search tools let you see data on
all objects in a certain part of sky. Or, if you know SQL, you can use
the search tools to return all objects that meet whatever criteria you can
think of.
Did you get all that? The best places to start are with the
Famous Places and Navigation tools. And don't worry; all the tools have Help pages.
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What help is available?
SkyServer has an extensive Help section, including
a Glossary and How-To Tutorials. The Schema Browser is essential for using the Search tool. SkyServer's
About Astronomy and About SDSS sections also contain readings that help explain concepts from astronomy and the SDSS.
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How can I use SkyServer to learn about astronomy?
SkyServer's Projects use SDSS data to interactively
teach astronomy. With our Projects, you can learn about the evolution of
stars, the types of galaxies, the history of the universe, and much more.
Teachers, we welcome you to use and adapt any of our projects in
your classes, free of charge. For more information on what you can do
with SkyServer in the classroom, see our
Teacher FAQ.
- What is the difference between Target and Best ?
Because the survey imaging and processing is always being improved, the SDSS
often obtains improved photometric measurements of objects AFTER they have
been chosen ("targeted"
) for spectroscopy. However, it is important to keep
a record of the photomeric measurements at the time objects were targeted.
We therefore maintain two versions of the photometric catalog:
- Target:
Known as TARGDR1 in the DR1 CAS, this database contains the
photometric catalogs AS THEY WERE WHEN OBJECTS WERE CHOSEN FOR SPECTROSCOPY.
This database contains the union of all target chunks
. It may cover a slightly
different area than Best; blended objects may be deblended differently;
image quality may be worse; photometric calibration may be less accurate.
However, if you want to see what the SDSS thought the magnitudes and other
properties of an object were when it was chosen for spectroscopy, this is the
place to look. Note that this database DOES NOT contain links from the
photometric objects to the spectroscopy (you can always get the Target data
for spectroscopic objects using the TargObjID field in the SpecObjAll table
),
nor does it contain the tiling information. This is because the Target
database is intended to be a snapshot of the survey before any spectroscopy
is done.
- Best:
Known as BESTDR1 in the DR1 CAS, this database contains the latest,
best versions of the imaging data, processed with the latest version of the
photometric processing software, and with the most recent understanding of the
photometric calibration applied. For any science based on object photometry,
you will want to use the Best data. In addition, only the Best database
contains all of the spectroscopy and tiling information.
- What is the difference between SpecObj and SpecObjAll? What does sciencePrimary mean?
The SpecObjAll table contains ALL spectroscopic objects, regardless of their status in the survey. Queries on this table can produces unusual or undesired objects. Thus, we have created the SpecObj view, which contains data for ONLY those fibers defined as SciencePrimary. To be SciencePrimary, an object must meet all of the following criteria:
- It was targeted in the target skyVersion;
- The plate on which the spectrum was taken is the primary observation of that tile;
- The plate was a main survey plate (not part of the Southern survey or a special project);
- The objType is not QA, SKY, or SPECTROPHOTO_STD (these object types are repeatedly observed);
- The fiber was mapped correctly (this is the
zWarning check)
As a result, some plates may have many (or even all) of their fibers excluded from SpecObj. Some of these instances are:
- What are the differences between PhotoObj, PhotoTag, and PhotoObjAll?
PhotoObjAll is a table in the Best and Target databases which contains
all of the measured photometric quantities for all of the imaging objects.
Because we measure so many different parameters for each object, this is a
very large table, and queries can take very long to run.
In an effort to
speed up queries, we have created a table with only a subset of the
parameters (a "thin table") that are requested most often. This table is
called PhotoTag.
If you have a query which uses and returns only values
stored in PhotoTag, it will execute much faster than if you used PhotoObjAll.
In addition, we have created a view ofPhotoObjAll which contains only those objects which are Primary or Secondary. This view is called PhotoObj. Because this view effectively contains fewer objects than PhotoObjAll, but all the measured quantities for these objects, queries will execute faster.
Given the above, a user should:
- Query from PhotoTag if it contains everything you are looking for;
- Query from PhotoObj otherwise, UNLESS you are interested in data for objects which are neither PRIMARY nor SECONDARY. In that case, you will need to use PhotoObjAll.
- Importantly, the "shorthand" quantities u,g,r,i,z do not exist in the PhotoTag table. Instead, you must use ModelMag_[ugriz], which is indexed to make queries faster. HOWEVER, in PhotoObjAll and its views, only the u,g,r,i,z are indexed, and not the ModelMags!
Because PhotoTag has many fewer parameters, larger portions of it can be cached, improving performance. We have found that for almost all queries which contain parameters fully in PhotoTag, it is faster. In the case of looking for objects that are detected multiple times, one could perform a join on PhotoTag with itself, requiring that one object be Primary and the other Secondary.
- How do I get photometry for spectroscopic objects? What is the SpecPhotoAll table?
The SpecPhotoAll table is a precomputed join between the Best PhotoObjAll and SpecObjAll tables. It includes the most requested parameters from these two tables, as well as a few pieces of information about tiling. It also includes the TargetObjID, which allows user to retrieve the Target version of the photometry.
- What is the difference between SpecPhoto andSpecPhotoAll?
As described above, The SpecPhotoAll is a precomputed join between the Best PhotoObjAll and SpecObjAll tables. This includes all non-science objects, and a variety of objects many users will not be interested in. The SpecPhoto view includes only those pairs where the SpecObj is a sciencePrimary (see the definition above), and the BEST PhotoObj is a PRIMARY.
- Why do z and zErr (in SpecObj) have different numerical
precision?
Internally, these numbers are stored to their full precision as they come out
of the spectroscopic pipeline. When you perform a query, they have some
default string format applied that cuts them to what you see. But you can use
the str() function to change the string format to whatever you like.
To get z to 6 decimals, e.g., change your query to 'select str(z,8,6) as z'
instead of just z, and analogously for zErr. This applies the function str()
to the values in column z and returns the result with column label z (without
the "as", the result of a function has no column label). The
str(col,length,dec) function takes the numerical value in 'col' and formats it
as a string of length 'length' and with 'dec' significant digits, i.e. it's
the SQL equivalent to the C function printf("%8.6f",z). str() rounds the
result to the number of decimals you request.
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Who is responsible for all this?!
See our Credits page.
