Frequently Asked Questions
This page gives a list of frequently asked questions about the SDSS and Data Release 13.
Don’t see your question answered here, or elsewhere on the DR13 website? Email the SDSS Helpdesk.
About DR13 data interfaces
- What interfaces are available to SDSS data?
- My Skyserver query no longer works in DR13 – what happened?
- What is the difference between
SpecObjAll? What do
- What are the differences between
- How do I get photometry for spectroscopic objects? What are the
- Why do some values (such as
SpecObj) have different numerical precision?
- What is the difference between
typefor spectroscopic objects, and which one should I use?
- I want to mirror the SDSS catalog archive – how can I get a copy of all the data?
- Why can’t I log in to CasJobs?
- Why doesn’t my query work on SDSS CasJobs? It works on other SDSS sites.
About Data Release 13
- What help is available for DR13?
- What is the sky coverage of DR13? Where in the sky do the data come from?
- How can I see if DR13 has an image or spectrum of my favorite object?
- How can I search for data?
- How can I match a list of objects to see what data are available for them in DR13?
- How do I convert from the SDSS’s ugriz magnitudes to UBVRI magnitudes?
About the SDSS
What is the Sloan Digital Sky Survey?
The Sloan Digital Sky Survey is an ongoing astronomy project that has been working since 1998 to make a detailed map of the universe, including our Milky Way galaxy. Since 2014, the survey has been in operating its fourth phase. Results from all phases (including the current fourth one) are available at www.sdss.org.
What data does SDSS have? What can SDSS tell me about the sky?
The most recent SDSS data release, the thirteenth overall, is SDSS Data Release 13 (DR13), made public on July 31, 2016. It includes most data from prior data releases; so to get the most recent, up-to-date data for anywhere in the sky, use Data Release 13.
Data Release 13 includes imaging data for about one-third of the night sky. The imaging data include images from the camera on the SDSS’s 2.5-meter telescope as preview images (JPGs) and as FITS files. The data also include catalogs of detected objects, with parameters measured from imaging, including positions and magnitudes. DR13 also includes spectroscopic data for more than three million stars, galaxies, and quasars, Spectra are available as preview images (PNGs) and FITS files. Spectroscopic catalog data include object types and redshifts.
All DR13 data are available from this site. See DR13 Data Access to learn how to view and download DR13 data.
Prior SDSS-III data releases are also available. Its final data release, Data Release 12 was made publicly available on July 31, 2015. Previous data releases are still available as Data Release 10 (July 30, 2013), Data Release 9 (July 31, 2012), and Data Release 8 (January 11, 2011).
The final data release for SDSS-I and SDSS-II is Data Release 7.
I am a teacher. How can I use the data in my classes?
The SDSS Education page describes what educational resources are available from the SDSS project.
The SDSS Voyages and SkyServer websites includes a variety of educational projects that use SDSS data to teach topics in astronomy and other sciences, using guided and open inquiry. With our Projects, you and your students can learn about spectra and colors of stars, galaxy types, the history of the universe, and much more.
You are welcome 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.
Why doesn't the SDSS have data for well-known visible stars (Sirius, Vega, etc.)?
The SDSS had a very sensitive camera. Stars that you can see with your unaided eyes are too bright for the SDSS’s camera; they are saturated, and the light from them spills all over the detector. The SDSS still gets an image of those stars (for example, here is an image of Pollux from SkyServer), but the image processing software is unable to handle these images, and there are no entries in the SDSS catalog.
Why are some bright stars classified as galaxies?
The SDSS distinguishes between stars and galaxies based on their shapes: single points of light are stars, and fuzzy patches of light are galaxies. Some stars are bright enough that their light saturates the camera, and thus the light spills over the image, so to the SDSS’s camera, they look like fuzzy disks instead of single points of light. Their appearance fools the SDSS’s software into classifying them as galaxies.
About Data Release 13
What is the sky coverage of DR13? Where in the sky do DR13 data come from?
The SDSS includes imaging data in long, narrow “stripes”, 2.5 degrees wide. Part of the processing of SDSS images is to select some objects as targets for follow-up spectroscopy. The SDSS then collects spectra later. Most spectra were collected using the original SDSS-I/-II spectrograph. DR13 includes data collected using the BOSS spectrograph for the eBOSS and MaNGA surveys, and data collected using the APOGEE spectrograph for the APOGEE-2 survey.
The Scope of DR13 page shows what areas of sky (sky coverage) are included in DR13. The Scope page also includes a Coverage Check form that allows you to see what data DR13 has for a given point on the sky.
How can I see if DR13 has an image or spectrum of my favorite sky object?
Go to the SkyServer Navigate tool. Enter the name of your object in the “Name” box, then press Enter. The RA/dec coordinates of the object will appear in the boxes below. Then, click Get Image.
If a sky image appears in the main Navigate frame, then DR13 has an image for your object.
If there is an image for your object, you can also check to see whether DR13 includes a spectrum. Under the RA/Dec boxes, find the Drawing options. Click the checkbox next to Objects with spectra. If a red square appears around your object, then your object has a measured spectrum in DR13.
Whether or not your object has a spectrum in DR13, the object’s magnitude data will appear in the right-hand pane. Click Quick Look to go see additional basic data about that object. Click Explore for more detailed data.
How can I search for data?
When you search for data in the SDSS, you are going through the SDSS database and looking for objects that match criteria you choose. For simple searches of photometric data, use the Imaging Query Form. For simple searches of spectroscopic data, use the Spectroscopic Query Form. For more complex searches, use Structured Query Language (SQL). See SkyServer’s guide on Searching for Data to learn more about SQL. To see thumbnail results of objects that meet your criteria, use the Image List tool.
For large, complex queries that will take a long time to run, use CasJobs, the SDSS’s batch query interface.
Many other search tools are available. See the DR13 Data Access pages for more options.
An important note if you are using Excel with the SkyServer educational projects: SDSS object IDs are so long that they get cut off in Excel, and show up with 000 as the last three digits. This means you won’t be able to find your objects anymore! To get around this problem, see this workaround.
How can I match a list of objects to see what data are available for them in DR13?
If you have a fairly small list of objects to match – a few hundred or so – use the SkyServer Cross-ID tool. Paste your list of objects, or upload a file containing data with the last two columns as (ra, dec) in decimal degrees. Click Submit. The next page will show only those objects that appear in the SDSS, with SDSS Object IDs that link to the Explore tool.
To see a thumbnail SDSS image of each matching object, use the Image List tool. Enter your list in the textbox on the upper left and click “Get Image”. Click on one of the thumbnails to go to that position in the Navigate tool, or on one of the object names to go to that object’s Explore tool entry.
For longer lists, use the Neighbors Search feature of CasJobs. See the CasJobs FAQ entry on “How can I cross-identify (find matching objects in SDSS) for my list of sources for which I have RA,decs?” for more information.
How do I convert from the SDSS's ugriz magnitudes to UBVRI magnitudes?
The SDSS measures magnitudes through ugriz filters, which give ugriz AB magnitudes. These magnitudes can be converted into UBVRI magnitudes using a set of transformations described on the Algorithms page of this site.
About DR13 data interfaces
What interfaces are available to SDSS data?
There are multiple interfaces to SDSS data, including:
- Also known as the Catalog Archive Server (CAS), SkyServer is designed for astronomers, students and the general public.
- For bigger queries, CasJobs provids a batch (asynchronous) system for querying the database and storing results, designed to allow astronomers to search SDSS catalog data flexibly and efficiently.
- Science Archive Server
- The Science Archive Server (SAS) provides direct access to the full SDSS data archive, including all directories and files listed in the Data Model.
- Science Archive Webapp
- The Science Archive Webapp provides a searchable interface for optical and infrared spectra, images of fields and mosaics, and includes an interactive view of optical spectra and infrared spectra, and a data download facility (supports both rsync and wget). All searches are cached on the server so that you can return later, via a permalink, or email the permalink to share your search results.
What is the difference between
SpecObjAll? What do
SpecObjAll table contains all spectroscopic objects, even duplicate spectra of the same object. Thus, we have created the
SpecObj view, which contains data for only those fibers defined as sciencePrimary – essentially, the best spectrum that the SDSS has obtained for that object. That is,
specObj contains no duplicate observations.
sciencePrimary, another parameter called
bossPrimary flags the best spectrum that BOSS has obtained for an object. Exact definitions of
bossPrimary can be found in the spectroscopic catalogs documentation.
What are the differences between
PhotoObjAll is a table that contains all of the measured photometric quantities for all of the imaging detections for every object. Because we measure hundreds of parameters for each of 1.2 billion detections, this is a very large table, and queries can take very long to run. Also,
PhotoObjAll includes duplicate and “special” detections such as parent or bright detections, which are normally not of interest to science users.
In an effort to speed up catalog data queries, we have created
PhotoTag, a view (virtual or logical table) of PhotoObjAll with only a subset of the photometric parameters that are most often requested. Queries on this “thin” version of PhotoObjAll run much faster usually than queries on the larger table. If you have a query that uses and returns only values stored in
PhotoTag, then you should definitely use
In addition, we have created
PhotoObj, a view of
PhotoObjAll that contains only those objects that are survey primary or survey secondary.
PhotoObj excludes special objects such as parent or bright detections. Because
PhotoObj contains the same parameters as
PhotoObjAll but effectively contains fewer objects, any queries for survey primary or survey secondary objects will run faster on
Finally, there is
PhotoPrimary, a view of
PhotoObjAll that only includes survey primary detections; if you are not interested in duplicate detections at all, this is the view to use.
To summarize, the
PhotoTag view is a vertical partition of
PhotoObjAll (fewer columns), and
PhotoSecondary are horizontal partitions of
PhotoObjAll (fewer rows).
Given the above, you should consider:
- Querying from
PhotoTagif it contains all the parameters you are using to search and all the parameters you want returned
- Querying from
PhotoObjotherwise, UNLESS you are interested in data for objects that are neither PRIMARY nor SECONDARY. In that case, you will need to use the full
- Importantly, the “shorthand” quantities u,g,r,i,z do not exist in
PhotoTag(because we want to keep the view as thin as possible). Instead, you must use the modelMag_[ugriz] columns. HOWEVER, in
PhotoObjAlland its views, only the u,g,r,i,z are indexed, and NOT the ModelMags! This difference in indexed columns is to save space (since indexes on a huge table like
PhotoObjAllare expensive), not to confuse you!
PhotoTag has many fewer parameters, larger portions of it can be cached, improving performance. We have found that for almost all queries that contain parameters fully in
PhotoTag, it is faster.
How do I get photometry for spectroscopic objects? What are the
SpecPhotoAll table and
The SpecPhotoAll table is a precomputed join between the PhotoObjAll and SpecObjAll tables. It includes the most requested parameters from these two tables. Because the join has already been performed, it can be faster than computing the join on the fly. The
SpecPhoto view contains the same parameters as
SpecPhotoAll, but only for objects that are survey primary or survey secondary.
Why do some values (such as
SpecObj) have different numerical precisions?
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 SQL’s
str() function to change the string format to whatever you like.
To get z to 6 decimals, for example, change your query to search for
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 function
str(col,length,dec) takes the numerical value in
col and formats it as a string of length length and with dec significant digits. In other words,
str(z,8,6) is the SQL equivalent to the C function
str() function rounds the result to the number of decimals you request.
What is the difference between class and type for spectroscopic objects, and which one should I use?
For any object in DR13, the
type parameter in
SpecObj and other tables was set when that object was targeted for spectroscopy (i.e., it is based on its morphology in the imaging data). The
class parameter is set by the spectroscopic pipeline after the spectrum is observed (i.e., it is based on features in the spectrum).
In nearly all cases, you should believe the classification in
class, since it tells you what the measured spectrum actually was. The
type field tells you about why it was targeted. (However, there is more information about the object’s target selection history in the target bits; see the target bitmasks pages for more information.
I want to mirror the SDSS catalog archive - how can I get a copy of all the data?
Why can't I log in to CasJobs?
As of May 10, 2016, CasJobs is part of the new SciServer collaborative data-driven science framework, and CasJobs users need to register on the SciServer portal with their original CasJobs credentials so that they can obtain a new account on the SciServer single-sign-on system that is linked to their existing CasJobs account.
Why doesn't my query work on SDSS CasJobs? It works on other Skyserver sites.
CasJobs uses the idea of query contexts, allowing you to specify what data sources you can query. The default context is to search your MyDB personal database space. To search DR13, the context should be set to DR13. You can choose from the Context drop-down menu above the area where you run queries. Before you run a CasJobs query, check what context you are searching. See the CasJobs user guide for more information.