On June 30, a small project we’ve done together with the Armenian Virtual Observatory has ended. Its objective was to publish the spectra from the First Byurakan Survey (the DFBS) in a VO-compilant way. The data comes from one of the big surveys with Schmidt telescopes that form a sizable part of the observational heritage from the second part of the 20th century (you’re still using a few of them daily if you tell Aladin to show a DSS plane).
In this case, spectra from objects on the entire northern sky off the milky way down to about 18th mag were obtained. In a previous cooperation between Armenian and Italian astronomers a good decade ago, the plates were digitised and calibrated, and spectra were extracted. However, they resided behind a web interface so far, which made them somewhat clumsy to work with.
Have a glance at the tutorial – you see, while the Byurakan survey certainly is a valuable resource by itself, I happen to believe at this point it’s particularly valuable because with the next Gaia data release (planned for next year), a deluxe version of it will come: Gaia’s RP/BP spectra will be all-sky, properly calibrated, and quite a bit deeper, but still low-resolution. So, if you’re just waiting for such a data collection, you can train your methods right now on the DFBS.
One of the major usability issues our publishing suite DaCHS has for operators (i.e., people who want publish data) is the “horror vacui”: How do I start a Resource Descriptor (RD – the file DaCHS interprets to build services)?
I used to recommend to start by having a look at the RDs of our existing services and pick whatever matches best your publication project. But finding a matching service and figuring out what is generic, what’s a special property of the concrete data collection, and what’s a hack that should not be reproduced isn’t straightforward at all, not to mention the fact that some of those RDs have been in maintenance mode for almost 10 years and hence may show deprecated practices.
I had planned to generalise Mikhail’s approach to several types of resources supported by DaCHS, ideally inferring the questions to ask from the built-in documentation of mixins and applys. But during the last year, whenever I felt it would be a good time to tackle that generalisation, I quickly gave up again. It was mostly rather trivial stuff such as how to tell apart repeatable metadata (waveband, say) and non-repeatable metadata (instrument, say). But it was bad enough that I quickly found something else to do each time I got started.
Eventually, I gave up on a menu interface altogether – making it flexible and generatable at the same time seemed a fairly complex problem. But that doesn’t mean I forgot about overcoming the horror vacui thing. So, when forms aren’t flexible enough for data entry, where do you turn? Right! A text editor.
Enter dachs start. That’s a new DaCHS subcommand that gets you started with your RD. For one, you can list the templates available:
$ dachs start list
siap -- Image collections via SIAP1 and TAP
ssap+datalink -- Spectra via SSAP and TAP, going through datalink
epntap -- Solar system data via EPN-TAP 2.0
scs -- Catalogs via SCS and TAP
More templates are planned; siap+datalink, for instance, would cover some frequent use cases. Feel free to mail in requests.
Once you find a suitable template, create your future resource directory, enter it and run dachs start again, this time passing the name of the template you want:
$ mkdir ex_data
$ cd ex_data
$ dachs start scs
$ head -16 q.rd | tail -9
<meta name="title">%title -- not more than a line%</meta>
%this should be a paragraph or two (take care to mention salient terms)%
<!-- Take keywords from
dachs start uses the directory name as the new schema name and then writes a file q.rd (which is the canonical name for the “main” RD in a resource). Within this file, you’ll see things to fill out between pairs of percent signs with short explanantions. Where longer explanations are necessary, embedded comments should help.
To give you an idea of the intended use: As a vim user, I’ve put
au BufRead,BufNewFile *.rd imap /%[^%]*%a
au BufRead,BufNewFile *.rd imap cf%
into my ~/.vimrc. That way, while editing the template into an actual RD, hitting F8 takes me to the next thing to be edited; I can then read the instructions, and when I have made up my mind, I can either delete the template element or hit F9 and replace the explanation text with whatever belongs there.
The command is available starting with the 1.1.3 beta (available now by switching to the beta repo) and will be part of the 1.2 release, planned for early June after the Victoria interop.
If you have a publication project: just try it out and give feedback. Note that the templates haven’t actually been tested yet, and the comments were written by a DaCHS and VO nerd, so they might not always be great either. Thus, when you get stuck: complain early, complain often!
A histogram of times for which the Palomar-Leiden service has images: That’s temporal service coverage right there.If you are an astronomer and you’ve ever tried looking for data in the Virtual Observatory Registry, chances are you have wondered “Why can’t I enter my position here?” Or perhaps “So, I’m looking for images in [NIII] – where would I go?”
Both of these are examples for the use of Space-Time Coordinates (STC) in data discovery – yes, spectral coordinates count as STC, too, and I could make an argument for it. But this post is about something else: None of this has worked in the Registry up to now.
It’s time to mend this blatant omission. To take the next steps, after a bit of discussion on some of the IVOA’s mailing lists, I have posted an IVOA note proposing exactly those last Thursday. It is, perhaps with a bit of over-confidence, called A Roadmap for Space-Time Discovery in the VO Registry. And I’d much appreciate feedback, in particular if you are a VO user and have ideas on what you’d like to do with such a facility.
In this post, I’d like to give a very quick run-down on what is in it for (1) VO users, (2) service operators in general, and (3) service operators who happen to run DaCHS.
First, users. We already are pretty good on spatial coverage (for about 13000 of almost 20000 resources), so it might be worth experimenting with that. For now, the corresponding table is only available on the RegTAP mirror at http://dc.g-vo.org/tap. There, you can try queries like
select ivoid from
natural join rr.stc_spatial
and ucd like 'phot.flux;em.radio%'
to find – in this case – services that have radio fluxes in the area of the Hubble Deep Field. If these lines scare you or you don’t know what to do with the stupid ivoids, check the previous post on this blog – it explains a bit more about RegTAP and why you might care.
Similarly cool things will, hopefully, some day be possible in spectrum and time. For instance, if you were interested in SII fluxes in the crab nebula in the early sixties, you could, some day, write
SELECT ivoid FROM
NATURAL JOIN rr.stc_spectral
NATURAL JOIN rr.stc_spatial
As you can see, the spectral coordiate will, following (admittedly broken) VO convention, be given in meters of vacuum wavelength, and time in MJD. In particular the thing with the wavelength isn’t quite settled yet – personally, I’d much rather have energy there. For one, it’s independent of the embedding medium, but much more excitingly, it even remains somewhat sensible when you go to non-electromagnetic messengers.
A pattern I’m trying to establish is the use of the user-defined function ivo_interval_overlaps, also defined in the Note. This is intended to allow robust query patterns in the presence of two intrinsically interval-valued things: The service’s coverage and the part of the spectrum you’re interested in, say. With the proposed pattern, either of these can degenerate to a single point and things still work. Things only break when both the service and you figure that “Aw, Hα is just 656.3 nm” and one of you omits a digit or adds one.
But that’s academic at this point, because really few resources define their coverage in time and and spectrum. Try it yourself:
SELECT COUNT(*) FROM (
SELECT DISTINCT ivoid FROM rr.stc_temporal) AS q
(the subquery with the DISTINCT is necessary because a single resource can have multiple rows for time and spectrum when there’s multiple distinct intervals – think observation campaigns). If this gives you more than a few dozen rows when you read this, I strongly suspect it’s no longer 2018.
To improve this situation, the service operators need to provide the information on the coverage in their resource records. Indeed, the registry schemas already have the notion of a coverage, and the Note, in its core, simply proposes to add three elements to the coverage element of VODataService 1.1. Two of these new elements – the coverage in time and space – are simple floating-point intervals and can be repeated in order to allow non-contiguous coverage. The third element, the spatial coverage, uses a nifty data structure called a MOC, which expands to “HEALPix Multi-Order Coverage map” and is the main reason why I claim we can now pull off STC in the Registry: MOCs let databases and other programs easily and quickly manipulate areas on the sphere. Without MOCs, that’s a pain.
So, if you have registry records somewhere, please add the elements as soon as you can – if you don’t know how to make a MOC: CDS’ Aladin is there to help. In the end, your coverage elements should look somewhat like this:
The waveband elements are remainders from VODataService 1.1. They are still in use (prominently, for one, in SPLAT), and it’s certainly still a good idea to keep giving them for the forseeable future. You can also see how you would represent multiple observing campaigns and different spectral ranges.
Finally, if you’re running DaCHS and you’re using it to generate registry records (and there’s almost no excuse for not doing so), you can simply write a coverage element into your RD starting with DaCHS 1.2 (or, if you run betas, 1.1.1, which is already available). You’ll find lots of examples at the usual place. As a relatively interesting example, the resource descriptor of plts. It has this:
This particular service archives plate scans from the Palomar-Leiden Trojan surveys; these were looking for Trojan asteroids (of Jupiter) using the Palomar 122 cm Schmidt and were conducted in several shortish campaigns between 1960 and 1977 (incidentally, if you’re looking for things near the Ecliptic, this stuff might still hold valuable insights for you). Because the fill factor for the whole time period is rather small, I manually extracted the time coverage; for that, I ran select dateobs from plts.data via TAP and made the histogram plot above. Zooming in a bit, I read off the limits in TOPCAT’s coordinate display.
The other coverages, however, were put in automatically by DaCHS. That’s what the updater element does: for each axis, you can say where DaCHS should look, and it will then fill in the appropriate data from what it guesses gives the relevant coordiantes – that’s straightforward for standard tables like the ones behind SSAP and SIAP services (or obscore tables, for that matter), perhaps a bit more involved otherwise. To say “just do it for all axis”, give the updater a single sourceTable attribute.
Finally, in this case I’m overriding mocOrder, the order down to which DaCHS tries to resolve spatial features. I’m doing this here because in determining the coverage of image services DaCHS right now only considers the centers of the images, and that’s severely underestimating the coverage here, where the data products are the beautiful large Schmidt plates. Hence, I’m lowering the resolution from the default 6 (about one degree linearly) to still give some approximation to the actual data coverage. We’ll fix the underlying deficit as soon as pgsphere, the postgres extension which is actually dealing with all the MOCs, has support for turning circles and polygons into MOCs.
When you have defined an updater, just run dachs limits q.rd, and DaCHS will carefully (preserving your indentation) re-write the RD to contain what DaCHS has worked out from your table (but careful: it will overwrite what was previously there; so, make sure you only ask DaCHS to only deal with axes you’re not dealing with manually).
If you feel like writing code discovering holes in the intervals, ideally already in the database: that would be great, because the tighter the intervals defined, the fewer false positives people will have in data discovery.
The take-away for DaCHS operators is:
Add STC coverage to your resources as soon as you’ve updated to DaCHS 1.2
If you don’t have to have the tightest coverage declaration conceivable, all you have to do to have that is add
to your RD (where my_table is the id of your service’s “main” table) and then run dachs limits q.rd
For special effects and further information, see Coverage Metadata in the DaCHS reference documentation
If you have a nice postgres function that splits a simple coverage interval up so the filling factor of a set of new intervals increases (or know a nice, database-compatible algorithm to do so) – please let me know.
Today I was up on Heidelberg’s signature mountain, Königstuhl, at the Max-Planck-Institute for Astronomy for a little talk on what I’d provisionally call “intermediate ADQL” – discussing some aspects of ADQL and some TAP techniques that may not be immediately obvious but still generally and straightforwardly applicable to everyday problems. Since I suspect the lecture notes for that talk may be of interest to some readers of this blog, I thought I should share them here.
What this also contains is a very quick piece of pyVO-based python (which needs both this helper and a recent pyVO) for a use case that comes up fairly often: “Give me all proper motions (radio fluxes, distances, radial velocities, whatever) for object in this region.”
This uses a discovery case I’ve been after for quite a while now: Find services by the UCDs of tables within them. And while that’s been possible for quite a while on GAVO’s Registry UI WIRR, there’s still too many services that don’t declare their tables to the Registry, and when talking about TAP, the situation is still a bit worse (as has been mentioned in my account of the last interop). So – enjoy the code, but very frankly, you’ll still see wires sticking out for a several months yet.
And if you run a TAP service yourself, please have a look at how to enable table discovery over on the IVOA wiki so we can finally get those pesky wires out of our users’ eyes.
DaCHS, the Data Center Helper Suite, is a comprehensive suite for publishing astronomical data to the Virtual Observatory, supporting most major protocols out there. On Dec 12, GAVO released a new version, 0.9.8. The most notable change is that now SODA is supported as specified in the last IVOA Proposed Recommendation.
This is fairly big news, as SODA is the VO’s answer to providing cutout services and the like, which obviously is important part with datasets in the Multi-Gigabyte range and the VO’s wider programme of trying to enable users to only download what they need. But even for spectra, which aren’t typically terribly large, we have been using SODA; for instance, when you just want to see the development of a single line over time, say,, it’s nice to not have to bother with the the full spectrum. The spectral client SPLAT has been offering such functionality for a couple of years now — watch out for the scissors icon in discovery results. These indicate SODA support on the respective services.
Another client that will support SODA and its basis Datalink is Aladin – we’ve seen a promising demo of that during the last Interop in Trieste. Until the clients are there, DaCHS contains a (largely re-usable) stylesheet that generates simple UIs for Datalink documents and SODA services. Some examples:
Note again that all of these are not actually web pages, they’re machine-readable metadata collections; if you don’t believe it, pull the URLs with curl. To learn more about the combo of Datalink and SODA, check out this ADASS 2015 poster (preferably before even looking at the not terribly readable standards texts).
UWS stands for Universal Worker Service and is an IVOA standard provides a protocol which can be used for accessing databases and other web services from the command line, e.g. using the python uws-client.
This allows to create (asynchronous) jobs for a web service (e.g. an SQL query), check their status, retrieve their results, abort or delete them.
The updated version 1.1 was approved at the InterOperability Meeting last week and brings some nice new features:
Job list filtering: When retrieving the job list, one can now retrieve only jobs created after a certain date, the latest n jobs or jobs with a certain phase (e.g. EXECUTING or COMPLETED)
WAIT: When asking for job details, it is now possible to append a WAIT parameter and provide an integer as wait-time in seconds. This means that the job details will only be returned when the wait-time is over or the job’s phase has changed, whichever comes first.