VStar

My work – “work”, this is supposed to be amateur astronomy! – in variable star astronomy is mainly observational. I love being out under the sky, estimating variables using the time-tested tools of variabilists that’s been around since, well, Argelander’s days (not really, since I don’t use his step method, but never mind): maps with comp stars printed on paper, a 20 cm Newton reflector and a pair of 15×70 binoculars. Or, not as fun as visual observing but with the added possibility of going a lot fainter, remotely controlled telescopes with the FITS images analysed in Vphot.

So, I am an observational amateur. Statistics and Excel spreadsheets are not my forte, other people are much better at analysing large photometric datasets. For example, my Swedish variabilist colleague, Thomas Karlsson, juggles numbers and comes up with truly amazing results.

Still, I would like to do a bit of analysis. And that’s were VStar enters the picture. It is a great piece of software!

Great software should make the beginning user able to perform central tasks with a minimum of hassle but also have more advanced capabilities available, as the user gets more advanced.

For example, determining a time of maximum for a Mira variable is easily done in VStar; observations are imported from the AAVSO International Database, a polynomial curve is fitted, and the maximum of that function gives the time of max. Other datasets, not in AID, can of course be imported. There are many other powerful features in VStar, for the more advanced user.

Besides its many features and well-designed nature, VStar is free, in active development and cross-platform (which I like, being a Mac user – the world of amateur astronomy software is very Windowscentric). New features being developed or planned for future releases are visible at the project’s SourceForge page.

David Benn, the programmer behind this amazing program, keeps a well-written blog which, among other things, discuss features of VStar such as finding a Mira’s maximum.

If you are, like me, interested in beginning to learn analysing variable star data, a good starting point is VStar.

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Comet 168P/Hergenrother

I observed comet 168P/Hergenrother yesterday, at October 6.88 (UT). Instrument: 20 cm Newton, 120 x. Location: Lund, Sweden. Sky: moderate quality, city lights.

The coma was estimated to be 0.5′ and the magnitude 9.8 (Tycho catalogue comparison stars). The comet was compact and easily detected; no tail was seen.

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Printing

I’m printing a new batch of charts for variable star observing; in this electronic age, I still prefer to have paper charts with sequences of compstars with me out at the telescope. For one thing, they can handle the damp and dew far better than my MacBook, and I kind of like the tactile aspects of flipping through binders rather than clicking through screen menus in the dark.

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SS Cyg in outburst

Yesterday I observed SS Cygni at 11.2 and 11.1, the early stages of an outburst.

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Time for a nova?

Since I got back to amateur astronomy in November 2011, after a hiatus since around 1990, I’ve had the opportunity to observe several types of objects and celestial phenomena: a total lunar eclipse; U Geminorum in outburst; a fading of that northern beauty (as RCB’s go), Z Ursae Minoris; a well-placed comet visible in binoculars, in the form of comet Garradd; maxima of classic miras T Cephei, R Leonis and chi Cygni. Add to that a whole zoo of objects observed digitally using robotic CCD-telescopes, ranging from blazars to extragalactic supernovae and literally thousands of variable stars, among them a bunch of formerly neglected miras picked up by a group of fellow Swedish variabilists.

Quite a lot in eight months of observing.

But I haven’t seen a nova. I have the impression that the novae visible recently have been stuff deep down in the southern sky, all but invisible from my vantage point here at 55 degrees northern latitude.

Who knows what the sky will have in store for us? Back in 2007 and 2008, there were novae in Cygnus and Vulpeculae, and further back during the last couple of decades there’s been bright novae in Cygnus, Aquila and Cassiopeia.

Maybe it’s time for the northern Milky Way the next time? All the nova action can’t possibly be all Sagittarius all the time.

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4C 32.55

When reducing CCD images in Vphot, I often get several variables in the field, other than the star intended, especially with wide field instruments such as the iTelescope 10 cm refractor. The other day, as I was analysing observations of IX Lyrae, one of the Miras on the SVO programme on neglected Miras, Vphot identified – through the AAVSO VSX database – an object called 4C 32.55 in the field. I became curious, and decided to look it up.

It turned out to be an active galactic nucleus with variation in the visual, just like its more well-known brethren BL Lac. It is, as noted by Gary Poyner, rather neglected by amateurs, even though it shows quite marked variations. Poyner has the object on his programme. Looked kind of interesting, and I decided to re-reduce my observations of IX Lyrae made since March. The result was eight observations of this interesting object.

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Miras in the Kepler field

We run a programme of studying 50 neglected miras in the Swedish variable star community. After having found out, by chance, that one of the stars was in the Kepler field, I decided to check out if more of our programme stars also were in the Kepler field. It turned out that of the 17 stars in our programme that belong to the Kepler constellations of Lyra and Cygnus, only four stars seems to be in the Kepler field. They are also in the ASAS Kepler Field data release.

A table with cross identifications, periods etc is here.

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Neglected miras

Here is a status report (in Swedish) for the project on 50 neglected miras observed by SAAF/SVO observers.

Update: Thomas Karlsson has made a page that gives an overview of the observations in SAAF V/SVO programme of neglected Miras.

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Variable star observers meet in Gothenburg

Just came back from the very inspiring spring meeting of SVO/SAAF Swedish variable star observers. Here are some pictures: [Not a valid template]

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KK Aurigae

I’ve been observing KK Aurigae for some six weeks or so. It is situated close to YY Aurigae, a star I am observing for a programme on neglected Miras together with some fellow Swedish amateurs, and sometimes it ends up in the same CCD frame as YY Aurigae.

The star doesn’t behave according to what the catalogues state. It should, by now, be drifting downwards in magnitude after a maximum in late January. Instead, it is rising towards a maximum, who knows when.

The star was discovered by M. Popowa in the early 1960’s, following her analysis of the Sonneberg plate stacks1. Her elements referred to a maximum in 1934 and a period of 297.4 days. The catalogues, both GCVS and VSX, still use these elements; the star hasn’t been much studied since it was discovered.

  1. M. Popowa, “40 Neue Veränderliche,” Astronomische Nachrichten 286 (January 1, 1961): 81 []
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