Some Lightcurve Results

We have been taking pictures of microlensing targets for 2 months now and in this blog we will show the results of some of our observations on the lightcurve for one of our targets (KB-09-232).

Here is this target's lightcurve before we made our observations, on 11 June 2009


And here it is on 19 June 2009, after we made our observations


The arrows on the graph point out what our group contributed are highlighted in this image. They are shown as blue dots (H- Faulkes North Telescope) and dark green dots (I- Faulkes South Telescope).


The other points on the lightcurve are from observations made by other groups using different telescopes from around the world. The different colour letters on the right hand side of the graph show which points came from which group or telescope. Here is a list of the groups/telescopes and the letter which represents it:

Surveys (groups):
O(OGLE)
K(MOA)

Follow-up (Telescopes):
Z(Danish 1.54m)
A(SAAO 1.0m)
C(CTIO 1.3m)

Overall project summary

This blog entry is a summary of all the work we have done over the two months of our project. There will be one or two more entries after this, but as the blog will be judged by the end of June, we feel it is important for this entry to be posted as soon as possible. We will also continue to observe as regularly as possible, so the following estimates of the work we have done will continue to increase.


We started our project early in May and after a training session with our mentor Greg Hallinan from NUIG we made our first observation on May 11th with the Faulkes Telescope.

We managed to get a total of 14 hours of actual observations done, almost equal in May and June. We were unable to observe about 13 hours of observation time which we had booked, due to the bad weather and telescope malfunctions. During that time we observed just under 20 microlensing targets and made 165 individual observations.

We have 15 blog posts so far. It is impossible to estimate the time we have spent on the blog, as we work on it in our own time, as well as in a group. As we have said before, the blog is divided into 2 aspects: writing the entries and IT. We have all spent a considerable length of time on our blog, especially since we had no previous experience with blogs before.

We have also received an email from the Faulkes Telescope mailing list asking school groups to help with another project involving Pluto. We will post a separate entry to explain our small part in this project.

Our project for this challenge has also been a part of the LCOGT microlensing project. This has been quite enjoyable and a great experience.

So, that is a basic summary of our project so far. It is now time to thank everyone again. Special Thanks to Mr. Ryder and Ms. Herbert for getting us involved in this project. A very important thank you to Gregg Hallinan for choosing such an interesting project that is part of a much larger world wide project. A big thank you to Yiannis Tsapras and Edward Gomez of LCOGT for contacting us, providing support, and helping us with our problems regarding the microlensing targets and lightcurves.

Pluto's Rotational Lightcurve

As part of the BAA (British Astronomical Association) to determine Pluto's rotational lightcurve the schools taking part in the Faulkes challenge have been asked to use a small part of their observing session to image Pluto.


Pluto's rotational lightcurve hasn't been observed since it was studied in 1995 by the Hubble Telescope. Since that time a dwarf planet has moved further away from the sun and there are indications that the cooling of the planet may have caused a change in the atmosphere and/or weather on Pluto, which might very well be visible if the rotational lightcurve is measured. This particular dwarf planet is a very slow rotator taking about 6.4 days to turn once.

The group of astronomers in charge of the faulkes telescope want us to take one RGB image to go towards their research. An RGB image, sometimes referred to as a truecolour image, is a method a taking a picture that defines red, green, and blue color components for each individual pixel. RGB images do not use a palette. The color of each pixel is determined by the combination of the red, green, and blue intensities stored in each color plane at the pixel's location. Which means that they take 1 red, 1 green and 1 blue picture and mix them together to get the real colours.

We attempted to take a picture of Pluto but, unfortunately, the telescope was closed due to bad weather. We will try again during our next session if we are granted more time. It was very exciting and an honor to be asked to help the BAA's campaign and research and we hope to post our picture of Pluto as soon as possible.

This is a good site with information on pluto

Great news and observations

We have been in contact with Edward Gomez of LCOGT these past few weeks, and we have just heard some very nice news. Our team have been contributing greatly to the microlensing project. We have had more success than the actual astronomers! We have been booking the telescope for around 2 o'clock as much as possible (it fits in with lunch and school well). This turns out to be a very lucky turn for us, as we seem to be observing with the clearest skies.

This has made us feel rather proud about our project, as we are just a small school group, but we have been contributing even more than we thought.

Our observing has also been smooth lately. However, with 98% humidity last Friday, and a weather warning today, it is unlikely that we will get our desired 25 pictures today.

There is still no word on the judging of the blog, so we shall continue as we have until we are told otherwise. Even now the judges may be looking at our blog, so we have been tightening things up, and hoping for good news.