Project 1.

Participant Name: Ignasi Reichardt

Project description: Identification of possible counterparts for transient gamma-ray sources

Several times per week, X-ray and gamma-ray satellites like Swift or Fermi alert a number of facilities interested in transient sources. Most often, the source happens to be a GRBs, but can also be due to galactic transients or AGN outbursts, for instance. When possible, such alerts are followed by ground based gamma-ray (Cherenkov) telescopes. In any case, the angular resolution of high-energy facilities is poor compared to that of X-ray, optical, etc. and the nature of the flaring object often remains unkonwn. In this project I suggest to:

  1. Select non-GRB burst alerts from GCN (for instance). If it existed an integrated tool inside VO it would be very nice, but I don't know it.
  2. Look for known sources in other wavelengths inside the 68% confidence contour of the gamma-ray source with the following filters:
    • Redshift lower than 0.5 OR
    • Galactic latitude lower than 9║ in case redshift is unknown
  3. Check broad band spectral energy distributions of selected sources. Reject those with no hint of a non-thermal component.
  4. Check light curves of remaining sources. Reject those with no hint of variability.
  5. Produce a list of "Targets of Opotunity" for Cherenkov telescopes.


Project 2.

Participant Name : Nicolas Laporte

Project description : Search for high redshift galaxies (z>6)

During the last decade considerable advances have been made in the exploration of the early Universe, from the discovery and detailed studies of redshift z=4 galaxies, to galaxies at z>6, close to what is believed to be the end of reionization epoch of the Universe . But the instrumental constraints to perform this research are very strong, for example we must work with pictures at very large depth (25 mag in H band) and in several bands. It's why the numbers of multi-wavelength surveys with these properties is very weak. The VO can help to group all data with good depth and to increase the numbers of interesting surveys. The project that I suggest is the following :

  • create a catalog of objects from pictures in several bands (particularly in bands Y,J, H and K with a large depth ).
  • find objects which are detected at large wavelengths and not detected in visible. (Objects must be detected in more than one filters to conclude).
  • apply to these objects a color-color selection (diagrams JHK, YJH, IzY ,...)
  • determine the photometric redshift with a SED fitting method.


Project 3.

Participant Name: Tiina Liimets

Project description: Measuring the expansion of the nova remnant GK Per in real-time

GK Per (aka Nova Persei 1901) was discovered in 1901 when a rare bright classical nova explosion occurred. Soon after the nova outburst superluminal light echoes where observed, which was the first time ever astronomers witnessed this geometrical illusion. 15 years later the actual nebular shell around Nova Persei finally became visible. This expanding nova remnant has turned out to be the longest living and most energetic among classical novae and appears more like a supernova remnant in miniature but evolving on human time-scales. The remnant is expanding 1" per year which means it is detectable with data obtained with a separation of just a couple of years.

1. Search imaging data of GK Per (RA=03 31 11.82 DEC=+43 54 16.8) from different dates and telescopes with following constraints:

  • observations done in narrow band filters Halpha or [N II] ,
  • data has to be older than 2004 (I have newer data which can be used for completeness of the analysis),
  • FOV at least 2x2 arcminutes.

2. Reduce the data if not done already. Note: for the purpose of this project data can also be not reduced.

3. Crop the images to have a similar size in the sky.

4. Choose an appropriate astrometrical catalogue and make a list of stars in the field of GK Per and register all images. I can provide a script (IRAF+Python) which can do the astrometry once the list of stars is ready. Note: images can be deep therefore also fainter stars are usable for astrometrical solution.

5. Choose a reference image from earlier dates and match others to it so that they all have the same pixel size and stars fall into a same place on all frames. I can provide a procedure to do it in IRAF.

6. Make a movie (for example in DS9) from the images to show the expansion of the nebula.

7. If there is more time, make a study on how big the expansion is of the individual knots/spikes in the nebula.


Project 4.

Participant Name: Elisabeta Lusso

Project description: Multiwavelength analisys of Type 2 AGN selected

1. Create a catalog of X-ray selected Seyfert galaxy (Sy type > 1.5-2.0) detected with INTEGRAL and Swift surveys

2. Search for multiwalength information (from radio and far-IR to UV)

3. Compute color-color diagrams

4. Compute the broad-band SED for each source

5. SED fitting in order to deconvolve the host galaxy using a set of host galaxy templates.

- - - - -

Project 5.

Participant Name: Paloma InÚs MartÝnez Navajas

Project description: Spectroscopic redshift in the CDFS

1. Search for objects with spectroscopic redshift in CDFS

2. Create a catalogue of X-Ray, IR and radio sources in this area

3. Create a z - Right Ascension diagram for see the distribution

4. Search for information of these objects

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Project 6.

Partecipant Name: Claudia Greco

Project Description: Archival data as a resource to study Variable stars in Star Clusters

The identification, analysis and classification of variable stars in star clusters
-- either globular clusters or open clusters -- is a demanding task, based on the
collection and the combination of long time series of the same field of observations
(FOO), each one containing several stars.
In this context, archive information are fundamental to complete the informations
and, in some case, to confirm the classification.
In this short project, I suggest two complementary approaches that may be useful in studies involving
variable stars.
Approach 1: Given a certain star cluster of interest:
a) get photometric catalogues of the FOO and find easy solutions to calibrate our own data to a
standard system;
b) get astrometric catalogue of the FOO and find easy solutions to have precise sky
coordinates of the stars within;
c) for each star in the fdo, check if more informations are available: spectroscopical
studies, proper motions, radial velocity, chemical composition, period, etc..;
d) learn if the FOO has ever been observed by a survey and which additional information we can get from it;
e) learn if time series are available for some stars in the FOO;
f) get the proper references.

Approach 2:Given a certain type of variable star:
a) Get a list of all the example of this type ever identified in the literature;
b) Get about them more more information: see 1.c
c) Learn if time series are available for some of these examples.

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Example Projects

-- MarkAllen - 18 Dec 2009

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