/portal/howtos/man_howto_tutorial_data_mining/man_howto_tutorial_data_mining.shtmlprevious | /portal/howtos/man_howto_tutorial_introduction/man_howto_tutorial_introduction.shtmlhome | /portal/howtos/man_howto_tutorial_vo/man_howto_tutorial_vo.shtmlnext |
Sci-EHELMICH-WFI-------#842---Coadd---Sci-54552.5317447-4d2189f46deed79e536 cdbfb0af72ae24187ffd8.fitsPresumably you don't want to type in the full name, so use a wildcard:
awe> c = CoaddedRegriddedFrame.filename.like('*ffd8.fits')[0]Lets have a look at this image, and select a galaxy from it.
awe> c.retrieve() awe> c.display()A SourceList exists for this image:
awe> sl = (SourceList.SLID == 423431)[0]Make a skycat catalog for the image and find the SID of an interesting source.
awe> sl.make_skycat_on_sources()Now overplot the catalog in skycat. Open the file and select Data-Servers ->
Take the source with SID 16246 in the SourceList with SLID 423431.
It is instructive to first read the http://www.astro-wise.org/portal/howtos/man_howto_galphot/man_howto_galphot.shtmlGalphot HOW-TO, in particular to get an idea of the names of classes and methods defined for Galphot.
Isophotes can be fit to sources using the Galphot package. The main classes used to store the information of the fit are GalPhotModel and GalPhotEllipse. Lets follow an example here.
awe> task = GalPhotTask(slid=423431, sids=[16246], commit=1) awe> task.execute() # or awe> dpu.run('GalPhot', slid=423431, sids=[16246], C=1)
awe> m = (GalPhotModel.SLID == 423431).user_only().max('GPID')The methods get_model(), get_residual(), get_science() can be used on a GalPhotModel to visually inspect its quality.
awe> s = m.get_science() awe> s.display() awe> r = m.get_residual() awe> r.display()The fitted ellipses are stored in the model, and they can also be obtained:
awe> m.ellipses[0].rFor a description of the ellipse parameters see the help page of one of the ellipses:
awe> help(m.ellipses[0])You can obtain/visualize the ellipse parameters:
awe> ellipses = m.get_model_parameters() awe> rad = [e['r'] for e in ellipses] awe> pos = [e['pos'] for e in ellipses] awe> pylab.scatter(rad, pos)
For more information see the http://www.astro-wise.org/portal/howtos/man_howto_galphot/man_howto_galphot.shtmlGalphot HOW-TO.
The main classes used to store Galfit models are GalFitModel and a number of classes named e.g. GalFitSeric, each of which is a function that can be fit to the data. See the first section of the http://www.astro-wise.org/portal/howtos/man_howto_galfit/man_howto_galfit.shtmlGalfit HOW-TO for an overview of the important classes defined for using Galfit in Astro-WISE.
awe> task = GalFitTask(slid=423431, sids=[16246], models=[{'name': 'sersic', 'iN': 3, 'free_N': 0}], commit=1) awe> task.execute() # or awe> dpu.run('GalFit', slid=423431, sids=[16246], m=[{'name': 'sersic', 'iN': 3, 'free_N': 0}], C=1)
awe> m = (GalFitModel.SLID == 423431).user_only().max('GFID')
awe> sci = m.get_science() awe> res = m.get_residual() awe> mod = m.get_model() awe> sci.display() etc.
awe> m.show_model_parameters() # or awe> m.info() awe> m.components[0].info()
For more information see the http://www.astro-wise.org/portal/howtos/man_howto_galfit/man_howto_galfit.shtmlGalfit HOW-TO.
/portal/howtos/man_howto_tutorial_data_mining/man_howto_tutorial_data_mining.shtmlprevious | /portal/howtos/man_howto_tutorial_introduction/man_howto_tutorial_introduction.shtmlhome | /portal/howtos/man_howto_tutorial_vo/man_howto_tutorial_vo.shtmlnext |