NGC 3115, George Vander Tuig
In finding the best fit for the light profile I found that it is not just a simple logarithmic fit, as an elliptical galaxy would be. Rather, it is broken up into 3 distinct sections. After plotting the profile on a logarithmic scale I found that the graph has 3 sections having perfect linear fits. One guess is that these sections represent the parts of the bulge and the disk. These findings confirm that this galaxy is neither an elliptical nor a spiral, but it is in fact an intermediate form.
For further study of my galaxy I tried to fit the profile as if it were a spiral galaxy,with a disk that decreases exponentially in brightness. I found that there is a linear correlation at a radius of 1.75 kpc and beyond. From this it could be concluded that the bulge begins as far away as 1.75 kpc from the center. This is a depiction of the massive size of this galaxy.
This image is taken by the 2MASS telescope, taken in the near infrared.This image is not drastically different from the color combined image, though it does have a nicely defined circular bulge.
This is the rotation curve graph for NGC 3115. The rotation curve shows us the orbital velocity of the galaxy based on its distance from the center. Using this we can see the distribution of mass in the galaxy. We see that the graph levels out for the majority of the time indicating that there is more mass out there that is not generating any light that we could have picked up in the light profile. This illustrates the effects of dark matter. Also by using this graph we can visibly see the distance of the bulge from the center in kpc. It does seem to confirm that the bulge begins in the vicinity of 1.75 kpc.
This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Description of Data Reduction
The image has a gamma level of 0.3, a minimum of 35 and a maximum of 10000.
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