The primary factor to consider is the directivity of the parabolic antenna. It is given as:
$$d=\frac{(\pi D)^2}{\lambda^2} \tag 1$$
where D is the diameter of the dish and $\lambda$ is the wavelength of operation, both in the same units.
To convert frequency to wavelength in meters, we use:
$$\lambda=\frac{300}{f} \tag 2$$
where f is the frequency in megahertz.
Since your frequency of interest is 1420 MHz, we apply formula 2 to convert this to a wavelength of 0.211 meters. With a dish diameter of 2.5 meters, formula 1 give us a directivity of:
$$d=\frac{(\pi D)^2}{\lambda^2}=\frac{(\pi 2.5)^2}{0.211^2}=1386$$
We now need to convert this directivity to linear gain. Here the standard antenna formula applies:
$$G=d*e \tag 3$$
where d is the directivity from formula 1 and e is unitless efficiency with a value of 1 indicating 100% efficiency.
Most parabolic antennas have efficiencies in the 60% to 70% range. For a conservative estimate, if we assume a 50% efficiency, the linear gain of your parabolic antenna is 693. We can convert this to dBi gain using:
$$G_{dBi}=10\log_{10}(G) \tag 4$$
which nets ~28 dBi in this case.
With diligence, you may be able to obtain a 70% efficiency which will raise the gain to ~30 dBi.
The beamwidth of the parabolic antenna is given as:
$$\theta\approx\frac{70\lambda}{D} \tag 5$$
The 3 dB beamwidth of your parabolic antenna will therefore be ~6°.
The focal point of a parabolic antenna is given as:
$$f=\frac{D^2}{16c} \tag 6$$
where c is the depth of the parabolic reflector.
You can see from this formula, that it is not a function of wavelength. So the focal point of the dish remains largely the same regardless of frequency.
You now must consider the sensitivity and noise of your receive system and the expected field strength of a 1420 MHz hydrogen marker to determine if this is sufficient gain for your radio telescope operation. There is hope for success as several university students have used a similar configuration for their projects.