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Skywarden,
Ursa Astronomical Association
Kopernikuksentie 1
00130 Helsinki
taivaanvahti(at)ursa.fi

Ursa Astronomical Association

Spektroskooppihavaintoja, Vega, Menkalinam and P Cygni - 10.11.2020 at 01.00 - 10.11.2020 at 05.00 Järvenpää Observation number 94857

Visibility Unclassified

Ari Jokinen, Etelä-Suomen kosmol. seura

Spectroscopic observations, Vega, Menkalinam and P Cygni

I got a Star Analyzer 200l / mm grid a few months ago. The aim is to investigate how to observe the spectra of stars at a relatively cheap lattice in our conditions. Now with some accumulated experience, surprisingly well, however, it succeeds (especially from the spectral class A stars that I have studied several). The software is RSpec whose learning curve is relatively easy. It is important (as is usually the case in star photography) to have the right shutter speed and above all to focus which may cause a bit of a headache as well as reading the correct calibration. I have used non-linear calibration, it produces a good result.

Figure 1 shows the processed raw image of Vega and the spectrum produced by the Star Analyzer, Vega is an A spectral class star with strong hydrogen absorption lines.
Figure 2 shows the intensity curve calibrated and corrected (normalized (= flux density corresponding to the continuous spectrum = 1)) from this raw image.
Figure 3 shows the reference curve (blue) of the AOV spectrum class added to the previous figure, from which it can be examined how well the calibration was successful. The shape of the curve differs because the normalized observation curve (red) is not corrected for the sensitivity of the ccd cell on the curve. The wavelengths of the Hydrogen Balmer series are marked in the pictures

In Figure 4, a similar normalized intensity curve from the Star of the Driver Menkalina, also in the A-spectral class

In Figure 5, an interesting object, i.e. P Cygni himself with a large and wide hydrogen emission at about 6563 Ångström, it came out well with the Analyzer as well. From the point of view of spectroscopy, all Be (e = emission) stars are also interesting because they show noticeable changes in the hydrogen region (e.g. the gas shell expanding around the star in every movement), I will continue to follow them because it seems to be quite possible with this configuration. Ursan Astronomy Basics book good basic information on these things.

It would also be interesting to monitor the light and spectral curves simultaneously. Mainly if there are changes in the light curve, then whether the changes are also noticeable on the spectroscopy side and towards a certain one.

As a device SW 120ED, Atik460Ex with a resolution of about 9Å / pix.

The Star Analyzer must also have been tested in the Jyväskylä region. Is there experience from there.



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Additional information
  • Observation target
    • Deep space object
  • Designation
    • Spektroskooppihavaintoja, Vega, Menkalinam ja P Cygni
    • Luokittelematon
Technical information

SW 120Ed, ATIK460Ex, Star Analyzer 200l / mm

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