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Changes in H alpha over past 6 days
The He I 6680 line (approximately 15x weaker than H alpha)
Radial Velocity of both lines (km/s, plotted in system rest frame)
Cheers
Robin
Meteor spectroscopy is possible with the Star Analyser and a wide field camera
http://www.threehillsobservatory.co.uk/astro/spectra_20.htm
but a grating with higher dispersion would be better eg 300 or even 600 l/mm depending on the lens focal length and sensor size. Bill Ward would be able to advise on the optimum setup
https://britastro.org/user/213
Cheers
Robin
Here is how the H alpha line looks currently. (LHIRES 2400 grating, R~15000). Also uploaded to the BAA spectroscopic database
Robin
Latest feedback from Gabriel Murawski based on the spectrum is that this may in fact be a YSO. It is currently being looked at by experts in this area.
Robin
I have posted some information specifically about spectroscopy in the spectroscopy section
https://britastro.org/node/15540
Robin
Hi Tony,
the ARAS forum has a new for sale section now, “Petites Annonces” though there are not really many constructors there.
The astronomical_spectroscopy yahoo group probably has more self builders and I see there was a recent ad there for an L200 for example, you could check with Ken who owns the group if it would be acceptable
Also Stargazers Lounge perhaps where there is some interest in spectroscopy ?
Robin
According to BeSS, it is not catalogued as a Be star unfortunately otherwise there would undoubtedly have been a good history of H alpha spectra of this bright object. Does anyone know why it is not in the Be Star catalogue ?
Robin
Looking in detail at the distribution of these warm pixels in my camera it seems most of them fall between 500-800 ADU, causing the “knee” in the cumulative distribution described in the ARAS thread. They are in fixed positions and only represent ~1 in every 2000 pixels though and are low enough to be corrected by a dark provided they are otherwise well behaved.
Robin
Hi John,
Here is a link to a dark taken under the same conditions as yours using my ATIK 428. This camera is identical except for using a smaller version of the same CCD so should be a direct comparison.
https://drive.google.com/file/d/1QkocrvkQRBCOlTK9NbxOhSVxWMwM7COg/view?usp=sharing
If you have ISIS, it includes a nice feature which you can use to calculate the gain, and noise figures described here
http://www.astrosurf.com/buil/isis/noise/result.htm
These warm pixels are not specifically measured using this technique though. To get the dark current figures quoted by ATIK and measured by Christian Buil, you have to chose a measured area free of warm pixels.
Robin
Hi John,
I remember there was some discussion on the ARAS forum about the long tail of warm pixels seen in cameras with Sony CCD which seems to have got progressively worse with each generation.
http://www.spectro-aras.com/forum/viewtopic.php?f=8&t=1919&p=9871
I recently saw an article somewhere which suggested this was a characteristic of CCD with anti-blooming, a connection had not been aware of before.
Discounting these, the noise figure of these CCD is very good though and they seem to respond well to dark subtraction.
Running at a lower temperature might help. I run my similar ATK428 at -10C all the year round.
Robin
A potential target for a spectrum. mag 15 is just about bright enough for a standard ALPY 600 and a modest (say> 10 inch) aperture.
Robin
Hi Woody,
I have it on my list but have not had a chance to look at it yet. It looks a very crowded field. I make it this one in centre of the DSS image. Is that correct ? From VSX J2000 18 20 12.99 +07 15 52.1
Cheers
Robin
Here is the reduced spectrum. Very noisy but the H alpha emission is clear. The continuum is very red but there is high extinction in this direction. Total galactic E(B-V) is ~1.0 according to IRSA. The Na D line is clear but again that could be Interstellar.
Robin
On it now with the ALPY600. It is very weak but there is clear H alpha in emission. Raw spectrum image (30min) attached
Robin
I wondered this too. A piece of Mg alloy not large enough to have been tracked but enough to produce a trail ?
Robin
Michael Richmond’s on line calculator can be used to estimate the performance of a given setup for example
http://spiff.rit.edu/richmond/signal.shtml
Robin
added replies to #9 and #11 above
(Note to webmaster – we need a quote button so we can keep to a linear thread and not lose replies back up the thread)
Robin
Then you are currently slightly undersampled already and would not want to go any shorter in focal length. Undersampling in photometry is much less desirable than oversampling.
Robin
Yep sorry, factor of 4 out but the ratio (and hence the increased counts) is the same. Changing the magnification (ie focal length) changes the counts per pixel (both star and sky background counts) but makes no different to the counts in the aperture, either the star counts or the sky background counts. The only difference is if you spread the light over more pixelsthan you need to, you increase the camera noise contribution. In practise this is only the thermal noise, not the read noise as you can compensate for this (in CCD cameras) by binning pixels. Thermal noise is very low in modern CCD, particularly at typical exposure times used for photometry so the net effect is that changing focal length does not improve photometry SNR, only increasing the aperture does this
Robin
