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前田
登録日: 2004.09.01 記事: 2754 所在地: Miyazai JAPAN (E131.4, N31.8)
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日時: Fri Nov 27, 2015 11:44 pm 記事の件名: spectrum of NTA |
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Hi,
I got the NTA fireball (Mag -4, Dur.1.7sec) tonight. It has an interesting light curve which is some small explosions in the trail. The fireball had a short duration train which spectrum is mainly Na line.
I have gotten many spectra of Tau shower but this is the first fireballs in this season.
Best regards,
Koji
説明: |
SONY A7s + 24mmF1.4 with 600 lines/mm grating
Trimming from 4K 30p video and compressed about 50%
Background is Pegasus. |
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最終編集者 前田 [ Sat Nov 28, 2015 4:36 pm ], 編集回数 2 回 |
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SonotaCo Site Admin
登録日: 2004.08.07 記事: 12653 所在地: 139.67E 35.65N
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日時: Sat Nov 28, 2015 7:38 am 記事の件名: Re: spectrum of NTA |
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前田 wrote: | Hi,
I got the NTA fireball (Mag -4, Dur.1.7sec) tonight. It has an interesting light curve which is some small explosions in the trail. The fireball had a short duration train which spectrum is mainly Na line.
I have gotten many spectra of Tau shower but this is the first fireballs in this season.
Best regards,
Koji |
This will be the reference !!
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前田
登録日: 2004.09.01 記事: 2754 所在地: Miyazai JAPAN (E131.4, N31.8)
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日時: Sat Nov 28, 2015 4:24 pm 記事の件名: train |
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It's thanks to you, SonotaCo.
This is one of the best oneand well composed.
-----
This is one frame picture from the video. We can see a long train, and it shows mainly Na line.
Koji
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Martin Dubs
登録日: 2014.03.04 記事: 56
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日時: Mon Nov 30, 2015 7:44 am 記事の件名: |
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Hi Koji,
this is an excellent spectrum, one of the nicest I have ever seen. I would like to use my calibration method on it and use the result for a presentation on meteor spectroscopy. As far as I can see you have used the same equipment as in your previous spectrum, so the calibration should be quite easy. My own results are disappointing in comparison, but I have made some progress applying the instrument response to calibrate the line intensities in relative flux. A first example is given below. I used a Venus spectrum for the determination of the instrument response, recorded shortly afterwards, as it was nearby at the time.
Best regards, Martin
説明: |
Leonid meteor, Watec 902H, f/1.2 7mm, 600L/mm |
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added spectrum, red: without, blue with instrument response applied |
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added spectrum (20 fields) without instrument response applied |
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前田
登録日: 2004.09.01 記事: 2754 所在地: Miyazai JAPAN (E131.4, N31.8)
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日時: Wed Dec 02, 2015 12:10 am 記事の件名: |
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Hello Martin,
Thank you for your comment. The equipment is the same of my spectrum on July 27th.
This spectrum picture was trimmed from original image. I will send you the original one. Please check again.
As you say, calibration of sensitivity on wave length is important to classify a spectrum. I have use alpha AUR or alpha CMa , but I don’t have much experience.
Koji
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Martin Dubs
登録日: 2014.03.04 記事: 56
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日時: Wed Dec 02, 2015 7:30 am 記事の件名: |
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Hi Koji,
I made a quick test to linearize your spectrum, using the same parameters as for the spectrum M20150729. Linearity of the spectrum is within +/- 2 nm, but this can be improved considerably.
So this is only a preview.
Regards, Martin
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linearized spectrum, preview scale 0.25 |
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linearized spectrum, preview scale 0.5 |
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m20151127_222709_jpmz1_hep-d3r3s.jpg |
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Bill W
登録日: 2012.02.13 記事: 182 所在地: Glasgow
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日時: Fri Dec 18, 2015 6:11 pm 記事の件名: |
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Hi,
Had 4 good nights observing from Tenerife. There was some cloud on 2 of the nights but it was a great short winter break with plenty of sun during the day!
Here is a time lapse of all of the wide field shots I took compiled into a short time lapse.
https://www.youtube.com/watch?v=rL_emFIjSPM
I did catch a single fireball and it's spectrum but it's very poor and it shows the clear advantage of video over integrated still images. Reducing the spectrum is almost impossible with all the "contamination" from the field stars.
Merry Christmas and a good new year (with plenty of clear skies) to all.
cheers,
Bill.
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Martin Dubs
登録日: 2014.03.04 記事: 56
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日時: Mon Dec 21, 2015 7:13 am 記事の件名: |
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Hello,
once again Koji's spectrum (thanks for permitting to use his data to show the power of the method to linearize meteor spectra) and the result of the analysis.
Note that all spectra have been extracted from the transformed images with the same linear dispersion (0.624 nm/pixel)
In the spectrum movie the train is well visible, the individual images were registered to the zero order of the meteor.
Have fun,
Martin
説明: |
spectrum series 100 msec interval |
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animated spectrum 100 msec time interval between spectra |
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orthographic transformation, peak image |
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1127morph.mp4 |
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linearized spectrum from avi-file, zero and first order shown |
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M20151127_linear_win4.mp4 |
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Bill W
登録日: 2012.02.13 記事: 182 所在地: Glasgow
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日時: Mon Dec 21, 2015 6:11 pm 記事の件名: |
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Hi Martin,
NICE!
I don't know whether it is an installation problem or something else (probably me being stupid!) but I have been trying to make similar "movies" without success with Visual Spec for quite a while. I just can't seem to get them to run properly.
Do you do it directly through GNUplot or by some other means?
cheers,
Bill.
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Martin Dubs
登録日: 2014.03.04 記事: 56
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日時: Tue Dec 22, 2015 5:57 am 記事の件名: |
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Hi Bill,
for the animation of spectra I modified an ISIS script for gnuplot.
I ran the script directly in Gnuplot.
I am no expert in it, so I try modifying running examples. Maybe my template is of use to you.
Best regards, Martin
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animation_gnuplot.zip |
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Bill W
登録日: 2012.02.13 記事: 182 所在地: Glasgow
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日時: Tue Dec 22, 2015 7:55 am 記事の件名: |
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Hi,
Thanks!, that's exactly the same strategy I was using with the script as provided from Visual Spec.
But somethings not happy somewhere....
I'll give yours a go.
Thanks again,
Cheers,
Bill.
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前田
登録日: 2004.09.01 記事: 2754 所在地: Miyazai JAPAN (E131.4, N31.8)
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日時: Fri Jan 08, 2016 9:15 pm 記事の件名: a new year present |
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Hi,
I got a typical Fe-type spectrum last night by HD video. This type
meteor is usually dark, but this meteor was a likely fireball brightness.
The brightest star and spectrum in the image is alpha CMa. The magnitude
of the meteor can not evaluate for a lack of zero order image.
I have the first time to observe a bright Iron meteroids.
This is a new year present for us.
Have a good night,
Koji Maeda
説明: |
Canon EOS6D + 35mmF1.4 + 600 lines grating
trimmed from HD video |
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Martin Dubs
登録日: 2014.03.04 記事: 56
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日時: Sat Jan 09, 2016 1:05 am 記事の件名: |
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Hi Koji,
congratulations to your nice spectrum. Here in Switzerland I have not been so lucky lately, besides your equipment is much superior. What a good luck that you also recorded alp CMa. This can be used to determine the instrument response. With the instrument response the spectrum can be flux calibrated, the next step in the processing after wavelength calibration. The magnitude of the meteor can then be determined by a weighted integration of the flux calibrated spectrum. I have done that for stellar spectra, in particular for the nova Delphini 2013. The method is described here (the zero order is not needed for that):
http://www.spectro-aras.com/forum/viewtopic.php?f=5&t=682&p=3099#p3099
Actually I used the method there to calculate the flux from observed magnitude, but the method works both ways.
If you put the zipped avi into Dropbox, I might give it a try, since I do not have any better meteor spectra to test the method on a meteor spectrum.
Regards, Martin
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前田
登録日: 2004.09.01 記事: 2754 所在地: Miyazai JAPAN (E131.4, N31.8)
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日時: Sun Jan 10, 2016 12:44 am 記事の件名: |
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Hi Martin,
Thank you for your comment. Sure, we can evaluate the magnitude from a calibrated spectrum. I really thought that it was difficult to carry it out. Please try to calculate from this sample.
Regards,
Koji
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Bill W
登録日: 2012.02.13 記事: 182 所在地: Glasgow
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日時: Sun Jan 10, 2016 6:43 am 記事の件名: |
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Koji, Another great result.
I've been running one of my cameras with an 830 g/mm grating on it and I caught only the second useable spectrum the other night.
The dispersion is just under 1nm/pixel and the effective resolution is ~2nm. I'm quite pleased with this improved performance.
The spectrum ran through the text field at the bottom of the fov so initially only had a look at the visible end. This is the first graph and synthetic version. The lines are quite nicely resolved for a video shot I think.
I noticed some extra lines in the near IR, these, I think these are strong emissions from Ca+ but produced by the overlapping second order. With the second order giving twice the dispersion, measuring the lines gives a separation twice that of what would be seen in the first order. This comes out to be an almost perfect match!
The second graph is the near IR section with the Ca+ lines and what might be Cr or Fe marked. Some of the other faint lines may well be Fe from the second order too. I've re-coloured the blue lines in the sythetic version. Thats what it might look like if our eyes could see the near UV and the near IR as well! The lines in the near IR graph are quite a bit broader due to de-focus. My systems are focussed on the blue green part
Cheers,
Bill.
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