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Fireball Spectrum
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前田



登録日: 2004.09.01
記事: 2754
所在地: Miyazai JAPAN (E131.4, N31.8)

記事日時: Fri Nov 27, 2015 11:44 pm    記事の件名: spectrum of NTA 引用付きで返信

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



M20151127_222709_JPMZ1_HEPc2.jpg
 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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M20151127_222709_JPMZ1_HEPc2.jpg




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
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登録日: 2004.08.07
記事: 12653
所在地: 139.67E 35.65N

記事日時: Sat Nov 28, 2015 7:38 am    記事の件名: Re: spectrum of NTA 引用付きで返信

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

Shocked Shocked Shocked
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)

記事日時: Sat Nov 28, 2015 4:24 pm    記事の件名: train 引用付きで返信

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



M20151127_222709_JPMZ1_HE_064_1s2.jpg
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M20151127_222709_JPMZ1_HE_064_1s2.jpg


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Martin Dubs



登録日: 2014.03.04
記事: 56

記事日時: Mon Nov 30, 2015 7:44 am    記事の件名: 引用付きで返信

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



M20151124_043551_MAI_2P.jpg
 説明:
Leonid meteor, Watec 902H, f/1.2 7mm, 600L/mm
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M20151124_043551_MAI_2P.jpg



M20151124_043551_IR.png
 説明:
added spectrum, red: without, blue with instrument response applied
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M20151124_043551_IR.png



M20151124_043551.png
 説明:
added spectrum (20 fields) without instrument response applied
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M20151124_043551.png


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前田



登録日: 2004.09.01
記事: 2754
所在地: Miyazai JAPAN (E131.4, N31.8)

記事日時: Wed Dec 02, 2015 12:10 am    記事の件名: 引用付きで返信

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

記事日時: Wed Dec 02, 2015 7:30 am    記事の件名: 引用付きで返信

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



m20151127_222709_jpmz1_hep-d3s4.jpg
 説明:
linearized spectrum, preview scale 0.25
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m20151127_222709_jpmz1_hep-d3s4.jpg



m20151127_222709_jpmz1_hep-d3r3s.jpg
 説明:
linearized spectrum, preview scale 0.5

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Bill W



登録日: 2012.02.13
記事: 182
所在地: Glasgow

記事日時: Fri Dec 18, 2015 6:11 pm    記事の件名: 引用付きで返信

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.



fireball_2015_12_14_0020UT_tenerife_s_small.jpg
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fireball_2015_12_14_0020UT_tenerife_s_small.jpg



fireball_spectrum_20151214_0020UT_tenerife_s_small.jpg
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Martin Dubs



登録日: 2014.03.04
記事: 56

記事日時: Mon Dec 21, 2015 7:13 am    記事の件名: 引用付きで返信

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



1127s3offm15.png
 説明:
spectrum series 100 msec interval
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1127s3offm15.png



1127s3ani_.gif
 説明:
animated spectrum 100 msec time interval between spectra
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1127s3ani_.gif



1127morph.mp4
 説明:
orthographic transformation, peak image

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M20151127_linear_win4.mp4
 説明:
linearized spectrum from avi-file, zero and first order shown

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Bill W



登録日: 2012.02.13
記事: 182
所在地: Glasgow

記事日時: Mon Dec 21, 2015 6:11 pm    記事の件名: 引用付きで返信

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

記事日時: Tue Dec 22, 2015 5:57 am    記事の件名: 引用付きで返信

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



animation_gnuplot.zip
 説明:
example gnuplot script

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Bill W



登録日: 2012.02.13
記事: 182
所在地: Glasgow

記事日時: Tue Dec 22, 2015 7:55 am    記事の件名: 引用付きで返信

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)

記事日時: Fri Jan 08, 2016 9:15 pm    記事の件名: a new year present 引用付きで返信

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



M20160107_225526_JPMZ1_HDPc.jpg
 説明:
Canon EOS6D + 35mmF1.4 + 600 lines grating

trimmed from HD video
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M20160107_225526_JPMZ1_HDPc.jpg


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Martin Dubs



登録日: 2014.03.04
記事: 56

記事日時: Sat Jan 09, 2016 1:05 am    記事の件名: 引用付きで返信

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)

記事日時: Sun Jan 10, 2016 12:44 am    記事の件名: 引用付きで返信

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

記事日時: Sun Jan 10, 2016 6:43 am    記事の件名: 引用付きで返信

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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