Call for monitoring of AG Dra by R. Galis & al.

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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Tim Lester » Tue May 01, 2018 4:38 pm

My result for May 1 compared to my last two recent spectra. Also showing recent drop in Raman feature.

agdra_20180501_138_tlester.png


Tim
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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Christophe Boussin » Tue May 01, 2018 6:00 pm

(message in English at the end)

Bonjour à tous,

Voici ma contribution au suivi de AG DRA à basse résolution (R = 500) ( http://www.astrosurf.com/aras/Aras_Data ... /AGDra.htm )
Les 2 spectres suivants ont été obtenus respectivement les 6 (JJ = 2458215.504) et 24 (JJ = 2458233.419) Avril.

Le spectre du 6 Avril à 23 h 50 TU est le résultat de 6 poses de 300 s
( format PNG dans la base ARAS : http://www.astrosurf.com/aras/Aras_Data ... 06_993.png )
( format FITS dans la base ARAS : http://www.astrosurf.com/aras/Aras_Data ... 06_993.fit )

_agdra_20180406_993_Christophe Boussin_3700_7570.png
spectre AG DRA 6 Avril 2018
_agdra_20180406_993_Christophe Boussin_3700_7570.png (59.54 KiB) Viewed 554 times


Le spectre du 24 Avril à 21 h 48 TU est obtenu à partir de 5 poses de 300 s
( format PNG: http://www.astrosurf.com/aras/Aras_Data ... 24_909.png )
( format FITS: http://www.astrosurf.com/aras/Aras_Data ... 24_909.fit )

_agdra_20180424_909_Christophe Boussin_3700_7570.png
spectre AG DRA le 24 Avril 2018
_agdra_20180424_909_Christophe Boussin_3700_7570.png (65.08 KiB) Viewed 554 times


Les raies identifiées avec Plotspectra sont les suivantes :

spectre_agdra_20180424_909_Christophe Boussin.png
spectre AG DRA 24 Avril 2018


L'animation ci-dessous permet de mieux apprécier l'évolution des intensités relatives des raies, en particulier les raies HeII (4686) et Hbeta (4861) entre ces 2 dates.

_agdra_20180406 et 20180424_Christophe Boussin_3700_7570.gif
Comparaison des spectres AG DRA les 6 et 24 Avril 2018
_agdra_20180406 et 20180424_Christophe Boussin_3700_7570.gif (85.01 KiB) Viewed 554 times


Bon ciel à tous,

Christophe Boussin

***********************

Hello everyone,

Here is my contribution to the monitoring of AG DRA at low resolution (R = 500) (http://www.astrosurf.com/aras/Aras_Data ... /AGDra.htm)
The two following spectra were obtained respectively the 6 (JJ = 2458215.504) and 24 (JJ = 2458233.419) April.

The spectrum of 6 April at 23 h 50 TU is the result of 6 x 300 s acquisitions
(PNG format in the ARAS base: http://www.astrosurf.com/aras/Aras_Data ... 06_993.png)
(FITS format in the base ARAS: http://) http://www.astrosurf.com/aras/Aras_Data ... 06_993.fit)

The spectrum of 24 April at 21 h 48 TU is obtained from 5 x 300 s acquisitions
(PNG format: http://www.astrosurf.com/aras/Aras_Data ... 24_909.png)
(FITS format: http://www.astrosurf.com/aras/Aras_DataBase/Symbiotics) /FitFiles/asdb_agdra_20180424_909.fit)

The lines identified with Plotspectra are the following (see at the top).
The animation at the top allows you to better appreciate the evolution of the relative intensities of the lines, especially HeII (4686) and Hbeta (4861 ) between these 2 dates.

Clear skies,

Christophe Boussin
CBO (Newton 200 F/5 / Alpy600 / Atik 314L+ / Atik Titan) @ ARAS database
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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Francois Teyssier » Tue May 01, 2018 6:12 pm

Status of the campaign

AGDra.JPG
AGDra.JPG (19.58 KiB) Viewed 553 times


AAVSO: mean day values.
ARAS Spectra; blue dots

From AAVSO data, the target looks returning to quiescent state. Thus, short outburst.

Of course, we undergo the monitoring. Target: one spectrum/day at least
Thanks to all for your contribution

All the best,

François Teyssier
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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Hubert Boussier » Wed May 02, 2018 7:50 am

Bonjour,
Ne disposant pas d'un spectro, le week-end dernier je me suis amusé à faire deux spectres en très basse résolution avec un SA200 les 24,25 et 26 avril.
J'avais un peu oublié la procédure de traitement avec un star analyseur, finalement par rapport au LISA, l'étalonnage et la réponse instrumentale ont été plus laborieux à faire et j'ai dû m'y reprendre plusieurs fois pour obtenir quelque chose qui approche le profil spectres postés sur AG Dra.
La résolution est entre 150 et 200
Image
Image
Image

Image

La comparaison des profils du 24 et 26 montre que le résultat de l'étalonnage n'est pas encore idéal.

Bon ciel à tous
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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Christian Buil » Wed May 02, 2018 11:10 pm

My latest observation (1.83/05/2018) and evolution:

Image

Image

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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Francois Teyssier » Fri May 04, 2018 4:57 pm

My series

raman OVI almost stable

agdra_OVI.png
agdra_OVI.png (48.53 KiB) Viewed 473 times


Variations of the width of He II

agdra_HeII.png
agdra_HeII.png (17.43 KiB) Viewed 473 times


agdra_Hb.png
agdra_Hb.png (16.73 KiB) Viewed 473 times


Significant variations of He I lines (singlets and triplets)

He I 5876
agdra_HeI576.png
agdra_HeI576.png (18.72 KiB) Viewed 473 times


He I 6678
agdra_HeI6678.png
agdra_HeI6678.png (21.12 KiB) Viewed 473 times




Pour mémoire, behavior of Raman OVI during the short and weak 2016 outburst

agdra_ovi_2017.JPG
agdra_ovi_2017.JPG (58.71 KiB) Viewed 472 times


in Eruptive Stars Information Letter :


François
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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Francois Teyssier » Thu May 10, 2018 10:10 am

Uopdate on the campaign and current outburst

Luminosity curves since 2016 Green = V band Blue= B-V
Outburts occured on April 2016, May 2017 (weak) and May 2018
AGDra_V1.JPG
AGDra_V1.JPG (36 KiB) Viewed 381 times


Current status
AGDra_V2JPG.JPG
AGDra_V2JPG.JPG (21.9 KiB) Viewed 381 times

Good coverage.
Message from Jaroslav: According to photometric observations of AG Draconis obtained in previous days, outburst is not over yet and the brightness continues to increase. This is very interesting behavior because of not a very steep increase in brightness. Moreover, AG Dra slowly achieves the values similar to the maximal brightness during 2016 outburst.
Spectroscopic coverage of the outburst is very good. Thanks to all which have so far been involved. Keep up the good work!


FWHM and EW of He II line
AGDra_HeII.JPG
AGDra_HeII.JPG (31.48 KiB) Viewed 381 times


All the best,

François
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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Peter Somogyi » Sun May 13, 2018 5:09 pm

Hello,

I've managed to process all of my 3 nightly series (already available on the database) into form of EWs.
As a new addition, I've extracted Pearson-correlation on the EW-serie between 2 features - in order to see which features are changing together (important to keep in mind: not absolutely).
See the calculated correlation values table in the bottom-right corner per nightly serie (here R1 denotes Raman OVI 6825 and R2 = Raman OVI 7083):
agdra.png
agdra.png (58.98 KiB) Viewed 286 times

The 3 graphs are scaled to show equal time differences (a similar night window).
The first 2 series were happening at beginning 2 nights of outburst, and 04.30 is special as the Raman OVI-feature was being at lowest.
Conclusion: at different phase we can see different correlations between the feature changes (at the beginning H-alpha is correlating highly with R1, whilst on 04.30 it's near to 0). The correlation between R1 and R2 is something expected. As for HeI 7065, I am suspecting continuum determination noise might be present on it (and maybe on R2), perhaps I could work on this harder in the future.
Error estimate was brought out by measuring a nearby continuum region per-feature, and taking a whole serie's EW stddev precisely.

- Peter
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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Francois Teyssier » Tue May 15, 2018 5:10 pm

An update: finally AG Dra is fading quickly at V = 9.5 (14-05)
AGDra_V3.JPG
AGDra_V3.JPG (21 KiB) Viewed 225 times

Of course, we undergo the monitoring
François
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Re: Call for monitoring of AG Dra by R. Galis & al.

Postby Peter Somogyi » Tue May 15, 2018 7:18 pm

Hello Benji,

The Pearson-correlation is more about a choice of convenience (here I used GDL's 'correlate' function, being at hand).

I'm wondering which error estimate method spc_ew is using (need a math formula or algorithm details).
The article "Chalabaev, A. and Maillard, J.P. 1983, A&A, 127, 279" (the eps-Aur project you mentioned referring to) focuses on analysis of some Be stars H-alpha variability, but can't find any final conclusion which formula to be used in general.
AG Dra is different in many ways (features shape are not gaussian, shortterm variance) so not sure if these theories apply here.

Cheers,
Peter
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