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Eruptive stars spectroscopyCataclysmics, Symbiotics, Novae

ARAS Eruptive StarsInformation Letter n° 35 #2017-05 29-06-2017

Observations of May 2017

Contents

F. Teyssier, S. Shore, R. Gàlis, J. Guarro, D. Boyd, P. Somogyi, O. Garde, W. Sims, T. Lester, C. Buil, P. Berardi, U. Sollecchia, F. Campos, P. Luckas, T. Bohlsen, J. Foster, J. Montier, T. Rodda, F. Boubault, J. Edlin, M. Verlinden, C. Kreider, J. West, E Bertrand

NovaeNova Cen 2017 observed by Paul Luckas (ATel) and Terry Bohlsen

Symbiotics

Ongoing campaign CH CygniAG Dra campaign: faint and weak outburst in MayNew burst of BF Cyg SU Lyn: monitoring of the newly discovered symbiotic

V694 Mon: new resultsCall for spectroscopic monitoring in AAVSO Alert Noticeby Adrian Lucy and Jeno Sokolovski: p. 51

SupernovaeBright Type IIp supernova SN 2017 eaw in NGC 6946

AG Dra campaign, Rudolf Galis p. 10

Steve’s notes: Novae: the effects of dust formation on line profiles Absorption line fine points: the Balmer decrement and theterminal absorption velocityp. 56-60

“We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this letter.”Kafka, S., 2015, Observations from the AAVSO International Database, http://www.aavso.org

Authors :

Nova Cen 2017NOVAE

Coordinates (2000.0)R.A. 13 20 55.32Dec -63 42 18.5Mag V 10.9 V (discovery)

http://www.astrosurf.com/aras/Aras_DataBase/Novae/2017_NovaCen2017.htm

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ASASSN-17gk 2017-05-18 10:16:49 R = 536 Paul Luckas

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10-12 Nova Cen 2017 2017-05-27 10:47:58 R = 978 Terry Bohlsen

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Nova Cen 2017 (V)

Nova Cen 2017 = ASSASN-17gkwas discovered in images obtained on 2017-05-17.28 at V~10.9 (ATel 10387)Paul Luckas got a confirmation spectrum (ATel #10339) See page 60

AAVSO light curve (V) and spectra in ARAS database

ARAS Eruptive Stars Information Letter 2017-05 - p. 2

http://www.astrosurf.com/aras/Aras_DataBase/Novae/2017_NovaCen2017.htm

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ASASSN-17gk Paul Luckas

2017-05-18.428

2017-05-19.436

2017-05-20.585

2017-05-21.520

2017-05-28.428

2017-05-29.456

2017-05-30.530

2017-05-31.470

2017-06-02.575

2017-05-22.433

2017-05-26.449

2017-05-27.440

2017-06-04.476

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Nova Cen 2017 (V)

Nova Cen 2017NOVAE

Monitoring of the first decline by Paul Luckas(LISA R = 1000) with an interesting oscillation at maximum luminosity


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SN 2017 eawSUPERNOVAE

2017-05-23.924

2017-05-29.043

2017-05-15.014

2017-05-25.065

2017-05-27.883

2017-06-03.226

Coordinates (2000.0)R.A. 20 34 44Dec +60 11 35.9Mag V 13

2017-05-20.970

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SN2017 eaw(V)

AAVSO V light curve and ARAS spectra

Discovered by Patrick Wiggins (Tooele, UT) at unfiltered CCD magnitude ~12.8on 2017 May 14.2383 UTThe supernova is located 153” NW of the center of NGC 6946. SN 2017eaw is Type II supernova (ATel #10374), more precisely Type IIP (ATel #10376)

Spectroscopic evolution in May from spectra ob-tained (bottom)

2017-05-15 : Etienne Bertrand2017-05-20 : Christian Buil2017-05-23 : Fran Campos2017-05-25 : Jacques Montier2017-05-27 : Paolo Berardi2017-05-29 : Peter Somogyi2017-06-03 : Jim Edlin


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10-14 SN 2017eaw 2017-05-27 21:10:54 R = 639 Paolo Berardi

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sn2017eaw 2017-05-29 01:01:52 R = 473 P. Somogyi

SN 2017 eawSUPERNOVAE

Radial velocities of Balmer linesby Peter Somogy in his spectrum obtained on 2017, May 29red: H-alphagreen: H-beta,blue: H-gammapurple: H-delta


Symbiotics in May

Observing : main targets

AG Dra: weak ouburst mid-May - Excellent coverage following R. Gàlis request - We continue the moni-toring at a lower cadency - at least one spectrum a week

CH Cygni : ongoing campaign upon the request of Augustin Skopal and Margarita Karovska CH Cygni is strongly rising

SU Lyn: observations requested by Katarzyna Drozd (Nicolaus Copernicus Astronomical Centre) V694 Mon: still in ‘quiescent’ stage - Observations requested by J. Sokolovski and

SYMBIOTICS


Name AD (2000) DE (2000)AG Dra 16 1 40.5 +66 48 9.5AG Peg 21 51 1.9 +12 37 29.4AX Per 01 36 22.7 +54 15 2.5BF Cyg 19 23 53.4 +29 40 25.1BX Mon 07 25 24 -03 36 00CH Cyg 19 24 33 +50 14 29.1CI Cyg 19 50 11.8 +35 41 03.2EG And 00 44 37.1 +40 40 45.7R Aqr 23 43 49.4 -15 17 04.2RS Oph 17 50 13.2 -06 42 28.4SU Lyn 06 42 55.1 +55 28 27.2T CrB 15 59 30.1 +25 55 12.6V443 Her 18 22 8.4 +23 27 20V694 Mon 07 25 51.2 -07 44 08Z And 23 33 39.5 +48 49 5.4

Have a look on classical symbiotics V443 Her, YY Her and recurrent nova RS Oph

BF Cygni : high luminosity (Mag V ~ 9.3)

AG Peg: in the morning sky

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BF Cygni (V)7

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92457600 2457690 2457780 2457870 2457960

CH Cygni (V)

ARAS Data Base Symbiotics : http://www.astrosurf.com/aras/Aras_DataBase/Symbiotics.htm

Symbiotics in ARAS Data Base Update : 05-06-2017SYMBIOTICS

ARAS Eruptive Stars Information Letter 2017-05 - p. 7 ARAS Eruptive Stars Information Letter 2017-05 - p. 7

48 stars2603 spectra

# Name AD (2000) DE (2000) Nb. of spectra First spectrum Last spectrum Days Since Last

1 EG And 0 44 37.1 40 40 45.7 70 12/08/2010 14/02/2017 1112 AX Per 1 36 22.7 54 15 2.5 160 04/10/2011 02/04/2017 643 V471 Per 1 58 49.7 52 53 48.4 7 06/08/2013 20/02/2017 1054 Omi Cet 2 19 20.7 -2 58 39.5 12 28/11/2015 09/02/2017 1165 BD Cam 3 42 9.3 63 13 0.5 27 08/11/2011 09/02/2017 1166 UV Aur 5 21 48.8 32 30 43.1 57 24/02/2011 18/04/2017 487 V1261 Ori 5 22 18.6 -8 39 58 11 22/10/2011 26/03/2017 718 StHA 55 5 46 42 6 43 48 2 17/01/2016 25/01/2016 4979 SU Lyn 06 42 55.1 +55 28 27.2 60 02/05/2016 24/05/2017 12

10 ZZ CMi 7 24 13.9 8 53 51.7 46 29/09/2011 30/04/2017 3611 BX Mon 7 25 24 -3 36 0 45 04/04/2011 11/04/2017 5512 V694 Mon 7 25 51.2 -7 44 8 207 03/03/2011 07/05/2017 2913 NQ Gem 7 31 54.5 24 30 12.5 59 01/04/2013 18/04/2017 4814 GH Gem 7 4 4.9 12 2 12 5 10/03/2016 20/02/2017 10515 CQ Dra 12 30 06 69 12 04 18 11/06/2015 12/05/2017 2416 TX CVn 12 44 42 36 45 50.6 43 10/04/2011 28/05/2017 817 IV Vir 14 16 34.3 -21 45 50 3 28/02/2015 20/06/2016 35018 T CrB 15 59 30.1 25 55 12.6 201 01/04/2012 31/05/2017 519 AG Dra 16 1 40.5 66 48 9.5 307 03/04/2013 04/06/2017 120 V503 Her 17 36 46 23 18 18 2 05/06/2013 13/08/2016 29621 RS Oph 17 50 13.2 -6 42 28.4 35 23/03/2011 27/05/2017 922 V934 Her 17 6 34.5 23 58 18.5 21 09/08/2013 02/05/2017 3423 AS 270 18 05 33.7 -20 20 38 2 01/08/2013 02/08/2013 140324 YY Her 18 14 34.3 20 59 20 21 25/05/2011 28/05/2017 825 FG Ser 18 15 6.2 0 18 57.6 3 26/06/2012 24/07/2014 104726 StHa 149 18 18 55.9 27 26 12 3 05/08/2013 14/10/2015 60027 V443 Her 18 22 8.4 23 27 20 35 18/05/2011 28/05/2017 828 FN Sgr 18 53 52.9 -18 59 42 4 10/08/2013 02/07/2014 106929 BF Cyg 19 23 53.4 29 40 25.1 114 01/05/2011 27/05/2017 930 CH Cyg 19 24 33 50 14 29.1 452 21/04/2011 28/05/2017 831 V919 Sgr 19 3 46 -16 59 53.9 2 10/08/2013 10/08/2013 139532 V1413 Aql 19 3 51.6 16 28 31.7 6 10/08/2013 31/10/2016 21733 V335 Vul 19 23 14 +24 27 39.7 7 14/08/2016 31/10/2016 21734 HM Sge 19 41 57.1 16 44 39.9 9 20/07/2013 26/08/2016 28335 QW Sge 19 45 49.6 18 36 50 7 14/08/2016 31/10/2016 21736 CI Cyg 19 50 11.8 35 41 3.2 136 25/08/2010 26/05/2017 1037 StHa 169 19 51 28.9 46 23 6 2 12/05/2016 14/05/2016 38738 V1016 Cyg 19 57 4.9 39 49 33.9 12 15/04/2015 01/12/2016 18639 PU Vul 20 21 12 21 34 41.9 12 20/07/2013 06/10/2016 24240 LT Del 20 35 57.3 20 11 34 4 28/11/2015 16/05/2017 2041 ER Del 20 42 46.4 8 40 56.4 5 02/09/2011 31/08/2016 27842 V1329 Cyg 20 51 1.1 35 34 51.2 8 08/08/2015 26/12/2016 16143 V407 Cyg 21 2 13 45 46 30 12 14/03/2010 18/04/201044 StHa 190 21 41 44.8 2 43 54.4 17 31/08/2011 30/10/2016 21845 AG Peg 21 51 1.9 12 37 29.4 201 06/12/2009 25/01/2017 13146 V627 Cas 22 57 41.2 58 49 14.9 20 06/08/2013 24/03/2017 7347 Z And 23 33 39.5 48 49 5.4 78 30/10/2010 18/02/2017 107

http://www.astrosurf.com/aras/Aras_DataBase/Symbiotics.htm

Symbiotics observed in May, 2017 SYMBIOTICS


# name Observer Date R # name Observer Date R

AG Dra W. Sims 01/05/2017 3866 7451 776 BF Cyg P. Somogyi 01/05/2017 4812 4957 10328AG Dra T. Lester 04/05/2017 6022 7123 9000 BF Cyg F. Campos 07/05/2017 3721 7258 783AG Dra W. Sims 04/05/2017 3866 7450 650 BF Cyg F. Teyssier 27/05/2017 4210 7150 11000AG Dra P. Berardi 05/05/2017 7566 8574 2770 CH Cyg P. Somogyi 30/04/2017 6500 6610 16928AG Dra U. Sollecchia 05/05/2017 3701 7381 613 CH Cyg P. Somogyi 30/04/2017 4813 4957 10684AG Dra C. Buil 06/05/2017 6819 6865 48000 CH Cyg T. Lester 04/05/2017 6022 7123 9000AG Dra C. Buil 06/05/2017 6546 6590 48000 CH Cyg F. Campos 07/05/2017 3719 7262 789AG Dra C. Buil 06/05/2017 5844 5884 48000 CH Cyg J. Guarro 08/05/2017 3980 7498 9000AG Dra C. Buil 06/05/2017 4674 4706 48000 CH Cyg F. Teyssier 13/05/2017 4207 7160 11000AG Dra D. Boyd 07/05/2017 3900 7380 753 CH Cyg J. Foster 14/05/2017 6407 6690 4316AG Dra F. Teyssier 09/05/2017 4208 7160 11000 CH Cyg J. Guarro 19/05/2017 3980 7498 9000AG Dra P. Somogyi 10/05/2017 6450 7160 3538 CH Cyg F. Teyssier 25/05/2017 4210 7150 11000AG Dra P. Somogyi 10/05/2017 4506 5225 2398 CH Cyg P. Somogyi 28/05/2017 3093 7915 472AG Dra P. Somogyi 10/05/2017 8019 8720 3412 CI Cyg D. Boyd 26/05/2017 3900 7380 769AG Dra J. Guarro 11/05/2017 4053 7498 9000 CI Cyg F. Teyssier 26/05/2017 4142 7160 11000AG Dra F. Campos 12/05/2017 6442 7207 4425 CQ Dra J. Guarro 12/05/2017 3980 7498 9000AG Dra U. Sollecchia 13/05/2017 3751 7370 599 LT Del P. Somogyi 11/05/2017 6445 7155 2727AG Dra F. Teyssier 13/05/2017 4208 7160 11000 LT Del W. Sims 14/05/2017 4001 7200 705AG Dra P. Somogyi 13/05/2017 6441 7150 2735 LT Del C. Kreider 16/05/2017 3801 7301 556AG Dra P. Somogyi 13/05/2017 4492 5210 1877 rsoph L. Franco 26/05/2017 3832 7235 531AG Dra J. Foster 14/05/2017 6407 6690 4253 rsoph F. Campos 27/05/2017 3751 7293 789AG Dra O. Garde 15/05/2017 4186 7314 9000 SU lyn T. Lester 04/05/2017 6023 7121 9000AG Dra U. Sollecchia 16/05/2017 3730 7370 601 SU lyn U. Sollecchia 05/05/2017 3685 7370 595AG Dra J. Guarro 16/05/2017 4053 7498 9000 SU lyn F. Campos 06/05/2017 3727 7266 887AG Dra F. Campos 16/05/2017 3748 7288 722 SU lyn J. Edlin 08/05/2017 3782 7301 787AG Dra O. Garde 16/05/2017 4186 7314 9000 SU lyn D. Boyd 09/05/2017 3901 7380 761AG Dra U. Sollecchia 17/05/2017 3701 7381 616 SU lyn O. Garde 09/05/2017 4186 7314 9000AG Dra J. Guarro 17/05/2017 4053 7498 9000 SU lyn F. Teyssier 10/05/2017 4207 7160 11000AG Dra P. Somogyi 17/05/2017 4514 5233 1731 SU lyn F. Campos 12/05/2017 6441 7207 5932AG Dra P. Somogyi 17/05/2017 5289 6005 2166 SU lyn O. Garde 24/05/2017 4186 7314 9000AG Dra T. Lester 18/05/2017 6020 7120 9000 T CrB P. Somogyi 30/04/2017 6500 6610 16819AG Dra P. Somogyi 18/05/2017 6448 7158 2639 T CrB W. Sims 01/05/2017 3866 7451 816AG Dra W. Sims 19/05/2017 3865 7448 668 T CrB P. Somogyi 01/05/2017 4812 4957 10536AG Dra J. Guarro 19/05/2017 3980 7498 9000 T CrB F. Campos 06/05/2017 3723 7261 796AG Dra C. Buil 19/05/2017 6819 6865 9000 T CrB J. Guarro 11/05/2017 4053 7498 9000AG Dra F. Campos 19/05/2017 3699 7193 792 T CrB F. Campos 13/05/2017 3773 7312 848AG Dra W. Sims 20/05/2017 3861 7446 752 T CrB F. Teyssier 13/05/2017 4208 7160 11000AG Dra J. Guarro 20/05/2017 4053 7498 9000 T CrB P. Somogyi 13/05/2017 4493 5213 1916AG Dra O. Garde 20/05/2017 4186 7314 9000 T CrB F. Campos 19/05/2017 3747 7190 761AG Dra W. Sims 21/05/2017 3864 7448 680 T CrB D. Boyd 25/05/2017 3901 7380 756AG Dra P. Berardi 21/05/2017 7564 8572 3093 T CrB F. Teyssier 25/05/2017 4210 7150 11000AG Dra U. Sollecchia 21/05/2017 3720 7370 618 T CrB L. Franco 26/05/2017 3832 7235 531AG Dra J. Guarro 22/05/2017 3980 7498 9000 T CrB F. Campos 26/05/2017 3765 7303 884AG Dra F. Campos 22/05/2017 6431 7200 5785 T CrB K. Graham 29/05/2017 3603 7404 518AG Dra F. Campos 23/05/2017 3763 7310 791 T CrB J. Guarro 31/05/2017 4053 7761 9000AG Dra J. Guarro 23/05/2017 3980 7498 9000 TX CVn F. Campos 06/05/2017 3718 7262 738AG Dra J. Guarro 24/05/2017 4047 7749 9000 TX CVn K. Graham 28/05/2017 3604 7404 546AG Dra J. Guarro 24/05/2017 4053 7498 9000 V443 Her F. Campos 28/05/2017 3748 7293 850AG Dra F. Campos 24/05/2017 3777 7309 816 V694 Mon T. Bohlsen 07/05/2017 3800 7220 993AG Dra F. Teyssier 24/05/2017 4210 7150 11000 V934 Her W. Sims 02/05/2017 3867 7452 741AG Dra D. Boyd 24/05/2017 3900 7380 742 YY Her D. Boyd 24/05/2017 3901 7380 749AG Dra J. Montier 24/05/2017 3700 7386 648 YY Her F. Campos 28/05/2017 3755 7293 810AG Dra J. Guarro 25/05/2017 3980 7498 9000AG Dra F. Campos 25/05/2017 6437 7202 4801AG Dra F. Teyssier 25/05/2017 4210 7150 11000AG Dra J. Guarro 26/05/2017 3980 7498 9000AG Dra F. Teyssier 26/05/2017 4210 7150 11000AG Dra F. Teyssier 26/05/2017 4210 7150 11000AG Dra J. Guarro 27/05/2017 4053 7761 9000AG Dra U. Sollecchia 28/05/2017 3720 7370 610AG Dra P. Somogyi 28/05/2017 3603 7401 471AG Dra F. Teyssier 30/05/2017 4210 7150 11000AG Dra J. Guarro 31/05/2017 3980 7498 9000AG Dra F. Teyssier 31/05/2017 4208 7160 11000AG Dra U. Sollecchia 31/05/2017 3760 7360 620AG Dra D. Boyd 31/05/2017 3901 7379 775AG Dra F. Teyssier 01/06/2017 4142 7160 11000

Range Range

AG Dra

Coordinates (2000.0)R.A. 16 01 41.0Dec +66 48 10.1Mag V 9.8

SYMBIOTICS


Ongoing campaign upon the request of R. Gális, J. Merc & L. LeedjärvA weekly coverage until the next outburst at resolution > 1800Low resolution (R = 1000), with a correct atmospheric response, can be useful for the campaign especially if flux calibrated

AAVSO lightcurve (V: right scale and B-V: left scale) since 2016Spectra obtained in 2017: blue dots on the top of the panel

Observer Date Res Observer Date ResW. Sims 01/05/2017 3866 7451 776 C. Buil 20/05/2017 4611 7177 725T. Lester 04/05/2017 6022 7123 9000 O. Garde 20/05/2017 4186 7314 11000W. Sims 04/05/2017 3866 7450 650 M. Verlinden 20/05/2017 2143 8751 592P. Berardi 05/05/2017 7566 8574 2770 M. Verlinden 21/05/2017 3741 7801 592U. Sollecchia 05/05/2017 3701 7381 613 W. Sims 21/05/2017 3864 7448 680C. Buil 06/05/2017 4674 4706 48000 P. Berardi 21/05/2017 7564 8572 3093D. Boyd 07/05/2017 3900 7380 753 U. Sollecchia 21/05/2017 3720 7370 618F. Teyssier 09/05/2017 4208 7160 11000 J. Guarro 22/05/2017 3980 7498 11000P. Somogyi 10/05/2017 6450 7160 3538 F. Campos 22/05/2017 6431 7200 5785P. Somogyi 10/05/2017 4506 5225 2398 F. Campos 23/05/2017 3763 7310 791P. Somogyi 10/05/2017 8019 8720 3412 J. Guarro 23/05/2017 3980 7498 11000J. Guarro 11/05/2017 4053 7498 11000 J. Guarro 24/05/2017 4047 7749 11000F. Campos 12/05/2017 6442 7207 4425 J. Guarro 24/05/2017 4053 7498 11000U. Sollecchia 13/05/2017 3751 7370 599 F. Campos 24/05/2017 3777 7309 816F. Teyssier 13/05/2017 4208 7160 11000 F. Teyssier 24/05/2017 4210 7150 11000P. Somogyi 13/05/2017 6441 7150 2735 D. Boyd 24/05/2017 3900 7380 742P. Somogyi 13/05/2017 4492 5210 1877 J. Montier 24/05/2017 3700 7386 648James R. Foster 14/05/2017 6407 6690 4253 J. Guarro 25/05/2017 3980 7498 11000O. Garde 15/05/2017 4186 7314 11000 F. Campos 25/05/2017 6437 7202 4801O. Garde 16/05/2017 4186 7314 11000 F. Teyssier 25/05/2017 4210 7150 11000U. Sollecchia 16/05/2017 3730 7370 601 P. Somogyi 26/05/2017 6452 7163 2757O. Garde 16/05/2017 4186 7314 11000 J. Guarro 26/05/2017 3980 7498 11000J. Guarro 16/05/2017 4053 7498 11000 F. Teyssier 26/05/2017 4210 7150 11000F. Campos 16/05/2017 3748 7288 722 P. Somogyi 27/05/2017 6448 7158 2773U. Sollecchia 17/05/2017 3701 7381 616 P. Somogyi 27/05/2017 4518 5238 1863J. Guarro 17/05/2017 4053 7498 11000 P. Somogyi 27/05/2017 5275 5990 1916P. Somogyi 17/05/2017 4514 5233 1731 J. Guarro 27/05/2017 4053 7761 11000P. Somogyi 17/05/2017 5289 6005 2166 U. Sollecchia 28/05/2017 3720 7370 610P. Somogyi 18/05/2017 6448 7158 2639 P. Somogyi 28/05/2017 3603 7401 471T. Lester 18/05/2017 6020 7120 9000 F. Teyssier 30/05/2017 4210 7150 11000W. Sims 19/05/2017 3865 7448 668 J. Guarro 31/05/2017 3980 7498 11000J. Guarro 19/05/2017 3980 7498 11000 F. Campos 31/05/2017 3762 7287 763C. Buil 19/05/2017 6819 6865 48000 F. Teyssier 31/05/2017 4208 7160 11000F. Campos 19/05/2017 3699 7193 792 U. Sollecchia 31/05/2017 3760 7360 620W. Sims 20/05/2017 3861 7446 752 D. Boyd 31/05/2017 3901 7379 775J. Guarro 20/05/2017 4053 7498 11000

Range Range

71 spectra were obtained in May, 2017

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AG Dra (V)

AG Dra undergone a weak and short outburst in May. The ARAS monitoring is almost dailyWe undergo the monitoring at a lower cadence (once a week)

AG Dra campaign, by Rudolf GàlisSYMBIOTICS


First of all, thank you very much for your effort during the observational campaign of the symbiotic star AG Dra. We are really delighted by your enthusiasm and passion in this task. Thanks this huge effort, 129 spectra were obtained from the beginning of the campaign to this day. So, for the first time in the history of spectroscopic observations of AG Dra, we have a possibility to study this symbiotic binary with around one-day resolution, which have not parallel in an investigation of symbiotic stars at all.

According to our statistical analysis of photometric observations, we know that the time interval be-tween outbursts of AG Dra vary from 300–400 d, with median around 360 d. Therefore we expected the next outburst in the interval from JD 2 457 877 (May 3, 2017) to JD 2 457 917 (June 12, 2017). Actu-ally, AG Dra manifested the third outburst of the recent activity stage in JD 2 457 890 (May 17, 2017) after 373 days after previous one. The last outburst of AG Dra looks quite untypical (as whole recent active stage, see below). After promising increase of its brightness (around 0.1 mag/day in B filter), the magnitude stopped to raise and it returned to almost the same level as before this event after only few days. The event recalls the pre-outburst in 2015 with maximal brightness around 10.7 mag in B filter.

The maximal magnitudes (10.7, 9.9 and 10.7 in B filter for the outbursts in 2015, 2016 and 1017, respectively) rank all these brightenings to the minor outbursts of symbiotic binary AG Dra. Such photometric behaviour of the active stage is very unusual. More often, the activity of AG Dra starts with major outburst, during which the brightness can reach the 8.8 and 8.4 mag in B and V band, respectively. Recent outburst activity resemble the weak activity stage 1963–66.

In our recent paper (Leedjärv et al. 2016) we demonstrated that the outbursts of AG Dra can be clearly distinguished also according to behaviour of the prominent emission lines in optical spectra. High-dispersion spectroscopy confirmed dramatic changes (significant increase of EWs) of the studied emission lines during recent active stage of AG Dra. The blue-wing absorption component observed in the profiles of the emission lines He I (λ6678), Hα and Hβ completely disappeared during the re-cent outbursts. Such spectroscopic behaviour is typical for the hot outbursts of AG Dra. On the other hand, at least the brightening in 2016 manifests the behaviour of the cool outbursts (all emission lines except He II 4686 Å) or some kind of transition between the hot and cool outbursts (emission line of He II 4686 Å). Is it a new type of outburst (or transition/combination of) the hot and cool outbursts? The analysis of obtained spectroscopic data for AG Dra is still in progress and we will inform the community about recent active stage of this interesting interacting binary in the forthcoming paper.

Even though the photometric behaviour of AG Dra indicates the typical quiescence low-am-plitude variability, some spectroscopic characteristics clearly demonstrate that the system is awakened state. Nevertheless, we do not expect another outburst in the following period.

On the other hand, the spectroscopic observations obtained during the campaign with around one-day resolution opened the possibility to study the orbital modulation of the spectral characteristics and thus the morphology of the circumbinary envelope. So, we suggest to continue in such the spectroscopic mon-itoring of AG Dra with lowered cadence (at least one R>10000 spectrum per 10-14 day) in the next period. Once again, thank you very much for all your observations and we look forward for our next cooperation.

On behalf of the scientific team,

Rudolf Gális16-06-2017

AG DraSYMBIOTICS


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The weak and short May, 2017 outburst in AAVSO V & B light curveThe outburst began 2017-05-13 (JD 2457887,5) from B = 11.0 and V = 9.65, the maximum is reached o, 2017-05-14 (JD 245888,5) at B = 10.7 and V = 9.35 (D mag ~ 0.3)

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102457850 2457880 2457910

Monitoring of the outburst in May at high resolution (R = 10000)LES = Tim Lester - FMT = François Teyssier - JGF = Joan Guarro Flo - OGA = Olivier Garde

233 04/05/2017 2:40 2457877.646 LES242 09/05/2017 20:14 2457883.372 FMT 247 11/05/2017 19:58 2457885.369 JGF243 13/05/2017 20:13 2457887.371 FMT 252 15/05/2017 19:35 2457889.365 OGA258 16/05/2017 20:00 2457890.397 JGF256 16/05/2017 19:32 2457890.363 OGA261 17/05/2017 20:33 2457891.413 JGF266 18/05/2017 2:04 2457891.618 LES268 19/05/2017 20:03 2457893.373 JGF272 20/05/2017 20:25 2457894.403 JGF274 20/05/2017 22:23 2457894.53 OGA279 22/05/2017 20:08 2457896.386 JGF282 23/05/2017 21:05 2457897.425 JGF283 24/05/2017 20:05 2457898.375 JGF284 24/05/2017 20:06 2457898.375 JGF286 24/05/2017 20:42 2457898.391 FMT 290 25/05/2017 20:18 2457899.393 JGF292 25/05/2017 20:42 2457899.388 FMT 294 26/05/2017 20:21 2457900.395 JGF288 26/05/2017 20:54 2457900.401 FMT 295 26/05/2017 20:54 2457900.401 FMT 300 27/05/2017 22:58 2457901.492 JFG304 30/05/2017 21:19 2457904.41 FMT 299 31/05/2017 20:56 2457905.394 FMT 305 31/05/2017 20:16 2457905.397 JGF

AG Dra: Equivalent widths from Echelle SpectraSYMBIOTICS


10152025303540

7840 7860 7880 7900 7920

EW Hb

0

2

4

6

7840 7860 7880 7900 7920

EW He I 5876

0

5

7840 7860 7880 7900 7920

EW He I 6678

50

60

70

80

90

100

7840 7860 7880 7900 7920

EW Ha

0

5

10

15

7840 7860 7880 7900 7920

Raman OVI 6830

0

5

10

7840 7860 7880 7900 7920

Raman OVI 7085

0.5

1.0

1.5

7840 7860 7880 7900 7920

HeII/Hb

10152025303540

7840 7860 7880 7900 7920

EW He II

0.0

0.5

1.0

1.5

7840 7860 7880 7900 7920

HeI 6678/7065

0.0

0.5

1.0

7840 7860 7880 7900 7920

7085/6830

2

3

4

7840 7860 7880 7900 7920

Ha/Hb

0

5

7840 7860 7880 7900 7920

EW He I 7065

JD - 2450000

AG Dra: The rise with Echelle SpectraSYMBIOTICS

10.5

11

11.5

9

9.5

102457880 2457890 2457900

Date Hour JD Obs243 13/05/2017 20:13 2457887.371 FMT 252 15/05/2017 19:35 2457889.365 OGA258 16/05/2017 20:00 2457890.397 JGF

Log of observationsThe first spectrum was obtained just before the riseNext time we need a spectrum the 14th!

0

1

2

3

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6

7

8

Rel

ativ

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tens

ity

-1500 -1000 -500 500 1000 1500Velocity (Km/sec)

2017-05-13.8432017-05-15.8302017-05-16.834

Hbeta - AG Dra

0.5

1

1.5

2

2.5

3

3.5

Rel

ativ

e in

tens

ity

-500 500Velocity (Km/sec)

2017-05-13.8432017-05-15.8302017-05-16.834

He I 5876 - AG Dra

0

2

4

6

8

10

12

Rel

ativ

e in

tens

ity

-1500 -1000 -500 500 1000 1500Velocity (Km/sec)

2017-05-13.8432017-05-15.8302017-05-16.834

He II - AG Dra

0.5

1

1.5

2

2.5

3

3.5

4

Rel

ativ

e in

tens

ity


2017-05-13.8432017-05-15.8302017-05-16.834

He I 6678 - AG Dra

0

0.2

0.4

0.6

0.8

1

1.2

1.4

1.6

1.8

2

Rel

ativ

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tens

ity

6800 6805 6810 6815 6820 6825 6830 6835 6840 6845 6850Wavelength (Angstrom)

2017-05-13.8432017-05-15.8302017-05-16.834

Raman OIV 6830 - AG Dra

0

0.2

0.4

0.6

0.8

1

1.2

1.4

1.6

1.8

2

Rel

ativ

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tens

ity

7065 7070 7075 7080 7085 7090 7095 7100 7105 7110Wavelength (Angstrom)

2017-05-13.8432017-05-15.8302017-05-16.834

Raman OIV 7088 - AG Dra


AG Dra at medium resolutionSYMBIOTICS


6500 6600 6700 6800 6900 7000 7100 7200

Wavelength (A)

0

5

10

15

rela

tive

in

ten

sity

AG Dra 2017-05-12 23:19:10 R = 4425 F. Campos

6500 6600 6700 6800 6900 7000 7100 7200

Wavelength (A)

0

5

10

15

rela

tive

in

ten

sity

AG Dra 2017-05-22 21:22:09 R = 5785 F. Campos

6500 6600 6700 6800 6900 7000 7100 7200

Wavelength (A)

0

5

10

15

rela

tive

in

ten

sity

AG Dra 2017-05-25 20:29:13 R = 4801 F. Campos

Fran Campos, with a DADOS 1200 l/mm R = 5000, just before and after the burst

AG Dra: flickering? by Peter SomogyiSYMBIOTICS


2

3

4

5

6

7

8

9

10

11

12

1.35

0

1.40

0

1.45

0

1.50

0

1.55

0

JD = 2457890 + ... (1.330 - 1.5834)

AG Dra EWs 2017.05.17.829 - 18.081 red: H-alpha (x 0.1), blue: Raman OVI 6825, green: Raman OVI 7083

magenta: He I 6678, black: He I 7065

6500 6600 6700 6800 6900 7000 7100 7200

Wavelength (A)

0

5

10

15

rela

tive

in

ten

sity

AG Dra 2017-05-27 20:06:54 R = 2773 P. Somogyi

Peter Somogyi’s work on flickering from series obtained with a Lhires III 600 l/mm (R = 2500)

AG Dra: flickering? by Peter SomogyiSYMBIOTICS


1

2

3

4

5

6

7

8

9

100.

330

0.34

0

0.35

0

0.36

0

0.37

0

0.38

0

0.39

0

0.40

0

0.41

0

JD = 2457900 + ... (.3247 - .4193)

AG Dra EWs 2017.05.26 red: H-alpha (x 0.1), blue: Raman OVI 6825, green: Raman OVI 7083


1

2

3

4

5

6

7

8

9

10

1.34

0

1.35

0

1.36

0

1.37

0

1.38

0

1.39

0

1.40

0

1.41

0

1.42

0

1.43

0

JD = 2457900 + ... (1.3364 - 1.4310)

AG Dra EWs 2017.05.27 red: H-alpha (x 0.1), blue: Raman OVI 6825, green: Raman OVI 7083


AG Dra: near IRSYMBIOTICS

8000 8100 8200 8300 8400 8500 8600 8700

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

AG Dra 2017-05-10 23:33:05 R = 3412 P. Somogyi

7600 7700 7800 7900 8000 8100 8200 8300 8400 8500 8600

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

AG Dra 2017-05-21 19:39:08 R = 3093 Paolo Berardi

Near IR range obtained by Peter Somogyi and Paolo Berardi with Lhires III 600 l/mmwith notably OI 8446 in weak emission


SYMBIOTICS

AG Dra: high resolution R = 48000 by C. Buil

0

2

4

6

8

10

12

14

16

18

20

Rel

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tens

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-1000 -500 500 1000Velocity (Km/sec)

H alpha - AG Dra 2017-05-06.923 C Buil

0

0.5

1

1.5

2

2.5

3

3.5

Rel

ativ

e in

tens

ity


He I - AG Dra 2017-05-06.923 C Buil

0

1

2

3

4

5

6

Rel

ativ

e in

tens

ity


He II - AG Dra 2017-05-06.923 C Buil

H alpha, He I 5876, He II 4686 a0 obtained by Christian Buil with his VHIRES at R = 48000

0

5

10

15

20

25

Rel

ativ

e in

tens

ity

-1000 -500 500 1000Velocity (Km/sec)

H alpha - AG Dra 2017-05-19.868 cbuil

00.5

11.5

22.5

33.5

44.5

55.5

Rel

ativ

e in

tens

ity


He I - AG Dra 2017-05-19.868 cbuil

0

5

10

15

20

25

30

35

Rel

ativ

e in

tens

ity


He II - AG Dra 2017-05-19.868 cbuil


AG Dra at high resolutionSYMBIOTICS


0

5

10

15

20

25

Rel

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tens

ity

-1500 -1000 -500 500 1000 1500Velocity (Km/sec)

Halpha - AG Dra 2017-05-18.086

0.5

1

1.5

2

2.5

3

3.5

4

Rel

ativ

e in

tens

ity

-500 -250 250 500Velocity (Km/sec)

He I 6678.15He I 7065.3

AG Dra He I 2017-05-18.086

0.80.9

11.11.21.31.41.51.61.71.81.9

Rel

ativ

e in

tens

ity

6790 6800 6810 6820 6830 6840 6850 6860Wavelength (Angstrom)

Raman OIV - AG Dra 2017-05-18.086

6000 6100 6200 6300 6400 6500 6600 6700 6800 6900 7000 7100

Wavelength (A)

0

5

10

15

20

rela

tive

in

ten

sity

AG Dra 2017-05-18 02:04:09 R = 9000 T Lester

AG Dra: flux calibrated spectraSYMBIOTICS


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

5

6

7

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-12 AG Dra 2017-05-07 21:29:00 R = 1000 D. Boyd

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-12 AGDra 2017-05-24 22:05:30 R = 1000 D. Boyd

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-12 AG Dra 2017-05-31 22:02:57 R = 775 D. Boyd

Flux calibrated spectra - David Boyd LISA R = 1000

AG Dra: low res spectra in MaySYMBIOTICS


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

10

rela

tive

in

ten

sity

AG Dra 2017-05-01 04:29:39 R = 1000 Woody Sims

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

10

rela

tive

in

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sity


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

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6

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10

rela

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in

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sity


Monitoring By Woody Sims with a LISA R = 1000


Monitoring By Fran Campos with a DADOS 200 l/mm R = 800

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

10

rela

tive

in

ten

sity

AG Dra 2017-05-16 20:43:08 R = 722 F. Campos

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

rela

tive

in

ten

sity

AG Dra 2017-05-24 20:27:56 R = 816 F Campos

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

rela

tive

in

ten

sity

AG Dra 2017-05-31 20:35:16 R = 1000 F Campos



Monitoring By Umberto Sollecchia with an Alpy R = 600

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

5

6

7

rela

tive

in

ten

sity

AG Dra 2017-05-05 20:43:53 R = 613 Umberto Sollecchia

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

rela

tive

in

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sity


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

rela

tive

in

ten

sity




4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.2

0.4

0.6

0.8

1

1.2

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-11 AG Dra 2017-05-24 23:31:12 R = 648 Jacques Montier

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

rela

tive

in

ten

sity

AG Dra 2017-06-02 06:50:35 R = 667 James R. Foster


Spectra acquired by Michel Verlinden, Jacques Montier, James Foster with ALPY R = 600

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

rela

tive

in

ten

sity

agdra 2017-05-21 00:00:04 R = 592 Michel Verlinden

BF Cyg

Coordinates (2000.0)R.A. 19 23 53.5Dec +29 40 29.2Mag 9.4 (2017-03)

SYMBIOTICS


9

10

11

12

13

142435000 2438650 2442300 2445950 2449600 2453250 2456900 2460550

AAVSO Visual lightcurve since 1955 - BF Cyg in high state since 2006

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

rela

tive

in

ten

sity

BF Cyg 2017-05-07 01:00:19 R = 783 F. Campos

9

9.5

10

10.5

112457000 2457200 2457400 2457600 2457800 2458000

BF Cygni (V)

BF CygSYMBIOTICS


4850 4900 4950

Wavelength (A)

0

1

2

3

4

5

6

rela

tive

in

ten

sity

BF Cyg 2017-05-01 02:27:39 R = 10328 P. Somogyi

0

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

Rel

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-1000 -500 500 1000Velocity (Km/sec)

Hbeta - BF Cyg 2017-05-01.103 1200 s (1 x 1200.001 s) PSO

0

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

5.5

Rel

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-1000 -500 500 1000Velocity (Km/sec)

H beta 4861.33Fe II 4923.92

BF Cyg 2017-05-01.103 1200 s (1 x 1200.001 s) PSO

H beta range obtained by Peter somogyi - Lhires III - 2400 l/mm

Comparison of H beta and Fe II 4924

0

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

5.5

Rel

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-1000 -500 500 1000Velocity (Km/sec)

H beta 4861.33Fe II 4923.92

BF Cyg 2017-05-01.103 1200 s (1 x 1200.001 s) PSO

BF CygSYMBIOTICS


4500 5000 5500 6000 6500 7000

Wavelength (A)

0

5

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15

rela

tive

in

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BF Cyg 2017-05-27 00:41:12 R = 11000 F Teyssier

4400 4450 4500 4550 4600

Wavelength (A)

0

0.2

0.4

0.6

0.8

1

rela

tive

in

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BF Cyg 2017-05-27 00 R = 11000 F Teyssier

5000 5050 5100 5150 5200 5250 5300 5350 5400

Wavelength (A)

0

0.5

1

1.5

2

rela

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BF Cyg 2017-05-27 00 R = 11000 F Teyssier

CH Cyg

Coordinates (2000.0)R.A. 19 24 33.1Dec +50 14 29.1Mag ~ 8.1

SYMBIOTICS

Ongoing campaign upon the request of Augustin SkopalAt least one spectrum a month (high resolution and low resolution, with a cor-rect atmospheric response)

Top : AAVSO V lightcurve since Au-gust,2016ARAS Spectra in May,2017 : blue dotsBottom : AAVSO V band: green B-V index: blueCH Cygni brightens


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

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4

6

8

rela

tive

in

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sity

CH Cyg 2017-05-07 00:16:00 R = 789 F. Campos

7

7.5

8

8.5

92457600 2457690 2457780 2457870 2457960

CH Cygni (V)

0

0.5

1

1.5

2

2.56

6.5

7

7.5

8

8.5

92457000 2457400 2457800 2458200

CH Cygni (V)

[OI] and [OIII] in emission in this low resolution spectrum obtained by Fran Campos with a DADOS 200 l/mm

CH CygSYMBIOTICS


6400 6500 6600 6700

Wavelength (A)

0

2

4

6

8

10

rela

tive

in

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sity

CH Cyg 2017-05-14 11:26:21 R = 4316 James R. Foster

-1000 -500 0 500 1000

velocity (km/s)

0

2

4

6

8

10

rela

tive

in

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sity

Halpha 2017-05-14

6000 6100 6200 6300 6400 6500 6600 6700 6800 6900 7000 7100

Wavelength (A)

0

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15

20

25

rela

tive

in

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CH Cyg 2017-05-04 04:36:37 R = 9000 T Lester

-1000 -500 0 500 1000

velocity (km/s)

0

5

10

15

rela

tive

in

ten

sity

Halpha 2017-05-04

CH Cyg in 2017SYMBIOTICS


Main lines evolution in 2017 from Echelle spectra

Note the complex behav-iour of [O III]

Journal of observations

-500 -250 0 250 500

velocity (km/s)

0

20

40

60

80

100

120

140

160

arb

itra

ry u

nit

CHCyg | Ha 6563

2017-01-21

2017-03-05

2017-03-20

2017-03-22

2017-04-02

2017-04-05

2017-04-10

2017-04-11

2017-04-16

2017-04-18

2017-04-22

2017-04-22

2017-05-08

2017-05-13

2017-05-19

2017-05-25

-500 -250 0 250 500

velocity (km/s)

0

10

20

30

40

50

60

70

80

90

arb

itra

ry u

nit

CHCyg | Hb 4861

2017-01-21

2017-03-05

2017-03-20

2017-03-22

2017-04-02

2017-04-05

2017-04-10

2017-04-11

2017-04-16

2017-04-18

2017-04-22

2017-04-22

2017-05-08

2017-05-13

2017-05-19

2017-05-25

-500 -250 0 250 500

velocity (km/s)

0

5

10

15

20

25

30

35

40

45

50

arb

itra

ry u

nit

CHCyg | [O III] 5007

2017-01-21

2017-03-05

2017-03-20

2017-03-22

2017-04-02

2017-04-05

2017-04-10

2017-04-11

2017-04-16

2017-04-18

2017-04-22

2017-04-22

2017-05-08

2017-05-13

2017-05-19

2017-05-25

-500 -250 0 250 500

velocity (km/s)

0

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10

15

20

25

30

35

40

45

50

arb

itra

ry u

nit

CHCyg | [OI] 6300

2017-01-21

2017-03-05

2017-03-20

2017-03-22

2017-04-02

2017-04-05

2017-04-10

2017-04-11

2017-04-16

2017-04-18

2017-04-22

2017-04-22

2017-05-08

2017-05-13

2017-05-19

2017-05-25

2017-01-21

2017-03-05

2017-03-20

2017-03-22

2017-04-02

2017-04-05

2017-04-10

2017-04-11

2017-04-16

2017-04-18

2017-04-22

2017-04-22

2017-05-08

2017-05-13

2017-05-19

2017-05-25

Observer DateF. Teyssier 21/01/2017F. Teyssier 05/03/2017J. Guarro 20/03/2017F. Teyssier 22/03/2017J. Guarro 02/04/2017O. Garde 05/04/2017J. Guarro 10/04/2017F. Teyssier 11/04/2017J. Guarro 16/04/2017J. Guarro 18/04/2017F. Teyssier 22/04/2017J. Guarro 22/04/2017J. Guarro 08/05/2017F. Teyssier 13/05/2017J. Guarro 19/05/2017F. Teyssier 25/05/2017

Comparison of [OI] (blue) and [OIII] (red)

CI Cyg


SYMBIOTICS


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

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3

4

5

6

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-12 Ci Cyg 2017-05-26 22:15:03 R = 1000 D. Boyd

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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35

rela

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in

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CI Cyg 2017-05-26 23:11:12 R = 11000 F Teyssier

10.5

11

11.5

122457200 2457565 2457930 2458295

CI Cyg

CQ Dra

Coordinates (2000.0)R.A. 12 30 06.6Dec +69 12 04.0Mag V ~ 5

SYMBIOTICS


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

CQ Dra 2017-05-12 19:52: R = 11000 J. Guarro

-1000 -500 0 500 1000

velocity (km/s)

0

0.5

1

1.5

rela

tive

in

ten

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Halpha 2017-05-12

LT Del: outburstSYMBIOTICS


Coordinates (2000.0)R.A. 20 35 57.2Dec +20 11 27.5Mag V = 13

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

rela

tive

in

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LT Del 2017-05-16 01:44:37 R = 556 C. Kreider

0

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10

Rel

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4000 4500 5000 5500 6000 6500 7000 7500Wavelength (Angstrom)

2017-05-14.385 Woody Sims2015-11-28.758 J. Guarro

LT Del

LT Del in low state (Joan Guarro - 2015-11-28) and in outburst (Woody Sims - 2017-05-14). Classical increase of recombination lines ; note that the EW of He I triplet (5876- 7065) remain almost constant.

LT DEl has been detected in outburst in May by U. Munari & al. (ATel # 10361) - see page 60Several spectra have been obtained by the team during this event

0

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14

Rel

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ity

-1500 -1000 -500 500 1000 1500Velocity (Km/sec)

Halpha - LT Del 2017-05-11.078 P. Somogyi

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14

Rel

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6450 6500 6550 6600 6650 6700 6750 6800 6850 6900 6950 7000 7050 7100 7150Wavelength (Angstrom)

LT Del 2017-05-11.078 P. Somogyi

LT Del: outburstSYMBIOTICS


RS OphSYMBIOTICS

Coordinates (2000.0)R.A. 17 50 13.2Dec -06 42 28.48Mag


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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8

10

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tive

in

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sity

RS Oph 2017-05-26 22:56:07 R = 531 L Franco

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

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8

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12

rela

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RS Oph 2017-05-27 23:00:30 R = 789 F. Campos

SU LynSYMBIOTICS



SU Lyn is newly discovered bright symbiotic (K. Mukai & al., 2016)The emission lines remain very faint at this phase and almost desappears in the last spectrum obtained by Olivier Garde

Katarzyna Drozd (Nicolaus Coperni-cus Astronomical Centre) is strongly interested by further observations (spectroscopy and BVR photometry). She also suggests working on short time variability, especially in B Band

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-12 SU Lyn 2017-05-09 20:59:32 R = 1000 D. Boyd

SU LynSYMBIOTICS


6000 6100 6200 6300 6400 6500 6600 6700 6800 6900 7000 7100

Wavelength (A)

0

1

2

3

4

rela

tive

in

ten

sity

SU Lyn 2017-05-04 01:13:17 R = 9000 T Lester

-500 0 500

velocity (km/s)

0.5

1

1.5

2

rela

tive

in

ten

sity

Halpha 2017-05-04

6500 6600 6700 6800 6900 7000 7100 7200

Wavelength (A)

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1

2

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4

5

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tive

in

ten

sity

SU Lyn 2017-05-12 20:11: R = 5932 F. Campos

-500 0 500

velocity (km/s)

0.8

1

1.2

1.4

1.6

rela

tive

in

ten

sity

Halpha 2017-05-12

H alpha region obtained by Tim Lester with a home made spectrograph (R = 9000) and Fran Campos with DADOS equiped with a 1200 l/mm gratings (R = 6000)


SU LynSYMBIOTICS

1

1.5

2

2.5

3

3.5

Rel

ativ

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tens

ity


VY Leo 2017-04-03.813 fteyssierSU Lyn 2017-05-24.827 Olivier Garde

Halpha -

0.5

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1.5

2

2.5

3

3.5

4

Rel

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tens

ity


2017-04-03.8132017-05-10.847

Halpha - fteyssier

Echelle spectra obtained by F. Teyssier (10-05) and Olivier Garde (24-05)

H alpha in comparison to a M5 III continuum (VY Leo)

4500 5000 5500 6000 6500 7000

Wavelength (A)

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rela

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SU lyn 2017-05-10 20:19:43 R = 11000 F. Teyssier

SU LynSYMBIOTICS


F. Teyssier 21/01/2017F. Teyssier 16/02/2017O. Garde 28/03/2017F. Teyssier 02/04/2017J. Guarro 03/04/2017J. Guarro 06/04/2017J. Guarro 12/04/2017F. Teyssier 20/04/2017F. Teyssier 10/05/2017O. Garde 24/05/2017

-500 -250 0 250 500

velocity (km/s)

0

2

4

6

8

10

12

arb

itra

ry u

nit

SULyn | Ha 6563

2017-01-21

2017-02-16

2017-03-28

2017-04-02

2017-04-03

2017-04-06

2017-04-12

2017-04-20

2017-05-10

2017-05-24

-500 -250 0 250 500

velocity (km/s)

0

2

4

6

8

10

12

14

16

arb

itra

ry u

nit

SULyn | Hb 4861

2017-01-21

2017-02-16

2017-03-28

2017-04-02

2017-04-03

2017-04-06

2017-04-12

2017-04-20

2017-05-10

2017-05-24

-500 -250 0 250 500

velocity (km/s)

0

2

4

6

8

10

12

14

16

18

20

22

arb

itra

ry u

nit

SULyn | [O III] 5007

2017-01-21

2017-02-16

2017-03-28

2017-04-02

2017-04-03

2017-04-06

2017-04-12

2017-04-20

2017-05-10

2017-05-24

-500 -250 0 250 500

velocity (km/s)

0

2

4

6

8

10

12

arb

itra

ry u

nit

SULyn | [OI] 6300

2017-01-21

2017-02-16

2017-03-28

2017-04-02

2017-04-03

2017-04-06

2017-04-12

2017-04-20

2017-05-10

2017-05-24

Journal of observations

Evolutions in 2017 from Echelle spectra (R = 11000)

In the last spectrum obtained by Olivier Garde, H beta is almost in pure absorp-tion

T CrBSYMBIOTICS

Coordinates (2000.0)R.A. 15 59 30.1Dec 25 55 12.6Mag 9.8 (2017-01)


AAVSO V light curve 2016-2017ARAS Spectra in May, 2017: blue dots

The symbiotic recurrent nova is a main target in our ob-serving program for the next years until the next nova event.

T CrB in the morning skyHe II and [OIII] reamains intense

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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T CrB 2017-05-01 06:03:56 R = 816 Woody Sims

9

9.5

10

10.52457300 2457400 2457500 2457600 2457700 2457800 2457900 2458000

T CrB

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

5

6

Flu

x [e

rg.c

m-2

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.Å-1

]

10-12 TCrB 2017-05-25 22:00:12 R = 1000 D. Boyd

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

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6

Flux

[erg

.cm

-2.s

-1.Å

-1]

10-12 TCrB 2017-05-25 22:00:12 R = 1000 D. Boyd

T CrB: lines evolution SYMBIOTICS


-500 -250 0 250 500

velocity (km/s)

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50

100

150

arb

itra

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nit

TCrB | Hb 4861

2015-04-180.475

2015-04-270.514

2015-05-080.563

2015-05-160.598

2016-02-170.815

2016-02-290.868

2016-04-010.009

2016-04-140.066

2016-04-160.074

2016-04-230.105

2016-04-280.127

2016-04-300.136

2016-05-140.197

2016-06-080.307

2016-06-250.382

2016-07-060.430

2016-07-160.474

2016-08-050.562

2016-08-220.637

2017-01-210.305

2017-03-050.494

2017-03-250.582

2017-04-110.656

2017-04-220.705

2017-05-130.797

2017-05-250.850

2017-05-310.876

phase

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velocity (km/s)

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60

80

100

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140

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180

arb

itra

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TCrB | Ha 6563

2015-04-180.475

2015-04-270.514

2015-05-080.563

2015-05-160.598

2016-02-170.815

2016-02-290.868

2016-04-010.009

2016-04-140.066

2016-04-160.074

2016-04-230.105

2016-04-280.127

2016-04-300.136

2016-05-140.197

2016-06-080.307

2016-06-250.382

2016-07-060.430

2016-07-160.474

2016-08-050.562

2016-08-220.637

2017-01-210.305

2017-03-050.494

2017-03-250.582

2017-04-110.656

2017-04-220.705

2017-05-130.797

2017-05-250.850

2017-05-310.876

phase

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velocity (km/s)

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arb

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TCrB | He I 5876

2015-04-180.475

2015-04-270.514

2015-05-080.563

2015-05-160.598

2016-02-170.815

2016-02-290.868

2016-04-010.009

2016-04-140.066

2016-04-160.074

2016-04-230.105

2016-04-280.127

2016-04-300.136

2016-05-140.197

2016-06-080.307

2016-06-250.382

2016-07-060.430

2016-07-160.474

2016-08-050.562

2016-08-220.637

2017-01-210.305

2017-03-050.494

2017-03-250.582

2017-04-110.656

2017-04-220.705

2017-05-130.797

2017-05-250.850

2017-05-310.876

phase

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velocity (km/s)

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50

100

150

arb

itra

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TCrB | He II 4686

2015-04-180.475

2015-04-270.514

2015-05-080.563

2015-05-160.598

2016-02-170.815

2016-02-290.868

2016-04-010.009

2016-04-140.066

2016-04-160.074

2016-04-230.105

2016-04-280.127

2016-04-300.136

2016-05-140.197

2016-06-080.307

2016-06-250.382

2016-07-060.430

2016-07-160.474

2016-08-050.562

2016-08-220.637

2017-01-210.305

2017-03-050.494

2017-03-250.582

2017-04-110.656

2017-04-220.705

2017-05-130.797

2017-05-250.850

2017-05-310.876

phase

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velocity (km/s)

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TCrB | [O III] 5007

2015-04-180.475

2015-04-270.514

2015-05-080.563

2015-05-160.598

2016-02-170.815

2016-02-290.868

2016-04-010.009

2016-04-140.066

2016-04-160.074

2016-04-230.105

2016-04-280.127

2016-04-300.136

2016-05-140.197

2016-06-080.307

2016-06-250.382

2016-07-060.430

2016-07-160.474

2016-08-050.562

2016-08-220.637

2017-01-210.305

2017-03-050.494

2017-03-250.582

2017-04-110.656

2017-04-220.705

2017-05-130.797

2017-05-250.850

2017-05-310.876

phase

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velocity (km/s)

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60a

rbitra

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TCrB | He I 6678

2015-04-180.475

2015-04-270.514

2015-05-080.563

2015-05-160.598

2016-02-170.815

2016-02-290.868

2016-04-010.009

2016-04-140.066

2016-04-160.074

2016-04-230.105

2016-04-280.127

2016-04-300.136

2016-05-140.197

2016-06-080.307

2016-06-250.382

2016-07-060.430

2016-07-160.474

2016-08-050.562

2016-08-220.637

2017-01-210.305

2017-03-050.494

2017-03-250.582

2017-04-110.656

2017-04-220.705

2017-05-130.797

2017-05-250.850

2017-05-310.876

phase

Echelle spectra R = 10000 obtained by F. Teyssier and J. Guarro

T CrB, an updateSYMBIOTICS


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55000 55500 56000 56500 57000 57500 58000 58500

H alpha - EW

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55000 55500 56000 56500 57000 57500 58000 58500

He II 4686 EW

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55000 55500 56000 56500 57000 57500 58000 58500

H beta - EW

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55000 55500 56000 56500 57000 57500 58000 58500

He I 5876 EW

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55000 55500 56000 56500 57000 57500 58000 58500

He II / H beta

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2.5

55000 55500 56000 56500 57000 57500 58000 58500

He I 5875 / 6678

Equivalent widths from Aras databaseThe light blue dots are published value (Ilkiewicz & al., 2016)The dark blue dots are ARAS values, obtained with Plotspectrax scale: JD - 2400000

He II / H beta ratio as a proxi of the temperature of the hot component (left) and triplet/singlet He I ratio (right)

T CrBSYMBIOTICS


4500 4600 4700 4800 4900 5000 5100 5200

Wavelength (A)

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T CrB 2017-05-13 22:17:09 R = 1916 P Somogyi

T CrBSYMBIOTICS


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Wavelength (A)

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T CrB 2017-05-06 23:13:13 R = 796 F. Campos

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Wavelength (A)

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T CrB 2017-05-26 20:26:04 R = 531 L Franco

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Wavelength (A)

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T CrB 2017-05-29 03:05:33 R = 518 K Graham

TX CVnSYMBIOTICS



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Wavelength (A)

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TX CVn 2017-05-06 21:32:35 R = 738 F. Campos

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TX CVn 2017-05-28 03:10:05 R = 546 K. Graham

V443 HerSYMBIOTICS

Coordinates (2000.0)R.A. 18 22 07.849Dec +23 27 19.96Mag 11,5

A classical symbioticInteresting target for the next months

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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V443 Her 2017-05-28 00:50:41 R = 850 F. Campos


V694 MonSYMBIOTICS

Coordinates (2000.0)R.A. 7 25 51.2Dec -7 44 8Mag

V694 Mon remains at high luminosity (Mean mag ~9.5)

End of the season

V694 Mon remains in “low” state with maximal veloc-ity of the absorption at ~ 2000 km/s

See: call for observations by A. Lucy and J. Sokolovski p. 51


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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V694 Mon 2017-05-07 09:14:29 R = 993 T. Bohlsen

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-3000 -2000 -1000 1000 2000 3000Velocity (Km/sec)

Halpha - V694 Mon 2017-05-07.385 T. Bohlsen

8.5

9

9.5

10

10.5

112457000 2457365 2457730 2458095

V694 Mon

V694 MonSYMBIOTICS

6000 6100 6200 6300 6400 6500 6600 6700 6800 6900 7000 7100 7200

Wavelength (A)

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V694 Mon 2017-05-26 08:01:59 R = 2976 J West

-2000 -1000 0 1000 2000

velocity (km/s)

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Halpha 2017-05-26

4500 5000 5500 6000 6500 7000

Wavelength (A)

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V694 Mon 2017-05-16 09:05:59 R = 1645 J West

Spectrograph L-200 600 l/mm

Spectrograph L-200 300 l/mm

Spectra acquired in May by J. West with a L-200


V934 HerSYMBIOTICS

Coordinates (2000.0)R.A. 17 06 34.5Dec +23 58 18.5Mag ~ 7.5

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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1.5

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V934 Her 2017-05-02 08:50:30 R = 741 Woody Sims


YY HerSYMBIOTICS


12

12.5

13

13.5

142457400 2457500 2457600 2457700 2457800 2457900 2458000

YY Her (V)

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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x [e

rg.c

m-2

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]

10-13 YY Her 2017-05-24 23:22:39 R = 749 D. Boyd

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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YY Her 2017-05-28 02:19:43 R = 810 F. Campos


V694 Mon: call for observationsby Adrian Lucy and Jeno Sokolovski(AAVSO Alert Notice #429)

SYMBIOTICS


Special Notice #429: V694 Mon (MWC 560) spectroscopy requested

May 2, 2017: Further to AAVSO Alert Notice 538, the campaign from 2016 on V694 Mon (MWC 560) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. V694 Mon is presently nearing opposition, but the request for spectroscopy continues until further notice.

Investigator Adrian Lucy writes: “Adrian Lucy and Dr. Jeno Sokoloski (Columbia Univer-sity) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations ob-tained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a per-fect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful.

“Broad, blue-shifted Balmer absorption lines in MWC 560 have signified a variable high-velocity out-flow for decades, sometimes extending up to 6000 km/s (e.g., Tomov et al. 1990, Nature, 346, 637). Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281). We cannot know whether interesting changes in velocity will happen, but we can hope!

“Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpre-dictable ways. For example, ‘amateur’ spectra obtained by Somogyi Péter in 2015 Decem-ber demonstrated that the velocity of absorption was very low only a month before an opti-cal outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible.

“Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_Data-Base/DataBase.htm), or sent to Adrian and Jeno directly at <[email protected]>. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ide-al, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration.”

Coordinates: R.A. 07 25 51.28 Dec. -07 44 08.2 (2000.0)

AAVSO finder charts for V694 Mon with comparison stars may be generated using the AAVSO Vari-able Star Plotter (VSP).Please submit variable star observations to the AAVSO International Database using the name V694 MON.This campaign is being followed on the AAVSO Observing Campaigns page. The thread that was cre-ated on the Campaigns forum for this campaign in 2016 (https://www.aavso.org/v694-mon-mwc-560-campaign) should be used to continue the discussion for the current phase of the campaign.

This AAVSO Alert Notice was prepared by Elizabeth O. Waagen with text provided by Adrian Lucy.

Link to AAVSO Notice: https://www.aavso.org/aavso-special-notice-429

http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm

http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm

DQ Her = Nova Her 1934In late 1934, after a precipitous rise to around V = 1.5 mag in only about a week, its slow, unsteady decline was followed by a fall of nearly deltaV 10 mag beginning about 100 days after the peak.This was followed by a slow recover to a nearly monotonic decline over many decades. The deep minimum has been interpreted for decades as the formation of dust within the expanding ejecta and, since this is an open question and easily stud-ied by your spectroscopy, let’s discuss it. A small, but not insignicant, number of classical nova have light curves of the DQ Her type (see Strope et al.2010, AJ, 140, 34. In their taxonomy, this is a D-type light curve, meaning “dust”).A list of likely dust forming classical novae comes from optical photometry: OS And 1986, V1370, Aql 1982, V1419 Aql 1993, T Aur 1891, V705 Cas 1993, V842 Cen 1986, V476 Cyg 1920, V2274, Cyg 2001, DQ Her, V445 Pup, V732 Sgr 1936, V992 Sco 1992, FH Ser 1970, LW Ser 1978, NQ Vul, 1976, QV Vul 1987. High resolution UV spectra were not obtained for any dur-ing the period of dust formation, and only V705 Cas was followed through the initial stages of the event.

http://adsabs.harvard.edu/abs/1994Natur.369..539S

The signal of dust formation is, in fact, usually not seen in the UV or even the optical at all. The infra-red, longward of 1 mm, usually follows the decline of the optical light and, following the initial reball stage, presents a thermal continuum consistent with the expanding ejecta and the underlying white dwarf. In some systems, however, a strong continuum can develop longward of 5 mm and extending to longer wavelengths. This is not expected from nearly trans-parent hot gas of the sort you infer to be present from the strong emission lines of high ions following the transition to the nebular spectrum. The energy distri-bution can, at times, show broad structure, an emis-sion band at around 9.8 mm with Dl / l ~ 0.1 that has long been identified as silicate (SiC) emission. A further peak at around 20 mm has a similar origin, and there is also a peak around 11 mm attributed to silicon carbide (SiC). These are all seen in many dusty environments from red supergiants to B[e] stars.

1.1 Solids in the cosmos: dust grainsIt’s useful to step back, for a moment, and discuss the identification and excitation mechanism because dust is not just a hugely big molecule. When, earlier, we discussed molecular spectra, it was in the context of line identification. Individual motions (rotation, vibration) are each described by a set of quantum numbers and the energy levels are well spaced (even though numerous). With only the difference that the shape of the potential, and the individual ener-gies, depend on the electron configuration (because that determines how the atoms are arranged), the transitions can be handled just like atomic lines. All that changes if the body in question is a solid. The sheer number of adjacent atoms within the structure produces a collective motion. Any single atom that, for instance, displaces from its equilibrium position (analogous to a molecule) is linked to every other atom, no matter how distant, within the same struc-ture. Thus, a vibration is constrained to not only be quantized, but the frequency depends on the inertia of all of the neighboring atoms. Normally, the anal-ogy is o a single mass tied to others by a set of identi-cal springs so the harmonic motions are constrained and also completely coupled in three dimensions. This gets rather complicated in detail when account-ing for the symmetries of the arrangements (crystals, space symmetries) but the basics are quite simple. Vibrations are quantized and propagate as excita-tions down and up the ensemble of atoms. These are called phonons, in analogy with photons. The propa-gation of a phonon is the the transmission of a pulse, a momentum kick, that is constrained in wavelength (hence frequency) by the spacing of the atoms.Since phonons are all harmonics of a fixed frequency, the whole ensemble of them, scattering and interact-ing analogously to photons, produces a single distri-bution in energy. These thermalize, if the vibrations are in equilibrium the system can be described statis-tically as having a mean energy that depends only on the temperature, and when the excitation is due to absorption of incident photons, the system is said to be in radiative equilibrium. But this is the key point of a blackbody, and the deep meaning of thermal equi-librium: the temperature (spectral energy distribu-tion) of the incoming light is irrelevant, if every photon can be equally well absorbed it’s only the amount ofenergy that matters. The same amount of energy

Novae: the effects of dust formation on line profiles Steve Shore


that is absorbed will be re-radiated, that’s what radiative equilibrium means, an the internal tem-perature of the solid determines the amount and spectral energy distribution of the emitted light. This is the Planck function, or blackbody curve.The total emitted light depends only on the tem-perature

F = (constant) .T4

the Stefan-Boltzmann law, and the frequen-cy at which the spectral energy distribu-tion peaks depends only on the temperature, Vmax . T = (someotherconstant), also called Wien’s law. For a blackbody,this emitted spectrum is univer-sal, it doesn’t depend on the composition of the body.

The problem is that almost nothing is a black-body, equally efficiently absorbing at all wave-lengths. it But the efficiency, the proportion of the radiation that emerges from a solid, is a function only of T. That’s the central difference. For ther-mal equilibrium, Kirchhoff’s law is that the ratioof the emissivity Jn to absorption Kn of a solid - or anything else - in strict thermal equilibriumis a universal function only of T,

Jn / Kn = Bn(T)

and that Bn(T) is the Planck function. Consequently, if a body absorbs more at some part of the spectrum, it also will emit or there: a grey or colored body will not look like a blackbody and will never have a Planck form for the energy distribution. More to the point, in light of everything we’ve discussed for nova ejecta and symbiotics, the circumstellar medium is not one temperature (isothermal). A solid, say a piece of chalk or a person or whatever, is at some distance d from a central illuminator. Then the radiation intensity falls as d-2 and the temperature reached by the body re-quired to balance by emission all incident absorbed radiation gives a temperature that varies with dis-tance as T ~ d1/2 since the flux in balances the flux out.

1.2 Radiative Balancing

So let’s imagine you have a dust shell around a star, one that’s not so opaque as to be self-shielding.Then dust closer to the central body will be hotter,

peak at shorter wavelength, and emit more. That at greater distance will be cooler and less luminous. Summing all contributors up, the spectrum may look like a blackbody but it can’t be. It’s always pos-sible to force-t a particular functional form but that doesn’t make the result physically acceptable. OK, that’s just part of it. The emission also depends on temperature because the bands of the solid, the res-onances (in the solid it’s bands from conduction and valence, in a molecule it’s the individual levels, the idea is the same) come at specific frequencies and depend sensitively on the structure of the matter (amorphous, crystalline, something else) and even small compositional changes affect the wavelengths of the bands (e.g., SiO vs. SiC). So on top of the dis-tance effect, the emitted spectrum will also have the broad bands from each region where they can emit.

On the other side of the spectrum, in the UV, the rate of absorption also depends on the bandstructures. Resonances occur there too, just as there are resonance lines for atoms and molecules.These depend on composition. Carbon-rich solids have a band around 2175 A that is usually idenfitied as “astronomical graphite” (tongue in cheek, nowa-days, given the properties of real graphite) based on an early suggestion by Hoyle and Wickramasinghehttp://adsabs.harvard.edu/abs/1962MNRAS.124..417H)and a subsequent application to novae Clayton and Hoyle. If there’s sucient UV absorption, the dust absorbs it with extra efficiency compared to the optical because of this band. The grain, on the other hand, emits poorly. There’s no corresponding broad infrared feature for “graphite” so the grains heat un-til their temperature rise compensates the relatively low emission efficiency.Silicates, on the other hand, have no such absor-tion feature in the UV but emit very efficiently in the IR so their temperatures will be systemati-cally lower. Again, high absorption coefficient at any temperature also means high emissivity, and the temperature of a solid will rise as far as neces-sary to emit the all of the absorbed incident flux.1 Combined with the distance effect, the spectrum looks,even less like a single temperature blackbody!

In novae, as in all cosmic sources, formation of this solid phase - and from now on I’ll call it dust




and refer to grains - is not at all well understood. What we know is that it happens, the grains are not merely growing but forming at a critical stage in the expansion, and that the conditions in the nova ejecta are extreme and very different from normal laboratory condensation conditions.

You may be wondering where all this is going. Now to novae: during the steep drop in the optical and UV, the IR increases by similar amounts and a warm (about 1000 K) source appears in the IR as an emit-ting continuum. Note the word very carefully: in-stead of just line (molecular) emission, there’s now a continuum. A characteristic of solids, and that’s where dust enters, is the density of levels is tremen-dous. So when the continuum is present, especially in the otherwise transparent infrared (where the atomic opacity is much reduced and the only atomic continua are ionization and bremsstrahlung (also called free-free emission, the radiation of photons from collisions between charged particles and their deviation by electrostatic interactions) it’s taken as the signal of dust emission. The other is the tem-perature characterizing this continuum. Grains, we know from the laboratory, are comparatively fragile. The binding of atoms is only a few eV so if the solids are too hot they evaporate. The critical temperature is not more than a few thousand K, a good estimate is 1000-1500 K, so the peak of the radiation should be around 5-20 mm. Furthermore, the physical size of the grains is a part of their opacity. If a cluster grows above the nano-scale, to a few tenths of a mi-cron, it’s huge relative to a molecule (which is only a few A in size so, again, even if the dust is grey it will obscure the optical and ultraviolet. Since noth-ing is completely reflecting, illumination by the cen-tral WD (regardless of its spectral distribution) must produce heating so the infrared emission scales with the luminosity of the central star independent of the temperature or even the precise form of the dust (again, flux out balances flux in whatever the ratio).

1.3 Molecular precursorsSome of you may recall that in the early stages of the work on V339 Del, an important ques-tion was whether CN and CH were visible in the optical spectrum. It seems they weren’t but there have been claimed detections in a num-ber of other recent novae (e.g., C2 and CN)

https://ojs.cvut.cz/ojs/index.php/APP/article/viewFile/APP.2015.02.0212/2715

and one possible detection of CN,

http://www.aoc.nrao.edu/54mrupen/XRT/V445Pup/Papers/v445pupiijima08.pdf.

These may be correct, the data is sometimes kind of marginal but often quite suggestive (in the absence of more detailed modeling). The longer visibility of CN in DQ Her remains the one really suggestive con-nection. Molecular precursors have been detected in the IR for some novae (CO inemission, for in-stance, before the dust event). These remain tanta-lizing possibilities but a basicproblem remains that is another reason for urging you to concentrate on ear-ly time spectra (even at low resolution!): we don’t know how the matter passes from molecular to solid state. As I said, it’s not as simple as putting the buck-et in the freezer and waiting for it to solidify. That’s called nucleation, the same process that governs the formation of ice and drops in clouds. Condensation nuclei form, somehow, and these grow by being a favored, lower energy state of the gas. But that’s at densities at which you can apply normal ther-modynamic reasoning. In novae that doesn’t workthe background radiation field must be impor-tant and the densities are notably lower than any laboratory experiment to date. Indepen-dent of the details, the observation that dust does form is rock solid (sorry for the pun).

1 This is the same as the greenhouse mechanism driving climate change: if the opacity of a heated layer increases in the emission region, this impedes the loss of absorbed radiation and the temperature gradient increases to achieve bal-ance. Thus, the boundary temperature can actually decrease, where the matter is optically thin, but the surface will get warmer. The same holds for absorption lines in stellar atmospheres, the temperature is hotter in deeper layers be-cause of the higher absorption if metallic absorption lines dominate the opacity compared with continuous opacity.



1.4 So what about the evidence?

So now what happens if dust forms. That’s the new result and it’s best to use the comparison between V339 Del and V5668 Sgr. Both showed very asym-metric profiles, the red wing being considerably re-duced relative to the blue side. Perhaps remarkably, the two are almost the same (see the illustration, Fig. 3, comparing the resonance N IV] and recombination He II profiles on around the same day after outburst).

Now, for a trial idea, suppose the dust forms within the ejecta but in the inner parts. Then it’s conned not only in radius but also in velocity. Remember, in bal-listic expansion the two are interchangeable. So the blueward side is partially blocked while the redward side, having to pass through both sides of the ejecta and through the dust, is more strongly attenuated. That’s the model profile on the top of the figure. The original profile formed from the bipolar ejecta is in white, the model is in blue, and the N IV] or He II line profiles from the actual novae can be compared.(Fig. 4). The effect has also been noted in some superno-vae during their early expansions but that’s a harder

observation because of the extreme breadth of the line profiles and the complicated velocity structure produced by the shock ejection. Here it’s much simpler.

The next step is to see what polarization tells us, and especially spectropolarimetry. To see if different parts of the ejecta are also altered in ionization will require much more work but that’s ongoing (especially with Paul Kuin, of the Swift team, who was the PI on the HST/STIS observations of V5668 Sgr). But if this is on the right track, we may be able to use the persistent asymmetries (not those in the earliest stages that are from line optical depth effects, as we’ve discussed) to map the location of the dust. The only other chance is to use low resolution UV spectra, and that’s being worked on now for V5668 Sgr (grism spectra from Swift), but it’s a long shot because of the difficulty of the analysis. The only other nova that ever showed the dust directly, V705 Cas 1993, was observed in a sequence with IUE that can’t now be repeated. But that showed the dust formed relatively far out, above the pseudophotosphere, but the observa-tion only covered the start of the event. Stay tuned!

Fig. 1 - Nova Cas 1993 Luminosity curve (V)


Fig. 2 - Model of dust formation in a bipolar ejecta

Fig. 3 Resonance N IV] 1486and recombination He II 1640 profilesfor V339 Del (left) and V5668 Sgr (right)

Fig. 4 - white: original profile - blue : model



Fig. 3 Resonance N IV] 1486and recombination He II 1640 profilesfor V339 Del (left) and V5668 Sgr (right)

Absorption line fine points: the Balmer decrement and theterminal absorption velocity Steve Shore

During during the “Fe curtain” stage of a clas-sical nova, the ejecta are suciently optically thick in both the continuum and lines that a pseudophoto-sphere denes a boundary between emission and ab-sorption regions of the expanding gas. The innermost portions of the ejecta, those with lower outward velocities, are also denser. This depends on the de-tails of the ejection mechanism, how structured the medium is (fragments, individual absorption knots,

that sort of thing that you may recall from V339 Del) but the overall structure is simple and monotonic: the density decreases outward, the velocity increas-es outward, so the entire spectrum from the outer layers is shifted to the blue as you see it relative to the deeper portions. This picture holds for any ejec-tion { whether a shell or a wind { since the matter is ultimately lost from the source so must exceed the escape velocity at some distance from the origin.

From a high SNR spectrum ob-tained the 2017-05-29., Peter Somogyi built a velocity plot of Balmer lines

red: H-alphagreen: H-betablue: H-gammapurple: H-deltagenerated by IRAF/specplot

and raise the question :

“why only the emis-sions velocities match?”

Steve Shore answers:

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

sn2017eaw 2017-05-29 01:01:52 R = 473 P. Somogyi


For novae this is particularly simple so let’s use his as the example. For a ballistic ejection, the velocity varies as v(r) = vmax(r/R(t)) where r is the radial dis-tance and R(t) is the outermost radius of the gas. The ejecta mass is constant, so the density varies as r ~ r-3 Then the optical depth, for you as an external observ-er varies as tline = kline r Dr ~ kline r

-2 . The opacity for the transition, line depends only on atomic parameters (in this way of writing things), I’ll ignore the excitation effects. Think of it as arising from a line whose lower level can’t decay (the Lyman series for hydrogen, for instance). Note that if the Lyman (UV) line is suffi-ciently opaque, the Balmer series behaves as if its lower level has a xed population. Now, for the Balm-er lines, or for it any multiplet (I’ll remind you that a multiplet is a series of lines coming from the same electron configurations and connected in a transition set, like the He I triplets), each line has its own intrin-sic strength - the oscillator strength, f - and kline ~ fline .

For the Balmer series, for instance, going from Ha through Hd the oscillator strengths are (0.6, 0.07, 0.05, 0.02), tracking the transition probabilities. So the opacity is much higher for Ha than for Hd, for instance, and so on down the series. For a line of sight toward the pseudophotosphere, then, the lower Balmer lines (here I mean the upper quantum number, up = [3; 4; 5; ]), are much more opaque in the outer layers than the higher lines so you see absorption from the outer parts in your direction. In other words, you see a blueshifted absorption. On the redward side, though, the matter is seen mov-ing away so you see mission at the highest velocity and absorption only of the innermost, slower mov-ing part. Hence, the maximum absorption blueshift comes from greater distances for the Ha line than, say, Hg. This is the Balmer progression, first de-scribed in detail, I think, by Struve for the Be stars. It’s a general feature of all outflows, or ejections.

This is a familiar diagnostic for the Be stars, for instance, and in general it describes stellar winds. Since for a continuous outflow the velocity results from driving against gravity, the outer parts of the wind reach a terminal, constant outflow speed in steady state. This can vary, as you see in some symbi-otic stars, but it’s a general result: the outflow veloc-ity, in contrast to ballistic ejection, varies as v(r) → vmax as r → ∞. with some sort of power law (the so-called b-law”). The maximum velocity sampled by the higher Balmer lines is always lower than that from Ha because the density of the wind varies as r ~ r-2 v-1.

In the supernova spectra you’ve seen here, the same basic reasoning applies because the shock that ejects the matter accelerates the outer parts of the star to very high terminal speeds. So in the course of a series of observations, the higher Balmer lines pass over into emission while H may still show a P Cyg (emission plus absorption) prole. The maximum absorption velocity is never the ac-tual maximum speed of the ejecta since the den-sity is too low there but, for supernovae (especially SN II since these are very massive ejecta) it comes close. For novae, it’s never more than about 3/4 vmax, but that’s jut a rule-of-thumb and not an exact result. For a stellar wind, it is the maximum veloc-ity because the outer parts of the wind are expand-ing at nearly constant radial velocity. Thus, a photon emerging from a deeper layer has a greater chance of encountering an absorber at the same velocity in the outer parts, which effectively increases the line optical depth by decreasing the escape probability. Ultimately, however, there’s a limit as the density drops and the line has a distinct maximum edge, the classical cartoon of the P Cyg line. Note that this de-pends very much on the geometry (structure), mass loss rate (density), and acceleration (dynamics) of the wind. For novae and supernovae it’s unique be-cause the velocity field is impulsively set so the time development of their spectra follows a sequence

Absorption line fine points: the Balmer decrement and theterminal absorption velocity Steve Shore


After 23 years the yellow symbiotic star LT Del is again in outburst

ATel #10361; U. Munari (INAF Padova), P. Ochner (Univ. Padova), S. Dallaporta and R. Belligoli (ANS Collaboration)on 9 May 2017; 11:06 UTThe ANS Collaboration photometric and spectroscopic monitoring of symbiotic stars has detected LT Del (= Hen 2-467 = PK 063-12.1 = StHa 179) in outburst. This is the first recorded outburst since the last one of 1994-1995, which was discov-ered by Passuello et al. (1994, IAUC 6065 ) and described by Arkhipova et al. (1995a, ALett 21, 339; 1995b, ALett 21, 391).

LT Del is steeply rising in brightness. Last ANS photometric observation on UT May 6.005 found it at U=12.65, B=13.278, V=12.407, R=11.705 and I=11.135 (+/- 0.006 in BVRI, 0.01 in U), which is almost as bright as the peak of the 1994-1995 event. The current outburst unfolded in phase with the egress of the WD from superior conjunction with the G6III giant companion, a geometrical arrangement that may be responsible for the particularly steep rise in brightness, which amounts to an average of 0.02 mag per day. All colors turned bluer, with the B-V rising to +0.87 from an average quiescence value (for the same orbital phase) of +1.45.

A spectrum of LT Del in outburst has been obtained on UT May 8.1 with the Asiago 1.22m telescope (range 3200-7900 Ang, dispersion 2.31 Ang/pix). A strong blue continuum now veils the G6III continuum features, and the Balmer continuum is in strong emission. The outstanding emission lines are characterized by high ionization con-ditions, with HeII 4686 being slightly stronger than Hbeta (10.11 vs 9.71x10(-13) erg cm-2 s-1) and prominent lines being OIII 3444 and 3429, OIV 3411, [NeV] 3345 and 3427 Ang. The flux ratio of Balmer lines Ha:Hb:Hg:Hd is 3.53:1.00:0.46:0.36 consistent with low reddening and low self absorption. The weakness of HeI emission lines com-pared to those of HeII suggests density bounded conditions. No significant nebular lines are present other than [NeV].

Spectroscopic observations of ASASSN-17gk

ATel #10399Paul Luckas (International Centre for Radio Astronomy Research, University of Western Australia)on 19 May 2017; 00:32 UT

Spectroscopic observations were obtained of the new Galactic nova, ASASSN-17gk (ATel #10366), on 2017 May 18.4 UT, 600 sec exposure with an Alpy600 spectrograph (0.8 A/px, 3800-7400A) using an Atik414 CCD detector. Extended absorption of the Na I D lines, blended with a maximum velocity of -2000 km/s, also shows that He I 5876 was not present (nor was He I 6678). The same absorption velocity was shown by Fe II 4923, 5169, Ca II H and K (although as always the H-epsilon line is blended with Balmer emission), and the Balmer lines, H-alpha through H-gamma, with little difference in the maximum. The Balmer absorption is, however, relatively weak compared to the emission. Fe II 5018 showed a higher maximum velocity, -2700 km/s, and a further extension toward maximum velocity than the other related Fe-curtain lines. The emission to absorption ratio for the metallic lines was > 4, while for the Balmer lines it was > 10. The forbidden lines [O I]5577, 6300,6364 were absent as were the [N II] 5755,6548,6583 lines (including the nebular lines). The nova is clearly in the very optically thick stage of the expansion, with many weak metallic line blends form-ing the pseudocontinuum, but with no indications yet of asphericity or filamentary structure. There was also no evidence for enhanced absorption at CN or CH, yet the Na I D line absorption was very strong and shifted.


Astronomer’s Telegram

Please :- respect the procedure- check your spectra BEFORE sending themResolution should be at least R = 500For new transcients, supernovae andpoorly observed objects,SA spectra at R = 100 are welcome

1/ reduce your data into BeSS file format2/ name your file with: _ObjectName_yyyymmdd_hhh_Observer Exemple: _chcyg_20130802_886_toto.fit

3/ send you spectra to Novae, Symbiotics, Cataclysmics : François Teyssier

to be included in the ARAS database

Astronomical Ring for Access to Spectroscopy (ARAS) is an infor-mal group of volunteers who aim to promote cooperation between professional and amateur astronomers in the field of spectroscopy.

To this end, ARAS has prepared the following roadmap:

• Identify centers of interest for spectroscopic observa-tion which could lead to useful, effective and motivating co-operation between professional and amateur astronomers.• Help develop the tools required to transform this cooperation into action (i.e. by publishing spectrograph building plans, organizing group purchasing to reduce costs, developing and validating observa-tion protocols, managing a data base, identifying available resourc-es in professional observatories (hardware, observation time), etc.•Develop an awareness and education policy for amateur astrono-mers through training sessions, the organization of pro/am semi-nars, by publishing documents (web pages), managing a forum, etc.• Encourage observers to use the spectrographs available in mission obser-vatories and promote collaboration between experts, particularly variable star experts.• Create a global observation network.

By decoding what light says to us, spectroscopy is the most productive field in astronomy. It is now entering the amateur world, enabling amateurs to open the doors of astrophysics. Why not join us and be one of the pioneers!

Be Monthly reportPrevious issues : http://www.astrosurf.com/aras/surveys/beactu/index.htm

About ARAS initiative

Submit your spectra to ARAS Eruptive Stars Data Base


Download previous issues of the Information Letter :

http://www.astrosurf.com/aras/novae/InformationLetter/Informa-tionLetter.html

ARAS Database :http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm

http://www.astrosurf.com/aras/novae/InformationLetter/InformationLetter.html



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