cataclysmics, symbiotics, novae - astrosurf · 47 v1016 cyg 19 57 4.9 39 49 33.9 18 15/04/2015...

Eruptive stars spectroscopyCataclysmics, Symbiotics, Novae

Eruptive StarsInformation Letter n° 41 #2019-01 18-05-2019

Observations of Jan. - Mar. 2019Contents

Symbiotics

V694 Mon = MWC 560 in high luminosity AX Per: strong outburstAG Dra monitoring before the 2019 expected outburstCH Cyg at low luminosity

Mysterious l 5018 line in the spectrum of AG Dra in outburstFrançois Teyssier

TCP J05390410+4748030 Dwarf nova in outburstPaolo Berardi, Lorenzo Franco

New Online Database of Symbiotic VariablesJaroslav Merc, Rudolf Gális, Marek Wolf

Spin, angular momentum,and how they govern your spectraSteve Shore

“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

F. Teyssier, S. Shore, Jaroslav Merc, Rudolf Gális, Marek Wolf, D. Boyd, J. Guarro, F. Sims, T. Lester, F. Campos, U. Sollecchia, C. Boussin, P. Berardi, S. Charbonnel, O. Garde, P. Somogyi, C. Buil, V. Marik, G. Martineau, Y. Buchet, I. Diarrassouba, J. Michelet

p. 2

p. 63

p. 77

p. 79

p. 82

Authors :

ARAS Eruptive Stars Information Letter #41 2019-01 - p. 2

Authors:F. Teyssier, D. Boyd, J. Guarro, F. Sims, T. Lester, F. Campos, U. Sollecchia, C. Boussin, S. Charbonnel, O. Garde, P. Somogyi, P. Berardi, C. Buil, V. Marik, G. Martineau, Y. Buchet, I. Diarrassouba, J. Michelet

Spectroscopic observations of symbiotic stars in 2019-Q1

ARAS Eruptive Stars Information Letter #40 2019-01

Abstract:198 spectra of 23 symbiotic stars at resolution from 500 to 15000 were obtained during 2019-Q1 by 18 observers. AG Dra is monitored before the expected outburst in 2019. At the date (2019-05-18) no sign of outburst has been detected. AX Per soon after the oulet of its eclipse has been detected in strong classical outburst, characterized by the weakening of high emission lines [Fe VII]. CH Cyg is in low luminosity, several spectra has been obtained during a short flare. V694 Mon, in high luminos-ity, has been monitored at high cadency during the season. The profiles of Balmer and Fe II lines is un-usual with a classical P Cygni profile and the disappearence of the broad blue absorption lines.

Symbiotics: Observing program

SYMBIOTIC


Observing : main targetsName 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

Target Request Objective Notes StatusCH Cyg Independently

A. SkopalM. Karovska

Long term monitoring of a com-plex and highly variable object

Ongoing

AG Dra R. Gàlis J. Merc L. Leedjarv

Study of outbursts and orbital variability

He II / HbRaman OVI

One spectrum a week until next outburst (Spring 2019)

AX Per R. Gàlis J. Merc

Ongoing outburst

SU Lyn K. Drozd Study of the orbital variations of a newly discovered symbiotic

One spectrum a week

V694 Mon A. LucyJ. SokolovskiM. Karovska

Detection of active phases Balmer and Fe II lines

R Aqr M. Karovska Studying ongoing eclipse

RT Cru J. Luna see above

ARAS Eruptive Stars Information Letter #40 2019-01

Main targets for 2019, Quarter 2AG DraCH CygT CrBRT CruOther targets of interest: SU Lyn, V443 Her, YY Her, CI Cyg, BF Cyg, RS Oph And asap in the morning sky: R Aqr (eclipse), AG Peg, Z And, AX Per (outburst), V694 Mon

RT CruThe symbiotic RT Cru has been getting some attention in the last years due to its high energy emission in X-rays. I have published a couple of papers about it:

http://adsabs.harvard.edu/abs/2018A%26A...616A..53L

http://adsabs.harvard.edu/abs/2007ApJ...671..741L

I would like to call the ARAS observ-ers attention and encourage to follow spectroscopically this source. The AAVSO light curve is also showing an interesting behavior now, recovering from a faint state.

Joan Luna

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

Symbiotics in ARAS Data Base Update : 16-05-2019SYMBIOTICS


58 stars4425 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 45.7 124 12/08/2010 18/02/2019 892 AX Per 1 36 22.7 54 15 2.5 276 04/10/2011 12/05/2019 63 V471 Per 1 58 49.7 52 53 48.4 27 06/08/2013 14/02/2019 934 Omi Cet 2 19 20.7 -2 58 39.5 33 28/11/2015 09/02/2019 985 BD Cam 03 42 9.3 63 13 0.5 46 08/11/2011 29/04/2019 196 StHa 32 04 37 45.6 -01 19 11.8 5 02/03/2018 25/01/2019 1137 UV Aur 05 21 48.8 32 30 43.1 81 24/02/2011 28/03/2019 518 V1261 Ori 05 22 18.6 -8 39 58 16 22/10/2011 29/12/2019 09 StHA 55 05 46 42 6 43 48 8 17/01/2016 08/02/2019 99

10 SU Lyn 06 42 55.1 +55 28 27.2 160 02/05/2016 30/04/2019 1811 ZZ CMi 07 24 13.9 8 53 51.7 61 29/09/2011 21/04/2019 2712 BX Mon 07 25 24 -3 36 0 64 04/04/2011 25/03/2019 5413 V694 Mon 07 25 51.2 -7 44 8 298 03/03/2011 12/04/2019 3614 NQ Gem 07 31 54.5 24 30 12.5 76 01/04/2013 18/04/2019 3015 GH Gem 07 4 4.9 12 2 12 9 10/03/2016 15/02/2019 9216 CQ Dra 12 30 06 69 12 04 34 11/06/2015 11/05/2019 717 TX CVn 12 44 42 36 45 50.6 68 10/04/2011 28/04/2019 2018 RW Hya 13 34 18 - 25 22 48.9 18 28/06/2017 14/07/2018 30819 IV Vir 14 16 34.3 -21 45 50 10 28/02/2015 11/07/2018 31120 T CrB 15 59 30.1 25 55 12.6 283 01/04/2012 12/05/2019 621 AG Dra 16 01 40.5 66 48 9.5 584 03/04/2013 15/05/2019 322 AS 210 16 51 20.4 -26 00 26.7 2 14/06/2018 07/07/2018 31523 V503 Her 17 36 46 23 18 18 5 05/06/2013 15/05/2018 36824 RS Oph 17 50 13.2 -6 42 28.4 48 23/03/2011 20/07/2018 30225 V934 Her 17 06 34.5 +23 58 18.5 30 09/08/2013 31/08/2018 26026 RT Ser 17 39 52.0 -11 56 38.8 2 26/06/2012 13/07/2018 30927 AS 245 17 51 00.9 -22 19 35.1 1 15/07/2018 15/07/2018 30728 AS 270 18 05 33.7 -20 20 38 6 01/08/2013 07/07/2018 31529 AS 289 18 12 22.1 -11 40 07 3 26/06/2012 15/06/2018 33730 YY Her 18 14 34.3 20 59 20 27 25/05/2011 26/09/2018 23431 FG Ser 18 15 06.2 0 18 57.6 7 26/06/2012 22/06/2018 33032 StHa 149 18 18 55.9 27 26 12 6 05/08/2013 13/07/2018 30933 V443 Her 18 22 08.4 23 27 20 54 18/05/2011 11/12/2018 15834 FN Sgr 18 53 52.9 -18 59 42 9 10/08/2013 15/07/2018 30735 V919 Sgr 19 03 46 -16 59 53.9 7 10/08/2013 10/12/2018 15936 V1413 Aql 19 03 51.6 16 28 31.7 13 10/08/2013 10/12/2018 15937 V335 Vul 19 23 14 +24 27 39.7 11 14/08/2016 26/07/2018 29638 BF Cyg 19 23 53.4 29 40 25.1 154 01/05/2011 22/04/2019 2639 CH Cyg 19 24 33 50 14 29.1 726 21/04/2011 15/05/2019 340 HM Sge 19 41 57.1 16 44 39.9 13 20/07/2013 23/09/2018 23741 QW Sge 19 45 49.6 18 36 50 11 14/08/2016 26/07/2018 29643 CI Cyg 19 50 11.8 35 41 3.2 206 25/08/2010 12/04/2019 3644 StHa 169 19 51 28.9 46 23 6 5 12/05/2016 08/07/2018 31445 EF Aql 19 51 51.7 -05 48 16.7 1 11/11/2018 11/11/2018 18846 TCPJ19544251+172228119 54 42.9 +17 22 12.7 59 09/08/2018 31/10/2018 19947 V1016 Cyg 19 57 4.9 39 49 33.9 18 15/04/2015 10/12/2018 15948 RR Tel 20 04 18.5 -55 43 33.2 3 08/09/2017 30/10/2017 56549 PU Vul 20 21 12 21 34 41.9 21 20/07/2013 10/11/2018 18950 LT Del 20 35 57.3 20 11 34 17 28/11/2015 28/09/2018 23251 ER Del 20 42 46.4 8 40 56.4 11 02/09/2011 20/10/2018 21052 V1329 Cyg 20 51 1.1 35 34 51.2 20 08/08/2015 09/01/2019 12953 V407 Cyg 21 2 13 45 46 30 12 14/03/2010 18/04/201054 StHa 190 21 41 44.8 2 43 54.4 21 31/08/2011 21/10/2018 20955 AG Peg 21 51 1.9 12 37 29.4 252 06/12/2009 24/12/2018 14556 V627 Cas 22 57 41.2 58 49 14.9 33 06/08/2013 08/01/2019 13057 Z And 23 33 39.5 48 49 5.4 151 30/10/2010 15/02/2019 9258 R Aqr 23 43 49.4 -15 17 4.2 175 20/11/2010 30/12/2018 139

Symbiotic like59 SS Lep 06 04 59.1 -16 29 04.0 8 17/02/2018 14/02/2019 93

Symbiotics observed in January-March, 2019 1/2


Id. Observer Date Res. Id. Observer Date Res.AG Dra V. Marik 12/02/2019 3715 7401 660 EG And J. Foster 14/10/2018 3832 7397 634AG Dra D. Boyd 25/02/2019 3901 7380 1122 EG And T. Lester 15/11/2018 4031 7960 14000AG Dra F. Teyssier 27/02/2019 4200 7110 11000 EG And F. Sims 31/12/2018 3726 7275 978AG Dra T. Lester 13/03/2019 4031 7950 14000 EG And F. Campos 06/01/2019 3816 7364 736AG Dra U. Sollecchia 17/03/2019 6365 6748 8543 EG And J. Guarro 11/01/2019 4053 7499 9000AG Dra F. Sims 18/03/2019 3727 7276 1008 EG And F. Sims 17/01/2019 3727 7275 811AG Dra C. Buil 22/03/2019 3498 5955 322 EG And J. Guarro 25/01/2019 4053 7499 9000AG Dra U. Sollecchia 22/03/2019 6728 7085 9851 EG And F. Campos 01/02/2019 3822 7333 846AG Dra O. Garde 22/03/2019 3915 7591 11000 EG And J. Guarro 03/02/2019 4053 7499 9000AG Dra F. Campos 22/03/2019 3840 7382 917 EG And J. Guarro 06/02/2019 4053 7499 9000AG Dra C. Buil 23/03/2019 3499 6051 326 EG And J. Guarro 08/02/2019 4053 7499 9000AG Dra O. Garde 23/03/2019 4080 7582 11000 EG And J. Guarro 11/02/2019 4053 7499 9000AG Dra J. Guarro 23/03/2019 4056 7671 9000 EG And J. Guarro 14/02/2019 4053 7499 9000AG Dra T. Lester 24/03/2019 4031 7950 14000 EG And J. Guarro 18/02/2019 4053 7499 9000AG Dra U. Sollecchia 24/03/2019 6506 6897 8770 GH Gem F. Sims 09/02/2019 3727 7276 893AG Dra D. Boyd 24/03/2019 3900 7380 1136 GH Gem F. Campos 15/02/2019 3900 7285 763AG Dra C. Boussin 24/03/2019 3701 7571 501 NQ Gem F. Sims 03/01/2019 3727 7276 973AG Dra S. Charbonnel 24/03/2019 3917 7593 11000 NQ Gem F. Sims 08/02/2019 3726 7275 931AG Dra F. Sims 25/03/2019 3727 7276 1021 NQ Gem D. Boyd 24/02/2019 3901 7380 1105AG Dra S. Charbonnel 25/03/2019 3917 7118 11000 NQ Gem J. Guarro 03/03/2019 3980 7762 9000AG Dra S. Charbonnel 27/03/2019 3917 7118 11000 NQ Gem J. Guarro 25/03/2019 4053 7763 9000AG Dra O. Garde 28/03/2019 4080 7586 11000 NQ Gem S. Charbonnel 28/03/2019 3917 7118 11000AG Dra C. Boussin 28/03/2019 3701 7571 505 omi Cet J. Guarro 14/01/2019 4053 7499 9000AG Dra F. Teyssier 30/03/2019 4300 7100 11000 omi Cet J. Guarro 21/01/2019 3980 7763 9000AG Dra U. Sollecchia 30/03/2019 6506 6897 8670 omi Cet J. Guarro 08/02/2019 4053 7499 9000AG Dra U. Sollecchia 31/03/2019 6509 6893 8732 omi Cet J. Guarro 09/02/2019 4053 7499 9000AG Dra F. Sims 01/04/2019 3727 7275 985 SS Lep F. Sims 22/01/2019 3727 7276 918AG Dra T. Lester 02/04/2019 4031 7950 14000 SS Lep J. Guarro 06/02/2019 4053 7499 9000AXPer P. Somogyi 18/01/2019 3609 7886 683 SS Lep F. Sims 12/02/2019 3727 7276 941AXPer F. Campos 24/01/2019 3822 7363 963 SS Lep J. Guarro 14/02/2019 4053 7499 9000AXPer D. Boyd 28/01/2019 3901 7380 1118 stHa 32 F. Sims 25/01/2019 3725 7274 839AXPer F. Sims 12/02/2019 3727 7276 899 StHa 55 F. Sims 02/01/2019 3901 7270 978AXPer C. Boussin 17/02/2019 3701 7571 501 StHa 55 F. Sims 02/01/2019 3901 7270 978AXPer D. Boyd 22/02/2019 3901 7380 1094 StHa 55 F. Sims 24/01/2019 3926 7266 923AXPer C. Boussin 26/02/2019 3701 7571 502 StHa 55 F. Sims 08/02/2019 3726 7275 952AXPer F. Sims 14/03/2019 3725 7274 1002 SU Lyn F. Campos 07/01/2019 3801 7343 794AXPer F. Sims 15/03/2019 3727 7275 995 SU Lyn F. Campos 10/01/2019 6344 7111 4821AXPer C. Boussin 18/03/2019 3701 7571 508 SU Lyn F. Sims 11/01/2019 3726 7275 889AXPer F. Campos 24/03/2019 3854 7395 890 SU Lyn F. Sims 20/01/2019 3727 7276 858AXPer D. Boyd 24/03/2019 3901 7380 1105 SU Lyn J. Guarro 26/01/2019 4053 7499 9000BD Cam F. Sims 02/01/2019 3727 7276 972 SU Lyn F. Teyssier 03/02/2019 4034 7115 11000BD Cam F. Campos 07/01/2019 3804 7348 818 SU Lyn F. Sims 08/02/2019 3727 7276 954BD Cam J. Guarro 25/01/2019 3976 7753 9000 SU Lyn U. Sollecchia 08/02/2019 6392 6772 8710BD Cam F. Sims 27/01/2019 3727 7276 860 SU Lyn J. Guarro 09/02/2019 4053 7499 9000BD Cam V. Marik 12/02/2019 3724 7401 605 SU Lyn F. Sims 12/02/2019 3725 7274 967BD Cam C. Boussin 17/02/2019 3701 7571 505 SU Lyn F. Teyssier 13/02/2019 4034 7115 11000BX Mon F. Sims 22/01/2019 3726 7275 925 SU Lyn C. Boussin 16/02/2019 3701 7571 502BX Mon F. Campos 05/02/2019 3801 7324 881 SU Lyn J. Guarro 16/02/2019 4053 7499 9000BX Mon F. Sims 07/02/2019 3725 7274 952 SU Lyn D. Boyd 21/02/2019 3901 7380 1084BX Mon U. Sollecchia 17/02/2019 6393 6757 8524 SU Lyn F. Teyssier 25/02/2019 4034 7115 11000BX Mon J. Guarro 18/02/2019 4053 7499 9000 SU Lyn C. Boussin 26/02/2019 3701 7571 501BX Mon D. Boyd 24/02/2019 3901 7380 1125 SU Lyn J. Guarro 02/03/2019 4053 7762 9000BX Mon F. Campos 16/03/2019 3888 7427 864 SU Lyn F. Teyssier 07/03/2019 4035 7115 11000BX Mon F. Teyssier 25/03/2019 4300 7100 11000 SU Lyn T. Lester 09/03/2019 4031 7950 14000BX Mon J. Guarro 25/03/2019 4053 7762 9000 SU Lyn J. Guarro 10/03/2019 4053 7762 9000CH Cyg J. Guarro 05/01/2019 4053 7499 9000 SU Lyn F. Campos 14/03/2019 6308 7074 6761CH Cyg F. Teyssier 15/02/2019 4200 7100 11000 SU Lyn F. Sims 18/03/2019 3726 7275 985CH Cyg T. Lester 24/03/2019 4031 7950 14000 SU Lyn O. Garde 20/03/2019 4040 7586 11000CH Cyg F. Teyssier 30/03/2019 3969 7348 11000 SU Lyn T. Lester 24/03/2019 4031 7950 14000CQ Dra V. Marik 12/02/2019 3697 7401 610 SU Lyn J. Guarro 25/03/2019 4053 7763 9000CQ Dra F. Campos 15/02/2019 3895 7346 804 SU Lyn C. Boussin 29/03/2019 3701 7571 506CQ Dra J. Guarro 23/03/2019 4053 7761 9000 SU Lyn JMichelet 31/03/2019 3800 7399 578

Range Range


Symbiotics observed in January-March, 2019 1/2

Id. Observer Date Res. Id. Observer Date Res.T CrB F. Teyssier 15/02/2019 4500 7100 11000 V694 Mon F. Campos 06/01/2019 3798 7344 798T CrB C. Boussin 16/02/2019 3701 7571 503 V694 Mon J. Guarro 12/01/2019 4053 7499 9000T CrB P. Somogyi 24/02/2019 3602 7880 685 V694 Mon F. Sims 19/01/2019 3727 7275 865T CrB F. Campos 16/03/2019 3886 7427 909 V694 Mon F. Sims 19/01/2019 3727 7275 881T CrB C. Boussin 30/03/2019 3701 7571 504 V694 Mon F. Sims 20/01/2019 3727 7275 875TX CVn T. Lester 13/03/2019 4031 7950 14000 V694 Mon F. Sims 23/01/2019 3727 7276 948TX CVn F. Sims 15/03/2019 3727 7276 1025 V694 Mon F. Sims 24/01/2019 3727 7276 954TX CVn C. Buil 21/03/2019 3562 5966 440 V694 Mon J. Guarro 25/01/2019 3989 7756 9000TX CVn F. Campos 22/03/2019 3842 7381 925 V694 Mon J. Guarro 26/01/2019 4053 7499 9000TX CVn C. Buil 22/03/2019 3562 6235 344 V694 Mon F. Sims 27/01/2019 3727 7276 922TX CVn D. Boyd 28/03/2019 3901 7380 1100 V694 Mon F. Sims 28/01/2019 3726 7274 926TX CVn J. Guarro 28/03/2019 4094 7727 9000 V694 Mon F. Teyssier 03/02/2019 4034 7115 11000TX CVn S. Charbonnel 29/03/2019 3917 7118 11000 V694 Mon D. Boyd 04/02/2019 3902 7380 1101TX CVn J. Guarro 29/03/2019 4062 7592 9000 V694 Mon F. Campos 05/02/2019 3800 7326 874UV Aur J. Guarro 15/01/2019 4053 7499 9000 V694 Mon F. Sims 07/02/2019 3727 7276 951UV Aur F. Sims 23/01/2019 3726 7276 932 V694 Mon J. Guarro 11/02/2019 4053 7499 9000UV Aur D. Boyd 30/01/2019 3901 7379 1042 V694 Mon F. Sims 12/02/2019 3725 7274 958UV Aur V. Marik 12/02/2019 3697 7401 605 V694 Mon F. Teyssier 13/02/2019 4200 7100 11000UV Aur D. Boyd 26/02/2019 3901 7380 1119 V694 Mon C. Buil 15/02/2019 3447 7928 730UV Aur D. Boyd 28/03/2019 3900 7380 1116 V694 Mon J. Guarro 19/02/2019 4053 7499 9000V1329 Cyg D. Boyd 09/01/2019 3901 7380 1095 V694 Mon U. Sollecchia 21/02/2019 6393 6756 9050V1329 Cyg D. Boyd 09/01/2019 3901 7380 1095 V694 Mon D. Boyd 21/02/2019 3901 7379 1100V471 Per F. Campos 24/01/2019 3822 7362 930 V694 Mon V. Marik 24/02/2019 4100 7380 608V471 Per D. Boyd 14/02/2019 3901 7380 1123 V694 Mon F. Teyssier 26/02/2019 4034 7115 11000V627 Cas D. Boyd 08/01/2019 3901 7380 1106 V694 Mon Ibrahima 28/02/2019 4043 8420 600Z And J. Guarro 07/01/2019 4053 7499 9000 V694 Mon U. Sollecchia 03/03/2019 6392 6762 8568Z And J. Guarro 07/01/2019 4053 7499 9000 V694 Mon J. Guarro 03/03/2019 3980 7762 9000Z And D. Boyd 09/01/2019 3901 7380 1057 V694 Mon J. Guarro 10/03/2019 3980 7762 9000Z And J. Guarro 11/01/2019 4053 7499 9000 V694 Mon F. Teyssier 11/03/2019 4033 7115 11000Z And J. Guarro 25/01/2019 3992 7743 9000 V694 Mon T. Lester 13/03/2019 4031 7950 14000Z And D. Boyd 15/02/2019 3901 7380 1111 V694 Mon F. Campos 16/03/2019 3888 7427 879ZZ CMi U. Sollecchia 06/02/2019 6393 6772 7688 V694 Mon P. Somogyi 17/03/2019 6505 6614 15916ZZ CMi G. Martineau 20/02/2019 3602 7598 1100 V694 Mon F. Teyssier 20/03/2019 4300 7100 11000ZZ CMi D. Boyd 22/02/2019 3900 7380 1121 V694 Mon F. Teyssier 22/03/2019 4060 7110 11000ZZ CMi T. Lester 09/03/2019 4031 7950 14000 V694 Mon J. Guarro 23/03/2019 4053 7761 9000ZZ CMi F. Campos 22/03/2019 3842 7385 831 V694 Mon P. Somogyi 23/03/2019 3856 4013 4494

V694 Mon F. Teyssier 24/03/2019 4036 7115 11000V694 Mon D. Boyd 25/03/2019 3901 7380 1130V694 Mon J. Guarro 28/03/2019 4053 7762 9000V694 Mon J. Guarro 30/03/2019 4053 7762 9000

Range Range

AG Dra 2018

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

SYMBIOTICS

Continuous observations of AG Dra upon the request of J. Merc and R. GàlisOngoing survey until the next outburst ex-pected during Spring 2019.Still in quiescent state late April.


9

9.5

102458100 2458190 2458280 2458370 2458460 2458550 2458640

AG Dra (V)

9.5

102458500 2458590 2458680

AG Dra (V)

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

5

10

15

20

25

rela

tive

in

ten

sity

AG Dra 2019-04-19 23:39:24 R = 549 Ibrahima

Spectrum obtnained by Ibrahima with Lhires III (150 l/mm)

Date Time JD Observer Res Range12/02/2019 23:06 2458527.469 VMA 660 3715-740025/02/2019 23:13 2458540.489 DBO 1122 3901-738027/02/2019 2:53 2458541.649 FMT 11000 4200-711013/03/2019 6:09 2458555.800 LES 14000 4030-795017/03/2019 19:33 2458560.373 SOL 8543 6364-674818/03/2019 6:35 2458560.786 FAS 1008 3726-727522/03/2019 1:46 2458564.627 BUI 322 3497-595522/03/2019 18:41 2458565.351 SOL 9851 6728-708522/03/2019 21:03 2458565.426 OGA 11000 3915-759122/03/2019 21:25 2458565.385 PSO 2663 6463-717022/03/2019 22:11 2458565.421 PSO 1844 4507-522322/03/2019 23:46 2458565.508 FCA 917 3840-738122/03/2019 23:53 2458565.481 PSO 3346 7992-869123/03/2019 1:20 2458565.611 BUI 326 3498-605123/03/2019 21:00 2458566.424 OGA 11000 4080-758223/03/2019 23:39 2458566.513 JGF 9000 4055-767024/03/2019 4:44 2458566.755 LES 14000 4030-795024/03/2019 4:44 2458566.755 LES 14000 4030-795024/03/2019 18:41 2458567.361 SOL 8770 6505-689724/03/2019 21:20 2458567.424 DBO 1136 3900-737924/03/2019 21:59 2458567.428 CBO 501 3700-757024/03/2019 23:21 2458567.508 SCH 11000 3917-759325/03/2019 7:16 2458567.814 FAS 1021 3726-727525/03/2019 23:19 2458568.507 SCH 11000 3917-711727/03/2019 23:42 2458570.523 SCH 11000 3917-711728/03/2019 20:49 2458571.416 OGA 11000 4080-758628/03/2019 21:12 2458571.399 CBO 505 3700-757030/03/2019 3:06 2458572.653 FMT 11000 4300-710030/03/2019 19:12 2458573.364 SOL 8670 6505-689630/03/2019 19:12 2458573.364 SOL 8670 6505-689630/03/2019 22:13 2458573.418 PSO 3351 8006-869131/03/2019 18:31 2458574.343 SOL 8732 6509-689201/04/2019 0:41 2458574.564 SCH 11000 3917-759301/04/2019 5:50 2458574.754 FAS 985 3726-727402/04/2019 4:21 2458575.732 LES 14000 4030-795004/04/2019 21:02 2458578.398 FCA 878 3764-728305/04/2019 19:01 2458579.349 SOL 8962 6505-689406/04/2019 22:25 2458580.423 PSO 2778 6464-717006/04/2019 23:29 2458580.479 PSO 1896 4535-525010/04/2019 21:55 2458584.436 DBO 1132 3900-737910/04/2019 23:06 2458584.484 MVE 571 3630-780011/04/2019 23:24 2458585.504 IBR 537 4100-739011/04/2019 23:34 2458585.498 CBO 502 3700-757012/04/2019 0:32 2458585.557 SCH 11000 3917-759312/04/2019 0:49 2458585.563 FMT 11000 4300-710012/04/2019 21:58 2458586.436 GMYB 923 3704-740013/04/2019 5:33 2458586.743 FAS 990 3726-727513/04/2019 21:53 2458587.433 FCA 6110 4318-504013/04/2019 23:28 2458587.495 FCA 4792 6458-722514/04/2019 3:58 2458587.724 LES 14000 4030-795014/04/2019 5:44 2458587.751 FAS 990 3726-727517/04/2019 19:41 2458591.362 OGA 11000 4080-758619/04/2019 20:15 2458593.389 BER 3884 4608-507319/04/2019 20:45 2458593.388 DBO 999 3901-737919/04/2019 23:39 2458593.528 IBR 549 4130-740021/04/2019 0:05 2458594.529 CBO 503 3700-757022/04/2019 3:20 2458595.689 LES 14000 4030-795024/04/2019 20:52 2458598.429 SOL 7815 6509-689225/04/2019 21:24 2458599.415 DBO 1087 3901-738026/04/2019 20:40 2458600.388 FCA 6683 6457-722526/04/2019 20:44 2458600.400 SOL 8538 6509-689226/04/2019 22:18 2458600.455 FCA 5268 4333-505427/04/2019 6:44 2458600.792 FAS 874 3726-727527/04/2019 21:21 2458601.439 JGF 9000 4052-776228/04/2019 20:15 2458602.373 FMT 11000 4300-730030/04/2019 20:26 2458604.381 FMT 11000 4060-7300

AG Dra 2019 Log of observations 2019-02 to 04SYMBIOTICS


VMA Vincent MarikDBO David BoydFMT François TeyssierLES Tim LesterSOL Umberto SollecchiaFAS Woody SimsOGA Olivier GardePSO Peter SomogyiFCA Fran CamposBUI Christian BuilJGF Joan Guarro FloCBO Christophe BoussinSCH Stéphane CharbonnelMVE Michel VerlindenGM Gérard MartineauYB Yvonne BuchetBER Paolo BerardiIBR Ibrahima Diarrassouba,

-800 -400 0 400 800Radial velocity [km/s]

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AG Dra H alpha

2019-02-27

2019-03-13

2019-03-22

2019-03-23

2019-03-24

2019-03-24

2019-03-25

2019-03-27

2019-03-28

2019-04-01

2019-04-02

2019-04-12

2019-04-12

2019-04-14

2019-04-17

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2019-04-27

2019-04-28

2019-04-30


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AG Dra H beta

2019-02-27

2019-03-13

2019-03-22

2019-03-23

2019-03-24

2019-03-24

2019-03-25

2019-03-27

2019-03-28

2019-04-01

2019-04-02

2019-04-12

2019-04-12

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2019-04-22

2019-04-27

2019-04-28

2019-04-30


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AG Dra He II 4686

2019-02-27

2019-03-13

2019-03-22

2019-03-23

2019-03-24

2019-03-24

2019-03-25

2019-03-27

2019-03-28

2019-04-01

2019-04-02

2019-04-12

2019-04-12

2019-04-14

2019-04-17

2019-04-22

2019-04-27

2019-04-28

2019-04-30

AG Dra 2018SYMBIOTICS


Pages 10-11: profiles of selected lines from Echelle spectra (R = 9000 to 13000)


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AG Dra He I 5875

2019-02-27

2019-03-13

2019-03-22

2019-03-23

2019-03-24

2019-03-24

2019-03-25

2019-03-27

2019-03-28

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AG Dra He I 6678

2019-02-27

2019-03-13

2019-03-22

2019-03-23

2019-03-24

2019-03-24

2019-03-25

2019-03-27

2019-03-28

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2019-04-02

2019-04-12

2019-04-12

2019-04-14

2019-04-17

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2019-04-30


ARAS Eruptive Stars Information Letter #41 2019-01 - p. 10 ARAS Eruptive Stars Information Letter #41 2019-01 - p. 11

8540 8550 8560 8570 8580 8590 8600 8610

JD - 2450000

60

70

80AG Dra - EW Halpha

8540 8550 8560 8570 8580 8590 8600 8610

JD - 2450000

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30AG Dra - EW Hbeta

8540 8550 8560 8570 8580 8590 8600 8610

JD - 2450000

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1AG Dra - EW HeI4922

8540 8550 8560 8570 8580 8590 8600 8610

JD - 2450000

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8540 8550 8560 8570 8580 8590 8600 8610

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20AG Dra - EW HeII4686

8540 8550 8560 8570 8580 8590 8600 8610

JD - 2450000

6

6.5

7

7.5

8AG Dra - EW RamanOVI6830

AG Dra 2019 02 to 04, 2019SYMBIOTICS


Equivalent widths of selected lines from Echelle spectra

3500 4000 4500 5000 5500 6000

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AG Dra 2019-03-23 01:20:33 R = 326 C Buil

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AG Dra 2019-04-19 20:15:47 R = 3884 Paolo Berardi

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AG Dra 2019-03-22 23:53:50 R = 3346 P. Somogyi

UVEX prototype C. Buil showing the Balmer jump

Near IR spectrum obtained by Peter Somogyi with Lirhes III (600 l/mm) Ca II triplet in absorption. OI in fain emission.



6500 6600 6700 6800 6900

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AG Dra 2019-04-24 20:52:27 R = 7815 Umberto Sollecchia




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AG Dra H alpha

2019-03-24

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2019-04-26


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AG Dra He I 6678

2019-03-24

2019-03-30

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2019-04-19

2019-04-24

2019-04-26

Lines profiles from Umbert Sollecchia spectra (R = 8000)

AX PerSYMBIOTICS

Coordinates (2000.0)R.A. 01 36 22.7Dec +54 15 02.4Mag 11.5 (2019-01)


V mag with respectect to phase. Current cycle: brown squares.

10

11

12

130 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1

10

10.5

11

11.5

12

12.52458250 2458430 2458610

AX Per (V)

8

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13

142444000 2446000 2448000 2450000 2452000 2454000 2456000 2458000 2460000

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AX Per 2019-03-24 19:21:19 R = 890 F. Campos

AAVSO (V) light curve and ARAS Spectra (blue dots)

The prototypical symbiotic AX Per is emerging from eclipse. The light-curve is significantly different from other orbital cycles. Spectra obtained by David Boyd and Fran Campos in March indicate that AX Per entered in classical symbiotic outburst with notably the desappearence of [Fe VII] high excitation lines (see e.g. F. Campos' spectrum below)

AX PerSYMBIOTICS


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4000 4500 5000 5500 6000 6500 7000

Wavelength (Angstrom)

2019-01-28.8172019-02-22.8232019-03-24.8262019-04-10.846

AX Per 2019 D. Boyd

Flux

(erg

.cm

-2.s

-1.A

-1)

Flux calibrated spectra obtained by David Boyd with LISA (R = 1000)

AX PerSYMBIOTICS


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AX Per

2019-04-10.846

2019-03-24.826

2019-03-14.116

2019-02-22.823

2019-02-12.101

2019-01-28.817

2018-12-30.115

Spectroscopic evolution of the outburst with spectra obtained by Woody Sims and David Boyd with a LISA (R = 1000). The blend NIII/CIII strongly inevesaed when [Fe VII] vanished

[Fe

VII]

6087

NIII

/CIII

464

0-60


AX PerSYMBIOTICS


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AX Per Christophe Boussin

2019-04-24.854

2019-04-20.874

2019-04-11.867

2019-02-26.918

2019-02-17.865

The outburst monitored by Chistophe Boussin with ALPY600

Line analysis by David Boyd on calibrated flux spectrausing PlotSpectra (Tim Lester)

AX PerSYMBIOTICS

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H alpha

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H beta

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[Fe VII] 6087

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He II 4684

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He I 5876

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He I 6678

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He I 5876 / He I 6678

Flux of Ha, Hb, [Fe VII], He II 4686, He I 5876, He I 6678 in units of 10-12 erg.cm-2.s-1

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8420 8440 8460 8480 8500 8520 8540 8560 8580 8600

He II / H beta

Diagnostic lines ratios - The ratio He I triplets/singlets decreases before the outburst detected by the weakening of [Fe VII]. It is relevant to orbital phase.

Date JD -2450000 Phase Ha Hb He II [Fe VII] 6087 He I 5876 He I 667821-nov-18 8444.351 0.000 31.8 5.1 4.6 1.57 2.7 0.513-déc-18 8466.243 0.032 32.3 4.8 4.6 1.26 2.4 0.529-déc-18 8482.355 0.056 31.4 5.0 4.8 1.38 2.2 0.528-janv-19 8512.348 0.100 41.0 5.9 6.1 1.21 2.3 1.622-févr-19 8537.405 0.136 46.5 8.8 8.2 0.88 1.7 1.924-mars-19 8567.330 0.180 110.1 18.9 15.6 0.17 5.1 9.410-avr-19 8584.337 0.205 147.7 36.8 19.4 0.00 7.4 12.4

in units of 10-12 erg.cm-2.s-1


AX PerSYMBIOTICS


The symbiotic star AX Per is going into strong outburstATel #12660J. Merc (UPJS in Kosice, Charles University), R. Galis (UPJS in Kosice), F. Teyssier, D. Boyd, W. Sims, C. Boussin, F. Campos (ARAS)on 13 Apr 2019; 11:21 UTCredential Certification: Jaroslav Merc ([email protected])

AX Per is a well-known eclipsing symbiotic binary consisting of a giant of type M4.5 III (Muer-set & Schmid 1999, A&AS, 137, 473) and probably a white dwarf. The orbital period of the bi-nary system is around 680 days (Mikolajewska & Kenyon 1992, AJ, 103, 579). The light curve of AX Per is characterized by the wave-like variations whose shape is changing from cycle to cycle. After major outbursts of the system in 1988-1992, a new activity stage has begun in 2007, with minor outbursts observed in 2009, 2010, 2012 and 2014 (Munari & Siviero 2009, CBET, No. 1757; Munari , Siviero, et al. 2010, CBET, No. 2555; ATel #4265, ATel #6382). All recent outbursts were sig-nificantly lower in magnitude (maximal V around 10) than the major outbursts in 90s (with V < 9).

In this Astronomer's Telegram, we report the beginning of a new outburst of AX Per with a strong increase in brightness. In the previous orbital cycle, the brightness of the symbiotic system reached the maximum of B=11.589 and V=10.873 (October 15, 2017; JD 2458042.319). During the binary eclipse in August/September 2018, the magnitudes decreased to the minimum of B=13.387 and V=12.355 on August 21, 2018 (JD 2458352.375). Since then, the brightness of AX Per has started to increase and the March 2019 measurements have shown that it has reached a similar level or was higher than the previous maximum of B=11.516 and V=10.652 (March 24, 2019; JD 2458567.330). Our observation obtained on April 10, 2019 (JD 2458584.337) indicate that the AX Per brightness continues to rise (B=11.109 and V=10.330) in what looks like a promising major outburst of this symbiotic binary.

The low resolution spectroscopic observations (R < 1000) obtained during March and April 2019 showed significant changes in the prominent emission lines and in the continuum compared to the spectra acquired at the end of 2018. We note the disappearance of the highly ionized lines (e. g. [Fe VII]) or the change of the He I singlet/triplet ratio. Several emission lines of the He I which were not observable are fairly strong in the recent spectra, and similar behavior is observed in the case of Fe II lines. The Balmer lines equivalent widths have also increased significantly (1.3 times since December 2018). Nebular-to-auroral line ratio of [OIII] 5007/4363 has increased from 0.7 to 1.6. This behavior points to a classical symbiotic outburst during which a accreting layer on white dwarf expands and cools down. We will continue the photometric and spectroscopic monitoring of the AX Per current outburst. It will be interesting to see if the outburst is another of a series of minor out-bursts, or we will finally observe a major outburst of this symbiotic system. Recent spectroscopic observations could be found in the ARAS Spectral Database .

BD Cam

Coordinates (2000.0)R.A. 03 42 09.3Dec +63 13 00.0Mag

SYMBIOTICS


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BD Cam 2019-01-02 02:15:53 R = 972 Forrest Sims

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BD Cam 2019-02-12 21:24:12 R = 605 V. Marik

Still no emission lines in visible range


BD CamSYMBIOTICS

-1000 -500 0 500 1000

velocity (km/s)

0.2

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1.6Halpha 2019-01-25

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velocity (km/s)

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1.4Hbeta 2019-01-25

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BD Cam 2019-01-25 21 R = 9000 J. Guarro


SYMBIOTICS

BX Mon

Coordinates (2000.0)R.A. 19 23 53.5Dec +29 40 29.17Mag 9.6


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102457910 2458275 2458640

BX Mon

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BX Mon 2019-01-22 06:49:20 R = 925 Forrest Sims

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BX Mon 2019-02-05 20:07:11 R = 881 FPC

SYMBIOTICS

BX Mon

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BX Mon 2019-02-18 20:57:22 R = 9000 J. Guarro

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velocity (km/s)

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2Hbeta 2019-02-18

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velocity (km/s)

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5Halpha 2019-02-17

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velocity (km/s)

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1.3FeII5018 2019-03-25

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velocity (km/s)

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2Hbeta 2019-03-25

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velocity (km/s)

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4.5Halpha 2019-03-25


CH Cyg

Coordinates (2000.0)R.A. 19 24 33.1Dec +50 14 29.1Mag ~ 7.2 (2017-07)

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)


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92458200 2458260 2458320 2458380 2458440 2458500 2458560 2458620

CH Cygni (V)

AAVSO V lightcurve (daily mean) and ARAS spectra (blue dots) from 2019-01-05 to 04-20

The interesting thing is that CH Cyg (V and B) its getting fainter (abruptly) and in a relatively short time period; When this happened in the past, it indicated a jet ejection and dimming of the LC by the ejecta/dust in the inner circumbi-nary environment. So close spectral and pho-tometric monitoring in the next few months would be of a great interest.Margarita Karovska (communication to ARAS observers)

After its fading in the second part of 2018, CH Cygni remains at low luminosity (~ 8,5) but a short flare late march.


CH CygSYMBIOTICS

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92458200 2458260 2458320 2458380 2458440 2458500 2458560 2458620

CH Cygni (V)

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CH Cyg H alpha

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2019-03-30

2019-04-11

2019-04-20

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CH Cyg H beta

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2019-03-30

2019-04-11

2019-04-20

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CH Cyg [O III]5007]

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2019-03-24

2019-03-30

2019-04-11

2019-04-20

The flare monitored by Echelle spectra(J. Guarro, T. Lester, F. Teyssier)

CH Cyg Echelle spectraSYMBIOTICS


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2019-02-15.1812019-03-24.3432019-03-30.1852019-04-11.1342019-04-20.048

CH Cyg

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CH Cyg

2019-04-20.048

2019-04-11.134

2019-03-30.185

2019-03-24.343

2019-02-15.181

The emission of Na I D is strongly anti-correlated with the luminosity

Variation of [OIII] profile

CQ DraSYMBIOTICS

Coordinates (2000.0)R.A. 12 30 06.7Dec +69 12 04.Mag V 4.9


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CQ Dra 2019-02-12 23:44:34 R = 610 V. Marik

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CQ Dra 2019-02-15 22:13:43 R = 804 F. Campos

No emission lines

CQ DraSYMBIOTICS

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ten

sity

CQ Dra 2019-03-23 22:12:04 R = 9000 J. Guarro

-500 0 500

velocity (km/s)

0.2

0.4

0.6

0.8

1

1.2Halpha 2019-03-23

-500 0 500

velocity (km/s)

0.2

0.4

0.6

0.8

1

1.2

1.4

1.6Hbeta 2019-03-23


GH GemSYMBIOTICS


Coordinates (2000.0)R.A. 07 01 25.3Dec +12 08 05.7Mag V

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

GH Gem 2019-02-09 04:13:40 R = 893 Forrest Sims

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

GH Gem 2019-02-15 20:10:39 R = 763 F. Campos

12

12.5

13

13.5

142457180 2457545 2457910 2458275 2458640 2459005

GH Gem

NQ GemSYMBIOTICS



4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

NQ Gem 2019-01-03 05:24:02 R = 973 Forrest Sims

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

5

6

flu

x (

erg

cm

- 2 s

- 1 A

- 1)

10-12 NQ Gem 2019-02-24 19:23:37 R = 1105 D. Boyd

-500 0 500

velocity (km/s)

0.5

1

1.5

2

2.5Halpha 2019-03-28

-500 0 500

velocity (km/s)

0.2

0.4

0.6

0.8

1

1.2

1.4

1.6Hbeta 2019-03-28

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2re

lative

in

ten

sity

NQ Gem 2019-03-03 22:22: R = 9000 J. Guarro

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

NQ Gem 2019-03-28 20:41:51 R = 575551 S. Charbonnel

NQ GemSYMBIOTICS

omi CetSYMBIOTICS

Coordinates (2000.0)R.A. 02 19 20.79Dec -02 58 39.4Mag V 5.5 (2019-02)

2

3

4

5

6

7

8

9

10

112457550 2457915 2458280 2458645

o Cet (Vis )

AAVSO Vis Light Curveand ARAS spectra (blue dots)

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

rela

tive

in

ten

sity

Omi Cet 2019-01-14 19:18:36 R = 9000 J. Guaro

-500 0 500

velocity (km/s)

0.6

0.7

0.8

0.9

1

1.1Halpha 2019-01-14

-500 0 500

velocity (km/s)

1.5

2

2.5

3

3.5

4

4.5Hbeta 2019-01-14

-500 0 500

velocity (km/s)

0

5

10

15

20Hgamma 2019-01-14

SS Lep= 17 LepSYMBIOTICS

Coordinates (2000.0)R.A. 06 04 59.1Dec -16 29 04.0Mag V

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

rela

tive

in

ten

sity

SS Lep 2019-01-22 06:05:09 R = 918 Forrest Sims

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

2.5

3

rela

tive

in

ten

sity

SS Lep 2019-02-12 04:03:33 R = 941 Forrest Sims

StHa 32SYMBIOTICS

Coordinates (2000.0)R.A. 04 37 45.6Dec -01 19 11.89Mag V 12.7


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

5

10

15

rela

tive

in

ten

sity

StHa 32 2019-01-25 04:15:11 R = 839 Forrest Sims

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

5

rela

tive

in

ten

sity


Ratio EW FluxOVI 6830 / Ha 0.04 0.05

He I 5876 / Hb 0.22 0.37

He II 4686 / Hb 0.70 0.58

StHa 55SYMBIOTICS

Coordinates (2000.0)R.A. 05 46 42.07Dec +06 43 47.07Mag V


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

StHa55 2019-02-08 04:12:46 R = 952 Forrest Sims

SU LynSYMBIOTICS

Coordinates (2000.0)R.A. 06 42 55.1Dec +55 28 27.2Mag V ~ 8.5


4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

0.2

0.4

0.6

0.8

1

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-11 SU Lyn 2019-02-21 19:15:52 R = 1084 D. Boyd

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

2.5

rela

tive

in

ten

sity

SU Lyn 2019-03-31 19:25:10 R = 578 J Michelet

0

1

2

3

4

5

6

7

8

9

Arbi

trary

uni

ts

-500 -250 250 500

Velocity (Km/sec)

Halpha 6562.8 - SU Lyn

2019-03-31.827

2019-03-25.818

2019-03-24.010

2019-03-20.773

2019-03-10.781

2019-03-09.137

2019-03-07.783

2019-03-02.876

2019-02-25.801

2019-02-16.904

2019-02-13.772

2019-02-09.968

2019-02-03.781

2019-01-26.878

0

0.5

1

1.5

2

2.5

3

3.5

Arbi

trary

uni

ts

-500 -250 250 500

Velocity (Km/sec)

[O III] 5006.84 - SU Lyn

2019-03-31.827

2019-03-25.818

2019-03-24.010

2019-03-20.773

2019-03-10.781

2019-03-09.137

2019-03-07.783

2019-03-02.876

2019-02-25.801

2019-02-16.904

2019-02-13.772

2019-02-09.968

2019-02-03.781

2019-01-26.878

SU LynSYMBIOTICS


Ha and [OIII] variations - Echelle spectra R = 9000 to 13000

T CrBSYMBIOTICS



4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

5

rela

tive

in

ten

sity

T CrB 2019-02-16 02:23:55 R = 503 Christophe Boussin

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

5

rela

tive

in

ten

sity

T CrB 2019-03-16 23:23:35 R = 909 F. Campos

9

9.5

10

10.52457000 2457365 2457730 2458095 2458460 2458825

T CrB

8000 8100 8200 8300 8400 8500 8600 8700

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

T CrB 2019-03-23 01:14:11 R = 3393 P. Somogyi

-1000 -500 0 500 1000

velocity (km/s)

0

1

2

3

4

5

6

7Halpha 2019-03-24

4500 4600 4700 4800 4900 5000 5100 5200

Wavelength (A)

0

1

2

3

4

5

rela

tive

in

ten

sity

T CrB 2019-03-30 23:20:14 R = 1901 P. Somogyi


T CrBSYMBIOTICS

TX CVnSYMBIOTICS


4000 4500 5000 5500 6000

Wavelength (A)

0

0.2

0.4

0.6

0.8

1

1.2

rela

tive

in

ten

sity

TX CVn 2019-03-21 23:11:14 R = 440 C. Buil


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.2

0.4

0.6

0.8

1

1.2

rela

tive

in

ten

sity

TX CVn 2019-03-15 06:14:45 R = 1025 Forrest Sims

4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

1

2

3

4

5

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-13 TX CVn 2019-03-28 21:51:23 R = 1100 D. Boyd

TX CVnSYMBIOTICS


TX CVnSYMBIOTICS

4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

TX CVn 2019-03-29 00:04:33 R = 11000 S. Charbonnel

-1000 -500 0 500 1000

velocity (km/s)

0.2

0.4

0.6

0.8

1

1.2Halpha 2019-03-29

-1000 -500 0 500 1000

velocity (km/s)

0.4

0.6

0.8

1

1.2

1.4Hbeta 2019-03-29


V471 PerSYMBIOTICS



4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

10

20

30

40

rela

tive

in

ten

sity

V471 Per 2019-01-24 20:08:42 R = 930 Fran Campos

4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

0.2

0.4

0.6

0.8

1

1.2

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-12 V471 Per 2019-02-14 19:19:51 R = 1123 D. Boyd

V627 CasSYMBIOTICS



4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

1

2

3

4

5

6

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-13 V627 Cas 2019-01-08 19:54:22 R = 1106 D. Boyd

V694 Mon = MWC 560SYMBIOTICS

Coordinates (2000.0)R.A. 07 25 51.28Dec -07 44 08.07Mag 9.0


8.5

9

9.5

10

10.5

112455500 2455865 2456230 2456595 2456960 2457325 2457690 2458055 2458420 2458785

V694 Mon

-3000 -2000 -1000 0 1000 2000 3000

velocity (km/s)

0

0.5

1

1.5

2

2.5

3

3.5

4

rela

tive

in

ten

sity

V694 Mon | H beta

2016-02-23

2019-03-22

-3000 -2000 -1000 0 1000 2000 3000

velocity (km/s)

0

2

4

6

8

10

12

rela

tive

in

ten

sity

V694 Mon | H beta

2016-02-23

2019-03-22

Fig. 3 - Comparison of Hb profiles during the two last optical outburts of V694 Mon - F. Teyssier R = 11000During the 2016 outburst, the classical broad absorption was strong with a maximum velocity ~ 2200 km.s-1

8.5

9

9.5

10

10.5

112457000 2457365 2457730 2458095 2458460 2458825

V694 Mon

V694 Mon is in strong optical out-burst, at V mag = 8.95 in 2019, April.The lines profiles are atypical for this star dring the current event. The emission lines of Balmer series, He I and Fe II shows a clas-sical P Cygni while the classical broad ab-sorption is absent or very weak (see Fig. 2)

Fig. 1 - AAVSO (Vis) Light Curve (15 days mean) and ARAS Spectra (blue dots)

-1000 -500 0 500 1000velocity (km/s)

0

5

10

15

arb

itra

ry u

nit

H alpha H beta Fe II 5169 |2019-03-13

H alpha

H beta

Fe II 5169

Fig. 2 - Ha, Hb and Fe II l 5169 profiles in the spectrum obtained by Tim Lester on 2019-03-13 (JD 2458556). The maximum veloc-ity of Ha is ~ 800 km.s-1. The P Cygni profiles peaks respectively at -85, -60 and -20 km.s-1.

8

9

10

11

122445500 2449150 2452800 2456450 2460100

V694 Mon



Fig. 3 - AAVSO (Vis) Light Curve (15 days mean) showing the two recent optical outburts (2016, 2018-2019) at the same level as 1990 one.

0

5E-13

1E-12

1.5E-12

2E-12

2.5E-12

3E-12

3.5E-12

4E-12

4.5E-12

Flux

(erg

/cm

2/se

c/A)

4000 4500 5000 5500 6000 6500 7000Wavelength (Angstrom)

2019-02-21.8712016-02-10.917

V694Mon D.Boyd

Fig. 4 - Flux calibrated spectra obtained by David Boyd in 2016 and 2019. The SED is almost the same.

8.5

9

9.5

10

10.5

112457000 2457365 2457730 2458095 2458460 2458825

V694 Mon



4000 4100 4200 4300 4400 4500 4600 4700 4800 4900 5000

Wavelength (A)

0

2

4

6

8

10

rela

tive

in

ten

sity

V694 Mon 2019-03-13 00:00:56 R = 14000 T. Lester

5000 5100 5200 5300 5400 5500 5600 5700 5800 5900 6000

Wavelength (A)

0

1

2

3

4

5

rela

tive

in

ten

sity

V694 Mon 2019-03-13 00:00:56 R = 14000 T. Lester

6000 6100 6200 6300 6400 6500 6600 6700 6800 6900 7000

Wavelength (A)

0

1

2

3

4

5

rela

tive

in

ten

sity

V694 Mon 2019-03-13 00:00:56 R = 14000 T. Lester

Typical Echelle spectrum during this peculiar phase, obtnained by Tim Lester


-1000 -500 0 500 1000


0

2

4

6

8

10

12

14

16

18

20

arb

itra

ry u

nit

V694 Mon Fe II 5169

2019-01-12

2019-01-26

2019-02-03

2019-02-11

2019-02-13

2019-02-19

2019-02-26

2019-03-03

2019-03-10

2019-03-11

2019-03-13

2019-03-20

2019-03-22

2019-03-23

2019-03-28

2019-03-30

2019-04-12

-1000 -500 0 500 1000


0

2

4

6

8

10

12

14

16

18

20

arb

itra

ry u

nit

V694 Mon H alpha

2019-01-12

2019-01-26

2019-02-03

2019-02-11

2019-02-13

2019-02-19

2019-02-26

2019-03-03

2019-03-10

2019-03-11

2019-03-13

2019-03-20

2019-03-22

2019-03-23

2019-03-28

2019-03-30

2019-04-12

-1000 -500 0 500 1000


0

2

4

6

8

10

12

14

16

18

20

arb

itra

ry u

nit

V694 Mon H beta

2019-01-12

2019-01-26

2019-02-03

2019-02-11

2019-02-13

2019-02-19

2019-02-26

2019-03-03

2019-03-10

2019-03-11

2019-03-13

2019-03-20

2019-03-22

2019-03-23

2019-03-28

2019-03-30

2019-04-12

Id. Observer Date Res.V694 Mon J. Guarro 12/01/2019 4053 7499 9000V694 Mon J. Guarro 25/01/2019 3989 7756 9000V694 Mon J. Guarro 26/01/2019 4053 7499 9000V694 Mon F. Teyssier 03/02/2019 4034 7115 11000V694 Mon J. Guarro 11/02/2019 4053 7499 9000V694 Mon F. Teyssier 13/02/2019 4200 7100 11000V694 Mon J. Guarro 19/02/2019 4053 7499 9000V694 Mon F. Teyssier 26/02/2019 4034 7115 11000V694 Mon J. Guarro 03/03/2019 3980 7762 9000V694 Mon J. Guarro 10/03/2019 3980 7762 9000V694 Mon F. Teyssier 11/03/2019 4033 7115 11000V694 Mon T. Lester 13/03/2019 4031 7950 14000V694 Mon P. Somogyi 17/03/2019 6505 6614 15916V694 Mon F. Teyssier 20/03/2019 4300 7100 11000V694 Mon F. Teyssier 22/03/2019 4060 7110 11000V694 Mon J. Guarro 23/03/2019 4053 7761 9000V694 Mon F. Teyssier 24/03/2019 4036 7115 11000V694 Mon J. Guarro 28/03/2019 4053 7762 9000V694 Mon J. Guarro 30/03/2019 4053 7762 9000

Range 8.5

9

9.5

10

10.5

112458000 2458365 2458730

V694 Mon

Echelle spectra - Log of observations


8.5

9

9.5

10

10.5

112458000 2458365 2458730

V694 Mon


-1000 -500 0 500 1000


0

2

4

6

8

10

12

14

16

18

20

arb

itra

ry u

nit

V694 Mon Na I D

2019-01-12

2019-01-26

2019-02-03

2019-02-11

2019-02-13

2019-02-19

2019-02-26

2019-03-03

2019-03-10

2019-03-11

2019-03-13

2019-03-20

2019-03-22

2019-03-23

2019-03-28

2019-03-30

2019-04-12

-1000 -500 0 500 1000


0

2

4

6

8

10

12

14

16

18

20

arb

itra

ry u

nit

V694 Mon He I 5875

2019-01-12

2019-01-26

2019-02-03

2019-02-11

2019-02-13

2019-02-19

2019-02-26

2019-03-03

2019-03-10

2019-03-11

2019-03-13

2019-03-20

2019-03-22

2019-03-23

2019-03-28

2019-03-30

2019-04-12


-1000 -500 0 500 1000velocity (km/s)

0

1

2

3

4

rela

tive

in

ten

sity

V694 Mon | Fe II 4924

2019-01-12

2019-03-13

2019-04-12

-1000 -500 0 500 1000velocity (km/s)

0

5

10

15

relative

intens

ity

V694 Mon | H alpha

2019-01-122019-03-132019-04-12

-1000 -500 0 500 1000velocity (km/s)

0

1

2

3

4

5

rela

tive

in

ten

sity

V694 Mon | H beta

2019-01-12

2019-03-13

2019-04-12

-1000 -500 0 500 1000velocity (km/s)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

V694 Mon | He I 5875

2019-01-12

2019-03-13

2019-04-12

-1000 -500 0 500 1000velocity (km/s)

0

5

10

15

rela

tive

in

ten

sity

V694 Mon | H alpha

2019-01-12

2019-03-13

2019-04-12





3850 3900 3950 4000

Wavelength (A)

0

0.5

1

1.5

2

2.5

rela

tive

in

ten

sity

V694 Mon 2019-03-23 20:55:53 R = 4494 P. Somogyi

-1000 -500 0 500 1000

velocity (km/s)

0

5

10

15

20

25

30

35Halpha 2019-02-21

-1000 -500 0 500 1000

velocity (km/s)

0

5

10

15

20

25

30

35

40Halpha 2019-03-17

-1000 -500 0 500 1000

velocity (km/s)

0

10

20

30

40

50Halpha 2019-04-06

V694 Mon = MWC 560

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

5

10

15

20

rela

tive

in

ten

sity

V694 Mon 2019-02-15 19:48:37 R = 730 C. Buil

3900 4400 4900

Wavelength (A)

0

0.5

1

1.5

2

2.5

3

rela

tive

in

ten

sity

V694 Mon 2019-02-15 19:48:37 R = 730 C. Buil

SYMBIOTICS

Spectrum obtained by C. Buil with UVEX and crop on the near UV/Blue range




4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

0.5

1

1.5

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-11 V694 Mon 2019-02-04 21:23:57 R = 1101 D. Boyd

4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

0.5

1

1.5

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-11 V694 Mon 2019-02-21 20:53:58 R = 1100 D. Boyd

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

flu

x (

erg

cm

- 2 s

- 1 A

- 1)

10-11 V694 Mon 2019-03-25 20:05:33 R = 1130 D. Boyd

0

2

4

6

8

10

12

14

Arbi

trary

uni

ts

4000 4500 5000 5500 6000 6500 7000


V694 Mon

2019-04-01.139

2019-03-16.861

2019-02-12.199

2019-02-07.223

2019-01-28.267

2019-01-27.249

2019-01-23.247

2019-01-20.203

2019-01-19.352

2019-01-19.301



V1329 CygSYMBIOTICS

Coordinates (2000.0)R.A. 20 51 01.2Dec +35 34 54.1Mag 13.8 (2018-10)


4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

2

4

6

8

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-13 V1329 Cyg 2019-01-09 18:53:53 R = 1095 D. Boyd

4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

0.5

1

1.5

2

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-13 V1329 Cyg 2019-01-09 18:53:53 R = 1095 D. Boyd

Z AndSYMBIOTICS

Coordinates (2000.0)R.A. 23 33 39.5Dec 48 49 5.4Mag V 9.8 (2019-01)


Return to quiescent state after 2018 outburst

8.5

9

9.5

10

10.5

112458100 2458190 2458280 2458370 2458460 2458550 2458640

Z And (V)

4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

0.2

0.4

0.6

0.8

1

Flu

x [e

rg.c

m-2

.s-1

.Å-1

]

10-11 Z And 2019-01-09 20:26:59 R = 1057 D. Boyd

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

flu

x (

erg

cm

- 2 s

- 1 A

- 1)

10-12 Z And 2019-02-15 20:09:29 R = 1111 D. Boyd

Z AndSYMBIOTICS


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

5

10

15

20

25

30

35

rela

tive

in

ten

sity

Z And 2019-01-25 R = 9000 J. Guarro

-1000 -500 0 500 1000

velocity (km/s)

0

5

10

15

20

25

30

35Halpha 2019-01-25

-500 0 500

velocity (km/s)

0

1

2

3

4

5

6HeI5876 2019-01-25

-500 0 500

velocity (km/s)

0.5

1

1.5

2

2.5

3

3.5HeI6678 2019-01-25

-500 0 500

velocity (km/s)

0

5

10

15

20HeII4686 2019-01-25

-500 0 500

velocity (km/s)

0

0.5

1

1.5

2

2.5

3[FeVII]6087 2019-01-25

-500 0 500

velocity (km/s)

0

1

2

3

4

5[OIII]5007 2019-01-25

-500 0 500

velocity (km/s)

0

5

10

15

20

25

30Hbeta 2019-01-25

ZZ CMiSYMBIOTICS


Coordinates (2000.0)R.A. 07 24 14.0Dec +08 53 51.8Mag V 10.1 (2019-04)

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

2.5

3

3.5

rela

tive

in

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sity

ZZ CMi 2019-02-20 22:21:08 R = 1100 Martineau Buchet

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

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3

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rela

tive

in

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ZZ CMi 2019-03-22 20:36:49 R = 831 F. Campos

ZZ CMiSYMBIOTICS

-500 0 500

velocity (km/s)

0

1

2

3

4

5

6Halpha 2019-02-06

6400 6500 6600 6700

Wavelength (A)

0

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6

8

rela

tive

in

ten

sity

ZZ CMi 2019-02-06 18:05:27 R = 7688 Umberto Sollecchia

ZZ CMiSYMBIOTICS

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

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4

6

8

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rela

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in

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sity

ZZ CMi 2019-03-09 00:25:21 R = 14000 T. Lester

-1000 -500 0 500 1000

velocity (km/s)

0

1

2

3

4

5

6Halpha 2019-03-09

-1000 -500 0 500 1000

velocity (km/s)

1

2

3

4

5

6Hbeta 2019-03-09

-500 0 500

velocity (km/s)

0.5

0.6

0.7

0.8

0.9

1

1.1

1.2HeI5876 2019-03-09

-500 0 500

velocity (km/s)

0.1

0.15

0.2

0.25

0.3

0.35[OIII]5007 2019-03-09

-1000 -500 0 500 1000

velocity (km/s)

1

1.2

1.4

1.6

1.8

2

2.2

2.4[OI]6300 2019-03-09

Campaign: Suspected Symbiotics StarsSYMBIOTICS

This campaign is initiated by Adrian Lucy and Jeniffer Sokolovski (Columbia University). The aim is to de-tect symbiotic stars among a list of suspected tragets proposed by Adran Lucy.AAVSO Alert Notice https://www.aavso.org/aavso-alert-notice-650

One of the target has been clearly identified as a symbiotic star (Lucy & al., based on spectra obtained by Terry Bohlsen)

Share results and check the status of the campaign on ARAS forum:http://spectro-aras.com/forum/viewtopic.php?f=37&t=2124


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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1.5

2

rela

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in

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ASASSN -V J081823 2019-01-12 22:41:07 R = 872 Fran Campos

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

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1

1.5

2

2.5

rela

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in

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GDS J0731468-195434 2019-03-29 20:12:41 R = 941 Fran Campos

Campaign: Suspected Symbiotics StarsSYMBIOTICS


Suspected Symbiotics StarsSummary of Observations

Observations

Name RA (2000.0) Dec (2000.0) V mag* M giant Em. Lines 05 09 10 11 12 01 02 03 04

1 GAIA DR2 4636654969717900032 01 50 49.53 -76 49 42.6 12.9 no 1

2 UCAC3 157:43452 06 55 51.36 -11 44 05.3 12.3 no 1

3 GDS J0731468-195434 07 31 46.82 -19 54 34.5 13.2 1

4 ASASSN-V_J081823.00-111138.9 08 18 23.00 -11 11 38.9 12.5 no 1

5 UCAC3 80:46364 08 34 45.15 -50 26 58.2 13.7 no 1

6 GSC9507:2249 11 03 10.83 -83 57 11.3 11.2 1

7 12 01 20.93 -79 20 14.7 12.3

8 GAIA DR2 4131587500273361280 16 39 59.65 -18 44 38.1 13.9 1

9 ASASSN-V J164007.54-382216.1 16 40 07.54 -38 22 16.1 13.86-14.74

10 GAIA DR2 6019720819446985984 16 45 31.78 -36 22 31.6 12.9

11 V2096 Oph 16 56 05.46 -24 06 37.0 12.9-14.0

12 ER Oph 17 00 42.14 -26 10 12.4 11.8-<14.8

13 ASASSN-V J170231.98-275954.2 17 02 31.98 -27 59 54.4 13.98-14.94

14 GAIA DR2 4334886650491663104 17 06 08.44 -10 58 33.0 14.3

15 SS 295 17 07 38.16 -07 44 48.6 13.1 1

16 V2525 Oph 17 15 05.27 -09 23 50.1 11.9-<15.1

17 GAIA DR2 4115021291723497088 17 17 45.67 -21 31 16.9 13.7

18 GSC 09276-00130 17 18 09 -67 57 26.0 13.6

19 GAIA DR2 4168021909706732672 17 25 26.34 -07 48 27.5 14.3

20 GAIA DR2 4111779763989583232 17 26 18.27 -22 12 46.4 14.1

21 GAIA DR2 4120809606303456896 17 27 08.69 -21 39 04.5 13.1

22 GAIA DR2 5919388180059095296 17 30 58.39 -56 29 53.4 12.6 no 1

23 ASASSN-V J173832.43-492840.2 17 38 32.42 -49 28 40.1 13.96-14.55

24 FASTT 1100 17 53 45.30 -01 07 46.8 14.04-14.30 H a 1

25 GAIA DR2 4150446010182968192 17 56 04.34 -13 10 03.4 13.1 M4 1

26 GAIA DR2 4150099732733146112 17 59 43.87 -13 58 32.0 13.9

27 SY Cra 18 03 21.54 -42 37 56.8 13.0-16.5p

28 GAIA DR2 6345873798283774848 18 14 18.07 -85 59 06.5 11.7 no 1

29 GAIA DR2 4048168377818693632 18 28 31.28 -28 45 02.9 11.9 no 1

30 ASASSN-V J185421.70-274827.4 18 54 21.70 -27 48 27.8 12.89-13.63

31 EN Sgr 19 22 42.08 -13 59 56.5 11.95-14.61 H I 2 2

32 ASASSN-V J192916.53-224040.3 19 29 16.53 -22 40 40.3 12.52-13.02 M 3.5 Ha Hb 1

33 ASAS J195948-8252.7 19 49 48.4 -82 52 37.5 11.6 yes 2

2018 2019


AG Dra: a mysterious l 5018 line during outburstsSYMBIOTICS

We have obtained 122 Echelle spectra of AG Dra since 2016. In some spectra, during outbursts, an emission line appears at l ~ 5016.0 Å , l ~5018.5 Å once the systemic radial velocity (-147.7 km.s-1) is deduced.

Fig.1 Echelle spectrum obtained near the peak of 2016 outburst, on JD 2457523.364

The Fe II lines are common in symbiotic binaries, but they are missing in AG Dra spectra due to the low metallicity of the yellow giant donor. At first glance, it is very unlikely that the line detected at l5016.0 Å is Fe II. As a matter of fact, the other lines of the multiplet 42 (ll5016, 5169) are not dectected (see fig. 2)

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

Rel

ativ

e in

tens

ity

-400 -300 -200 -100 100 200 300 400Velocity (Km/sec)

Fe II 4923.92Fe II 42 5018.43Fe II 42 5169.03

AG Dra 2016-05-14.853 F Teyssier

Fig. 2 Fe II 42 multiplet, systemic radial velocity is deduced. Only l 5018 appears. The other emission lines are He I ll 4922 and 5016

5000 5005 5010 5015 5020 5025 5030

Wavelength (A)

0

1

2

3

rela

tive

in

ten

sity

? 5

018

Å


SYMBIOTICS


4910 4915 4920 4925 4930

Wavelength (A)

0

1

2

3

rela

tive

in

ten

sity

5865 5870 5875 5880

Wavelength (A)

0

1

2

3

rela

tive

in

ten

sity

6665 6670 6675 6680 6685

Wavelength (A)

0

1

2

3

rela

tive

in

ten

sity

7055 7060 7065 7070 7075

Wavelength (A)

0

1

2

3

4

rela

tive

in

ten

sity

4460 4465 4470 4475 4480

Wavelength (A)

0

0.5

1

rela

tive

in

ten

sity

5005 5010 5015 5020 5025

Wavelength (A)

0

0.5

1

1.5

2

2.5

3

rela

tive

in

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sity

?

A second line appears clearly only in blue part of the singlet He I 5016 Å. A very weak bump appears rarely in the blue edge of the other F → P transition He I 6678Å

AG Dra: a mysterious l 5018 line during outbursts


7200 7400 7600 7800 8000 8200 8400 8600

JD - 2450000

0

0.5

1

1.5

2

2.5

3AG Dra - EW He I 5016

7200 7400 7600 7800 8000 8200 8400 8600

JD - 2450000

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7AG Dra - EW 5018

SYMBIOTICS

The intensity of the 5018 line is strongly correlated to the outburst activity of AG Dra. It weakens and disappears between outburts. The shape of the intensities of singlet and triplet lines are different during outbursts, especillay during 2017 outburst (see p. 13). The behavior of l 5018 is closer to the bahavior of singlets lines., but slighly different.


At the peak of the outbursts, the ratio of the equivalent widths l 5018 / He I 6678 is 0.3 to 0.35.

Note : measures under 0.15 should be read as ~ 0

0

0.05

0.1

0.15

0.2

0.25

0.3

0.35

0.4

7000 7200 7400 7600 7800 8000 8200 8400 8600 8800

ratio EW(5018)/ EW(He I 5016)



SYMBIOTICS

7200 7400 7600 7800 8000 8200 8400 8600

JD - 2450000

0

1

2

3

4


7200 7400 7600 7800 8000 8200 8400 8600

JD - 2450000

0

1

2

3


7200 7400 7600 7800 8000 8200 8400 8600

JD - 2450000

0

1

2

3

4


7200 7400 7600 7800 8000 8200 8400 8600

JD - 2450000

0

0.5

1

1.5

2

2.5



Equivalent widths of the main He I lines


SYMBIOTICS


5005 5010 5015 5020 5025

Wavelength (A)

0

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1

1.5

2

2.5

3

rela

tive

in

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AG Dra 2016-05-14 20:28:45 R = 11000 fteyssier

5005 5010 5015 5020 5025

Wavelength (A)

0

0.5

1

1.5

2

2.5

3

rela

tive

in

ten

sity

AG DRA 2017-05-19 20:03:27 R = 9000 J. Guarro

5005 5010 5015 5020 5025

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

AG Dra 2018-04-24 20:44:26 R = 11000 Olivier Garde

5005 5010 5015 5020 5025

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

AG Dra 2018-05-15 20:53:11 R = 11000 FMTeyssier

5005 5010 5015 5020 5025

Wavelength (A)

0

0.2

0.4

0.6

0.8

1

rela

tive

in

ten

sity

AG Dra 2018-04-20 20:01:12 R = 11000 FMTeyssier

5005 5010 5015 5020 5025

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

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sity

AG Dra 2018-04-21 04:10:44 R = 12000 tlester

At first sight, the shapes of He I 5876 and l 5018 vary toghether. Notably during 2018 outburst the lines appear to have at least a double component.


SYMBIOTICS


AG DRA He I 5016

-400 -200 0 200 400

0

1

22015-04-11

-400 -200 0 200 400

0

1

22015-04-12

-400 -200 0 200 400

0

1

22015-04-13

-400 -200 0 200 400

0

1

22015-04-13

-400 -200 0 200 400

0

1

22016-04-16

-400 -200 0 200 400

0

1

22016-04-18

-400 -200 0 200 400

0

1

22016-04-23

-400 -200 0 200 400

0

1

22016-04-27

-400 -200 0 200 400

0

1

22016-04-28

-400 -200 0 200 400

0

1

22016-04-29

-400 -200 0 200 400

0

1

22016-05-01

-400 -200 0 200 400

0

1

22016-05-03

-400 -200 0 200 400

0

1

22016-05-14

-400 -200 0 200 400

0

1

22017-03-29

-400 -200 0 200 400

0

1

22017-04-02

-400 -200 0 200 400

0

1

22017-04-02

-400 -200 0 200 400

0

1

22017-04-05

-400 -200 0 200 400

0

1

22017-04-06

-400 -200 0 200 400

0

1

22017-04-07

-400 -200 0 200 400

0

1

22017-04-11

-400 -200 0 200 400

0

1

22017-04-12

-400 -200 0 200 400

0

1

22017-04-18

-400 -200 0 200 400

0

1

22017-04-19

-400 -200 0 200 400

0

1

22017-04-23

-400 -200 0 200 400

0

1

22017-04-23

-400 -200 0 200 400

0

1

22017-04-26

-400 -200 0 200 400

0

1

22017-04-28

-400 -200 0 200 400

0

1

22017-05-09

-400 -200 0 200 400

0

1

22017-05-11

-400 -200 0 200 400

0

1

22017-05-13

-400 -200 0 200 400

0

1

22017-05-15

-400 -200 0 200 400

0

1

22017-05-15

-400 -200 0 200 400

0

1

22017-05-16

-400 -200 0 200 400

0

1

22017-05-16

-400 -200 0 200 400

0

1

22017-05-16

-400 -200 0 200 400

0

1

22017-05-17

-400 -200 0 200 400

0

1

22017-05-19

-400 -200 0 200 400

0

1

22017-05-20

-400 -200 0 200 400

0

1

22017-05-20

-400 -200 0 200 400

0

1

22017-05-22

-400 -200 0 200 400

0

1

22017-05-23

-400 -200 0 200 400

0

1

22017-05-24

-400 -200 0 200 400

0

1

22017-05-24

-400 -200 0 200 400

0

1

22017-05-24

-400 -200 0 200 400

0

1

22017-05-25

-400 -200 0 200 400

0

1

22017-05-25

-400 -200 0 200 400

0

1

22017-05-26

-400 -200 0 200 400

0

1

22017-05-26

-400 -200 0 200 400

0

1

22017-05-27

-400 -200 0 200 400

0

1

22017-05-30

-400 -200 0 200 400

0

1

22017-05-31

-400 -200 0 200 400

0

1

22017-05-31

-400 -200 0 200 400

0

1

22017-06-01

-400 -200 0 200 400

0

1

22017-06-03

-400 -200 0 200 400

0

1

22017-06-05

-400 -200 0 200 400

0

1

22017-06-09

-400 -200 0 200 400

0

1

22017-06-11

-400 -200 0 200 400

0

1

22017-06-12

-400 -200 0 200 400

0

1

22017-06-16

-400 -200 0 200 400

0

1

22017-06-21

-400 -200 0 200 400

0

1

22017-07-03

-400 -200 0 200 400

0

1

22017-07-04

-400 -200 0 200 400

0

1

22017-07-05

-400 -200 0 200 400

0

1

22017-07-14

-400 -200 0 200 400

0

1

22017-07-18

-400 -200 0 200 400

0

1

22017-07-26


AG DRA He I 5016

-400 -200 0 200 400

0

1

22015-04-11

-400 -200 0 200 400

0

1

22015-04-12

-400 -200 0 200 400

0

1

22015-04-13

-400 -200 0 200 400

0

1

22015-04-13

-400 -200 0 200 400

0

1

22016-04-16

-400 -200 0 200 400

0

1

22016-04-18

-400 -200 0 200 400

0

1

22016-04-23

-400 -200 0 200 400

0

1

22016-04-27

-400 -200 0 200 400

0

1

22016-04-28

-400 -200 0 200 400

0

1

22016-04-29

-400 -200 0 200 400

0

1

22016-05-01

-400 -200 0 200 400

0

1

22016-05-03

-400 -200 0 200 400

0

1

22016-05-14

-400 -200 0 200 400

0

1

22017-03-29

-400 -200 0 200 400

0

1

22017-04-02

-400 -200 0 200 400

0

1

22017-04-02

-400 -200 0 200 400

0

1

22017-04-05

-400 -200 0 200 400

0

1

22017-04-06

-400 -200 0 200 400

0

1

22017-04-07

-400 -200 0 200 400

0

1

22017-04-11

-400 -200 0 200 400

0

1

22017-04-12

-400 -200 0 200 400

0

1

22017-04-18

-400 -200 0 200 400

0

1

22017-04-19

-400 -200 0 200 400

0

1

22017-04-23

-400 -200 0 200 400

0

1

22017-04-23

-400 -200 0 200 400

0

1

22017-04-26

-400 -200 0 200 400

0

1

22017-04-28

-400 -200 0 200 400

0

1

22017-05-09

-400 -200 0 200 400

0

1

22017-05-11

-400 -200 0 200 400

0

1

22017-05-13

-400 -200 0 200 400

0

1

22017-05-15

-400 -200 0 200 400

0

1

22017-05-15

-400 -200 0 200 400

0

1

22017-05-16

-400 -200 0 200 400

0

1

22017-05-16

-400 -200 0 200 400

0

1

22017-05-16

-400 -200 0 200 400

0

1

22017-05-17

-400 -200 0 200 400

0

1

22017-05-19

-400 -200 0 200 400

0

1

22017-05-20

-400 -200 0 200 400

0

1

22017-05-20

-400 -200 0 200 400

0

1

22017-05-22

-400 -200 0 200 400

0

1

22017-05-23

-400 -200 0 200 400

0

1

22017-05-24

-400 -200 0 200 400

0

1

22017-05-24

-400 -200 0 200 400

0

1

22017-05-24

-400 -200 0 200 400

0

1

22017-05-25

-400 -200 0 200 400

0

1

22017-05-25

-400 -200 0 200 400

0

1

22017-05-26

-400 -200 0 200 400

0

1

22017-05-26

-400 -200 0 200 400

0

1

22017-05-27

-400 -200 0 200 400

0

1

22017-05-30

-400 -200 0 200 400

0

1

22017-05-31

-400 -200 0 200 400

0

1

22017-05-31

-400 -200 0 200 400

0

1

22017-06-01

-400 -200 0 200 400

0

1

22017-06-03

-400 -200 0 200 400

0

1

22017-06-05

-400 -200 0 200 400

0

1

22017-06-09

-400 -200 0 200 400

0

1

22017-06-11

-400 -200 0 200 400

0

1

22017-06-12

-400 -200 0 200 400

0

1

22017-06-16

-400 -200 0 200 400

0

1

22017-06-21

-400 -200 0 200 400

0

1

22017-07-03

-400 -200 0 200 400

0

1

22017-07-04

-400 -200 0 200 400

0

1

22017-07-05

-400 -200 0 200 400

0

1

22017-07-14

-400 -200 0 200 400

0

1

22017-07-18

-400 -200 0 200 400

0

1

22017-07-26

AG Dra He I 5016

-400 -200 0 200 400

0

1

22017-07-28

-400 -200 0 200 400

0

1

22017-08-01

-400 -200 0 200 400

0

1

22017-08-04

-400 -200 0 200 400

0

1

22017-08-06

-400 -200 0 200 400

0

1

22017-08-10

-400 -200 0 200 400

0

1

22017-08-14

-400 -200 0 200 400

0

1

22017-08-17

-400 -200 0 200 400

0

1

22017-09-01

-400 -200 0 200 400

0

1

22017-10-17

-400 -200 0 200 400

0

1

22018-02-26

-400 -200 0 200 400

0

1

22018-04-20

-400 -200 0 200 400

0

1

22018-04-20

-400 -200 0 200 400

0

1

22018-04-21

-400 -200 0 200 400

0

1

22018-04-21

-400 -200 0 200 400

0

1

22018-04-23

-400 -200 0 200 400

0

1

22018-04-23

-400 -200 0 200 400

0

1

22018-04-24

-400 -200 0 200 400

0

1

22018-04-25

-400 -200 0 200 400

0

1

22018-04-25

-400 -200 0 200 400

0

1

22018-04-26

-400 -200 0 200 400

0

1

22018-04-26

-400 -200 0 200 400

0

1

22018-04-27

-400 -200 0 200 400

0

1

22018-04-28

-400 -200 0 200 400

0

1

22018-05-01

-400 -200 0 200 400

0

1

22018-05-01

-400 -200 0 200 400

0

1

22018-05-02

-400 -200 0 200 400

0

1

22018-05-02

-400 -200 0 200 400

0

1

22018-05-02

-400 -200 0 200 400

0

1

22018-05-03

-400 -200 0 200 400

0

1

22018-05-04

-400 -200 0 200 400

0

1

22018-05-06

-400 -200 0 200 400

0

1

22018-05-08

-400 -200 0 200 400

0

1

22018-05-13

-400 -200 0 200 400

0

1

22018-05-15

-400 -200 0 200 400

0

1

22018-05-17

-400 -200 0 200 400

0

1

22018-05-18

-400 -200 0 200 400

0

1

22018-05-19

-400 -200 0 200 400

0

1

22018-05-19

-400 -200 0 200 400

0

1

22018-05-20

-400 -200 0 200 400

0

1

22018-05-23

-400 -200 0 200 400

0

1

22018-05-24

-400 -200 0 200 400

0

1

22018-05-24

-400 -200 0 200 400

0

1

22018-06-02

-400 -200 0 200 400

0

1

22018-06-11

-400 -200 0 200 400

0

1

22018-06-24

-400 -200 0 200 400

0

1

22018-06-29

-400 -200 0 200 400

0

1

22018-07-03

-400 -200 0 200 400

0

1

22018-07-12

-400 -200 0 200 400

0

1

22018-07-17

-400 -200 0 200 400

0

1

22018-08-04

-400 -200 0 200 400

0

1

22018-08-21

-400 -200 0 200 400

0

1

22018-08-23

-400 -200 0 200 400

0

1

22018-09-28

-400 -200 0 200 400

0

1

22018-10-12

-400 -200 0 200 400

0

1

22018-10-19

-400 -200 0 200 400

0

1

22019-02-27

SYMBIOTICS



SYMBIOTICS


0

0.5

1

1.5

2

2.5

3

3.5

4

Rel

ativ

e in

tens

ity

-800 -600 -400 -200 200 400 600 800Velocity (Km/sec)

2017-05-20.933 Olivier Garde2018-04-23.843 FMTeyssier2018-05-15.870 FMTeyssier

He I 6678.15 - AG Dra

A very weak bump is sometimes detected in the red part of the bright singlet He I 6678 Å at ~ +220 km.s-1

Radial velocity of the sytem is deduced

Provisional findings

1. An emission line appear sometimes at l 5018 Å in the spectra of AG Dra, once deduced the system-ic radial velocity.2. At firts glance, this line is unlikely Fe II 5018 because other lines the Fe II (42) multiplet are absent3. The line appears during outbursts and then weakens/dessappears4. The trend of the intensity (measured as EW) is similar to He I 5016 Å5. The profile of the line seems similar to He I 5016 Å6. We do not dectect a counterpart in the blue edge of He I 5016 Å7. The some phenomenon isn't detected in other He I lines unless, perhaps the bright singlet line 6678, but at much lower intensity and at a different radial velocity.8. The SNR of the rare Echelle spectra under 4000 Å is too low to investigate the behavior of the 4p2s transition l 3964 Å

From 4. & 5., the l5018 line could be to be a "ghost" of He I l 5016 line displaced by ~ 170 km.s-1 with respect to He I 5018, whose intensity peaks at ~ 0.35 times He I l 5016 at the peak of outbursts, dis-placed by ~ + 170 km.s-1. But the lack of a such a conterpart in other He I lines make this hypothesis unlikely.

Occasionnaly in other symbiotics, Fe II 5018 can appear while the other lines of the multiplet are undetectable, see p. 71-73. At the date, the identification of the line could be Fe II (notwithstanding with the abnomalous ratio bteween the thre lines of the multiplet. The upcoming outburst of AG Dra while be the occasion to reinforce the hypothesis. Thus, appeareance of 5018 could become a signa-ture of outburst in AG Dra system (R. Galis, private communication)


-300 -150 0 150 300

velocity (km/s)

0

2

4

6

8

10

arb

itra

ry u

nit

AGPeg |2015-12-07

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

1

2

3

4

arb

itra

ry u

nit

AGPeg |2016-10-29

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

1

2

3

arb

itra

ry u

nit

AXPer |2016-09-09

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

2

4

6

8

10

arb

itra

ry u

nit

AXPer |2017-10-27

FeII 4924

FeII 5018

FeII 5169

-500 -250 0 250 500

velocity (km/s)

0

1

2

3

arb

itra

ry u

nit

BFCyg |2015-09-01

FeII 4924

FeII 5018

FeII 5169

-500 -250 0 250 500

velocity (km/s)

0

1

2

3

arb

itra

ry u

nit

BFCyg |2016-09-21

FeII 4924

FeII 5018

FeII 5169

SYMBIOTICS


Fe II (42) multiplet in various symbiotic satrs


-500 -250 0 250 500

velocity (km/s)

0

1

2

3

arb

itra

ry u

nit

CHCyg |2015-04-21

FeII 4924

FeII 5018

FeII 5169

-500 -250 0 250 500

velocity (km/s)

0

5

10

arb

itra

ry u

nit

CHCyg |2015-10-02

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

1

2

3

4

5

arb

itra

ry u

nit

CICyg |2016-10-29

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

1

2

3

arb

itra

ry u

nit

CICyg |2017-04-23

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

5

10

15

arb

itra

ry u

nit

RAqr |2017-10-09

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

2

4

6

8

10

arb

itra

ry u

nit

Vend47 |2018-10-18

FeII 4924

FeII 5018

FeII 5169

SYMBIOTICS



-300 -150 0 150 300

velocity (km/s)

0

2

4

6

8

arb

itra

ry u

nit

V443Her |2016-09-08

FeII 4924

FeII 5018

FeII 5169

-500 -250 0 250 500

velocity (km/s)

0

1

2

3

4

arb

itra

ry u

nit

V694Mon |2017-02-16

FeII 4924

FeII 5018

FeII 5169

-500 -250 0 250 500

velocity (km/s)

0

1

2

3

4

arb

itra

ry u

nit

V694Mon |2019-02-11

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

1

2

3

arb

itra

ry u

nit

ZAnd |2015-11-25

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

1

2

3

arb

itra

ry u

nit

ZAnd |2017-01-26

FeII 4924

FeII 5018

FeII 5169

-300 -150 0 150 300

velocity (km/s)

0

0.5

1

1.5

2

2.5

arb

itra

ry u

nit

ZAnd |2018-02-25

FeII 4924

FeII 5018

FeII 5169

SYMBIOTICS



Date Time (UT) J.D. mid Observer Resolution l_min l_max File12/04/2015 19:40 2457125.345 FMT 11000 4211 7163 asdb_agdra_20150412_820.fit13/04/2015 20:02 2457126.377 BUI 11000 4279 7360 asdb_agdra_20150413_835.fit13/04/2015 23:20 2457126.525 BUI 11000 4279 7360 asdb_agdra_20150413_973.fit16/04/2016 21:45 2457495.423 FMT 11000 4144 7161 asdb_agdra_20160416_907.fit18/04/2016 19:57 2457497.353 FMT 11000 4144 7161 asdb_agdra_20160418_831.fit23/04/2016 21:21 2457502.402 FMT 11000 4144 7161 asdb_agdra_20160423_890.fit27/04/2016 20:26 2457506.373 FMT 11000 4144 7161 asdb_agdra_20160427_852.fit28/04/2016 20:36 2457507.375 FMT 11000 4144 7161 asdb_agdra_20160428_859.fit29/04/2016 20:32 2457508.398 OGA 11000 4178 7314 asdb_agdra_20160429_856.fit01/05/2016 20:18 2457510.367 FMT 11000 4144 7161 asdb_agdra_20160501_846.fit03/05/2016 20:28 2457512.371 FMT 11000 4144 7161 asdb_agdra_20160503_853.fit14/05/2016 20:28 2457523.364 FMT 11000 4144 7161 asdb_agdra_20160514_853.fit29/03/2017 20:44 2457842.434 OGA 11000 4185 7313 asdb_agdra_20170329_864.fit02/04/2017 1:03 2457845.6 JGF 11000 3979 7497 asdb_agdra_20170402_044.fit02/04/2017 21:20 2457846.411 FMT 11000 4208 7396 asdb_agdra_20170402_890.fit05/04/2017 19:58 2457849.402 OGA 11000 4185 7314 asdb_agdra_20170405_833.fit06/04/2017 19:44 2457850.352 FMT 11000 4210 7150 asdb_agdra_20170406_823.fit07/04/2017 22:29 2457851.466 JGF 11000 3979 7497 asdb_agdra_20170407_937.fit11/04/2017 19:43 2457855.35 FMT 11000 4300 7150 asdb_agdra_20170411_822.fit12/04/2017 21:14 2457856.476 OGA 11000 4185 7313 asdb_agdra_20170412_885.fit18/04/2017 21:04 2457862.406 FMT 11000 4207 7396 asdb_agdra_20170418_878.fit19/04/2017 19:53 2457863.357 FMT 11000 4210 7150 asdb_agdra_20170419_829.fit23/04/2017 20:07 2457867.366 FMT 11000 4208 7394 asdb_agdra_20170423_839.fit23/04/2017 21:50 2457867.438 JGF 9000 4052 7497 asdb_agdra_20170423_910.fit23/04/2017 21:50 2457867.438 JGF 11000 4052 7497 asdb_agdra_20170423_910.fit26/04/2017 20:19 2457870.375 FMT 11000 4208 7394 asdb_agdra_20170426_847.fit28/04/2017 21:18 2457872.434 JGF 9000 4052 7497 asdb_agdra_20170428_888.fit09/05/2017 20:14 2457883.372 FMT 11000 4208 7159 asdb_agdra_20170509_844.fit11/05/2017 19:58 2457885.369 JGF 9000 4052 7497 asdb_agdra_20170511_832.fit13/05/2017 20:13 2457887.371 FMT 11000 4208 7159 asdb_agdra_20170513_843.fit13/05/2017 20:13 2457887.371 FMT 11000 4208 7159 asdb_agdra_20170513_843.fit15/05/2017 19:35 2457889.365 OGA 11000 4185 7314 asdb_agdra_20170515_816.fit15/05/2017 19:35 2457889.365 OGA 11000 4185 7314 asdb_agdra_20170515_816.fit16/05/2017 19:32 2457890.363 OGA 11000 4185 7314 asdb_agdra_20170516_814.fit16/05/2017 20:00 2457890.397 JGF 9000 4052 7497 asdb_agdra_20170516_834.fit17/05/2017 20:33 2457891.413 JGF 9000 4052 7497 asdb_agdra_20170517_857.fit19/05/2017 20:03 2457893.373 JGF 9000 3979 7497 asdb_agdra_20170519_836.fit20/05/2017 20:25 2457894.403 JGF 11000 4052 7497 asdb_agdra_20170520_851.fit20/05/2017 22:23 2457894.53 OGA 11000 4185 7313 asdb_agdra_20170520_933.fit22/05/2017 20:08 2457896.386 JGF 9000 3979 7497 asdb_agdra_20170522_839.fit23/05/2017 21:05 2457897.425 JGF 9000 3979 7497 asdb_agdra_20170523_879.fit24/05/2017 20:05 2457898.375 JGF 9000 4046 7748 asdb_agdra_20170524_837.fit24/05/2017 20:06 2457898.375 JGF 9000 4052 7497 asdb_agdra_20170524_838.fit24/05/2017 20:42 2457898.391 FMT 11000 4210 7150 asdb_agdra_20170524_863.fit25/05/2017 20:42 2457899.388 FMT 11000 4210 7150 asdb_agdra_20170525_863.fit25/05/2017 20:18 2457899.393 JGF 9000 3979 7497 asdb_agdra_20170525_846.fit26/05/2017 20:21 2457900.395 JGF 9000 3979 7497 asdb_agdra_20170526_848.fit26/05/2017 20:54 2457900.401 FMT 11000 4210 7150 asdb_agdra_20170526_871.fit26/05/2017 20:54 2457900.401 FMT 11000 4210 7150 asdb_agdra_20170526_871.fit27/05/2017 22:58 2457901.492 JFG 11000 4052 7760 asdb_agdra_20170527_957.fit30/05/2017 21:19 2457904.41 FMT 11000 4210 7150 asdb_agdra_20170530_889.fit31/05/2017 20:56 2457905.394 FMT 11000 4208 7159 asdb_agdra_20170531_873.fit31/05/2017 20:56 2457905.394 FMT 11000 4208 7159 asdb_agdra_20170531_873.fit31/05/2017 20:16 2457905.397 JGF 11000 3979 7497 asdb_agdra_20170531_845.fit01/06/2017 21:02 2457906.398 FMT 11000 4142 7159 asdb_agdra_20170601_877.fit03/06/2017 21:07 2457908.417 JGF 11000 4052 7760 asdb_agdra_20170603_880.fit05/06/2017 20:25 2457910.404 JGF 11000 4052 7497 asdb_agdra_20170605_851.fit09/06/2017 20:28 2457914.417 JGF 11000 4058 7667 asdb_agdra_20170609_853.fit11/06/2017 20:47 2457916.422 JGF 9000 3979 7760 asdb_agdra_20170611_867.fit12/06/2017 21:37 2457917.422 FMT 11000 4208 7159 asdb_agdra_20170612_901.fit16/06/2017 21:34 2457921.423 FMT 11000 4208 7159 asdb_agdra_20170616_899.fit21/06/2017 20:26 2457926.401 JGF 9000 4052 7497 asdb_agdra_20170621_852.fit03/07/2017 20:30 2457938.41 JGF 9000 4052 7497 asdb_agdra_20170703_854.fit04/07/2017 3:00 2457938.66 LES 13000 4030 7949 asdb_agdra_20170704_125.fit

SYMBIOTICS


Log of observationsAG Dra Echelle spectra (R = 9000 to 13000) in ARAS database (1/2)


Date Time (UT) J.D. mid Observer Resolution l_min l_max File05/07/2017 20:41 2457940.404 JGF 11000 4052 7497 asdb_agdra_20170705_862.fit14/07/2017 20:53 2457949.419 JGF 9000 4052 7760 asdb_agdra_20170714_871.fit18/07/2017 4:05 2457952.713 LES 13000 4030 7949 asdb_agdra_20170718_171.fit26/07/2017 20:29 2457961.41 JGF 9000 4052 7760 asdb_agdra_20170726_854.fit28/07/2017 20:38 2457963.416 JGF 9000 4052 7760 asdb_agdra_20170728_860.fit01/08/2017 20:43 2457967.421 JGF 9000 4052 7497 asdb_agdra_20170801_864.fit04/08/2017 20:47 2457970.394 JGF 9000 4052 7497 asdb_agdra_20170804_866.fit06/08/2017 20:16 2457972.366 FMT 11000 4206 7159 asdb_agdra_20170806_845.fit10/08/2017 21:06 2457976.428 JGF 9000 4052 7760 asdb_agdra_20170810_879.fit14/08/2017 20:22 2457980.405 JGF 9000 4052 7760 asdb_agdra_20170814_849.fit17/08/2017 1:11 2457982.606 LES 13000 4030 7949 asdb_agdra_20170817_049.fit17/10/2017 18:28 2458044.317 FMT 11000 4141 7394 asdb_agdra_20171017_770.fit26/02/2018 7:50 2458175.883 LES 13000 4030 7948 asdb_agdra_20180226_327.fit18/04/2018 1:45 2458226.584 BUI 11000 3869 5286 asdb_agdra_20180418_073.fit20/04/2018 20:01 2458229.363 FMT 11000 4209 7394 asdb_agdra_20180420_834.fit20/04/2018 20:49 2458229.452 OGA 11000 4185 7314 asdb_agdra_20180420_868.fit21/04/2018 4:10 2458229.738 LES 12000 4030 7947 asdb_agdra_20180421_174.fit21/04/2018 20:22 2458230.362 BUI 11000 4055 7358 asdb_agdra_20180421_849.fit23/04/2018 20:13 2458232.372 FMT 11000 4210 7350 asdb_agdra_20180423_843.fit23/04/2018 22:21 2458232.477 BUI 11000 3869 7358 asdb_agdra_20180423_931.fit24/04/2018 20:44 2458233.448 OGA 11000 4185 7315 asdb_agdra_20180424_864.fit25/04/2018 2:44 2458233.642 JGF 9000 3979 7498 asdb_agdra_20180425_114.fit25/04/2018 20:05 2458234.366 FMT 11000 4300 7350 asdb_agdra_20180425_837.fit26/04/2018 20:13 2458235.391 BUI 11000 3867 7359 asdb_agdra_20180426_843.fit26/04/2018 20:50 2458235.452 OGA 11000 4185 7313 asdb_agdra_20180426_868.fit27/04/2018 4:07 2458235.728 LES 13000 4030 7947 asdb_agdra_20180427_172.fit28/04/2018 20:12 2458237.356 FMT 11000 4210 7350 asdb_agdra_20180428_842.fit01/05/2018 3:19 2458239.702 LES 13000 4030 7947 asdb_agdra_20180501_138.fit01/05/2018 20:00 2458240.422 BUI 11000 3860 7359 asdb_agdra_20180501_834.fit02/05/2018 2:50 2458240.682 LES 13000 4030 7947 asdb_agdra_20180502_118.fit02/05/2018 20:21 2458241.377 FMT 11000 4210 7350 asdb_agdra_20180502_848.fit02/05/2018 21:20 2458241.424 JGF 9000 3979 7498 asdb_agdra_20180502_889.fit03/05/2018 20:24 2458242.379 FMT 11000 4210 7350 asdb_agdra_20180503_850.fit04/05/2018 20:11 2458243.37 FMT 11000 4210 7350 asdb_agdra_20180504_841.fit06/05/2018 2:12 2458244.656 LES 13000 4030 7947 asdb_agdra_20180506_092.fit08/05/2018 1:38 2458246.632 LES 12000 4030 7947 asdb_agdra_20180508_069.fit13/05/2018 3:37 2458251.7 LES 13000 4030 7947 asdb_agdra_20180513_151.fit15/05/2018 20:53 2458254.403 FMT 11000 4300 7350 asdb_agdra_20180515_870.fit17/05/2018 1:19 2458255.612 LES 13000 4030 7947 asdb_agdra_20180517_055.fit18/05/2018 20:32 2458257.385 FMT 11000 4300 7350 asdb_agdra_20180518_856.fit19/05/2018 20:36 2458258.387 FMT 11000 4300 7350 asdb_agdra_20180519_858.fit19/05/2018 20:28 2458258.396 BUI 11000 3864 7360 asdb_agdra_20180519_853.fit20/05/2018 20:34 2458259.386 FMT 11000 4300 7350 asdb_agdra_20180520_857.fit23/05/2018 2:23 2458261.656 LES 13000 4030 7947 asdb_agdra_20180523_100.fit24/05/2018 20:48 2458263.396 FMT 11000 4300 7350 asdb_agdra_20180524_867.fit24/05/2018 21:33 2458263.451 OGA 11000 4090 7587 asdb_agdra_20180524_898.fit02/06/2018 20:59 2458272.404 FMT 11000 4300 7350 asdb_agdra_20180602_875.fit11/06/2018 21:11 2458281.411 JGF 11000 3979 7762 asdb_agdra_20180611_883.fit16/06/2018 20:53 2458286.412 JGF 11000 3979 7762 asdb_agdra_20180616_870.fit24/06/2018 20:36 2458294.408 JGF 9000 3979 7762 asdb_agdra_20180624_859.fit29/06/2018 20:44 2458299.406 JGF 9000 3979 7762 asdb_agdra_20180629_864.fit03/07/2018 20:37 2458303.401 JGF 9000 3979 7761 asdb_agdra_20180703_859.fit12/07/2018 20:29 2458312.396 JGF 9000 3979 7762 asdb_agdra_20180712_854.fit17/07/2018 22:14 2458317.455 SCH 9000 3920 7595 asdb_agdra_20180717_927.fit04/08/2018 22:20 2458335.453 FMT 11000 4290 7350 asdb_agdra_20180804_931.fit21/08/2018 20:21 2458352.372 FMT 11000 4300 7150 asdb_agdra_20180821_848.fit28/09/2018 18:28 2458390.301 FMT 11000 4286 7389 asdb_agdra_20180928_770.fit12/10/2018 18:14 2458404.304 JGF 9000 4052 7762 asdb_agdra_20181012_760.fit19/10/2018 18:42 2458411.314 SCH 11000 4036 7592 asdb_agdra_20181019_779.fit27/02/2019 2:53 2458541.649 FMT 11000 4200 7110 asdb_agdra_20190227_121.fit

SYMBIOTICS


Log of observationsAG Dra Echelle spectra (R = 9000 to 13000) in ARAS database (2/2)


TCP J05390410+4748030 Dwarf nova in outburstCATCYSMICS


R.A. 05h39m04.10s, Decl. +47°48'03.0" (J2000.0)2019 Mar. 14.4227 UT, 13.3 mag (CCD, unfiltered)Discoverer: Yuji Nakamura (Kameya-ma, Mie, Japan)

4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

rela

tive

in

ten

sity

TCP J05390410+4748030 2019-03-15 18:13:01 R = 628 Paolo Berardi

Paolo Berardi obtained a spectrum (Lhires III, 150 l/mm, R = 6000) on 2019-03-15.759 typical of a dwarf nova in outburst: Ha and Hb in emission (with perhaps a weak broad absorption), as well as He I 5856, 6678, He II 4686 and the complex NIII/CIII. The FWHM of the Ha and He I 6678 emissions are respectively ~ 900 km.s-1 and 800 km.s-1.

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

5

6

7

rela

tive

in

ten

sity

TCP J05390410+4748030 2019-03-15 19:54:09 R = 549 L Franco

TCP J05390410+4748030 Dwarf nova in outburstCATCYSMICS

0

2E-14

4E-14

6E-14

8E-14

1E-13

1.2E-13

1.4E-13

Rel

ativ

e in

tens

ity

4500 5000 5500 6000 6500 7000


2019-03-15.7592019-03-17.7722019-03-22.775

TCP J05390410+4748030 Paolo BerardiHe

II 4

686

He I

5876

He I

6678

NIII

/CIII

464

0-60

Ha

Hb

Spectral evolution during the decline of the outburst (disk coolling)

New Online Database of Symbiotic Variables

Jaroslav Merc, Rudolf Gális, Marek Wolf

Symbiotic variables belong to an interesting class of interacting binary stars. These objects are unique astrophysical laboratories in studying accretion pro-cesses, winds, jets, and moreover, may be one of the progenitors of type Ia supernovae. These objects are interesting not only from theoretical but also an ob-servational point of view. They display a wide vari-ety of photometric and spectroscopic activity. Not only they vary over long timescales, but they found to be conspicuously variable from night to night and some even from hour to hour. Their outbursts are accompanied by remarkable spectral changes and increases of brightness, vanishing or emerging of the emission lines.

Search for symbiotic binaries

In the previous century, most of the symbiotic bina-ries were found accidentally, but in the last decades, systematic search for such objects have begun. This effort has brought the first results. The surveys have led to discoveries of many new objects and dozens of candidates in the Milky Way (e.g. Miszalski et al., 2013; Miszalski & Mikołajewska, 2014) and the Lo-

cal Group (e.g. Gonçalves et al., 2008, 2012, 2015; Kniazev et al., 2009; Mikołajewska et al., 2014, 2017; Roth et al. 2018). Subsequently, the number of known systems is growing rapidly. Although new approaches and techniques are explored in order to identify new systems (e.g. machine-learning al-gorithms; Akras et al., 2019a), the majority of the surveys is still based on spectroscopic methods. Spectroscopic observations, e.g. the presence of the Raman-scattered OVI lines in the spectra (Akras et al., 2019b), play a dominant role in the confirmation of the symbiotic nature of candidate binaries as well.

Cataloging of the systems and the NewOnline Database of Symbiotic Variables

The growing number of objects is allowing more sys-tematic (and statistical) research. The latest catalog of symbiotic binaries (Belczyński et al., 2000) was almost two decades old when Akras et al. (2019b) published a new census of galactic and extragalactic symbiotics with valuable discussion on their IR SEDs or the presence of the OVI lines.

Galaxy Confirmed SuspectedMilky Way 276 204

Draco Dwarf 1 0IC 10 1 0LMC 10 29M31 31 13M33 13 0M81 0 1M87 0 9

NGC 55 0 3NGC 185 1 0NGC 205 1 2NGC 300 0 8

NGC 2403 0 1NGC 6822 1 11

SMC 12 10Total 347 291

Table 1 - Numbers of confirmed and suspected symbiotic stars in the database. Please refer to an online version of the database for up-to-date numbers.


We have decided to prepare a new, online database of the galactic and extragalactic symbiotic systems (Merc et al., 2019). In addition to the catalog of data for all known symbiotic systems with consistent ref-erences, we created a web-portal for easy access to this information. Making the whole database on-line allows us the addition of new objects as soon as they are discovered and adding or updating data when available. In this way, up-to-date lists of sym-biotic variables and information about objects can be available to the community at any time. The database contains data about the position of the objects, their brightness in different spectral regions and bands and other observational properties (e.g. presence of outbursts, flickering, detectable X-ray or radio emission, symbiotic type), orbital proper-

ties (orbital period, orbital ephemeris, presence of eclipses, etc.) and parameters of the binary compo-nents (their spectral types, effective temperatures, masses, radii, luminosities, presence of pulsations, etc.). The data of symbiotic variables are presented in the form of tables, which can be explored directly through the web-portal or can be downloaded and used offline in different formats (csv, xlsx, txt and pdf). Moreover, for all symbiotic binaries included in the database, we have prepared their object pages covering all available information, references, notes, and useful links. For example, the object pages of symbiotic stars observed by ARAS Group will contain the link to the ARAS database of observations.



Figure 1 - Example of the object page of symbiotic star LIN 9.



The database is divided into two main parts ac-cording to the location of symbiotic variables. The first part consists of 71 confirmed and 87 suspect-ed extragalactic symbiotic systems which are lo-cated in 14 galaxies (LMC, SMC, Draco Dwarf, IC 10, M31, M33, M81, M87, NGC 55, NGC 185, NGC 205, NGC 300, NGC 2403, NGC 6822). The second part of the database, consisting of more than 480 galactic objects will be fully released later this year. How-

ever, the list of galactic symbiotic was already pub-lished on the website recently. The latest version of the web-portal and the New Online Database of Symbiotic Variables, including the up-to-date lists of all known symbiotic variables and candidates as well as the documentation, is available at the address: http://astronomy.science.upjs.sk/symbiotics/

The detailed User’s Guide is available there too.



Figure 2 - Distribution of the galactic symbiotic stars overlaid on the 2MASS infrared image of the sky. Confirmed and suspected symbiotic stars are denoted by blue dots and red squares, respectively.

Several systems are poorly studied. Moreover, for some systems, which were suspected to be symbi-otic based on their photometric behavior, spectro-scopic information is completely missing. Therefore, we think there is a great space for cooperation be-

tween amateur and professional astronomers. The list of the symbiotics which need the spectroscopic observation will be published on the website of the database. ARAS observers might obtain the first spectra for some of the interesting objects.

References

• Akras, S., Leal-Ferreira, M. L., Guzman-Ramirez, L., et al. 2019a, MNRAS, 483, 5077• Akras, S., Guzman-Ramirez, L., Leal-Ferreira, M. L., et al., 2019, ApJS, 240, 21• Belczyński, K., Mikołajewska, J., Munari, U., Ivison, R. J., Friedjung, M. 2000, Astronomy and Astrophysics Supplement Series, 146, 407• Gonçalves, D. R., Magrini, L., Munari, U., et al. 2008, MNRAS, 391, L84• Gonçalves, D. R., Magrini, L., Martins, L. P., et al. 2012, MNRAS, 419, 854• Gonçalves, D. R., Magrini, L., de la Rosa, I. G., et al. 2015, MNRAS, 447, 993• Kniazev, A. Y., Väisänen, P., Whitelock, P. A., et al. 2009, MNRAS, 395, 1121• Merc, J., Gális, R., Wolf, M. 2019, Research Notes of the American Astronomical Society, 3, 28• Mikołajewska, J., Caldwell, N., & Shara, M. M. 2014, MNRAS, 444, 586• Mikołajewska, J., Shara, M. M., Caldwell, N., et al. 2017, MNRAS, 465, 1699• Miszalski, B., Mikołajewska, J., & Udalski, A. 2013, MNRAS, 432, 3186.• Miszalski, B., & Mikołajewska, J. 2014, MNRAS, 440, 1410• Roth, M. M., Sandin, C., Kamann, S., et al. 2018, A&A, 618, A3

Spin, angular momentum, and how they govern your spectra Steve Shore


The 150th anniversary of the publication of Men-deleev's periodic table of the elements and the 90th anniversary of Russell, Shenstone, and Turner's stan-dardization of spectroscopic notation provide a his-torical background for our discussion of state classi-fication. When the "periodicity'' of electrochemical and structural properties of the elements was first systematized, it wasn't at all clear why atoms should know about some specific order. It was Moseley's X-ray spectyroscopy (what we would now refer to as the resonance lines) that revealed the link between the nuclear charge -- the atomic number -- and the systematic displacement of the resonance lines in a row of that table.

Recollections of a chemical childhood

Atomic structure is modeled as a set of shells but these are really descriptions of the base state. Atomic neutrality guarantees that the number of electrons is equal to that of the protons (I know this is childish but it's better too start from the real ba-sics) so one would expect that with infinite super-imposability you could combine the electrons in any mean charge distribution that would minimize the total energy of the system. Rutherford's scattering experiment already demonstrated that this doesn't work since the charge distribution is not mixed and there is no way to place electrons in the nucleus. Instead, and this was, at first, an inference from the chemical and spectroscopic properties, the elec-trons sort into shells with definite gaps and occupa-tions. The first (first row of the PT), has 2 members, the next has 8, and so on. The right hand column doesn't form compounds under normal laboratory conditions, hence the moniker ``noble'', while the first column is extremely reactive (e.g., Li or Na). Looking at the spectral line distribution for He, Ne, and Ar, you see similarities in the distribution of the strongest lines across the elements. But it's the pat-tern that's similar, the wavelengths differ. The astro-nomical contribution

Realizing that the Pickering line series in O star spec-tra provided the clue to what sets the scaling for the energies. The series, which is He II, has lines nearly coinciding with every H I line but with what appear as interlaced series with the same sequences but different separations. The difference in the nuclear charge, two for He, i enough even in the indepen-dent particle picture to provide the scaling. This was taken as a confirmation of the original Bohr-Sommerfeld model for atoms in which the electrons are treated as massive, charged bodies in definite orbits. Although we still ruin young minds with this fiction, forget the Bohr atom: the microworld is not a shrunken solar system. This pseudo-mechanical fantasy required unacceptable, arbitrary tweaks to insure atomic stability and spectroscopic fidelity. Bohr required two properties, however, that actu-ally still hold: (a) any motions (we'll say structure) be closed on itself, therefore coherent on some pe-riodic (angular) coordinate around the nucleus and, (b) a set of integer numbers describe the angular and radial distributions of individual electrons. But in the same way a bicycle wheel rotates when seen in one plane and oscillates between fixed extremes when viewed orthogonally, we're going to make the same pass with atomic structure: replace orbits by oscillations and then ask where the electron would be most likely seen if sampled at random1.

Levels as states

Let's first treat atoms. All energy levels in bound systems, be it an atom or molecule, are discrete (we'll return to one exceptional, but related case, at the end of our discussion). The constituent par-ticles, protons and neutrons -- nucleons -- on one hand, and electrons on the other, are all you need for this discussion. The mass ratio of the nucleons to the electron is about 2000, sufficiently great that atomic structure is centrally symmetric with the nu-cleons located, as you'd guess from their name, in the central nucleus whose size is and properties are

1As an aside, think of taking a time exposure of a lantern swinging on a cord in the dark. You're going to have the strongest exposure at the extremes of the oscillation because the time spent there is longer than in the mid-passage. Harmonic oscillators are the analogy of choice because they're, well, harmonic: they're strictly periodic with fixed frequency and overtones and we know how to solve this motion in closed form for a small amplitude. While this isn't strictly true for any arbitrary motion, strictly periodic motions allow this representation.


determined by the combination of the strong and Coulomb (electromagnetic) forces. This symmetry is essential: the interaction between the electrons and the nucleus depends only on radius and is me-diated through the opposite but equal in magnitude charges of the proton and electron. Since the sim-plest symmetry with a fixed point is a sphere, the base state of a one electron atom -- hydrogen -- is isotropic with a single radius, called the Bohr radius. A state, in our case, is a level in a bound system. It has a definite energy. But it won't have a specific ``identifier''. By that, I mean the classification we've been using all along, based on the combination of attributes (spin, angular momentum) of the individ-ual electrons by which the state is produced. The electric field that binds the individual electrons to the nucleus is purely radial, depending only on the atomic number of the nucleus.

Now to get a bit more detailed and this is where classification of the state enters. I suggest thinking of the atom as a cloud of electrons rather than sin-gle particles, even at the risk of recalling the original Thomson picture. This is a natural pictorial realiza-tion of the time exposure of the oscillators. Com-bining the clouds with different radii and different symmetries (nodes) in an allowed manner produces a state. It's the rules for those combinations that are called a classification scheme. I'll treat the most familiar one, what was originally called Russell-Saunders or spin-orbit coupling, but others are pos-sible. These serve one purpose: they allow a simple labeling of the states and predict what lines can arise from transitions between states. Attributing any nonsphericity to a state is the same, in quantum mechanics, as describing the angular dependence with an angular momentum, l. This is the same as saying that the harmonic oscillator has overtones, the radial contribution is not the same for all pos-sible of the angular momentum and, instead, there

is particular energy associated with each l combina-tion when they superimpose: the electron clouds must combine in phase-coherent ways, so only cer-tain combined values of the total L are permitted for a set of individual l values. Even the next simplest atom, He0, challenges the independent particle pic-ture2.

The intrinsic attribute called "spin"

Spin is an internal property of electrons, depending neither on spatial coordinates nor time, that mani-fests itself only relative to something else. In effect, a free electron has a spin of ħ/2, where ħ=h/2p (h is the Planck constant) just as it has a charge, e. But this matters only if the electron interacts with either light, an external field, or other particles. This isn't at all counter-intuitive or difficult: analogously, you can't tell the color of a picture in the dark although, chemically, it has this attribute. Any scattering ex-periment with another particle is partly mediated by their spins, which are summed over to get the total cross section. The occupation of a state is amusingly similar to sit-ting in a theater. The seats are arranged in integer occupation sites and with a fixed number per row. Full occupation means each seat is taken but if peo-ple were identical they could be permuted among the seats without changing either the occupation number or the total energy of the state. Now that's in a civilized audience. Add the possibility that each seat actually can sustain two occupants, one sitting on the other's lap3. Again, the laps that are either occupied or not can be permuted without changing any state attribute but there is a maximum multi-plicity for each row equal to twice the number of available seats. The rows are filled in order, starting from the bottom. To make the analogy more spe-cific, the H row has two places, the Li row 8, and so on. To extend the analogy, each person can be sit-

2 While I don't mean to be too polemical here, I want to offer a parenthetical observation. The language we still employ in quantum mechanics when describing atoms has conserved in its vocabulary this solar system picture that, I think, interferes with understanding. Angular momen-tum is another way of talking about a spatial symmetry, not that the electrons are orbiting. Orbitals, a term you know from chemistry, are the same. Spin was chosen as a label because it seemed to be the quantum mechanical analog of the only previously untreated property of the microworld solar system, like the spins of planets. But in each of these cases, you're forced to make the arbitrary leap of imagining that what in the macroworld is a continuously variable quantity, magically becomes discrete (quantized) on a microscale. It's too late to hope for a reform of the language but at least try to think of symmetries instead of motions. This is natural from crystals and molecular models.

3 OK, we could imagine them head or feet up too but that requires acrobatic skills.



ting upright or upside down indifferently. So there are two possible alignments. If one person climbs over the seat back to get to the next row, that leaves an unoccupied seat in one row and occupies a seat in another so this is a distinct difference in configu-ration and, therefore, a different energy. But as the front row obscures the view from the back, the same for the nucleus and the electrons. A single occupied seat in the third row with the first two occupied is not the same as a single occupant of the first row. Put more precisely, the electrons screen the nuclear charge and the more inner shells are occupied the greater the screening; hence the scaling is not based only on the protons but also on the particular state occupation and how that screens the nucleus for each electron.

This is where spin becomes vital. The individual electrons don't only interact through their charge, they also overlap in this internal property and have a limited set of permitted combinations. Pairwise, they can be either both head up or head both down or one up and one down indifferently. This is the point where one applies the Pauli exclusion princi-ple that, remember, is an axiom: no two electrons can have precisely the same label, i.e., precisely the same quantum numbers. Since every electron has a radial quantum number, n, angular momentum l and its projection ml (although this is really a set of the possible projected values that l can take if an axis is arbitrarily defined, to put two electrons in the same shell requires another number, in this case s. Note that while l can have any positive integer value, s is unique, 1/2. For H, this is simple. Having only one electron, each state has two possible projec-tions of s relative to the nucleus so each state is real-ly a doublet, regardless of its (n,l) value. Transitions occur only between states of different angular sym-metry so δl = ±1 (so 2s → 1s is, for example, strictly forbidden for the hydrogen atom (this is, actually, a two-photon transition but that's a different story: it's observed in nebular spectra as a blue continuum but not in comparatibvely normal sources such as stellar atmospheres).

Again using the He atom, in its ground state, 1s2, both electrons have l = 0 and the same n. There is

only one permitted pairing, s1 and s2 have to cancel so the total S vanishes. This gives a unique state, 1s2 1S0 for the ground state. An excited state, 1s2s now has two different n values so there are two possible combinations for the projections of spin, one with S = 1 and another with S = 0 for the same angular mo-mentum. Thus there are two, non-identical combi-nations leading to slightly different energies, 1S0 and 3S1. No passage is possible between the two since that would require a change in the projection of the spin, which is not possible in the central field of the atom. It could be induced if the right radiation were to excite one of the states, but it has no dipole mo-ment so cannot happen as a permitted transition. More to the point, the 3S1 state is pseudo-stable since, like the transition between the sublevels, the state can't decay by dipole emission. Then each excited state of He I has the same pairing, a singlet and triplet sequence depending on the combina-tion of the two electrons. The original observation that pointed to the incompleteness of this descrip-tion was that while there is a singlet for the ground state transition of neutral helium, there is no corre-sponding line for the triplets. The analog system is H-. This too has a 1s2 configuration but with a hitch: the nucleus has only one proton so the electrons are much more weakly bound than in neutral hydrogen. More to the point, an excited state (i, s)1(n,l)2 sees a very screened nuclear charge from the 1, and so is very weakly bound. The ionization energy of Ho is 13.6 eV, that of H- is less than 1 eV while for Heo it is about 25 eV.

Imposing an external magnetic field

One way of imagining spin-field interactions I owe to my siamese cats. Ptolemy was a trusting little fel-low. Held belly up in your arms he would remain that way if tossed lightly upward, being firmly con-vinced he'd be caught (which he always was, so the behavior was a self-reinforcing belief system). But Hodge, who was far more skeptical, would always flip. Both sensed that there was a field providing a preferred direction in space (gravity, down) and their internal process made them react to it (and differently): Ptolemy was like a boson, Hodge like a fermion.



Now that's for a steady field. For the electron, it be-haves as if it has a polarizability such that if a mag-netic field is introduced, there are two possible sub-states of "aligned'' and "anti-aligned'' electrons. This is the Zeeman effect. The magnitude of the splitting in energy depends on the projections of the overall polarizability produced by the combined electrons in a state and the transitions between these sublev-els produce an ensemble of very closely spaced lines whose separations also depend linearly on the field strength (if the field is relatively weak). Since the states are individually coherent, the transitions are polarized (as Christian Buil's beautiful spectropolari-metric observations show for magnetic stars). If no field is imposed, the states are degenerate; there is no discernible difference between the different sub-states for a given total (L,S) combination. Relative to the nucleus the electrons also polarize depending on their dipole strengths. This comes from the dual polarizability of the protons and electrons. I need to again emphasize that the spins are not a spatial property so the proton and electron individually have this intrinsic property that shows itself when they interact. Thus, the 1s state of H is very slightly split, corresponding to the 21 cm transition of inter-stellar fame, but with so weak a transition strength that the flip occurs with a characteristic transition timescale of megayears instead of nanoseconds.

Now imagine you excite the state by irradiating the atom with a time dependent electromagnetic field. If you think of the polarizability as a two state system, it has a specific frequency at which it reso-nates. A transition between states, when separated by a steady state field, causes the system to emit or absorb at a specific frequency, a resonance. In MRI, this uses the nuclear spins and their combined reac-tion to other nuclei in their vicinity (as in a molecule, in which the atoms are linked by bonds so respond collectively. The molecules are individual but the at-oms aren't.

Selection rules and transitions

As a final point, once the states have been specified within a coupling scheme, you also know what tran-sitions can occur and what their intrinsic strength

is. In LS coupling (Russell-Saunders, the classifi-cation scheme used in Moore's Revised Multiplet Table and listed in the NIST database, the individual electron configurations produce multiplets are la-beled by the combined orbital L, spin, S, and total, J, angular momenta as (2S+1)LJ, e.g., 3D1. To obtain these, the projections are summed and only those combinations that respect the exclusion principle are permitted (the difference between, say, the nd2 and ndn'd basis state. Noting that no transition is ever truly impossible, merely highly improbable (a line from The Hitchhiker's Guide to the Galaxy), any process that requires only the spin to change is for-bidden as an electric dipole transition (so there is no permitted conversion of triplet to singlet states for neutral helium, for example). In a recombination cascade, one multiplicity will not combine with an-other except by collisional de-excitation (since the collisions mix the spin states). So in stellar atmo-spheres, there is collisional coupling even between multiplets. It's important to keep in mind that the electron configuration is what matters, the coupling rules label the states. The usual procedure for iden-tification is actually an inverse process: computing the separations based on a coupling approximation and scaling the energies to the observed spectrum for an ion.

Finally, there's one case that arises from the strong interaction of the electrons in a basis configuration: autoionization. This is the most extreme example of a state mixing, caused in part by the electron's spin. It's possible that the combination of the different spin-orbit values produces a level that lies above the ionization limit. Although hydrogen doesn't show this, all other atoms do. This is the same as say-ing the electron is metastably bound, that it can re-main bound for a time but then becomes free. The alternate picture is that absorption leads to more than one electron transitioning at a time so the final configuration is not the same as would happen with only one "valence'' electron. Such states are also possible in the inverse process to ionization, when the cascade internally excites transitions (radiation-less), a process called dielectronic recombination. Both are observed in stellar spectra, and DR is very important in the ionization balance of the corona




and the interstellar medium (diffuse media that are nearly collisionless).

Coda

I want to thank Francois for suggesting the topic this issue. I hope the topic has been interesting and this discussion helpful. As you get progressively deeper in your use of spectroscopic diagnostics , it can be useful to understand on what physical assumptions they're based and atomic structure is the most es-sential. In the next column,I'll generalize this dis-cussion to molecules since, as you get more familiar with cool stellar spectra, diatomic molecules will become familiar friends. Thank you and warmest wishes for your observing success, I hope to see you at OHP in August. Please let me know if there's any-thing you'd like to suggest or ask or critique.


Some sugested resources for the stout-hearted, beside the notes in the NIST Atomic Database website:

Osterbrock, D. and Ferland, G. 2005, Astrophysics of Gaseous Nebulae and Active Galactic Nuclei,2nd Ed (Sacramento: University Science Books)Merrill, P. 1958, Lines of the chemical elements in astronomical spectra(http://adsabs.harvard.edu/abs/1958lcea.book.....M) (it doesn't get better!)Hubeny, I. and Mihalas, D. 2015, Theory of Stellar Atmsopheres (Princeton: Princeton Univ.Press)Cowan, R. D. 1981, The Theory of Atomic Structure and Spectra (Berkeley: Univ. of CaliforniaPress) (heavy, computationally oriented, but it's all here; Cowan authored the basic code thatwas extended by Kurucz for computing the line lists used for model stellar atmospheres)Griem, H. R. 1997, Principles of Plasma Spectroscopy (Cambridge: Cambridge Univ. Press) (moreaccessible, and current, than the classic from 1962) Ünsold, A. 1955, Physik der Sternatmosphären (Berlin: Springer) (the genuine classic, still worththe trouble; for my German speaking friends) Saltzmann, D. 1998, Atomic physics in hot plasmas, (Oxford: Oxford University Press) Jeries, J. 1968, Spectral Line Formation (Mass: Blaisdell) (leaning toward the Sun, this has realinsights without heavy mathematics) Cowley, C. R. 1970, The Theory of Stellar Spectra (NY: Gordon and Breach) (a sadly little knowngem on atmospheres, spectra, and more) Letokhov, Vl. and Johansson, S. 2009, Astrophysical Lasers (Oxford: Oxford Univ. Press) (by themaster of laboratrory spectroscopy, Johansson was the worthy successor to Ångström at Lund) ... and although I hesitate on this one, Shore, S. N. 2003, The Tapestry of Modern Astrophysics(NY: Wiley-Interscience)

A Census of Symbiotic Stars in the 2MASS, WISE, and Gaia SurveysAkras, Stavros; Guzman-Ramirez, Lizette; Leal-Ferreira, Marcelo L.; Ramos-Larios, GerardoThe Astrophysical Journal Supplement Series, Volume 240, Issue 2, article id. 21, 23 pp. (2019)

We present a new census of Galactic and extragalactic symbiotic stars (SySts). This compilation contains 323 known and 87 candidate SySts. Of the confirmed SySts, 257 are Galactic and 66 extragalactic. The spectral energy distributions (SEDs) of 348 sources have been constructed using 2MASS and AllWISE data. Regarding the Galactic SySts, 74% are S types, 13% D, and 3.5% D′. S types show an SED peak between 0.8 and 1.7 μm, whereas D types show a peak at longer wavelengths between 2 and 4 μm. D′ types, on the other hand, display a nearly flat profile. Gaia distances and effective temperatures are also presented. According to their Gaia distances, S types are found to be members of both thin and thick Galactic disk populations, while S+IR and D types are mainly thin disk sources. Gaia temperatures show a reasonable agreement with the temperatures derived from SEDs within their uncertainties. A new census of the O VI λ6830 Raman-scattered line in SySts is also presented. From a sample of 298 SySts with available optical spectra, 55% are found to emit the line. No significant preference is found among the different types. The report of the O VI λ6830 Raman-scattered line in non-SySts is also discussed as well as the correlation between the Raman-scattered O VI line and X-ray emission. We conclude that the presence of the O VI Raman-scattered line still provides a strong criterion for identifying a source as a SySt.

Hen 3-160 - the First Symbiotic Binary with Mira Variable S StarGałan, C.; Mikołajewska, J.; Monard, B.; Iłkiewicz, K.; Pieńkowski, D.; Gromadzki, M. Acta Astronomica, vol 69, no 1, p. 25-44

Hen 3-160 is reported in Belczyński et al. catalog as a symbiotic binary system with M7 giant donor. Using V- and I-band photometry collected over 20 years we have found that the giant is a Mira variable pulsating with 242.5-day period. The period-luminosity relation locates Hen 3-160 at the distance of about 9.4 kpc, and its Galactic coordinates (l=267.°7, b=-7.°9) place it ≍1.3 kpc above the disk. This position combined with relatively high proper motions (μαcosδ=-1.5 mas/yr, μ_δ=+2.9 mas/yr, Gaia DR2) indicates that Hen 3-160 has to be a Galactic extended thick-disk object. Our red optical and infrared spectra show the presence of ZrO and YO molecular bands that appear relatively strong compared to the TiO bands. Here we propose that the giant in this system is intrinsic S star, enriched in products of slow neutron capture processes occurring in its interior during an AGB phase which would make Hen 3-160 the first symbiotic system with Mira variable S star.

First Release of the New Online Database of Symbiotic VariablesMerc, Jaroslav; Gális, Rudolf; Wolf, Marek Research Notes of the American Astronomical Society, Volume 3, Issue 2, article id. 28 (2019).

Spectroscopic observations of symbiotic stars in 2018-Q4Teyssier, F.; Boyd, D.; Guarro, J.; Sims, F.; Foster, J.; Somogyi, P.; Berardi, P.; Sollecchia, U.; Charbonnel, S.; Bohlsen, T.; Campos, F.; Martineau, G.; Buchet, Y.; Graham, K.; Boussin, C.; Boubault, F.; Franco, L.; Rodda, T.; Marik, V.; Buil, C. Kantola, T.; Coffin, J.Eruptive Stars Information Letter, vol.40, p. 4-75

202 spectra of 26 symbiotic stars at resolution from 500 to 15000 were obtained during 2018-Q4. AG Dra has recovered its quiescent state after April 2018 outburst. CH Cyg has been monitoring at a high cadency during its monotonically decline from mag V = 6.4 early august to V = 8.5. More than 700 spectra of CH Cygni are now gathered in the database. First spectrum of the poorly studied EF Aql in the database. Spectra of the new symbiot-ic Hen 3-1768 detected within the context of the program "suspected symbiotic stars" show strong He II l 4686 and Raman OVI 6830. The new symbiot-ic star HbHa 1704-058 observed during its decline show increasing raman OVI band (EW = -3.3) while [OIII] and [Fe VII] remain very weak if present. V694 Mon, at high luminosity (V 9) , presents unusual shape of Balmer and Fe II lines: the common broad absorption is replaced by P Cygni profiles at much low-er velocities (maximum of absorption -100 km s-1). The prototypical Z And returns to quiescent state after the outburst which occurred in January 2018.

An investigation of the eclipsing symbiotic binary BF Cyg during a period of activity after 2014Tomov, Nikolai A.; Tomova, Mima T.; Bisikalo, Dmitry V.Bulgarian Astronomical Journal, Vol. 30, p. 60

The symbiotic system BF Cyg is an eclipsing binary. It flared in 2006 and in 2016 its optical brightness was in its fifth orbital minimum (eclipse) from the beginning of the eruption. We investigated the behaviour of the brightness during this minimum and considered the evolution of the accretion structure surrounding the outbursting compact object. We obtained the basic parameters of this structure from UBVR_{C}I_{C} data at the time of the fifth orbital minimum.

Infrared Spectroscopy of Symbiotic Stars. XII. The Neutron Star SyXB System 4U 1700+24 = V934 HerculisHinkle, Kenneth H.; Fekel, Francis C.; Joyce, Richard R.; Mikołajewska, Joanna; Gałan, Cezary; Lebzelter, ThomasThe Astrophysical Journal, Volume 872, Issue 1, article id. 43, 17 pp. (2019).

The X-ray symbiotic (SyXB) V934 Her = 4U 1700+24 is an M giant-neutron star (NS) binary system. Employing optical and infrared radial velocities spanning 29 yr combined with the extensive velocities in the literature, we compute the spectroscopic orbit of the M giant in that system. We determine an orbital period of 4391 days, or 12.0 yr, the longest for any SyXB and far longer than the 404 day orbit commonly cited for this system in the literature. In addition to the 12.0 yr orbital period, we find a shorter period of 420 days, similar to the one previously found. Instead of orbital motion, we attribute this much shorter period to long secondary pulsation of the M3 III SRb variable. Our new orbit supports earlier work that concluded that the orbit is seen nearly pole-on, which is why X-ray pulsations associated with the NS have not been detected. We estimate an orbital inclination of 11.°3 ± 0.°4. Arguments are made that this low inclination supports a pulsation origin for the 420 day secondary period. We also measure the CNO and Fe peak abundances of the M giant and find it to be slightly metal-poor compared to the Sun, with no trace of the NS-forming supernova event. The basic properties of the M giant and NS are derived. We discuss the possible evolutionary paths that this system has taken to get to its current state.

Recent publications

Symbiotics


Recent publications

Symbiotics


High-velocity equatorial mass ejections and some other spectroscopic phenomena of the symbiotic star CH Cygni in an active stageIijima, T.; Naito, H.; Narusawa, S.Astronomy & Astrophysics, Volume 622, id.A45, 15 pp.

TCH Cyg is one of the most studied symbiotic stars. Its properties, however, are still not well known. Two main periods, about 15 years and 750 days, are known in the photometric and spectroscopic variations, and two models are proposed for these origins. One is a binary system with an orbital period of 15 years consisting of a hot component and pulsating red giant with a 750-day period. The other is a triple system consisting of an inner symbiotic binary with an orbital period of about 750 days and third component with an orbital period of 15 years. Several active stages have been observed since the 1970s during which the object brightened up by ∆U = 3-5 mag and prominent emission lines appeared. Large mass outflows were observed at some active stages. Aims: The spectral variation of CH Cyg has been monitored at Asiago Observatories to understand the problems mentioned above. We have analysed spectra obtained in the time period from 1995 to 2004 which covers an active stage during the years 1998-2000. Methods: High- and low-resolution optical spectra obtained at the Asiago Observatories are used. Results: Narrow absorption lines of Fe I, Cr I, Ti I, and so on appeared in 1998 at an early phase of the active stage. These lines are clearly distin-guished from those of the M-type giant and are typically found on the spectrum of early A-type dwarfs. They were redshifted by about 30 km s-1 with respect to the absorption lines of the M-type giant. Assuming that their radial velocities represent the orbital motion of the hot component, its semi-amplitude is estimated to be 37.0 ± 0.5 km s-1. The masses of the hot component and the M-type giant are estimated to be 0.32 ± 0.02 M≍ and 4.6 ± 0.2 M≍, respectively, where a circular orbit with a period of 756 days is adopted. If the inner binary system has an elliptical orbit, e = 0.33, and a period of 750.1 days, the masses of the two components are 0.21 ± 0.01 M≍ and 2.2 ± 0.1 M≍, respectively. Our results lend sup-port to the triple system model, because if the period of the symbiotic binary were 15 years, the mass of the hot component would be expected to exceed the Chandrasekhar limit. Highly blueshifted absorption components of H I and He I lines appeared at a later phase of the active stage. Mass ejections with velocities on the order of 1000 km s-1 seem to have occurred along the orbital plane from December 1998 to March 1999. The highest outflow velocity, - 2383 km s-1, was observed on 1999 February 26. Narrow absorption components of Na I D1, D2, and Fe II lines redshifted by 10-15 km s-1 coexisted with the highly blueshifted broad absorption components of H I and He I lines. This phenomenon might have been related to an inner disc inflow expected in wind-compressed discs. In contrast to the bipolar mass outflows at the past active stages, high-velocity equatorial mass ejections likely occurred at the active stage during the years 1998-2000. There should have been an eclipse of the hot component by the M-type giant in the inner binary system in the time period of December 1998 to January 1999. A clear light curve of the eclipse, however, was not detected. Possibly, the luminosity of the hot component was due mainly to free-free emission from the ejected circumstellar matter which was likely more extended than the M-type giant. On the other hand, another eclipse by the third component with the period of 15 years began at the end of May 1999 during which the hot component as well as the emitting regions of Hβ and Fe II lines were well eclipsed. The obscuring matter around the third component should have been much more extended than the M-type giant, and it was likely semi-transparent, because the spectrum of the M-type giant was well seen during the eclipse. The third component appears to be similar to the invisible secondary component in the long-period eclipsing binary ≍ Aur. The spectra and velocities are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/622/A45

FUSE Spectroscopic Analysis of the Slowest Symbiotic Nova AG Peg During QuiescenceSion, Edward M.; Godon, Patrick; Mikolajewska, Joanna; Katynski, MarcusThe Astrophysical Journal, Volume 874, Issue 2, article id. 178, 8 pp. (2019).

We present a far-UV (FUV) spectroscopic analysis of the slowest known symbiotic nova AG Peg that underwent a nova explosion in 1850 followed by a very slow decline that did not end until ≍1996, marking the beginning of quiescence. In 2015 June, when AG Peg exhibited a Z And-type outburst with an optical amplitude of ≍1.5 mag. We used accretion disk and WD photosphere synthetic spectral modeling of a Far-Ultraviolet Spectroscopic Explorer (FUSE) spectrum obtained on 2003 June 5.618. The spectrum is heavily affected by ISM absorption as well as strong emis-sion lines. We dereddened the FUSE fluxes assuming E(B-V)=0.10, which is the maximum galactic reddening in the direction of AG Peg. We discuss our adoption of the pre-Gaia distance over the Gaia parallax. For a range of white dwarf surface gravities and surface temperatures, we find that the best-fitting photosphere is a hot WD with a temperature T wd = 150,000 K, and a low gravity log(g) ≍ 6.0─6.5. For a distance of 800 pc, the scaled WD radius is R wd ≍ 0.06 × R ≍, giving log(g) = 6.67 for a 0.65 M ≍ WD mass. The Luminosity we obtain from this model is L = 1729 L ≍. The hot photosphere models provide better fits than the accretion disk models, which have FUV flux deficits toward the shorter wavelengths of FUSE, down to the Lyman limit. Given the uncertainty of the nature of a true symbiotic accretion disk, and, while a very hot low gravity degenerate star dominates the FUV flux, the presence of a steady-state (standard) accretion disk cannot be summarily ruled out.

Optical spectroscopic and polarization properties of 2011 outburst of the recurrent nova T PyxidiPavana, M.; Anche, Ramya M.; Anupama, G. C.; Ramaprakash, A. N.; Selvakumar, G.Astronomy & Astrophysics, Volume 622, id.A126, 14 pp.

We aim to study the spectroscopic and ionized structural evolution of T Pyx during its 2011 outburst, and also study the variation in degree of polarization during its early phase. Methods: Optical spectroscopic data of this system obtained from day 1.28-2415.62 since discovery, and optical, broadband imaging polarimetric observations obtained from day 1.36-29.33 during the early phases of the outburst were used in the study. The physical conditions and the geometry of the ionized structure of the nova ejecta was modelled for a few epochs using the photo-ionization code, CLOUDY in 1D and pyCloudy in 3D. Results: The spectral evolution of the nova ejecta during its 2011 outburst is similar to that of the previous outbursts. The variation in the line profiles is seen very clearly in the early stages due to good coverage during this period. The line profiles vary from P Cygni (nar-rower, deeper, and sharper) to emission profiles that are broader and structured, which later become narrower and sharper in the late post-outburst phase. The average ejected mass is estimated to be 7.03 × 10-6 M≍. The ionized structure of the ejecta is found to be a bipolar conical structure with equatorial rings, with a low inclination angle of 14.75 ° ±0.65°. The spectra are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/622/A126

A UV and optical study of 18 old novae with Gaia DR2 distances: mass accretion rates, physical parameters, and MMRDSelvelli, Pierluigi; Gilmozzi, RobertoAstronomy & Astrophysics, Volume 622, id.A186, 16 pp.

We combine the results of our earlier study of the UV characteristics of 18 classical novae (CNe) with data from the literature and with the recent precise distance determinations from the Gaia satellite to investigate the statistical properties of old novae. All final param-eters for the sample include a detailed treatment of the errors and their propagation. The physical properties reported here include the absolute magnitudes at maximum and minimum, a new maximum magnitude versus rate of decline (MMRD) relation, and the inclination-corrected 1100-6000 Å accretion disk luminosity. Most importantly, these data have allowed us to derive a homogenous set of accretion rates in quiescence for the 18 novae. All novae in the sample were super-Eddington during outburst, with an average absolute magnitude at maximum of -7.5 ± 1.0. The average absolute magnitude at minimum corrected for inclination is 3.9 ± 1.0. The median mass accretion rate is log Ṁ1 M≍ = -8.52 (using 1 M≍ as WD mass for all novae) or log ṀMWD = -8.48 (using the individual WD masses). These values are lower than those assumed in studies of CNe evolution and appear to attenuate the need for a hibernation hypothesis to interpret the nova phenomenon. We identified a number of correlations among the physical parameters of the quies-cent and eruptive phases, some already known but others new and even surprising. Several quantities correlate with the speed class t3 including, unexpectedly, the mass accretion rate (Ṁ). This rate correlates also with the absolute magnitude at minimum corrected for inclination, and with the outburst amplitude, providing new and simple ways to estimate Ṁ through its functional dependence on (more) easily observed quantities. There is no correlation between Ṁ and the orbital period. Based mainly on INES data from the IUE satellite. Other UV data utilized in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST), see Paper I. This work has made use of data from the European Space Agency (ESA) mission Gaia (http://https://www.cos-mos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

Hubble Space Telescope Far-UV Spectroscopy of the Short Orbital Period Recurrent Nova CI Aql: Implications for White Dwarf Mass EvolutionSelvelli, Pierluigi; Gilmozzi, RobertoSion, Edward M.; Wilson, R. E.; Godon, Patrick; Starrfield, Sumner; Williams, Robert E.; Darnley, M. J.The Astrophysical Journal, Volume 872, Issue 1, article id. 68, 6 pp. (2019).

An Hubble Space Telescope Cosmic Object Spectrograph Far UV spectrum (1170 Å to 1800 Å) was obtained for the short orbital pe-riod recurrent novae (T Pyxidis subclass), CI Aquilae. CI Aql is the only classical Cataclysmic variable (CV) known to have two eclipses of a sensible depth per orbit cycle and also to have pre- and post-outburst light curves that are steady enough to allow estimates of mass and orbital period changes. Our far-ultraviolet (FUV) spectral analysis with model accretion disks and non-LTE high-gravity photospheres, together with the Gaia parallax, reveal that CI Aql's FUV light is dominated by an optically thick accretion disk with an accretion rate of the order of 4 × 10-8 M ≍ yr-1. Its database of light curves, radial velocity curves, and eclipse timings is among the best for any CV. Its orbit period (P), dP/dt, and reference time are rederived via a simultaneous analysis of the three data types, giv-ing a dimensionless post-outburst dP/dt of (-2.49 ± 0.95) × 10-10. The lack of information on the loss of orbital to rotational angular momentum leads to some uncertainty in the translation of dP/dt to the white dwarf (WD) mass change rate, dM1/dt, but within the modest range of +4.8× {10}-8 to +7.8 × 10-8 {M}≍ {yr}}-1. The estimated WD mass change through outburst for CI Aql, based on simple differencing of its pre- and post-outburst orbit period, is unchanged from the previously published +5.3× {10}-6{M}≍ . At the WD's estimated mass increase rate, it will terminate as a Type Ia supernova within 10 million years.

Recent publications

Novae


Astro2020 Science White Paper: A Shocking Shift in Paradigm for Classical NovaeChomiuk, Laura; Aydi, Elias; Babul, Aliya-Nur; Derdzinski, Andrea; Kawash, Adam; Li, Kwan-Lok; Linford, Justin; Metzger, Brian D.; Mukai, Koji; Rupen, Michael P.; Sokoloski, Jennifer; Sokolovsky, Kirill; Steinberg, Elad2019arXiv190308134C

The discovery of GeV gamma-rays from classical novae has led to a reassessment of these garden-variety explosions, and highlight-ed their importance for understanding radiative shocks, particle acceleration, and dust formation in more exotic, distant transients. Recent collaboration between observers and theorists has revealed that shocks in novae are energetically important, and can even dominate their bolometric luminosity. Shocks may also explain long-standing mysteries in novae such as dust production, super-Eddington luminosities, and `flares' in optical light curves. Here, we highlight the multi-wavelength facilities of the next decade that will further test our nova shock model and fulfill the promise of novae as powerful astrophysical laboratories.

The UBV Color Evolution of Classical Novae. III. Time-stretched Color─Magnitude Diagram of Novae in OutburstHachisu, Izumi; Kato, MarikoThe Astrophysical Journal Supplement Series, Volume 241, Issue 1, article id. 4, 67 pp. (2019).

We propose a modified color─magnitude diagram for novae in outburst, i.e., (B − V)0 versus (M V − 2.5 log f s), where f s is the time-scaling factor of a (target) nova against a comparison (template) nova, (B − V)0 is the intrinsic B − V color, and M V is the absolute V magnitude. We dub it the time-stretched color─magnitude diagram. We carefully reanalyzed 20 novae based on the time-stretching method and revised their extinctions E(B − V), distance moduli in the V-band (m − M) V , distances d, and time-scaling factors f s against the template nova LV Vul. We have found that these 20 nova outburst tracks broadly follow one of the two template tracks, the LV Vul/V1668 Cyg or V1500 Cyg/V1974 Cyg group, in the time-stretched color─magnitude diagram. In addition, we estimate the white dwarf masses and (m − M) V of the novae by directly fitting the absolute V model light curves (M V ) with observational ap-parent V magnitudes (m V ). A good agreement of the two estimates of (m − M) V confirms the consistency of the time-stretched color─magnitude diagram. Our distance estimates are in good agreement with the results of Gaia Data Release 2.

Novae

Recent publications


Eruptive stars spectroscopyCataclysmics, Symbiotics, Novae


cataclysmics, symbiotics, novae - astrosurf · 47 v1016 cyg 19 57 4.9 39 49 33.9 18 15/04/2015...

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