cataclysmics, symbiotics, novae - astrosurf

Eruptive stars spectroscopyCataclysmics, Symbiotics, Novae

Eruptive StarsInformation Letter n° 39 #2018-03 24-11-2018

Observations of Jul. - Sept. 2018Contents

Nova4 novae observed: Nova Sct 2018 Nova Lup 2018 Nova Oph 2018c detected in AugustNova Sct 2017 in nebular phase

Symbiotics

The new symbiotic HaHb 1705-04 Z And outburst (declining)CH Cygni: fading in July New faint symbiotics in the database (J. Foster)

Notes

Spectroscopy with Omicron 1 m telescop in southern FranceOlivier Garde, Pascal Le Du, Bertrand Guegan

Miscellanous notes: MWC 560, Recurrents, Narrow lines in novaeSteve Shore

Conference Small Telescopes - Tatranskà Lomnica (Slovakia) F. Teyssier

“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, J. Guarro, J. Foster, P. Somogyi, C. Boussin, D. Boyd, T. Lester, K. Graham, F. Sims, C. Buil, T. Bohlsen, P. Lucas, F. Campos, L. Franco, L. Franco, M. Verlinden, O. Garde, P. Berardi, J. Montier, P. Cazzato, T. Bohlsen, P. Cazzato, U. Sollecchia, V. Marik, G. Martineau, Y. Buchet, K. Bazan, B. Guegan, T. Rodda, P. Dubreuil, S. Charbonnel, T. Rodda, M. Mannucci, N.Montigiani, V. Andreoli, P. Le Du, H. Boussier

p. 2

p. 19

p. 103

p. 105

p. 109

NEWS Campaign on the request of Adrian Lucy andJennifer SokolovskiDiscover a symbiotic star!See page 99

Authors :

ARAS Eruptive Stars Information Letter 2018-03 - p. 2

List of galactic novae in 2018

GCVSName Date Mag A.D. (2000) DE (2000)

14 nova Oph 2018c PNV J17422408-2053088 2018-8 8.960 17 42 24.08 -20 53 08.813 nova Sct 2018 TCP J18292290-1430460 2018-6-29.577 10.3 18 29 22.93 -14 30 44.2 10.512 nova Lup 2018 PNV J15384000-4744500 2018-6-3.431 15 38 43.84 -47 44 41.1 911 nova Per 2018 V392 Per TCP J04432130+4721280 2018 -4-29.740 04 43 21.37 +47 21 25.8 6.310 nova Sgr 2018 PNV J18040967-1803581 2018-4-8.72 11.2 18 04 09.46 -18 03 55.7 10.89 nova CMa 2018 TCP J07134590-2112330 2018-3-24.496 12 07 13 45.84 -21 12 31.3 10.38 nova Car 2018 ASASSN-18fv 2018-3-20.32 <10.0 10 36 13.71 -59 35 55.1 5.97 nova Oph 2018b PNV J17140261-2849237 2018-3-10.805 17 14 2.53 -28 49 23.3 9.46 nova Sco 2018c ASSASN-18ds 2018-2-24.36 14.3 17 3 47.509 -38 16 57.14 9.85 nova Oph 2018 PNV J17244011-2421463 2018-2-12.834 12.5 17 24 40.11 -24 21 46.3 12.84 nova Sco 2018b PNV J16484962-4457032 2018-2-6.863 11.7 16 48 49.68 -44 57 2.9 10.13 nova Cir 2018 PNV J13532700-6725110 2018-1-19.708 9.1 13 53 27.59 -67 25 0.9 5.72 nova Sco 2018 PNV J17180658-3204279 2018-1-17.869 11 17 18 6.37 -32 4 27.7 10.21 nova Mus 2018 PNV J11261220-6531086 2018-1-14.486 11 26 15.16 -65 31 23.3 6.5

# Coordinates Mag MaxName Discovery

Authors:Teyssier, F.; Sollecchia, U. ; Garde, O.; Guarro, J.; Bohlsen, T.; Luckas, P.; Berardi, P.; Boyd, D.; Buil, C.; Char-bonnel, S.; Foster, J.; Graham, K.; Sims, F.; Somogyi, P.; Andreoli, V.; Bazan, X; Boubault, F.; Boussin, C.; Bu-chet, Y.; Campos, F.; Castellini, F.; Coffin, J. Dubreuil, P.; Franco, L.; Guegan, X; Kantola, T.; Lorenzo, F; Man-nucci, M.; Marik, V.; Martineau, G; Moltomoli, S.; Montigiani, N. Rodda, T.;

Spectroscopic observations of novae in 2018-Q3

ARAS Eruptive Stars Information Letter #39 2018-03

Abstract:

We present spectroscopic observations (R = 500 to 15000) of 4 novae during 2018, 3rd quarter.Nova Sct 2017: in nebular phase, shows quick and strong changes at a short time scale, noticely high excitation lines such as He II or [Fe VII]. Nova Lup 2018: discovered on June, 3rd Nova Sct 2018: discovered on June, 29th was identified as a nova by Umberto Sollecchia and Olivier Garde on June, 30 th (ATel#11802). The spectroscopic development is described using ATels#11802, 11826, 11859 written by Steve Shore for ARAS group.Nova Oph 2018c: By means of high cadency monitoriring, the helium flash is precisely dated (2018-08-29) and an unexpected weakening of helium lines is detecyed on 2018-09-08

Nova Sct 2017, Nova Lup 2018, Nova Sct 2018, Nova Oph 2018c

Nova Sct 2017NOVAE

Coordinates (2000.0)R.A. 18 31 45.9Dec -14 18 55.6Mag V 8.55 (Max)

AAVSO V band lighgtcurve and ARAS Spectra (blue dots)

Note: oscillations continue during nebular phase with a rebrightning of ~ 0.4 mag from mid-July (V ~13.3) to mid-August (V ~12.9)


The peculiar nova Sct 2017 (strong oscillations at maxi-mum is now in nebular stage(mag V ~ 13)James Foster and Terry Bohlsen obtained new spec-tra in nebular phase.

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Nova Sct 2017 (V)

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10-12 Nova Sct 2017 2018-07-17 12:02:38 R = 1694 TBohlsen

GCVSName Date Mag A.D. (2000) DE (2000)

14 nova Oph 2018c PNV J17422408-2053088 2018-8 8.960 17 42 24.08 -20 53 08.813 nova Sct 2018 TCP J18292290-1430460 2018-6-29.577 10.3 18 29 22.93 -14 30 44.2 10.512 nova Lup 2018 PNV J15384000-4744500 2018-6-3.431 15 38 43.84 -47 44 41.1 911 nova Per 2018 V392 Per TCP J04432130+4721280 2018 -4-29.740 04 43 21.37 +47 21 25.8 6.310 nova Sgr 2018 PNV J18040967-1803581 2018-4-8.72 11.2 18 04 09.46 -18 03 55.7 10.89 nova CMa 2018 TCP J07134590-2112330 2018-3-24.496 12 07 13 45.84 -21 12 31.3 10.38 nova Car 2018 ASASSN-18fv 2018-3-20.32 <10.0 10 36 13.71 -59 35 55.1 5.97 nova Oph 2018b PNV J17140261-2849237 2018-3-10.805 17 14 2.53 -28 49 23.3 9.46 nova Sco 2018c ASSASN-18ds 2018-2-24.36 14.3 17 3 47.509 -38 16 57.14 9.85 nova Oph 2018 PNV J17244011-2421463 2018-2-12.834 12.5 17 24 40.11 -24 21 46.3 12.84 nova Sco 2018b PNV J16484962-4457032 2018-2-6.863 11.7 16 48 49.68 -44 57 2.9 10.13 nova Cir 2018 PNV J13532700-6725110 2018-1-19.708 9.1 13 53 27.59 -67 25 0.9 5.72 nova Sco 2018 PNV J17180658-3204279 2018-1-17.869 11 17 18 6.37 -32 4 27.7 10.21 nova Mus 2018 PNV J11261220-6531086 2018-1-14.486 11 26 15.16 -65 31 23.3 6.5

# Coordinates Mag MaxName Discovery

Spectrum taken by Terry Bohlsen, with [Fe VII] lines

Nova Sct 2017NOVAE

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2018-06-16.3902018-07-15.398

nova sct 2017 James R. Foster

Spectra obtained by James Foster with LISA R = 1000


Spectra obtained by James Foster witha LISA. Note the fast and strong changes in one month, noticely high excitation lines [Fe VII] which vanished.

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nova sct 2017 2018-07-15.398 2569 s (6 x 420 s) James R. Foster

[O II

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VII]

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VII]

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V] 5

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VII]

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] 575

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I 587

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VII]

6087

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636

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[Fe

X] 6

375

He

I 667

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He

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5.3

Nova Sct 2017NOVAE

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Nova Sct 2017 2018-06-16 09:21:07 R = 803 James R. Foster

Comparison of Feros(Tigre) spectrum obtained late september (courtesy of Steve Shore) and James' result mid-June: similar shape on the range 6280-6380.

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AAVSO lightcurve (V) James' spectra: blue dotsFeros(Tigre) : red dot


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nova sct 2017 2018-07-15.398 2569 s (6 x 420 s) James R. Foster

[O II

I] 43

63.2

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He

I 447

1.48

N II

I 463

4.2

C II

I 464

7H

e II

4685

.68

He

I 492

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[O II

I] 49

58.9

1[O

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5006

.84

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309

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] 575

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I 587

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6087

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636

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X] 6

375

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I 667

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He

I 706

5.3

Nova Lup 2018NOVAE

Coordinates (2000.0)R.A. 15 38 43.84Dec -47 44 41.1Mag V 10.0 (max)

Discovered on June 3th


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Nova Lup 2018 (V)

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Nova Lup 2018 2018-08-27 11:40:57 R = 5653 T Bohlsen

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Halpha 2018-08-27

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[OI]6300 2018-08-27

Nova Lup 2018NOVAE

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Nova Lup 2018

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2018-08-20


Low resolution spectra obtained by Paul Lucas and Terry Bohlsen

Nova Sct 2018 = TCP J18292290-1430460NOVAE

Coordinates (2000.0)R.A. 18 29 22.93Dec -14 30 44.2Mag V 10.3 (max)

First spectroscopic observations of TCP J18292290-1430460 (Nova Sct 2018): an optically thick classical novaATel #11802; Olivier Garde, Umberto Sollecchia (ARAS Group)on 1 Jul 2018; 02:10 UTWe report early low and echelle spectroscopy of the newly discovered transient TCP J18292290-1430460Â (AAVSO Alert 621695, discovered by Yukio Sakurai on 2018 Jun 29.577UT) The observations confirm this as a classical nova. Echelle spectra were obtained by Olivier Garde (Observatoire de la Tourbiere, France, RC400 Astrosib-Eshel-ATIK460EX2018)Jun Jun 30.861UT (R ~11000), covering 4250-7585, 10x1200 sec); the average S/N > 50 at 6000A. Low resolution grim spectra were obtained by Umberto Sollecchia (L'Aquila, Italy; Alpy600, R~ 500, 3769-7288A, 5x960 sec exposure time), centered at 2018 Jun 30.874UT. The overall appearance of the spectrum is of strong, overlapping absorption features with few prominent emission lines (aside from Hal-pha) and high interstellar extinction. However, there are some notable features that warrant reporting. P Cyg structure is present on Fe II 6456, 5169, 4923, 5018 (the usual), v_max = -800 km/s, nearly symmetric absorp-tion and emission in higher multiplets. Hbeta shows deep absorption but no emission, Halpha displays very strong emission (em/abs ~1) with an unsaturated (ejecta-like) absorption extending to -1700 km/s (similarly for the red wing). No He I lines are present in the spectrum at this stage. The optical Mg I triplet (5167,72,83) shows displaced absorption at the same velocity as Na I D1,D2, about -700 km/s, with the Na I D lines well separated even in the displaced components. There appears to be weak associated emission at Na I; the ISM absorption is at about +20 km/s (several components seem to be present, the lines are not completely satu-rated). Mg II is absent. The Si II 6347,71 doublet shows weak P Cyg, v_max=-800 km/s on both components. There are many overlapping absorption transitions, the spectrum is typical of a classical nova in the optically thick (Fe-curtain) stage. Overall, the reality of the individual features is confirmed with the low resolution Alpy600 spectrum taken almost simultaneously. Observations are continuing, all spectra are publicly available though the ARAS database http://www.astrosurf.com/aras/Aras_DataBase/Novae/2018_NovaSct2018.htm

Discovered on June, 29th. Identified as a nova by Umberto Sollecchia and Olivier Gardeon June, 30 th (See ATel#11802)The spectroscopic development is described p. 8 to 14 from ATels#11802, 11826, 11859 written by Steve Shore

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Nova Sct 2018 2018-06-30 20:58:02 R = 500 Umberto Sollecchia


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Nova Sct 2018 (V)

First spectrum obtained by Umberto Sollecchia with an ALPY600The overall appearance of the spectrum is of strong, overlapping absorption features with few prominent emission lines (aside from Halpha)

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Halpha 2018-06-30

Halpha displays very strong emission (em/abs ~1) with an unsaturated (ejecta-like) absorption extending to -1700 km/s

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Nova Sct 2018 2018-06-30.862 Olivier Garde

Na I D lines well separated even in the displaced components (velocity about -700 km/s). There appears to be weak associated emis-sion at Na I - the ISM absorption is at about +20 km/s (several components seem to be present, the lines are not completely saturated).

Nova Sct 2018 = TCP J18292290-1430460


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Fe II 5169 |2018-06-30

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Si 6347 |2018-06-30

The Si II 6347,71 doublet shows weak P Cyg, v_max=-800 km/s on both components.

P Cyg structure is present on Fe II 6456, 5169, 4923, 5018 (the usual), v_max = -800 km/s, nearly symmetric absorp-tion and emission in higher multiplets

Spectrum obtained on June, 30 by Olivier Garde with an eShel R = 11000


Continuing echelle spectroscopy of the classical nova TCP J18292290-1430460 = Nova Sct 2018ATel #11826; Olivier Garde (ASAS Group)on 8 Jul 2018; 18:21 UTWe report continuing echelle spectroscopy of the newly discovered classical nova TCP J18292290-1430460Â = Nova Sct 2018 (ATel #11802, #11817). Echelle spectra were obtained 2018 Jul 7.85 UT (HJD 58307.4238) at Ob-servatoire de la Tourbiere, France, RC400 Astrosib-Eshel-ATIK460EX2018 with a resolution of ~11000 covering 4250-7585, 10x1200 sec; the average S/N ~ 40 at 6000A. The Na I D lines show two absorption features, -1500 km/s and -820 km/s, with the higher velocity absorption stronger but approximately the same velocity width. There is still strong emission in the line extending to +2000 km/s. The Mg I triplet shows virtually the same profile as Na I but the overlap of the multiplet components changes the absorption widths; Na I 5686 may also be present. Fe II RMT 42 lines show two components of unequal absorption strength (4923, -1600 km/s, 3.1A; -800, 1.3A; 5018, 2.2A,1.4A; 5169, 2.5A, 1.5A:) with the velocity widths 600 km/s and 400 km/s, respectively. The emission wing is similarly extended to +200 km/s, and structure is beginning to appear (double peak) at low velocity (-350,+500 km/s). Si II 6347,6371 show almost identical absorption features as Fe II but neither line shows emission. Al II 6237 is possibly present, blended with Fe II 6248, with weaker absorption but with a similar velocity extent as Na I. The Balmer lines show the same structures as Fe II with a broader high veloc-ity absorption component. The same two peaks at low velocity are present on Halpha and Hbeta, although less visible on Halpha; the emission peak ratio is about 3.6; the spectra were normalized and uncorrected for interstellar extinction. Although not displaying any emission component, He I 5876, 6678 show a broad detached absorption feature at -1500 km/s (full width at continuum ~ 500 km/s). This has been observed in several novae at this early stage, notably V339 Del. This feature is a broad absorption to the blue of the Na I narrower features. Neither [O I] nor [N II] are visible. The dominant emission lines are still from singly ionized metals, few if any forbidden lines are present (e.g. [Fe II] 5159 is absent) and the nova appears to be in a later stage of the Fe-curtain with the recombination Several DIBSs are visible in this last spectrum, notably 5780A (EW ~ 0.63A), 5797A (0.33A), 6613A (0.32A). Observations are continuing, all spectra are publicly available though the ARAS database http://www.astrosurf.com/aras/Aras_DataBase/Novae/2018_NovaSct2018.htm

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Na I 5889.95 - Nova Sct 2018 2018-07-07.854 Olivier Garde

The Na I D lines show two absorp-tion features, -1500 km/s and -820 km/s, with the higher veloc-ity absorption stronger but approxi-mately the same velocity width. There is still strong emission in the line extending to +2000 km/s

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Na I D2 |2018-07-06

ARAS Eruptive Stars Information Letter 2018-03 - p. 10 ARAS Eruptive Stars Information Letter 2018-03 - p. 11

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Fe II 4924Fe II 5018Fe II 5169 |2018-07-06

Fe II 4924Fe II 5018Fe II 5169

Fe II RMT 42 lines show two compo-nents of unequal absorption strength (4923, -1600 km/s, 3.1A; -800, 1.3A; 5018, 2.2A,1.4A; 5169, 2.5A, 1.5A:) with the velocity widths 600 km/s and 400 km/s, respectively. The emission wing is similarly extended to +200 km/s, and structure is beginning to appear (double peak) at low velocity (-350,+500 km/s)



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Si II 6347Si II 6371 |2018-07-06

Si II 6347Si II 6371

Si II 6347,6371 show almost iden-tical absorption features as Fe II but neither line shows emission

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He I 5875 He I 6678 |2018-07-06

He I 5875He I 6678

Although not displaying any emission component, He I 5876, 6678 show a broad detached absorption feature at -1500 km/s (full width at continuum ~ 500 km/s). This has been observed in several novae at this early stage, notably V339 Del. This feature is a broad absorption to the blue of the Na I narrower features.

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H alpha H beta |2018-07-06

H alphaH beta

The Balmer lines show the same struc-tures as Fe II with a broader high veloc-ity absorption component. The same two peaks at low velocity are present on Halpha and Hbeta, although less visible on Hal-pha; the emission peak ratio is about 3.6

Continuing spectroscopic monitoring of Nova Sct 2018ATel #11859; Paolo Bernardi, David Boyd, Christian Buil, Stephane Charbonnel, Lorenzo Franco,Olivier Garde, Keith Graham, Massimiliano Mannucci, Nico Montigiani, Umberto Sollecchia, Peter Somogyi ARAS Groupon 16 Jul 2018; 02:05 UTWe report further spectroscopic observations of the classical nova Nova Sct 2018 = TCP J18292290-1430460 between 2018 Jun 30.8 UT and Jul 14.8 UT. Dispersions range from 600 (Alpy600 and low resolution instru-ments) to 12000 (eShel and LHIRES) between 3700 and 7900A. Signal to noise values range from ~20 to >80. The low resolution spectra displayed little overall change in the spectrum since the observations re-ported in (ATel #11802). The Balmer lines remain the dominant emission with absorption troughs (and red wings) extending to about -2300 km/s (minimum around -2000 km/s) and narrow absorption at around -900 km/s, the emission profiles were slightly stronger on the blue side. The Halpha to Hbeta emission ra-tio was about 5 on Jul 14.8. Echelle observations show that the Na I D broad emission appeared between Jul 6.8 and Jul. 7.8 (ATel #11826) and was still present on the Jul 14.8 echelle spectrum, the detached ab-sorption broad absorption features, discernible even at low resolution, are now at -1800 km/s and -1000 km/s but have weakened relative to Jul 7. He I 5876, 6678 show persistent detached absorption at -1800 km/s and no emission. Fe II 4923, 5018 (partly blended in absorption with He I), 5169 all show the same broad absorption components but these appear to be slightly shifted (-1700 km/s,-900 to -1000 km/s) and possibly fragmenting relative to the earlier report. The Fe II emission profiles are show increasingly strong double peaked structure (-460,+670 km/s) with red wings as extended as those of the Balmer and Na I D emission lines. The Si II 6347,6371 lines are now undetectable. No [O I] or forbidden Fe-peak lines have ap-peared, additional neutral C and O lines are detectable throughout this period (e.g. O I 7773) and the nova remains in the optically thick stage of the expansion, and with the exception of the rapid onset and per-sistence of the sodium emission, the nova closely resembles the early stages of the Fe-curtain. The details of the individual observations and the reduced spectra are publicly available at http://www.astrosurf.com/aras/Aras_DataBase/Novae/2018_NovaSct2018.htm and ARAS group observations are continuing. met-als, few if any forbidden lines are present (e.g. [Fe II] 5159 is absent) and the nova appears to be in a later stage of the Fe-curtain with the recombination Several DIBSs are visible in this last spectrum, notably 5780A (EW ~ 0.63A), 5797A (0.33A), 6613A (0.32A). Observations are continuing, all spectra are publicly available though the ARAS database http://www.astrosurf.com/aras/Aras_DataBase/Novae/2018_NovaSct2018.htm



The low resolution spectra displayed little overall change in the spectrum since the observations reported in (ATel #11802)

Spectra obtained by Chistian Buil (30-06, 12-07), James Foster (06-07, 09-07), Kevin Bazan (16-07) with LISA R = 1000

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Echelle observations show that the Na I D broad emission appeared between Jul 6.8 and Jul. 7.8 (ATel #11826) and was still present on the Jul 14.8 echelle spectrum, the detached absorption broad absorption features, dis-cernible even at low resolution, are now at -1800 km/s and -1000 km/s but have weakened relative to Jul 7

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Fe II 4924 Fe II 5018 Fe II 5169 |2018-07-09

Fe II 4924Fe II 5018Fe II 5169

Fe II 4923, 5018 (partly blended in absorp-tion with He I), 5169 all show the same broad absorption components but these appear to be slightly shifted (-1700 km/s,-900 to -1000 km/s) and possibly fragment-ing relative to the earlier report. The Fe II emission profiles are show increasingly strong double peaked structure (-460,+670 km/s) with red wings as extended as those of the Balmer and Na I D emission lines

Tim Lester DIY Echelle R = 130002018-07-09.113


-3000 -2000 -1000 0 1000 2000 3000velocity (km/s)

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He I 5875 He I 6678 |2018-07-09

He I 5875He I 6678

He I 5876, 6678 show persistent detached absorption at -1800 km/s and no emission.

-3000 -2000 -1000 0 1000 2000 3000Wavelenght (A))

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Nova Sct 2018 - H alpha

2018-07-01

2018-07-03

2018-07-04

2018-07-05

2018-07-06

2018-07-08

2018-07-09

2018-07-11

2018-07-13

2018-07-19

2018-07-24

2018-07-01

2018-07-03

2018-07-04

2018-07-05

2018-07-06

2018-07-08

2018-07-09

2018-07-11

2018-07-13

2018-07-19

2018-07-24


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152458290 2458320 2458350 2458380 2458410

Nova Sct 2018 (V)

Ha profile Spectra obtained by Umberto Sollecchia (DIY spectroscope R = 8000) and Paolo Berardi (Lhires III 1200 l/mm - R = 5000)

The Balmer lines remain the dominant emission with absorption troughs (and red wings) extending to about -2300 km/s (minimum around -2000 km/s) and nar-row absorption at around -900 km/s, the emission profiles were slightly stronger on the blue side. The Halpha to Hbeta emission ratio was about 5 on Jul 14.8.


Nova Oph 2018c = PNV J17422408-2053088NOVAE Coordinates (2000.0)

R.A. 17 42 24.10Dec -20 53 08.8Mag V 9.5 (max)

Discovered on June, 29th.

9

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132458320 2458350 2458380 2458410

Nova Oph 2018c (V)


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Nova Oph 2018c 2018-08-09 20:17:55 R = 600 Umberto Sollecchia

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Nova Oph 2018c 2018-08-10 20:45:12 R = 916 bazan,guegan

During the rise, Umberto Sollecchia, Kevin Bazan and Bertrand Guegan obtained low resolution spectra, respectively with ALPY R 600 and LISA R = 1000



Nova Oph 2018c = PNV J17422408-2053088NOVAE

0

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0.81

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Relative intensity

4000

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6800

Wav

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gth

(Ang

stro

m)

Nov

a O

ph 2

018c

20

18-0

8-10

.865

66

47 s

(10

x 60

0 s)

ba

zan,

gueg

anFe II 4178.862

Fe II 4233.113

Fe II 4385.387

Fe II 4553.252Fe II 4583.837Fe II 4629.339

Fe II 4923.927

Fe II 5018.44

Fe II 5169.033Fe II 5197.577Fe II 5234.625Fe II 5276.002Fe II 5316.784

Fe II 6147.741

Fe II 6247.557

Si II 6347.11Si II 6371.37

Fe II 6455.837

Nova Oph 2018c NOVAE

4000 4500 5000 5500 6000 6500 7000 7500Wavelenght (A))

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Nova Oph 2018c

2018-08-17

2018-08-21

2018-08-24

2018-08-28

2018-08-29

2018-08-30

2018-09-08

2018-09-09


Helium flash

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132458340 2458350 2458360 2458370 2458380

Nova Oph 2018c (V)

[N II

] l 5

755

He I

l 70

85

He I

l 58

75

He I

l 66

78

Evolution of the nova with low resolu-tion spectra obtained by Umberto Sollec-chia, Pierre Dubreuil, Lorenzo Frano, Ser-gio Moltomoli, F. Castalleni, V. Andreoli.Note the helium flash which can be precise-ly dated (2018-08-29) and the unexpected weakening of helium lines on 2018-09-08)

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Nova Oph 2018c - H alpha

2018-08-27

2018-08-29

2018-08-30

2018-09-05

2018-09-08

2018-09-11


Nova Oph 2018c = PNV J17422408-2053088NOVAE

H alpha profileUmberto SolleccchiaR = 8000

Symbiotics: Observing programSYMBIOTICS


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 outburst and orbital vari-ability

He II / HbRaman OVI

One spectrum a week until next outburst (Spring 2019)

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

One spectrum a week

V694 Mon A. LucyJ. Sokolovski

Detection of active phases Balmer and Fe II lines New season

New symbiotic HbHa1704-05 in outburst

Z And : declining outburst

AG Dra: 2018 outburst monitoring

CH Cygni: atypic behaviour : fast fading in July

V694 Mon : blue edge of Balmer lines detectedin emission by Peter Somogyi, unusual shape for this star

New faint symbiotics AS 210 & AS 245 obtained by J. Fos-ter

Symbioticsin July - September, 2018

The observing program of Jaroslav Merc and Rudolf Galis is extented to AG Peg and Z And During his talk (See Small Telescopes Conference in Slovakia, p. 109) Jaroslav emphasized the importance of the long-term monitoringof symbiotic stars, but also how important pro/am collaborations are. ARAS Group is a perfect example that such collaboration can be very successful and can bring important results.

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

Symbiotics in ARAS Data Base Update : 18-11-2018SYMBIOTICS


57 stars4051 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 45.7 117 12/08/2010 25/01/2019 82 AX Per 1 36 22.7 54 15 2.5 261 04/10/2011 18/01/2019 153 V471 Per 1 58 49.7 52 53 48.4 28 06/08/2013 10/11/2018 844 Omi Cet 2 19 20.7 -2 58 39.5 31 28/11/2015 14/01/2019 195 BD Cam 03 42 9.3 63 13 0.5 42 08/11/2011 25/01/2019 86 StHa 32 04 37 45.6 -01 19 11.8 5 02/03/2018 05/03/2018 3347 UV Aur 05 21 48.8 32 30 43.1 77 24/02/2011 15/01/2019 188 V1261 Ori 05 22 18.6 -8 39 58 16 22/10/2011 02/12/2018 629 StHA 55 05 46 42 6 43 48 7 17/01/2016 24/01/2019 9

10 SU Lyn 06 42 55.1 +55 28 27.2 129 02/05/2016 20/01/2019 1311 ZZ CMi 07 24 13.9 8 53 51.7 54 29/09/2011 13/04/2018 29512 BX Mon 07 25 24 -3 36 0 56 04/04/2011 22/01/2019 1113 V694 Mon 07 25 51.2 -7 44 8 270 03/03/2011 28/01/2019 514 NQ Gem 07 31 54.5 24 30 12.5 67 01/04/2013 03/01/2019 3015 GH Gem 07 4 4.9 12 2 12 7 10/03/2016 15/12/2017 41416 CQ Dra 12 30 06 69 12 04 27 11/06/2015 18/11/2018 7617 TX CVn 12 44 42 36 45 50.6 56 10/04/2011 09/07/2018 20818 RW Hya 13 34 18 - 25 22 48.9 18 28/06/2017 14/07/2018 20319 IV Vir 14 16 34.3 -21 45 50 10 28/02/2015 11/07/2018 20620 T CrB 15 59 30.1 25 55 12.6 269 01/04/2012 23/09/2018 13221 AG Dra 16 01 40.5 66 48 9.5 507 03/04/2013 12/12/2018 5222 AS 210 16 51 20.4 -26 00 26.7 2 14/06/2018 07/07/2018 21023 V503 Her 17 36 46 23 18 18 5 05/06/2013 15/05/2018 26324 RS Oph 17 50 13.2 -6 42 28.4 48 23/03/2011 20/07/2018 19725 V934 Her 17 06 34.5 +23 58 18.5 32 09/08/2013 31/08/2018 15526 RT Ser 17 39 52.0 -11 56 38.8 2 26/06/2012 13/07/2018 20427 AS 245 17 51 00.9 -22 19 35.1 1 15/07/2018 15/07/2018 20228 AS 270 18 05 33.7 -20 20 38 6 01/08/2013 07/07/2018 21029 AS 289 18 12 22.1 -11 40 07 3 26/06/2012 15/06/2018 23230 YY Her 18 14 34.3 20 59 20 27 25/05/2011 26/09/2018 12931 FG Ser 18 15 06.2 0 18 57.6 7 26/06/2012 22/06/2018 22532 StHa 149 18 18 55.9 27 26 12 6 05/08/2013 13/07/2018 20433 V443 Her 18 22 08.4 23 27 20 59 18/05/2011 11/12/2018 5334 FN Sgr 18 53 52.9 -18 59 42 9 10/08/2013 15/07/2018 20235 V919 Sgr 19 03 46 -16 59 53.9 7 10/08/2013 10/12/2018 5436 V1413 Aql 19 03 51.6 16 28 31.7 13 10/08/2013 10/12/2018 5437 V335 Vul 19 23 14 +24 27 39.7 11 14/08/2016 26/07/2018 19138 BF Cyg 19 23 53.4 29 40 25.1 154 01/05/2011 31/10/2018 9439 CH Cyg 19 24 33 50 14 29.1 724 21/04/2011 05/01/2019 2840 HM Sge 19 41 57.1 16 44 39.9 13 20/07/2013 23/09/2018 13241 QW Sge 19 45 49.6 18 36 50 11 14/08/2016 26/07/2018 19143 CI Cyg 19 50 11.8 35 41 3.2 206 25/08/2010 11/12/2018 5344 StHa 169 19 51 28.9 46 23 6 5 12/05/2016 08/07/2018 20945 EF Aql 19 51 51.7 -05 48 16.7 1 11/11/2018 11/11/2018 8346 TCPJ19544251+172228119 54 42.9 +17 22 12.7 59 09/08/2018 31/10/2018 9447 V1016 Cyg 19 57 4.9 39 49 33.9 18 15/04/2015 10/12/2018 5448 RR Tel 20 04 18.5 -55 43 33.2 3 08/09/2017 30/10/2017 46049 PU Vul 20 21 12 21 34 41.9 21 20/07/2013 10/11/2018 8450 LT Del 20 35 57.3 20 11 34 17 28/11/2015 28/09/2018 12751 ER Del 20 42 46.4 8 40 56.4 11 02/09/2011 20/10/2018 10552 V1329 Cyg 20 51 1.1 35 34 51.2 20 08/08/2015 09/01/2019 2453 V407 Cyg 21 2 13 45 46 30 12 14/03/2010 18/04/2010 054 StHa 190 21 41 44.8 2 43 54.4 22 31/08/2011 21/10/2018 10455 AG Peg 21 51 1.9 12 37 29.4 255 06/12/2009 11/12/2018 5356 V627 Cas 22 57 41.2 58 49 14.9 33 06/08/2013 08/01/2019 2557 Z And 23 33 39.5 48 49 5.4 154 30/10/2010 25/01/2019 858 R Aqr 23 43 49.4 -15 17 4.2 178 20/11/2010 13/12/2018 51

Symbiotic like59 SS Lep 06 04 59.1 -16 29 04.0 5 17/02/2018 22/01/2019 11

Symbiotics observed in July-September, 2018 1/3SYMBIOTICS


Id. Observer Date Res. Id. Observer Date Res.AG Dra P. Somogyi 26/05/2018 6459 7166 2711 BX Mon F. Campos 06/03/2018 3766 7297 791AG Dra P. Somogyi 26/05/2018 4528 5243 1945 CI Cyg P. Somogyi 10/06/2017 7748 8450 3044AG Dra J. Foster 13/06/2018 3821 7400 839 CI Cyg J. Foster 14/06/2018 3826 7396 853AG Dra J. Foster 15/06/2018 3825 7396 832 CI Cyg T. Lester 05/07/2018 4031 7948 14000AG Dra J. Guarro 03/07/2018 3980 7762 9000 CI Cyg F. Teyssier 06/07/2018 4287 7395 11000AG Dra C. Boussin 09/07/2018 3701 7571 501 CI Cyg J. Foster 07/07/2018 3885 7400 769AG Dra J. Foster 09/07/2018 3870 7395 846 CI Cyg L. Franco 07/07/2018 3841 7236 515AG Dra J. Guarro 12/07/2018 3980 7763 9000 CI Cyg F. Teyssier 14/07/2018 4287 7395 11000AG Dra J. Foster 14/07/2018 3865 7400 804 CI Cyg J. Guarro 26/07/2018 4173 7749 9000AG Dra D. Boyd 15/07/2018 3901 7380 971 CI Cyg D. Boyd 31/07/2018 3901 7381 1062AG Dra C. Boussin 16/07/2018 3701 7571 507 CI Cyg F. Teyssier 02/08/2018 4287 7395 11000AG Dra S. Charbonnel 17/07/2018 3920 7595 11000 CI Cyg C. Boussin 06/08/2018 3701 7571 511AG Dra K. Bazan 18/07/2018 4000 7001 904 CI Cyg C. Buil 10/08/2018 3500 5070 1264AG Dra M. Verlinden 26/07/2018 7999 8984 3813 CI Cyg K. Graham 11/08/2018 3673 7388 552AG Dra D. Boyd 01/08/2018 3901 7381 1026 CI Cyg C. Buil 11/08/2018 3396 4533 1201AG Dra F. Teyssier 04/08/2018 4290 7350 11000 CI Cyg J. Guarro 21/08/2018 3980 7763 9000AG Dra C. Boussin 06/08/2018 3701 7571 504 CI Cyg F. Teyssier 22/08/2018 4287 7160 11000AG Dra F. Teyssier 21/08/2018 4300 7150 11000 CI Cyg J. Foster 27/08/2018 6421 6694 8845AG Dra T. Lester 23/08/2018 4031 7950 14000 CI Cyg P. Dubreuil 31/08/2018 3700 7500 561AG Dra D. Boyd 31/08/2018 3901 7380 1070 CI Cyg J. Montier 01/09/2018 3789 7511 668AG Dra F. Sims 21/09/2018 3727 7275 1025 CI Cyg F. Campos 28/09/2018 3871 7411 694AG Dra D. Boyd 23/09/2018 3901 7380 1111 ensgr T. Bohlsen 17/09/2018 3800 7300 1878AG Dra F. Teyssier 28/09/2018 4287 7390 11000 ensgr F. Sims 18/09/2018 3707 7294 988AG Peg M. Verlinden 09/07/2018 7964 8947 3688 ER Del J. Foster 14/07/2018 3870 7396 731AG Peg T. Lester 11/07/2018 4031 7950 13000 FN Sgr J. Foster 13/06/2018 3912 7400 877AG Peg J. Foster 11/07/2018 3865 7400 738 FN Sgr J. Foster 15/07/2018 3870 7395 671AG Peg D. Boyd 14/07/2018 3902 7380 1091 gaiadr24048168377818693632T. Bohlsen 23/09/2018 3800 7360 1677AG Peg F. Teyssier 03/08/2018 4287 7395 11000 gaiadr25919388180059095292T. Bohlsen 29/09/2018 3900 7350 1862AG Peg K. Graham 20/08/2018 3629 7392 537 gaiadr26345873798283774848T. Bohlsen 18/09/2018 3800 7300 1648AG Peg T. Lester 23/08/2018 4031 7950 14000 HM Sge F. Campos 23/09/2018 3877 7417 599AG Peg J. Guarro 24/08/2018 4062 7756 9000 IV Vir J. Foster 13/06/2018 3912 7393 837AG Peg J. Guarro 25/08/2018 4053 7763 9000 IV Vir J. Foster 16/06/2018 3950 7390 845AG Peg J. Foster 31/08/2018 4716 5020 5962 IV Vir J. Foster 07/07/2018 3851 7400 776AG Peg J. Foster 31/08/2018 6424 6694 8769 IV Vir J. Foster 11/07/2018 3903 7396 787AG Peg D. Boyd 01/09/2018 3901 7380 1011 LT Del J. Foster 15/06/2018 3805 7390 835AG Peg G. Martineau 06/09/2018 3704 7400 1170 LT Del J. Foster 11/07/2018 3980 7397 863AG Peg J. Guarro 14/09/2018 4249 7749 9000 LT Del F. Campos 28/09/2018 3875 7410 674AG Peg J. Guarro 25/09/2018 3980 7763 9000 PU Vul J. Foster 15/06/2018 3805 7390 832AG Peg J. Guarro 01/10/2018 4059 7753 9000 PU Vul J. Foster 13/07/2018 3886 7400 641AS 270 J. Foster 12/06/2018 3915 7395 861 PU Vul K. Graham 13/08/2018 3692 7388 552AS 270 J. Foster 07/07/2018 3851 7400 828 R Aqr M. Verlinden 12/08/2018 3551 7901 589as210 J. Foster 14/06/2018 3912 7400 833 R Aqr J. Guarro 27/09/2018 4092 7756 9000as210 J. Foster 07/07/2018 3851 7400 908 RS Oph J. Foster 13/06/2018 3926 7396 853as245 J. Foster 15/07/2018 3901 7399 769 RS Oph J. Foster 15/06/2018 3925 7396 850as289 J. Foster 15/06/2018 3925 7392 836 RS Oph J. Foster 08/07/2018 3886 7400 850asassn-vj192916.53-2240403F. Sims 21/09/2018 3727 7275 1023 RS Oph T. Lester 20/07/2018 4031 7950 12000AXPer D. Boyd 12/07/2018 3901 7381 1098 RT Ser J. Foster 13/07/2018 3890 7396 785AXPer D. Boyd 23/07/2018 3902 7380 998 RW Hya J. Foster 12/06/2018 3920 7395 907AXPer D. Boyd 21/08/2018 3901 7380 1013 RW Hya J. Foster 13/06/2018 3926 7396 864AXPer D. Boyd 17/09/2018 3901 7380 1089 RW Hya J. Foster 08/07/2018 3925 7395 756AXPer G. Martineau 26/09/2018 3700 7400 1139 RW Hya J. Foster 14/07/2018 3870 7396 730BD Cam V. Marik 30/06/2018 3674 7362 674 StHa 149 J. Foster 15/06/2018 3805 7390 828BF Cyg P. Somogyi 11/06/2017 7748 8450 2950 StHa 149 J. Foster 13/07/2018 3865 7400 773BF Cyg P. Somogyi 11/06/2017 8403 9100 2308 StHa 169 J. Foster 08/07/2018 3865 7400 800BF Cyg J. Foster 13/06/2018 3916 7396 863 StHa 190 J. Foster 11/07/2018 3870 7391 754BF Cyg T. Lester 20/06/2018 4031 7948 13000 StHa 190 C. Boussin 12/08/2018 3701 7571 512BF Cyg T. Lester 04/07/2018 4031 7948 13000 stHa 32 F. Campos 05/03/2018 3764 7300 860BF Cyg L. Franco 07/07/2018 3841 7236 530 T CrB J. Foster 12/06/2018 3920 7395 917BF Cyg J. Foster 08/07/2018 3900 7395 889 T CrB J. Foster 08/07/2018 3865 7400 817BF Cyg C. Boussin 09/08/2018 3701 7571 501 T CrB D. Boyd 12/07/2018 3901 7380 1046BF Cyg K. Graham 10/08/2018 3603 7404 561 T CrB F. Teyssier 05/08/2018 4290 7350 11000BF Cyg L. Franco 29/08/2018 3841 7237 524 T CrB J. Foster 27/08/2018 6421 6694 8972BF Cyg F. Campos 23/09/2018 3877 7417 660 T CrB J. Montier 31/08/2018 3874 7356 654BF Cyg K. Graham 24/09/2018 3731 7324 543 T CrB J. Foster 19/09/2018 6430 6694 7261BF Cyg J. Guarro 02/10/2018 3980 7763 9000 T CrB F. Campos 23/09/2018 3874 7420 671

Range Range

SYMBIOTICS


Symbiotics observed in July-September, 2018 2/3

Id. Observer Date Res. Id. Observer Date Res.TX CVn J. Foster 11/06/2018 3821 7395 907 tcpj19544251+1722281 C. Buil 10/08/2018 3499 5069 1136TX CVn J. Foster 13/06/2018 3822 7395 851 tcpj19544251+1722281 O. Garde 10/08/2018 4200 7586 11000TX CVn J. Foster 09/07/2018 3890 7395 798 tcpj19544251+1722281 P. Berardi 09/08/2018 4361 7392 0V1016 Cyg T. Lester 18/07/2018 4031 7950 14000 tcpj19544251+1722281 U. Sollecchia 10/08/2018 3749 7373 1615V1329 Cyg D. Boyd 29/08/2018 3901 7380 1110 tcpj19544251+1722281 bazan,guegan 10/08/2018 4000 7000 860V1413 Aql J. Foster 15/06/2018 3805 7390 852 tcpj19544251+1722281 P. Berardi 10/08/2018 6490 6633 17124V1413 Aql T. Lester 12/07/2018 4031 7949 12000 tcpj19544251+1722281 O. Garde 11/08/2018 4200 7586 11000V1413 Aql J. Foster 13/07/2018 3886 7400 767 tcpj19544251+1722281 P. Berardi 11/08/2018 4475 5484 1851V1413 Aql F. Campos 23/09/2018 3871 7416 700 tcpj19544251+1722281 P. Somogyi 11/08/2018 6012 6134 13021V335 Vul T. Rodda 26/07/2018 3901 7381 615 tcpj19544251+1722281 C. Boussin 11/08/2018 3701 7571 502V443 Her K. Graham 17/08/2017 3667 7404 514 tcpj19544251+1722281 P. Somogyi 11/08/2018 4559 4708 8420V443 Her J. Foster 09/06/2018 3826 7395 897 tcpj19544251+1722281 C. Buil 11/08/2018 3392 4570 1289V443 Her J. Foster 14/06/2018 3826 7390 899 tcpj19544251+1722281 P. Somogyi 11/08/2018 4847 4991 9398V443 Her J. Foster 15/07/2018 3891 7395 806 tcpj19544251+1722281 P. Somogyi 12/08/2018 4964 5106 9420V443 Her K. Graham 10/08/2018 3732 7372 546 tcpj19544251+1722281 K. Graham 12/08/2018 3603 7404 572V443 Her J. Foster 28/08/2018 6421 6694 8973 tcpj19544251+1722281 P. Somogyi 12/08/2018 4570 4718 8352V443 Her J. Foster 30/08/2018 3773 4085 3224 tcpj19544251+1722281 P. Berardi 13/08/2018 4465 5497 2084V443 Her J. Foster 31/08/2018 4716 5019 5975 tcpj19544251+1722281 C. Boussin 13/08/2018 3701 7571 504V443 Her F. Campos 26/09/2018 3861 7416 740 tcpj19544251+1722281 O. Garde 15/08/2018 4200 7586 11000V627 Cas D. Boyd 29/08/2018 3901 7380 1111 tcpj19544251+1722281 C. Boussin 15/08/2018 3701 7571 505V694 Mon P. Somogyi 09/09/2018 4563 5278 1952 tcpj19544251+1722281 D. Boyd 16/08/2018 3900 7380 1070V694 Mon P. Somogyi 30/09/2018 4596 5311 1953 tcpj19544251+1722281 T. Lester 17/08/2018 4031 7950 12000V919 Sgr J. Foster 14/06/2018 3912 7400 782 tcpj19544251+1722281 P. Somogyi 17/08/2018 4571 4720 8623V919 Sgr J. Foster 13/07/2018 3906 7396 829 tcpj19544251+1722281 P. Somogyi 18/08/2018 4573 4721 8125V934 Her K. Graham 07/08/2018 3709 7391 540 tcpj19544251+1722281 C. Boussin 18/08/2018 3701 7571 509V934 Her J. Montier 31/08/2018 3947 7226 652 tcpj19544251+1722281 P. Somogyi 18/08/2018 4960 5102 9376YY Her J. Foster 13/06/2018 3822 7396 835 tcpj19544251+1722281 P. Somogyi 19/08/2018 4577 4725 8390YY Her F. Campos 26/09/2018 3861 7416 742 tcpj19544251+1722281 T. Lester 20/08/2018 4031 7950 12000Z And C. Boussin 17/07/2018 3701 7571 507 tcpj19544251+1722281 K. Graham 20/08/2018 3705 7372 560Z And F. Teyssier 02/08/2018 4287 7395 11000 tcpj19544251+1722281 P. Somogyi 20/08/2018 4575 4723 6882Z And D. Boyd 03/08/2018 3901 7380 978 tcpj19544251+1722281 P. Somogyi 20/08/2018 4805 4950 9057Z And J. Guarro 04/08/2018 4768 7759 9000 tcpj19544251+1722281 C. Boussin 25/08/2018 3701 7571 523Z And P. Somogyi 05/08/2018 3824 3981 5845 tcpj19544251+1722281 P. Berardi 28/08/2018 4476 5499 2095Z And C. Boussin 07/08/2018 3701 7571 501 tcpj19544251+1722281 L. Franco 28/08/2018 3831 7237 530Z And C. Buil 11/08/2018 3498 5070 1138 tcpj19544251+1722281 U. Sollecchia 28/08/2018 6378 6777 7167Z And T. Lester 23/08/2018 4031 7950 14000 tcpj19544251+1722281 C. Boussin 01/09/2018 3701 7571 507Z And J. Guarro 26/08/2018 4053 7763 9000 tcpj19544251+1722281 F. Sims 07/09/2018 3707 7294 1023Z And C. Buil 27/08/2018 3320 5221 639 tcpj19544251+1722281 C. Boussin 07/09/2018 3701 7571 506Z And D. Boyd 01/09/2018 3901 7380 1060 tcpj19544251+1722281 P. Somogyi 08/09/2018 6012 6134 12381Z And F. Sims 04/09/2018 3712 7299 1000 tcpj19544251+1722281 U. Sollecchia 10/09/2018 6378 6775 8022Z And F. Sims 06/09/2018 3707 7295 1029 tcpj19544251+1722281 C. Boussin 11/09/2018 3701 7571 504Z And F. Sims 07/09/2018 3707 7295 1024 tcpj19544251+1722281 P. Somogyi 12/09/2018 6493 7199 2691Z And P. Somogyi 09/09/2018 6500 6609 15556 tcpj19544251+1722281 C. Boussin 15/09/2018 3701 7571 505Z And J. Guarro 14/09/2018 4053 7763 9000 tcpj19544251+1722281 P. Somogyi 16/09/2018 6472 7176 2718Z And F. Teyssier 17/09/2018 4287 7156 11000 tcpj19544251+1722281 C. Buil 19/09/2018 3359 5802 600Z And F. Sims 18/09/2018 3708 7295 1022 tcpj19544251+1722281 C. Buil 22/09/2018 5801 8786 1353Z And C. Buil 19/09/2018 3298 5788 600 tcpj19544251+1722281 C. Boussin 25/09/2018 3701 7571 509Z And J. Guarro 20/09/2018 4053 7763 9000 tcpj19544251+1722281 D. Boyd 26/09/2018 3901 7380 966Z And C. Buil 22/09/2018 5801 8786 1278 tcpj19544251+1722281 C. Boussin 28/09/2018 3701 7571 507Z And J. Guarro 26/09/2018 3980 7763 9000 tcpj19544251+1722281 P. Somogyi 29/09/2018 5497 6210 2220Z And J. Guarro 28/09/2018 3980 7763 9000 tcpj19544251+1722281 P. Somogyi 30/09/2018 6478 7181 2655Z And J. Foster 30/09/2018 3777 4092 3665Z And J. Foster 01/10/2018 6426 6699 9153

Range Range

Symbiotics observed in July-September, 2018 3/3SYMBIOTICS

Id. Observer Date Res. Id. Observer Date Res.CH Cyg P. Somogyi 27/05/2017 3861 4015 5451 CH Cyg J. Guarro 26/07/2018 3980 7763 9000CH Cyg P. Somogyi 10/06/2017 7748 8449 3050 CH Cyg K. Graham 27/07/2018 3801 7399 547CH Cyg K. Graham 02/08/2017 3604 7405 539 CH Cyg J. Guarro 28/07/2018 3980 7763 9000CH Cyg P. Somogyi 26/05/2018 6501 6611 15846 CH Cyg J. Guarro 30/07/2018 3980 7763 9000CH Cyg P. Somogyi 26/05/2018 3858 4014 5271 CH Cyg F. Teyssier 31/07/2018 4287 7395 11000CH Cyg M. Verlinden 27/06/2018 7912 8899 3628 CH Cyg J. Guarro 31/07/2018 3980 7763 9000CH Cyg P. Somogyi 30/06/2018 6504 6614 15816 CH Cyg M. Verlinden 01/08/2018 7988 8970 3671CH Cyg M. Verlinden 30/06/2018 7952 8940 3726 CH Cyg J. Guarro 01/08/2018 3980 7763 9000CH Cyg P. Somogyi 30/06/2018 3817 3974 5432 CH Cyg G. Martineau 01/08/2018 3704 7400 1174CH Cyg V. Marik 30/06/2018 3635 7371 11000 CH Cyg J. Guarro 02/08/2018 3980 7763 9000CH Cyg J. Guarro 02/07/2018 3980 7762 9000 CH Cyg V. Marik 02/08/2018 3653 7393 3671CH Cyg J. Guarro 03/07/2018 3980 7762 9000 CH Cyg F. Teyssier 03/08/2018 4287 7395 11000CH Cyg P. Cazzato 04/07/2018 3701 7200 546 CH Cyg P. Somogyi 04/08/2018 3822 3979 5581CH Cyg H. Boussier 05/07/2018 3896 7468 618 CH Cyg J. Guarro 10/08/2018 4053 7762 9000CH Cyg J. Guarro 05/07/2018 3980 7762 9000 CH Cyg J. Guarro 11/08/2018 4053 7763 9000CH Cyg P. Cazzato 06/07/2018 3702 7201 542 CH Cyg J. Guarro 13/08/2018 4053 7763 9000CH Cyg J. Foster 06/07/2018 3887 7396 847 CH Cyg J. Guarro 14/08/2018 4053 7763 9000CH Cyg F. Teyssier 06/07/2018 4287 7395 11000 CH Cyg J. Guarro 15/08/2018 4053 7763 9000CH Cyg L. Franco 06/07/2018 3841 7236 531 CH Cyg F. Teyssier 18/08/2018 4287 7160 11000CH Cyg O. Garde 06/07/2018 4000 7586 11000 CH Cyg J. Guarro 18/08/2018 4053 7763 9000CH Cyg F. Teyssier 07/07/2018 4287 7395 11000 CH Cyg J. Guarro 19/08/2018 4053 7763 9000CH Cyg P. Somogyi 07/07/2018 3819 3976 4943 CH Cyg T. Lester 20/08/2018 4031 7950 14000CH Cyg J. Guarro 08/07/2018 3980 7762 9000 CH Cyg J. Guarro 20/08/2018 4053 7763 9000CH Cyg C. Boussin 09/07/2018 3701 7571 503 CH Cyg J. Guarro 21/08/2018 4053 7763 9000CH Cyg P. Cazzato 09/07/2018 3703 7200 523 CH Cyg J. Guarro 24/08/2018 4053 7763 9000CH Cyg J. Guarro 10/07/2018 3980 7762 9000 CH Cyg J. Guarro 25/08/2018 4053 7763 9000CH Cyg T. Lester 11/07/2018 4031 7950 13000 CH Cyg J. Foster 26/08/2018 6421 6694 8644CH Cyg F. Teyssier 11/07/2018 4287 7395 11000 CH Cyg J. Guarro 26/08/2018 4053 7763 9000CH Cyg J. Guarro 12/07/2018 3980 7762 9000 CH Cyg J. Guarro 27/08/2018 4053 7763 9000CH Cyg P. Somogyi 13/07/2018 3821 3978 5366 CH Cyg F. Sims 29/08/2018 3713 7300 948CH Cyg J. Guarro 14/07/2018 3980 7761 9000 CH Cyg L. Franco 29/08/2018 3841 7237 532CH Cyg F. Teyssier 14/07/2018 4287 7395 11000 CH Cyg F. Sims 30/08/2018 3713 7300 924CH Cyg P. Somogyi 14/07/2018 3818 3975 5154 CH Cyg J. Montier 01/09/2018 3753 7193 656CH Cyg P. Somogyi 15/07/2018 3818 3975 5382 CH Cyg F. Sims 04/09/2018 3711 7300 999CH Cyg J. Guarro 15/07/2018 3980 7762 9000 CH Cyg P. Somogyi 08/09/2018 3821 3978 5161CH Cyg J. Guarro 16/07/2018 3980 7499 9000 CH Cyg J. Guarro 13/09/2018 3980 7763 9000CH Cyg S. Charbonnel 17/07/2018 3919 7595 11000 CH Cyg J. Guarro 14/09/2018 3980 7763 9000CH Cyg K. Bazan 17/07/2018 3801 7383 937 CH Cyg P. Somogyi 15/09/2018 3826 3983 5039CH Cyg J. Guarro 17/07/2018 3980 7499 9000 CH Cyg J. Guarro 17/09/2018 3980 7763 9000CH Cyg F. Teyssier 18/07/2018 4287 7395 11000 CH Cyg F. Teyssier 18/09/2018 4370 7156 11000CH Cyg P. Cazzato 19/07/2018 3703 7200 525 CH Cyg J. Guarro 19/09/2018 3980 7762 9000CH Cyg T. Lester 19/07/2018 4031 7950 14000 CH Cyg J. Guarro 20/09/2018 3980 7763 9000CH Cyg J. Guarro 19/07/2018 3980 7499 9000 CH Cyg K. Graham 23/09/2018 3604 7404 563CH Cyg P. Somogyi 20/07/2018 3820 3977 5334 CH Cyg J. Guarro 23/09/2018 4053 7763 9000CH Cyg J. Guarro 22/07/2018 3980 7763 9000 CH Cyg J. Guarro 25/09/2018 3980 7763 9000CH Cyg J. Guarro 23/07/2018 3980 7763 9000 CH Cyg J. Guarro 26/09/2018 3980 7763 9000CH Cyg F. Teyssier 25/07/2018 4287 7395 11000 CH Cyg J. Guarro 27/09/2018 3980 7763 9000CH Cyg J. Guarro 25/07/2018 3980 7763 9000 CH Cyg J. Guarro 28/09/2018 3980 7763 9000

CH Cyg P. Somogyi 28/09/2018 3824 3981 5217CH Cyg F. Teyssier 28/09/2018 4287 7390 11000CH Cyg P. Somogyi 29/09/2018 3827 3983 5216CH Cyg J. Guarro 29/09/2018 4053 7763 9000CH Cyg O. Garde 29/09/2018 4100 7587 11000CH Cyg J. Foster 30/09/2018 6430 6699 9152CH Cyg P. Somogyi 30/09/2018 3826 3983 4882CH Cyg J. Guarro 30/09/2018 4053 7763 9000

Range Range


AG Dra 2018 Outburst

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. GàlisAfter the burst of AG Dra has returned to quiescent state. Ongoing survey until the next outburst expected during Spring 2019


0

0.2

0.4

0.6

0.8

1

1.2

1.4

1.6

1.89

9.5

102457390 2457480 2457570 2457660 2457750 2457840 2457930 2458020 2458110 2458200 2458290 2458380 2458470 2458560

AG Dra (V)

2016, May 2018, May2017, May

9

9.5

102458100 2458190 2458280 2458370 2458460

AG Dra (V)

4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

2

4

6

8

10

12

rela

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nsity

AG Dra 2018-07-18 00:17:02 R = 904 Kevin Bazan

AG Dra in July - Kevin Bazan - LISA R = 1000

AG DraSYMBIOTICS


0

2E-12

4E-12

6E-12

8E-12

1E-11

Flux

(erg

/cm

2/se

c/A)


2018-07-15.9172018-08-01.9132018-08-31.9032018-09-23.850

AG Dra D. Boyd

0

5E-13

1E-12

1.5E-12

2E-12

Flux

(erg

/cm

2/se

c/A)


2018-07-15.9172018-08-01.9132018-08-31.9032018-09-23.850

AG Dra D. Boyd

A series of flux calibrated spectra obtained by David Boyd with LISA R = 1000

4000 4500 5000 5500 6000 6500 7000Wavelength (A))

0

5

10

15

20

25

30

35

rela

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AG Dra - LISA R = 1000

2018-07-09

2018-07-15

2018-07-18

2018-08-01

2018-08-31

2018-09-21

2018-10-03

2018-10-18


AG DraSYMBIOTICS

Spectra obtained by James Foster, David Boyd, Kevin Bazan, Woody Sims (LISA R = 1000), Fran Campos (DADOS-200)

AG Dra 2018SYMBIOTICS


-1000 -500 0 500 1000Radial velocity [km/s]

0

10

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30

40

50

60

70

rela

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nsity

TCPJ19544251+1722281 H alpha

2018-07-03

2018-07-12

2018-08-04

2018-08-21

2018-08-23

2018-10-12


0

10

20

30

40

50

60

rela

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TCPJ19544251+1722281 H beta

2018-07-03

2018-07-12

2018-08-04

2018-08-21

2018-08-23

2018-10-12


0

2

4

6

8

10

12

14

rela

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TCPJ19544251+1722281 He I 5875

2018-07-03

2018-07-12

2018-08-04

2018-08-21

2018-08-23

2018-10-12


0

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8

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12

rela

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TCPJ19544251+1722281 He I 6678

2018-07-03

2018-07-12

2018-08-04

2018-08-21

2018-08-23

2018-10-12


0

10

20

30

40

50

60

70

rela

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TCPJ19544251+1722281 He II 4686

2018-07-03

2018-07-12

2018-08-04

2018-08-21

2018-08-23

2018-10-12

6800 6820 6840 6860Wavelength (A))

0

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5

6

7

rela

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AG Dra Raman OVI 6830

2018-07-03

2018-07-12

2018-08-04

2018-08-21

2018-08-23

2018-10-12

Profiles of selected lines from echelle spectra obtained by Joan Guarro, Tim Lester, François Teyssier

AG Dra 2018 Equivalent width in 2018SYMBIOTICS


8150 8200 8250 8300 8350JD - 2450000

0

20

40

60

80

100

120AG Dra - EW H alpha

8150 8200 8250 8300 8350JD - 2450000

0

10

20

30

40

50AG Dra - EW H beta

8150 8200 8250 8300 8350JD - 2450000

0

2

4

6AG Dra - EW He I 5876

8150 8200 8250 8300 8350JD - 2450000

0

2

4

6AG Dra - EW He I 6678

8150 8200 8250 8300 8350JD - 2450000

0

10

20

30

40

50AG Dra - EW He II 4686

8150 8200 8250 8300 8350JD - 2450000

0

2

4

6

8

10

12

14AG Dra - EW Raman OVI 6830

Echelle spectra obtained by Joan Guarro, Tim Lester, François Teyssier, Christian Buil, Olivier Garde


AG DraSYMBIOTICS

8200 8400 8600 8800Wavelength (A)

0

0.5

1

1.5

rela

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AG Dra 2018-07-26 01:35:23 R = 3813 Michel VERLINDEN

OI l 8446 in emission - Ca II ll9498, 8542, 8662 triplet in absorption

AS 210 = V1196 ScoSYMBIOTICS


Coordinates (2000.0)R.A. 16 51 20.41Dec -26 00 26.7Mag ~ 12 (?)

AS 2010 is D-type symbiotic contained a carbon mira (C3). The mean luminosity is 12.9 with DV = 2.0 .Pulsation of the Mira was detected in ASAS and SAAO programs with periods of 407 (14) and 423 (7) days. Ephemeris: Max(IR) = 2446162 + 423 * E(Gromazdi & al, 2009). James Foster obtained a spectrum with LISA (R = 1000) at Mount Pinos Observatory. The emission spec-trum show high ionized lines He II 4541, 4686, 5411, [Fe VII] 5721, 6087 and Raman OVI 6830. The high ratio [OIII] 4363/5007 suggest a high electronic density. An excellent target for low resolution spectrographs (monitoring of a pulsation)

4500 5000 5500 6000 6500 7000Wavelength (A)

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AS 210 2018-07-07 06:28:51 R = 908 James R. Foster

4500 5000 5500 6000 6500 7000Wavelength (A)

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14

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AS 245 SYMBIOTICS

Coordinates (2000.0)R.A. 17 51 00.9Dec -22 19 35.0Mag

4000 4500 5000 5500 6000 6500 7000Wavelength (A)

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Light curve of AS210 in Grmadzski & al. 2009)https://arxiv.org/pdf/0906.4136.pdf

Ephemeris: Max(JHKL) = 2446162+423×E


4000 4500 5000 5500 6000 6500 7000Wavelength (A)

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SYMBIOTICS

AS 270 = V5759 Sgr = Hen 3-1581

Coordinates (2000.0)R.A. 18 05 33.7Dec -20 20 38.1Mag 14 (2018-07)

6600 6800 7000 7200 7400 7600 7800 8000 8200JD - 2450000

11

12

13

14

15

Mag

V

AS270 AAVSO V lightcurve since 2014

SYMBIOTICS

AS 289 = V343 Ser = Hen 3-1627


4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

2

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8

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0

1

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3

4

5

6

Rel

ativ

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2013-08-10.878 cbuil2018-06-15.342 James R. Foster

AS289


Comparison with a spectrum obtained by Christian Buil in 2013: AS289 is clearly in outburst (vanish-ing of [fe VII] lines

BD Cam

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

SYMBIOTICS

4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

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1

1.5

rela

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BD Cam 2018-06-30 23:27:24 R = 674 V Marik


BF Cyg

Coordinates (2000.0)R.A. 19 23 53.5Dec +29 40 29.17Mag 9.9 (2018-06)

SYMBIOTICS


9

9.5

10

10.5

112457000 2457200 2457400 2457600 2457800 2458000 2458200 2458400 2458600

BF Cygni (V)

4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

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8

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BF Cyg 2018-08-10 03:52:19 R = 561 K Graham


BF CygSYMBIOTICS

9

9.5

10

10.5

112458200 2458300 2458400

BF Cygni (V)

Echelle spectraTim Lester and Joan Guarro


0

10

20

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40

50

60

arbi

trar

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it

BF Cyg H alpha

2018-05-08

2018-06-20

2018-06-26

2018-07-04

2018-10-02


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5

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arbi

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it

BF Cyg H beta

2018-05-08

2018-06-20

2018-06-26

2018-07-04

2018-10-02

4050 4150 4250 4350 4450 4550 4650Wavelength (A)

0

1

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4

rela

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BF Cyg 2018-07-04 02:51:20 R = 13000 T Lester

5000 5100 5200 5300 5400 5500Wavelength (A)

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3

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BF Cyg 2018-07-04 02:51:20 R = 13000 T Lester

6000 6100 6200 6300 6400 6500Wavelength (A)

0.5

1

1.5

2

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BF Cyg 2018-07-04 02:51:20 R = 13000 T Lester


BF CygSYMBIOTICS

SYMBIOTICS

BF Cyg

0

1

2

3

4

5

6

7

8

Arbi

trary

uni

ts

4000 4500 5000 5500 6000 6500 7000

Wavelength (Angstrom)

BF Cyg

2018-09-24.034

2018-09-23.858

2018-08-10.161

2018-08-09.960

Low resolution spectra obtained by James Foster (LISA R = 1000)CBO, F. Campos, Keith Graham (ALPy R = 600)

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)

AAVSO V and B lightcurve (1 day mean)CH Cygni reached a maximum at V mag ~ 6.5 in April-May, declined slightly until June 21th and dropped dramatically from V = 6.7 to 7.6 in only 6 days. It recovers late July at mag V 6.5 before decling again. (ongoing)


4000 4500 5000 5500 6000 6500 7000Wavelength (A)

0

0.5

1

1.5

2

rela

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CH Cyg 2018-07-05 20:53:15 R = 618 H. Boussier

6

7

8

92457000 2457180 2457360 2457540 2457720 2457900 2458080 2458260 2458440 2458620

CH Cygni (V)

7

7.5

8

8.5

9

9.5

10

10.56

6.5

7

7.5

8

8.5

92457600 2457965 2458330

CH Cygni (V)

AAVSO V lightcurve and ARAS spectra since 2015Between June and November 2018, CH Cyg is monitored with 88 spectra

CH CygSYMBIOTICS


2458264.8126.4135

2458291.1026.6765

2458297.5647.574

2 458 307.1427.545

2458339.0036.373

6

6.5

7

7.5

82458250 2458300 2458350

CH Cygni (V)

0

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0.6

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1.2

1.4

1.6

1.8

2

Rel

ativ

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tens

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-1000 -500 500 1000

Velocity (Km/sec)

2018-06-02.9552018-06-20.1432018-06-25.8612018-06-30.9032018-07-08.908

Hbeta 4861.363 - CH Cyg

0.4

0.6

0.8

1

1.2

1.4

1.6

1.8

Rel

ativ

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tens

ity

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

2018-06-02.9552018-06-20.1432018-06-25.8612018-06-30.9032018-07-08.908

[O I] 6300.32 - CH Cyg

The fast fading in July with Echelle spectra obtained by Tim Lester, Joan Guarro, François Teyssier

Note the inceasing of [OIII] relative to the con-tinuum

0

0.1

0.2

0.3

0.4

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0.7

0.8

0.9

Rel

ativ

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tens

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2018-06-02.9552018-06-20.1432018-06-25.8612018-06-30.9032018-07-08.908

CH Cyg

0

0.2

0.4

0.6

0.8

1

1.2

1.4

Rel

ativ

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tens

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4990 4995 5000 5005 5010 5015 5020 5025 5030Wavelength (Angstrom)

2018-06-02.9552018-06-20.1432018-06-25.8612018-06-30.9032018-07-08.908

CH Cyg


CH CygSYMBIOTICS


CH Cyg Near UVSYMBIOTICS

6

6.5

7

7.5

82458250 2458300 2458350 2458400 2458450

CH Cygni (V)

3800 3820 3840 3860 3880 3900 3920 3940 3960 3980Wavelength (A))

0

5

10

15

20

rela

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CH Cyg P. Somogyi

2018-07-07

2018-07-13

2018-07-14

2018-07-15

2018-07-20

2018-08-04

2018-09-08

2018-09-15

2018-09-28

2018-09-29

2018-09-30 [Ne

[III]

3868

.7

H8 3

889.

0

H9 3

885.

4

*

*

* *A series of near UV spectra ob-tained by Peter Somogyi with Lhires III 2400 l/mm (R ~ 5000)On July 7th and September 15th, Balmer H8 and H9 lines are in emission with very faint absorption while [Ne III] 3869 is strong. The first event (07-07) coincides to the mini-mum of V luminosity while the second one occurs during the decline.The spectra for these two dates are very similar.

3820 3840 3860 3880 3900 3920 3940 3960 3980Wavelength (A)

0

1

2

3

4

Arb

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CH Cyg P. Somogyi

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2018-09-15.8212018-09-28.829

[Ne

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CH Cyg Near UVSYMBIOTICS


CH Cyg Hb - 2018 June to November


Next pages: lines profiles from 70 Echelle spectra obtained between June and November by Joan Guarro, Francois Teysseir, Tim Lester, Stephane Charbonnel, Olivier Garde

CH Cyg Ha - 2018 June to November


CH Cyg [OIII] 5007 - 2018 June to November


We note a strong incease of [OIII] on september 14th with good correlation with the detection of [Ne III] in emis-sion in near UV spectra. But noting special for the 7th of July.

CH Cyg [OI] 6300 - 2018 June to November


[OI] line is perhaps the only "constant" in CH Cygni spectrum with a genral shape composed of a narrow line (FWHM ~32 km.s-1) on a broad triangular component (1/2 FWZI ~ 140 km.s-1). But, on the short september 14th event, the blue part of the line changed significatively

CH Cyg Fe II 5018 - 2018 June to November


CH Cyg He I 5876 - 2018 June to November


The shape of He I 5876 is very stochastic, with no general sheme (see EW graph page 50)


CH Cyg equivalent widths - 2018 June to November

SYMBIOTICS

TiO 1 indexas described in Kenyon and Fernandez-Castro (1987)


CI Cyg


SYMBIOTICS


Phase 0.32 (2018-09)

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CI Cyg

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CI Cyg 2018-08-31 23:25:59 R = 561 Pierre Dubreuil

CI Cygni Pierre Dubreuil Alpy R = 600

AAVSO V band lightcurce with respect to phasesince 2008Current cycle : large blue dots

O1

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CI CygSYMBIOTICS


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CI Cyg 2018-08-11 21:47:26 R = 1201 C Buil

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CI Cyg 2018-08-11 21:47:26 R = 1201 C Buil

Near UV with the UVEX2 prototype by Christian Buil


ER DelSYMBIOTICS



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ER Del 2018-07-14 11:10:33 R = 731 James R. Foster

FN SgrSYMBIOTICS


Coordinates (2000.0)R.A. 18 53 54.8Dec -18 59 40.6Mag V

Classical symbiotic star with [Fe VII] and Raman OVI lines and high HeII/Hb ratio

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FN Sgr 2018-06-13 10:03:32 R = 877 James R. Foster

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FN Sgr 2018-07-15 10:28:01 R = 671 James R. Foster

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SYMBIOTICS


TCP J19544251+1722281 (Vend 47) was discovered by Rob-ert Fridrich. The star was 12.0V on 31.9451 July and 11.66V on 3,9886 Aug. and 10.7V on 08.9381 Aug. http://www.cbat.eps.harvard.edu/unconf/followups/J19544251+1722281.html

Following the alert forwarded by Peter Somogyi, Paolo Berardi obtained a flux calibrated spectrum 2018 Aug. 09.840 UT with a LHIRES III 150 l/mm which clearly identify the transcient as a symbiotic star in outburst, with Balmer lines in emission on a M giant continuum and high ionized lines, notably He II 4686.

The transcient is identified as HbHa 1704-05 (ATel #11937)

Confirmation image obtained by Tamàs Tordaï on August 09.815 UThttp://vendegcsillagkereso.blogspot.com/2018/08/vend47-new-symbiotic-variable-in-sagitta.html

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AAVSO V lightcurve (raw data)and ARAS Spectra (blue dots)

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10-12 TCP J19544251+1722281 2018-08-09 20:08:54 R = 611 Paolo Berardi


Confirmation spectrum obtained by paolo Berardi (LHIRES III 150 l/mm)

TCPJ 19544251+1722281= HbHa 1704-058 = Vend 47 New symbiotic

HBHa 1704-05: a bright and newly discovered symbiotic star, currently undergoing an "hot-type" outburstATel #11937U. Munari (INAF Padova), S. Dallaporta, P. Valisa (ANS Collaboration), P. Ochner (Univ. Padova), R. Fidrich (HAA/VSS), P. Berardi, O. Garde, C. Buil (ARAS Group)on 11 Aug 2018; 11:20 UTCredential Certification: U. Munari ([email protected])

HbHa 1704-05 was first noted by Kohoutek and Wehmeyer in their catalog of emission line stars (1999, A&AS, 134, 255), as a source with a strong continuum (thus not a PN) and overexposed Halpha emission. It seems not much else is available in literature. The star is coincident with 2MASS J19544295+1722125 (=ASASSN-V J195442.95+172212.6) catalogued by VSX (Otero 2018) as an SR variable with a periodicity around 418 days, and a range of variability 13.2-12.4 in V band.On patrol sky observations obtained with a Canon EOS 1000D plus 180mm focus lens, one of us (R.F.) recently noted a rapid increase in bright-ness amounting to (preliminary calibrated) V~12.0 on July 31.945 UT, V~11.7 on Aug 3.989, and V~10.7 mag on Aug 8.938. The trend was confirmed by inspection of the on-line ASASSN database. An exploratory spectrum was soon obtained on UT Aug 9.839 by one of us (P.B.) with a 23cm+Lhires III telescope, showing a rich emission line spectrum that prompted to collect deeper observations.On UT Aug 10.837 we have observed HBHa 1704-05 with ANS Collaboration telescope ID 310 obtaining B=11.459, V=10.926, R=10.101, and I=9.199. Comparing with APASS mean values for quiescence, B=13.798 and V=12.637, the object is now 2.3 mag brighter in B and far bluer in color (from B-V=+1.16 to +0.53).A deep 3200-7900 Ang spectrum of HBHa 1704-05 was obtained on UT Aug 10.855 at 2.31 Ang/pix dispersion with the Asiago 1.22m tele-scope, while the Varese 84cm provided a high resolution Echelle spectrum on UT Aug 10.882. The spectrum of HBHa 1704-05 is characterized by TiO absorption bands from an M giant in the red, progressively veiled by nebular emission toward the blue, with a prominent Balmer continuum in emission. A lot of strong emission lines are present, with HeII 4686 of the same intensity of Hbeta, and [NeV] 3426 suggesting a photo-ionization temperature in excess of 100,000 K. A prominent NIII 4640 complex is accompanied by OIV 3411 and OIII 3313, 3429, and 3444, indicating that pumping under Bowen fluorescence, initiated by HeII Ly-alpha photons at 303.8 Ang, is active. Forbidden lines charac-terized by a low critical density are absent, and also absent is the Raman scattered OVI pair at 6825, 7088 Ang. On the Echelle spectrum, the emission lines appear remarkably sharp and symmetric, without P-Cyg absorptions or other signatures of mass loss being visible, and with broad wings for the Balmer lines that suggest a large electron pressure. Bowen-pumped OI 8446 is present as are low-excitation emission from FeII multiplet 42, NaI D1,D2 and infrared CaII triplet.We therefore conclude that HBHa 1704-05 is a previously unknown symbiotic binary, currently undergoing an "hot-type" outburst, with the wind of the cool giant being increasingly ionized by a hot companion rising in Teff. Its Gaia parallax suggests a distance of 3.6 kpc (albeit with a large error), and Schlafly et al. (2011, ApJ 737, 103) extinction maps indicate a reddening E(B-V)=0.28. The latter is confirmed by the low equivalent width for DIB 6614 and KI 7699. Combining APASS mean BVgri photometry in quiescence with 2MASS JHK data, a spectral type around M3III can be inferred for the M giant, in agreement with M(V)=-1.0 in quiescence from Gaia parallax.The large brightness attended by the ongoing outburst of HBHa 1704-05 and its favorable position on the sky will undoubtedly support a large, all-out observing effort, we plan to join.

SYMBIOTICS

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TCPJ 19544251+1722 2018-08-10 22:22:27 R = 1136 C. Buil


Near UV spectrum obtained by Christian Buil with his UVEX prototype



SYMBIOTICS

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TCP J19544251+17222 2018-08-10 20:17:05 R = Olivier Garde

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TCP J19544251+17222 2018-08-10 20:17:05 R = Olivier Garde



TCPJ 19544251+1722281= HbHa 1704-058 = Vend 47 New symbiotic SYMBIOTICS


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TCPJ19544251+1722281

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Low resolution series along the decline with spectra obtained by C. Boussin, K. Graham, L. Franco, K. Bazan, Guegan, U. Sollecchia. Note the strengthening ofRaman OVI

SYMBIOTICS


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Low resolution series along the decline with LISA spectra obtained by D. Boyd, W. Sims, G. Martinet, Y. Buchet


SYMBIOTICS


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TCPJ19544251+1722281 2018-09-19 19:50:33 R = 600 C. Buil

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TCPJ19544251+1722281 2018-09-19 19:50:33 R = 600 C. Buil


Near UV with UVEX2

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TCPJ19544251+1722281 2018-09-22 19:24:10 R = 1353 C. Buil

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TCPJ19544251+1722281 2018-09-22 19:24:10 R = 1353 C. Buil

SYMBIOTICS



Near IR with UVEX2 prototype

SYMBIOTICS


H alpha profile obtained by Um-berto SollecchiaR = 8000

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30Halpha 2018-08-10

H alpha profile Paolo Berardi Lhires III 2400 l/mmR = 15000

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H beta range obtained by Paolo berardi (Lhiress III, 600 l/mm, R = 2500)


SYMBIOTICS


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TCPJ19544251+1722281 H alpha

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TCPJ19544251+1722281 He II 4686

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H beta range obtained by Peter Somogyi (Lhiress III, 2400 l/mm, R = 8000)

Ha rangePeter Somogyi (Lhires III, 600 l/mm, R = 2500)

SYMBIOTICS


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TCP J19544251+1722281 2018-08-20 01:26:36 R = 12000 T. Lester

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TCPJ = HbHa = Vend 47 New symbiotic starSYMBIOTICS


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Raman OVI 6830


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TCPJ19544251+1722281 [Fe VII] 6087

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LISA Spectra R = 1000

ALPY Spectra R = 600

[Fe VII] 6087Echelle Spectra R = 9000-13000

HM SgeSYMBIOTICS

Coordinates (2000.0)R.A. 19 41 57.07Dec +16 44 39.8Mag V ~ 12.4


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HM Sge 2018-09-23 21:44:33 R = 599 F. Campos

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HM Sge 2018-09-23 21:44:33 R = 599 F. Campos

IV VirSYMBIOTICS



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IV Vir 2018-07-07 04:59:01 R = 776 James R. Foster

LT DelSYMBIOTICS


Coordinates (2000.0)R.A. 20 35 57.2Dec +20 11 27.5Mag V 13.1 (2018-09)

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LT Del 2018-07-11 10:16:55 R = 863 James R. Foster

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LT Del 2018-09-28 20:52:46 R = 674 F. Campos

PU VulSYMBIOTICS

Coordinates (2000.0)R.A. 20 21 13.3Dec +21 34 18.7Mag V


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PU Vul 2018-07-13 11:20:23 R = 641 James R. Foster

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PU Vul 2018-08-13 02:58:07 R = 552 K Graham

PU VulSYMBIOTICS


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PU Vul 2018-07-13 11:20:23 R = 641 James R. Foster

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PU Vul 2018-08-13 02:58:07 R = 552 K Graham


R AqrSYMBIOTICS



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R Aqr 2018-08-12 22:24:02 R = 589 Michel VERLINDEN

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R Aqr 2018-09-27 21:53:47 R = 535657 J. Guarro

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6[OI]6300 2018-09-27


R AqrSYMBIOTICS

RS OphSYMBIOTICS

Coordinates (2000.0)R.A. 17 50 13.15Dec -06 42 28.48Mag V 10.7 (2018-09)


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RS Oph 2018-06-15 07:18:53 R = 850 James R. Foster

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RS Oph 2018-07-08 08:27:47 R = 850 James R. Foster

RS OphSYMBIOTICS

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RS Oph 2018-07-20 R = 12000 T Lester

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RS Oph 2018-07-20 R = 12000 T Lester


RT SerSYMBIOTICS

Coordinates (2000.0)R.A. 17 39 51.98Dec -11 56 38.8Mag V ~ 15

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RT Ser 2018-07-13 07:29:54 R = 785 James R. Foster


RW HyaSYMBIOTICS

Coordinates (2000.0)R.A. 13 34 18.12Dec -25 22 48.9Mag ~ 9


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RW Hya 2018-06-13 04:48:38 R = 864 James R. Foster

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RW Hya 2018-07-14 04:38:04 R = 730 James R. Foster

StHa 32SYMBIOTICS

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

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StHa 32 2018-03-05 19:10:45 R = 860 F. Campos


StHa 149SYMBIOTICS


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StHa 149 2018-07-13 08:47:43 R = 773 James R. Foster


StHa 169SYMBIOTICS


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StHa 190SYMBIOTICS


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StHa190 2018-08-12 01:51:50 R = 512 Christophe Boussin


T CrBSYMBIOTICS

Coordinates (2000.0)R.A. 15 59 30.1Dec 25 55 12.6Mag 9.8 (2018-03)


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

AAVSO V band lightcurve and ARAS spectra (blue dots)


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T CrB 2018-08-31 21:25:55 R = 654 Jacques Montier

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T CrBSYMBIOTICS


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T CrB 2018-08-05 20:48:58 R = 11000 FM Teyssier

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TX CVnSYMBIOTICS

Coordinates (2000.0)R.A. 12 42 17.8Dec +37 02 14.9Mag ~10 (2018-03)


Faint Ha emission

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TX CVn 2018-07-09 04:58:50 R = 798 James R. Foster


V335 VulSYMBIOTICS

Coordinates (2000.0)R.A. 19 23 14.14Dec +24 27 39.6Mag ~12


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V335 Vul 2018-07-26 00:03:01 R = 615 Tony Rodda

V443 HerSYMBIOTICS

Coordinates (2000.0)R.A. 17 40 24.7Dec +25 25 48.4Mag 11.3


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V443 Her 2018-08-10 02:53:28 R = 546 K Graham

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V443 Her 2018-09-26 19:22:40 R = 740 Fran Campos


V443 HerSYMBIOTICS

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V443 Her 2018-08-28 04:26:37 R = 8973 James R. Foster

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V627 CasSYMBIOTICS

Coordinates (2000.0)R.A. 22 57 41.0Dec +58 49 12.6Mag 12.16


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10-13 V627 Cas 2018-08-29 22:48:43 R = 1111 D. Boyd

V694 Mon = MWC 560SYMBIOTICS

Coordinates (2000.0)R.A. 07 25 51.28Dec -07 44 08.07Mag 9.2

Firt spectra of the season. Peter Somogyi detected peculiar profiles for this star, with a lack of the typical absorption in the blue part of Balmer and Fe II lines as if the jets have desappeared.The emission is replaced by emis-sion up to -1000 km.s-1 with a classi-cal P Cygni absorption which peaks at -190 for Ha and -200 to -220 km.s-1 for Hb.Note also the increasing luminosity(mag V ~ 9.2, DV ~ 1 from spring to automn)See Steve's comment page 109)

Monitoring of the target at high cadency (low and high resolution) is strongly recommended for the next months


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V694 Mon H beta

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V919 SgrSYMBIOTICS

Coordinates (2000.0)R.A. 19 03 45.1Dec -16 59 55.37Mag 13.1 (2018-10)


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V919 Sgr 2018-07-13 09:41:46 R = 829 James R. Foster

V934 HerSYMBIOTICS

Coordinates (2000.0)R.A. 17 06 34.5Dec +23 58 18.65Mag


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V934 Her 2018-08-31 22:10:33 R = 652 Jacques Montier

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V934 Her 2018-08-07 03:10:54 R = 540 K Graham

V1016 CygSYMBIOTICS

Coordinates (2000.0)R.A. 19 57 05.0Dec +39 49 36.1Mag ~11.2 (Vis.)


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V1016 Cyg 2018-07-18 04:06:52 R = 14000 T. Lester

V1329 CygSYMBIOTICS



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10-13 V1329 Cyg 2018-08-29 21:14:43 R = 1110 D. Boyd


V1413 AqlSYMBIOTICS



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V1413 Aql 2018-07-13 10:33:58 R = 767 James R. Foster

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V1413 Aql 2018-09-23 22:21:28 R = 700 F. Campos

YY HerSYMBIOTICS

Coordinates (2000.0)R.A. 18 14 34.19Dec +20 59 21.18Mag V 13.2 (2018-09)

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YY Her 2018-06-13 08:45:31 R = 835 James R. Foster

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YY Her 2018-09-26 20:35:33 R = 742 F. Campos


Z AndSYMBIOTICS

Coordinates (2000.0)R.A. 23 33 39.5Dec 48 49 5.4Mag V 10.15


After the outburst (2018-02)smooth decline (V mag = 9.7 late october)

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10-11 Z And 2018-08-03 22:05:11 R = 978 D.Boyd

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10-11 Z And 2018-09-01 22:01:36 R = 1060 D. Boyd

Z And 2018SYMBIOTICS


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Z And 2018-09-19 21:31:24 R = 600 C. Buil

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Z And 2018-09-22 21:52:38 R = 1278 C. Buil


Near UV and near IR obtained by Christian Buil with his prototype UVEX2See http://www.astrosurf.com/buil/RCE2018/RCE2018_Buil.pdf

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10-12 Z And 2018-08-05 02:24:43 R = 5845 P. Somogyi



Near UV spectrum Peter Somogyi Lhires III 1200 l/mm

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

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


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ASASSN-V J192916.53-2240403 2018-09-21 03:40:52 R = 1023 Forrest Sims


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EN Sgr 2018-09-18 02:59:01 R = 988 Forrest Sims



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GAIA DR2 4048168377818693632 2018-09-23 10:46:47 R = 1677 T Bohlsen

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GAIA DR2 5919388180059095292 2018-09-29 11:29:31 R = 1862 T Bohlsen

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Gaia DR2 6345873798283774848 2018-09-18 11:15:35 R = 1648 T Bohlsen


SN 2018 gjxSupernovae


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SN 2018gjx 2018-09-19 23:39:50 R = 506 Olivier Garde, Pascal Le Du, Bertrand Guegan

The omicron telescop control room with Bertrand Pascal and Olivier (from left to right)

Spectrum of the supernova SN2018gjx with a LISA mounted on the 1M telescope

C2PU building with the west and east dome

Omicron 1 meter telescop in southern France


The Calern site was selected in 1970 by the Côte d'Azur Observatory (OCA), for the establishment of an astrometric observatory and the use of new in-struments. This site with an area of 20 km2 is semi desert. It enjoys a high number of clear nights. The humidity of the atmosphere is medium and the winds circulate in horizontal layers. Mists are very rare and there is no dust. The site consists of many buildings and domes. The C2PU building has two domes each housing a 1 meter telescop in diameter. The C2PU project (Centre Pédagogique Planète Univ-ers) is based on the rehabilitation and use of these two telescopes for scientific research and teaching.

The C2PU telescopes participate in several research programs in various fields of astronomy: asteroid tracking, confirmations of objects detected by the GAIA satellite. They are also used for science educa-tion at university level but also pre-university level.

The telescopes of the two domes East and West, are

of identical design. One is named Omicron (West dome) and the other Epsilon (East dome). The Omi-cron telescope was commissioned in August 2012 and the Epsilon telescope in May 2015. The pri-mary mirror is parabolic with 1040 mm diameter.

The telescope has 4 differents optical configurations:• Cassegrain with a hyperbolic secondary mirror that gives a focal length of 13 meters and an F/D ratio of 12.5 at the focus of the secondary mirror.• Fastar mode where the CCD is attached to the primary mirror focus instead of the second-ary mirror. In this configuration the telescope has a focal length of 3 meters and an F/D ratio of 3, but the field is strongly affected by coma.• Fastar mode with Wynne coma corrector: fo-cal length of 3.3 meters and F/D ration of 3.2.•Elbowed mode with a 3rd mirror plane in the op-tical axis of the secondary mirror, returning the light flux in the polar axis of the telescope mount: focal length of 36 meters and an F/D ratio of 12.5.

The omicron one meter telescopand the Yoke mount

Focus adjustment is effected by the translation of the secondary mirror support in the optical axis of the primary mirror.

The mount of the telescope is an equatorial Yoke, which limits the pointing of the telescope in certain directions. (no pointing below 20 de-grees in height and an area of the sky north is not accessible).

The mount is very stable mechanically with slight flexions. The tracking is very accurate even with a focal length of 7 meters and does not require autoguiding.

The Omicron telescope with its dome can be to-tally controlled remotely via internet.

Each telescope has a control room for control-ling the telescope and for acquiring images or spectra.

Mission September 2018 (S38)

During our mission, we use the Omicron telescope of the West dome in its Cassegrain configuration:https://c2pu.oca.eu).

The 1 meter telescope is natively F/D 12.5 ratio, two focal reducers are used to re-duce the F/D ratio of the telescope close to 7. The first reducer used is that of the C2PU, normally dedicated to this telescope. The second is an Astro-Physics CCDT67.The spectrograph is a LISA from Shelyak instru-ment (www.shelyak.com) with a native resolution of R = 1000. It is intended to work with a close ratio of F/D 5.

The LISA is equipped with 2 ATIK CCD cameras:

• An ATIK 314L + is used for autogu-iding and centering target on the slit. It has a large enough field that allows to check the centering of the target. In practice, autoguiding is not used because the telescope follows the target very well despite a focal length of 7 m.

• An ATIK 414 ex is used for spectral acqui-sition. The camera has pixels of 6.45μm and is set to acquire 1x1 binning images.A 50 μm slit is positioned on the spectrograph to optimize the chances of getting the signal on very weak targets. The signal flux is thus greater at the expense of the resolution.

Finally, the LISA (Tungsten and Neon) calibration lamps are remotely controlled to prevent any in-trusion into the dome.

The field of the autoguiding camera is oriented with the North at the top so as to facilitate field reconnaissance.

The spectrograph remains permanently on the telescope throughout the mission. During our mission week, we had during the night a very good seeing around 0.5 to 0.7 arcsec.

Olivier GardePascal Le Dû

Bertrand Guegan


Lisa spectrographon the omicron 1 meter telescop

Spectroscopy with Omicron 1 m telescop in southern France Olivier Garde Pascal Le Dû Bertrand Guegan

MWC 560 in eruption Steve Shore

MWC 560 in eruption again and some com-ments of dynamical changes in symbiotic spectra

In past columns we've discussed this source but, since it's again in eruption, I'd like to return to the problem of interpretation of profile changes.

The main weirdness of this symbiotic is the occasion-al appearance of rapidly evolving absorption troughs that reach velocities of order 1000 to 6,000 km.s-1

over timescales of days to weeks. These are transient features, as a walk through the database will show, but they can persist for some time. Usually inter-preted as jet or mass ejection events (in Z And these have been called jets, at velocities about 10 times lower). Recently (arxiv:1802.07743) the IUE spectra have been re-examined and it's been rediscovered that the Fe-curtain was not spherical and that there were high ionization lines (Al III, Si IV, C IV) species in the spectrum. Looking at the latest ARAS database contributions, the absorption lines have shown the same progression toward higher velocity and the red emission has also changed. We discussed some of these mirrored profile changes for novae, you may remember, in the dust forming events. But it's also possible as a generic result of changing absorption and scattering if the medium is sufficiently opaque. Think of what happens if you have a jet emitted by a star. For the moment, assume the axis is perpen-dicular to the orbital plane so there's no change in your line of sight to the jet. Now tilt this toward the observer. The driving dynamics may be constant over time so there's always some mass outflow at high velocity (hence the broad wings always) but, sometimes, the jet is loaded heavily with more mat-ter and the jets recombine. The receding component will simply disappear, if the column density is large enough, or be transparent only in the inner part of the jet where the change is rapid in the velocity (this is one of the pictures for the jet, that its radial -- rela-tive to the WD, not the observer -- velocity increases rapidly near the star due to an effective acceleration and then coasts at high velocity). The outer part will be more than usually opaque since the matter is all moving at nearly the same velocity.

This is the Sobolev approach we talked about for winds and novae, the change in the velocity across a line core determines the optical depth. So if you load mass into the flow, and there's a recombination, that may move ``outward'' as it does in LBVs and novae. Then the terminal velocity may actually never be seen, and while the recombination wave is progress-ing there's a more continuous blue edge to the ab-sorption profile that gradually steepens as the front approaches the maximum flow region of the jet.

What would cause the jet to change depends on what the companion is doing. The accretion in sym-biotics is from the wind but mediated through a disk, that seems a secure understanding. The timescale for structures to be injected into the red giant wind depends on the envelope of the star, pulsations don't have to be orderly to have a dynamical effect like a sort of spitting into the wind. The disk is then vari-ably loaded and it may have a state of triggering the dumping of matter onto the WD. That would not be unheard of for such stars, cataclysmics showing dwarf nova outbursts do it all the time. It's different here since DN don't show jets, and certainly noth-ing like this, and here the events aren't explosive. But they may also not be dynamical, the one thing I wanted to emphasize.

When you see a change in the centroid or extension of a line profile, it's easy to think this means some-thing restructuring and dynamical is happening. Yes, it may be. But to play devil's advocate for a moment, in the interest of illustrating how the phenomena are not so unambiguous, you see that changes in the way the line is formed can mask or mimic dynamical changes.

Recurrents

Nova M31N 2008-12a has appeared again, almost on its annual schedule (a slew of ATels beginning with the detection announcement ATel #12177). Most significantly, now that the culprit is so well known, its activity has been closely monitored and the latest announcement pins down the initiation of the explo-sion to within 0.3 days. This is a precision previously unknown in understanding the rate of rise of a nova


from minimum. Whether the source is ever in a "qui-escent'' state is, however, unknown since the mini-mum has not been observed spectroscopically (e.g., Henze et al. 2018, ApJ, 857, 68; Darnley et al. 2016, ApJ, 833, 149; Henze et al. 2015, A&A, 582, L8). The repetition rate is extreme but only relatively. Since its first repeat appearance in 2013, the 2008-12a has been joined by a growing number of rapidly recurring novae, none of which are Galactic. This isn't surpris-ing since monitoring is far easier in the small num-ber of fields required to external galaxies (M31, M81, and the Magellanic Clouds are under regular surveil-lance with the limits being only weather).

Whether this is a special, separate class of novae or just the tail of an otherwise continuous distribution remains to be seen, the population is still too small to know. But there is a distinction between those that arise in compact systems and their cousins in the symbiotic like, long period systems: the compact systems have the rapid repeaters while those in long period systems recur on decade timescales or longer. Otherwise, many of the characteristics are quite sim-ilar. The ejected masses are small, about an order of magnitude or more below those of classical systems. They do not seem to arise on ONe white dwarfs but there is still some further work needed here. Recent attempts to understand the accretion rates for these systems come up with a much higher value than that for cataclysmics (Shara et al. arXiv:1804.06880), but from such systems as 2008-12a it's obvious that something different is going on.

To understand what this means, and how your obser-vations are important, consider that the monitoring of Galactic systems such as U Sco (which it does have a relatively rapid recurrence rate, about a decade), let's look for a moment at the setup for an explosion, something about which we haven't spent much time in the past. If you eject about $10-7Ms, or perhaps a factor of 10 times that, it implies you've accreted that much in the interim between explosions. That implies a high accretion rate, about 104 times that expected for a cataclysmic in its normal state. This is. also so fast that the WD likely has little time to adjust to the newly added material. Why this doesn't just blow off because of compression in shocks and

heating is not known; to date, when modelling these events, the models treat the whole sequence very schematically. For instance, if you put mass on a star too quickly for it to adjust thermally and mechani-cally, thermal is likely to win and the material blows off and causes a messy structure of turbulence and convection to form in the envelope of the mass gain-ing star. The WD would sort of inflate, not the whole star but the envelope, and the resulting star would not be very receptive to mass accretion. While also problematic for classical nova systems, and even for. extreme symbiotic star WDs accreting from a wind, it is usually not a serious problem if the matter can be stored in a disk (the pile-up that prevents direct accretion) and the actual rate of deposition can be lower. It's not unlike how a bathtub fills even if the drain is open, if the rate of inflow from the tap is large enough. It's even possible to achieve balance, in this case the combination of gravity and viscosity trans-fer matter into the discharge. Here, the timescale for delivery must be very short and it's not clear how it's achieved, what sort of conditions prevail at the inner boundary of the disk and WD, and how the incoming material is mixed.

There's one other issue that comes to mind, espe-cially related to these fastest systems. What happens on the WD depends on how rapidly the star cools. When the nuclear source turns off, there's a charac-teristic timescale -- the thermal time -- over which the envelope readjusts to its pre-outburst state. That is not quick, it takes decades or even centuries. In these rapid cases, it's not clear the star is ever quiet, no less in anything but a dynamic state. But the prob-lem with models is that, at this stage, the actual ex-plosion and its recovery are not treated in detail. The ejection is a lift-off, anything above the sound speed is ejected -- that is, removed -- from the star. If, for example, the inner zones are pulsating from an un-stable burning shell, as happens in a slower and more dramatic way on the asymptotic giant branch (AGB, stars like a Ori, for example) there's currently no way to follow the thermal and mechanical reaction of the envelope. Some time ago, for instance, we discussed the light variations around maximum in some novae, for which clear pulses seem to be involved. This can't presently be reproduced. So one of the challenges,


Recurrents Steve Shore

and this holds for all recurrent novae, is to under-stand the relaxation. For 2008-12a, that may never occur and each successive accretion-explosion cycle may be happening on a WD that looks physically very different than, say, a classical nova. For the brightest systems, this is a key reason, even for the non-recur-rents, to follow the stars as long as possible. Keep-ing with the usual mantra: photometry is the lowest resolution spectroscopy but you can't recover the in-formation lost by that reduction.

Every nova is an ejection and doesn't happen sponta-neously. Unlike core-collapse supernovae for which the explosion is a consequence of the entire evolu-tionary path of the star toward its final critical state, the binary in which a nova occurs would otherwise be a passive pair of little creatures were they left to evolve separated. Not that they would be indepen-dent, since the orbital periods assure that tidal cou-pling of their spins and orbital motion. If synchro-nized, and if the larger (not necessarily more massive) cool companion is convective, the system will be ac-tive and would resemble some of the better known WD-red dwarf binaries (V471 Tau, for instance, which is a spotted active subgiant with a hot WD and 0.5 day period in the Hyades). Most of these are con-sidered post-common envelope systems, with short periods and hot, but not high mass, WD companions. For the recurrents, the WD mass is clearly high, 1.2 or 1.3 Ms, making the accretion more likely to lead to a quick ignition. Yet novae in general have WDs on the more massive end of the scale so this can't be the only reason for the difference. If there's a sug-gestion for 2008-12a by Henze and collaborators that the orbital period is very long, based on a delayed explosion in the sequence, but that would require a symbiotic like system (none of which are anywhere near this rapidly repeating) and would make the bi-nary strangely faint (the star is below B=22). The qui-escent system is well below the range you can study but, sooner or later, there has to be a counterpart to this in the Milky Way. There's already one, LMC 1968 (which was also named 1990b or 1990 #2) that's re-peated in less than a decade and is bright enough to catch spectroscopically with an Alpy600 or other low resolution instrument.

The environment of eruptive variables: pre-cursors, light echos, and spectra

One of the features showing up with your higher res-olution studies of novae in outburst is the presence of very narrow lines in the early spectrum, especially on the Balmer lines. In keeping with one of the themes of this month's column, let me make a few quick re-marks and then we'll discuss this in more depth in the next column (along with mergers, I promise). In several novae, V392 Per and KT Eri, for instance, a very pronounced narrow (500 km.s-1 or so, FWZI) ap-pears soon after the broad Balmer lines turn partially transparent. More to the pint, it remains (although fading, not enough of the spectra are flux calibrated to be sure, though) while the broad line of the ejecta change in intensity and shape. The line in V392 Per first appeared as a broad, almost parabolic shape that developed a distinct saddle-shape with the narrow peak appearing after about a week and dominating the profile. One possible explanation is that this is a separate polar blob, ejected perpendicular to a ring. That's the simplest geometrical (kinematic) construc-tion. But there's another possibility, also related to what's seen in the M 31 recurrent: this is a flash ion-ization of the environment. Take the case of a set of ejections, nonspherical, that are close enough that they are flashed and recombine. Further assume the gas has the same velocity structure as any ``normal'' nova ejecta, that the velocity increases with radius and the density decreases. Then if the whole gas emits, the part that is at lower density emits pro-gressively more weakly with time than the inner part and if you see both sides of the expanding gas the line width will decrease with time on roughly the recombination timescale. Now for V392 Per, that is about a few weeks which would imply a high density, about 106 cm-3, but this wouldn't be unreasonable fo a system that's undergone a nova explosion about 5 years ago if you are only seeing the inner portion of the ejecta. The maximum velocity of 2000 km.s-1 or so gives a limit on how far the ejecta could have got-ten, it's about 1000 AU (about 0.01 pc).


The environment of eruptive variables: precursors, light echos, and spectra Steve Shore

The same sort of thing might be seen in dusty ejec-ta were they formed in recurrent systems, or from the sort of light echo seen in GK Per 1901. That was from the environment, like the rings around SN 1987A, but it's not something usually consid-ered in the treatment of novae. The presence of a dusty ejecta (recall the discussion of the C-type -- in the light curve taxonomy proposed by Stope et al. (2010), as we discussed in arxiv:1807.07174 and arxiv:1309.7388) reflecting the light from the expanding gas changes the line profiles in width

and intensity.

Let's hold off on this for the moment, it will make more sense with cartoons and that will be in the next column. Any questions, comments, insults, or advice will always be appreciated (well, maybe not all of the above). Be sure to read Francois' contri-bution to the Slovakia meeting on small telescopes, it's a gem. And thank you all, always and sincerely, for your enormous contributions.

Steve Shore


Spectra of M31N 2008-12a inM31N 2008-12a — THE REMARKABLE RECURRENT NOVA IN M 31:PAN-CHROMATIC OBSER-VATIONS OF THE 2015 ERUPTION.https://arxiv.org/pdf/1607.08082.pdf

The environment of eruptive variables: precursors, light echos, and spectra Steve Shore



Observing techniques, instrumentation and sciencefor metre-class telescopes

II Tatranská Lomnica, Slovakia

September 24 — 28, 2018

The main objective of the conference is to exchange on the technological developments and scientific programs for small-size and robotic telescopes.

I have been kindly invited by Augustin Skopal to participate and give a talk during the second edition of this con-ference. I presented the setups we use (*very* small scopes), the results we are able to obtain, the cooperation with professional teams (Spectroscopic Monitoring of Eruptive Stars and the ARAS database - https://www.astro.sk/conferences/75AI2018/talks/B12.pdf).

There has been very nice synergy with the talks of:Jaroslav Merc on AG Dra campaign (Study of long-term spectroscopic variability of symbiotic stars based on observa-tions of the ARAS Group - https://www.astro.sk/conferences/75AI2018/talks/B13.pdf)Chochol on Nova Sct 2017 based on ARAS spectra and noticely the 70 spectra obtained by Joan Guarro during the oscillating decline of this peculiar nova (Optical photometry and spectroscopy of V612 Sct: slow classical nova with rebrightenings)

Rudolf Gàlis (The current active stage of the symbiotic system AG Draconis - https://www.astro.sk/conferences/75AI2018/talks/B08.pdf) and Augustin Skopal (Studying symbiotic stars and classical nova outbursts with small telescopes - https://www.astro.sk/conferences/75AI2018/talks/B07.pdf) emphasized the quality and utility of the spectra of Erup-tive stars gathered in the ARAS DataBase.

Presentations can be downloaded fromhttps://www.astro.sk/conferences/75AI2018/index.php?part=program

Two posters with ARAS observers as co-authors

Hα orbital variations of the symbiotic star EG And from optical spectroscopyN. Shagatova, A. Skopal, M. Sekeráš, F. Teyssier, S.Yu. Shugarov, R. Komžík, Z. Garai, E. Kundra, M. Vaňkohttps://www.astro.sk/conferences/75AI2018/posters/BP20.pdf

First glance to the recently discovered symbiotic star HBHA 1704-05 during its current outburstA. Skopal, M. Sekeráš, E. Kundra, R. Komžík, S.Yu. Shugarov, Z. Garai, C. Buil, P. Berardihttps://www.astro.sk/conferences/75AI2018/posters/BP20.pdf

Posters: https://www.astro.sk/conferences/75AI2018/index.php?part=posterstalks

High-resolution observations of the symbiotic system R Aqr Direct imaging of the gravitational effects of the secondary on the stellar wind

Bujarrabal, V.; Alcolea, J.; Mikołajewska, J.; Castro-Carrizo, A.; Ramstedt, S. Astronomy & Astrophysics, 2018, Volume 616

We have observed the symbiotic stellar system R Aqr, aiming to describe the gravitational inter-action between the white dwarf (WD) and the wind from the Mira star, the key phenomenon driving the symbiotic activity and the formation of nebulae in such systems. We present high-res-olution ALMA maps of the 12CO and 13CO J = 3-2 lines, the 0.9 mm continuum distribution, and some high-excitation molecular lines in R Aqr. The maps, which have resolutions ranging between 40 mas and less than 20 mas probe the circumstellar regions at suborbital scales as the distance between the stars is 40 mas. Our observations show the gravitational effects of the secondary on the stellar wind. The AGB star was identified in our maps from the continuum and molecular line data, and we estimated the probable position of the secondary from a new estimation of the orbital parameters. The (preliminary) comparison of our maps with theoretical predictions is surprisingly satisfactory and the main expected gravitational effects are directly mapped for the first time. We find a strong focusing in the equatorial plane of the resulting wind, which shows two plumes in opposite directions that have different velocities and very probably correspond to the expected double spiral due to the interaction. Our continuum maps show the very inner regions of the nascent bipolar jets, at scales of some AU. Continuum maps obtained with the highest resolution show the presence of a clump that very probably corresponds to the emis-sion of the ionized surroundings of the WD and of a bridge of material joining both stars, which is likely material flowing from the AGB primary to the accretion disk around the WD secondary Broad Wings around Hα and Hβ in the Two S-type Symbiotic Stars Z An-dromedae and AG DraconisChang, Seok-Jun; Lee, Hee-Won; Lee, Ho-Gyu; Hwang, Narae; Ahn, Sang-Hyeon; Park, Byeong-GonThe Astrophysical Journal, Volume 866, Issue 2, article id. 129, 13 pp. (2018)

Symbiotic stars often exhibit broad wings around Balmer emission lines, whose origin is still controversial. We present high-resolution spectra of the S type symbiot-ic stars Z Andromedae and AG Draconis obtained with the ESPaDOnS and the 3.6 m Canada–France–Hawaii Telescope to investigate the broad wings around Hα and Hβ. When Hα and Hβ lines are overplotted in the Doppler space, it is noted that Hα profiles are overall broader than Hβ in these two objects. Adopting a Monte Car-lo approach, we consider the formation of broad wings of Hα and Hβ through Raman scattering of far-UV radiation around Lyβ and Lyγ and Thomson scattering by free electrons. Raman scattering wings are simulated by choosing an H I region with a neutral hydrogen column density N H I and a covering factor CF. For Thomson wings, the ionized scattering region is assumed to fully cover the Balmer emission nebula and is characterized by the electron temperature T e and the electron col-umn density N e. Thomson wings of Hα and Hβ have the same width that is proportional to {T}{{e}}1/2. However, Raman wings of Hα are overall three times wider than Hβ counterparts, which is attributed to different cross sections for Lyβ and Lyγ. Normalized to have the same peak values and presented in the Doppler factor space, Hα wings of Z And and AG Dra are observed to be significantly wider than their Hβ counterparts, favoring the Raman scattering origin for broad Balmer wings.

Spectroscopic and photometric observations of symbiotic nova PU Vul during 2009-2016Tatarnikova, Anna; Burlak, Marina; Kolotilov, Eugene; Metlova, Natalia; Shenavrin, Victor; Shugarov, Sergei; Tarasova, Taisija; Tatarnikov, Andrey Research in Astronomy and Astrophysics, Volume 18, Issue 8, (2018).

A new set of low-resolution spectral and UBVJHKL-photometric observations of the symbiotic nova PU Vul is presented. The binary has been evolving after its sym-biotic nova outburst in 1977 and now it is in the nebular stage. It is found that the third orbital cycle (after 1977) was characterized by great changes in associated light curves. Now, PU Vul exhibits a sine-wave shape in all the light curves (with an amplitude in the U band of about 0.7 mag), which is typical for symbiotic stars in the quiescent state. Brightness variability due to pulsations of the cool component is now clearly visible in the VRI light curves. The amplitude of the pulsations increases from 0.5 mag in the V band to 0.8 mag in the I band. These two types of variability, as well as a very slow change in the physical parameters of the hot component due to evolution after the outburst of 1977, influence the spectral energy distribution (SED) of the system. The variability of emission lines is highly complex. Only hydrogen line fluxes vary with orbital phase. An important feature of the third orbital cycle is the first emergence of the OVI, 6828Å Raman scatter-ing line. We determine the temperature of the hot component by means of the Zanstra method applied to the He II, 4686Å line. Our estimate is about 150 000 K for the spectrumobtained near orbital maximum in 2014. The VO spectral index derived near pulsation minimum corresponds to M6 spectral class for the cool component of PU Vul.

Recent publications

Symbiotics


Recent publications

Symbiotics


X-ray, UV, and optical observations of the accretion disk and boundary layer in the symbiotic star RT Crucis

Luna, G. J. M.; Mukai, K.; Sokoloski, J. L.; Lucy, A. B.; Cusumano, G.; Segreto, A.; Arancibia, M. Jaque; Nuñez, N. E.; Puebla, R. E.; Nelson, T.; Walter, F.Astronomy & Astrophysics, Volume 616, id.A53, 12 pp. (A&A Homepage)

Compared to mass transfer in cataclysmic variables, the nature of accretion in symbiotic binaries in which red giants transfer material to white dwarfs (WDs) has been difficult to uncover. The accretion flows in a symbiotic binary are most clearly observable, however, when there is no quasi-steady shell burning on the WD to hide them. RT Cru is the prototype of such non-burning symbiotics, with its hard (δ-type) X-ray emission providing a view of its innermost accretion structures. In the past 20 yr, RT Cru has experienced two similar optical brightening events, separated by 4000 days and with amplitudes of ΔV 1.5 mag. After Swift became operative, the Burst Alert Telescope (BAT) detector revealed a hard X-ray brightening event almost in coincidence with the second optical peak. Spectral and timing analyses of multi-wavelength observations that we describe here, from NuSTAR, Suzaku, Swift/X-Ray Telescope (XRT) + BAT + UltraViolet Optical Telescope (UVOT) (photometry) and optical photometry and spectroscopy, indicate that accretion proceeds through a disk that reaches down to the WD surface. The scenario in which a massive, magnetic WD accretes from a magnetically truncated accretion disk is not supported. For example, none of our data show the minute-time-scale periodic modula-tions (with tight upper limits from X-ray data) expected from a spinning, magnetic WD. Moreover, the similarity of the UV and X-ray fluxes, as well as the approximate constancy of the hardness ratio within the BAT band, indicate that the boundary layer of the accretion disk remained optically thin to its own radiation throughout the brightening event, during which the rate of accretion onto the WD increased to 6.7 × 10-9M⊙ yr-1 (d/2 kpc)2. For the first time from a WD symbiotic, the NuSTAR spectrum showed a Compton reflection hump at E > 10 keV, due to hard X-rays from the boundary layer reflecting off of the surface of the WD; the reflection ampli-tude was 0.77 ± 0.21. The best fit spectral model, including reflection, gave a maximum post-shock temperature of kT = 53 ± 4 keV, which implies a WD mass of 1.25 ± 0.02 M⊙. Although the long-term optical variability in RT Cru is reminiscent of dwarf-novae-type outbursts, the hard X-ray behavior does not correspond to that observed in well-known dwarf nova. An alternative explanation for the brightening events could be that they are due to an enhancement of the accretion rate as the WD travels through the red giant wind in a wide orbit, with a period of about 4000 days. In either case, the constancy of the hard X-ray spectrum while the accretion rate rose suggests that the accretion-rate threshold between a mostly optically thin and thick boundary layer, in this object, may be higher than previously thought.

Broad absorption line symbiotic stars: highly ionized species in the fast outflow from MWC 560Lucy, Adrian B.; Knigge, Christian; Sokoloski, J. L.Monthly Notices of the Royal Astronomical Society, Volume 478, Issue 1, p.568-574

In symbiotic binaries, jets and disc winds may be integral to the physics of accretion on to white dwarfs from cool giants. The persistent out-flow from symbiotic star MWC 560 (≡V694 Mon) is known to manifest as broad absorption lines (BALs), most prominently at the Balmer transitions. We report the detection of high-ionization BALs from C IV, Si IV, N V, and He II in International Ultraviolet Explorer spectra ob-tained on 1990 April 29-30, when an optical outburst temporarily erased the obscuring `iron curtain' of absorption troughs from Fe II and similar ions. The C IV and Si IV BALs reached maximum radial velocities at least 1000 km s-1 higher than contemporaneous Mg II and He II BALs; the same behaviours occur in the winds of quasars and cataclysmic variables. An iron curtain lifts to unveil high-ionization BALs dur-ing the P Cygni phase observed in some novae, suggesting by analogy a temporary switch in MWC 560 from persistent outflow to discrete mass ejection. At least three more symbiotic stars exhibit broad absorption with blue edges faster than 1500 km s-1; high-ionization BALs have been reported in AS 304 (≡V4018 Sgr), while transient Balmer BALs have been reported in Z And and CH Cyg. These BAL-producing fast outflows can have wider opening angles than has been previously supposed. BAL symbiotics are short-time-scale laboratories for their giga-scale analogues, broad absorption line quasars (BALQSOs), which display a similarly wide range of ionization states in their winds.

Spectroscopic diagnostics of dust formation and evolution in classical nova ejecta

Shore, Steven N.; Kuin, N. Paul; Mason, Elena; De Gennaro Aquino, Ivanhttp://adsabs.harvard.edu/abs/2018arXiv180707174SIt has recently been discovered that some, if not all, classical novae emit GeV gamma rays during outburst, but the mechanisms involved in the A fraction of classical novae form dust during the early stages of their outbursts. The classical CO nova V5668 Sgr (Nova Sgr. 2015b) underwent a deep photometric minimum about 100 days after outburst that was covered across the spectrum. A similar event was observed for an earlier CO nova, V705 Cas (Nova Cas 1993) and a less optically significant event for the more recent CO nova V339 Del (Nova Del 2013). This study pro-vides a "compare and contrast" of these events to better understand the very dynamical event of dust formation. We show the effect of dust formation on multiwavelength high resolution line profiles in the interval 1200\AA\ - 9200\AA\ using a biconical ballistic structure that has been applied in our previous studies of the ejecta. We find that both V5668 Sgr and V339 Del can be modeled using a grey opacity for the dust, indi-cating fairly large grains (at least 0.1 micron) and that the persistent asymmetries of the line profiles in late time spectra, up to 650 days after the event for V5668 Sgr and 866 days for V339 Del, point to the survival of the dust well into the transparent, nebular stage of the ejecta evolu-tion. This is a general method for assessing the properties of dust forming novae well after the infrared is completely transparent in the ejecta.

V1369 Cen High-resolution Panchromatic Late Nebular Spectra in the Context of a Unified Picture for Nova Ejecta

Mason, Elena; Shore, Steven N.; De Gennaro Aquino, Ivan; Izzo, Luca; Page, Kim; Schwarz, Greg J.http://adsabs.harvard.edu/abs/2018ApJ...853...27MNova Cen 2013 (V1369 Cen) is the fourth bright nova observed panchromatically through high-resolution UV+optical multiepoch spectros-copy. It is also the nova with the richest set of spectra (in terms of both data quality and number of epochs) thanks to its exceptional bright-ness. Here, we use the late nebular spectra taken between day ~250 and day ~837 after outburst to derive the physical, geometrical, and kine-matical properties of the nova. We com pare the results with those determined for the other panchromatic studies in this series: T Pyx, V339 Del (nova Del 2013), and V959 Mon (nova Mon 2012). From this we conclude that in all these novae the ejecta geometry and phenomenology can be consistently explained by clumpy gas expelled during a single, brief ejection episode and in ballistic expansion, and not by a wind. For V1369 Cen the ejecta mass (~1 × 10-4 Mꙩ and filling factor (0.1 ≤ f ≤ 0.2) are consistent with those of classical novae but larger (by at least an order of magnitude) than those of T Pyx and the recurrent novae. V1369 Cen has an anomalously high (relative to solar) N/C ratio that is be-yond the range currently predicted for a CO nova, and the Ne emission line strengths are dissimilar to those of typical ONe or CO white dwarfs.

Recent publications

Novae

Eruptive stars spectroscopyCataclysmics, Symbiotics, Novae

cataclysmics, symbiotics, novae - astrosurf

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