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L’Osservatorio Astronomico Monte Baldo "A.Gelodi", unico osservatorio pubblico della provincia di Verona, è di proprietà del Comune di Ferrara di Monte Baldo ed è gestito dal Circolo Astrofili Veronesi. L'orto botanico, intende promuovere la conoscenza dell’ambiente naturale baldense con visite, escursioni, attività didattiche, laboratori che trasmettano ai visitatori la grande ricchezza naturale, culturale, storica ed umana del territorio. Il Rifugio di Novezzina, ha riaperto da l'anno scorso con la nuova gestione della Cooperativa il Ponte. |
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APERTURA PUBBLICA Nessuna apertura pubblica in programmazione |
Il cielo non è mai stato così vicino
Circolo Astrofili Veronesi
ATTIVITA'____________________________________________ |
Aperture Pubbliche
Durante il periodo primaverile ed estivo sono organizzate una serie di aperture pubbliche aperte a tutti. Non serve prenotazione |
Visite gruppi privati
L'Osservatorio apre anche su prenotazione di gruppi privati per una esperienza unica tutto il periodo dell'anno... |
Visite Scuole
Visite per le scuole di ogni tipo e livello, con lezione e osservazione sia del Sole di giorno, sia degli oggetti celesti alla sera. |
Stage Astronomia
Lo stage di Astronomia per i ragazzi del IV anno delle scuole superiori è stata una esperienza formativa dell'astronomia dal 2012 al 2016 Per saperne di più... |
RICERCA SCIENTIFICA__________________________ |
Fotografia
da settembre 2005  Andrea Peretti Gianfranco Martini |
Meteor Hunter
da novembre 2005  Maurizio Carli |
Astrometria
da gennaio 2006  Guido RoccaFlavio Castellani |
Spettroscopia
da marzo 2006  Flavio Castellani Sergio Moltomoli Vittorio Andreoli Gabriele Zampieri |
Fotometria
da gennaio 2007  Flavio Castellani Raffaele Belligoli Claudio Marangoni |
Supernovae
da aprile 2011  Raffaele Belligoli Flavio Castellani Claudio Marangoni |
Pubblicazioni gruppo ricerca Osservatorio Monte Baldo
2024 TCP J17490276-2324066 (=ASASSN 24fb) is a highly reddened nova, of the FeII class, caught close to maximum brightness ATel #16727; U. Munari (INAF Padova), A. Farina (UniPD), A. Maitan, S. Dallaporta, V. Andreoli (ANS Collaboration). TCP J17490276-2324066 has been discovered by K. Itagaki on 2024 Juy 20.476 UT. It coincides with ASASSN 24fb discovered by the ASAS-SN survey on 2024 July 17.05 UT at a reported V=12.43 mag. Refined coordinates listed in CBAT-TOCP (averaging on end figures 02s.735, 05".5) coincides within 0.384 arcsec with a Gaia DR3 star of G=20.8 mag (no BP, RP listed). We have obtained BVRI transformed photometry of the transient with ANS Collaboration telescopes ID 0310 and 2202, with the results listed in the table below. The local photometric sequence has been extracted from the APASS DR8 survey, and the quote errors include quadratically the transformation uncertainty from color equations. Low resolution spectra (3600-8000 Ang, dispersion 2.31 Ang/pix) of TCP J17490276-2324066 have been recorded between July 20.851 and 20.909 UT with the Asiago 1.22m + B&C spectrograph. They are dominated by a very red continuum, in fine agreement with the V-J=+2.2 photometric color index in the table above, with superimposed broad emission lines of the Balmer series and FeII multiplets. The strongest FeII multiplets in emission are 55, 74, and 49 (all with P-Cyg absorption components), with multiplets 42 and 48 present at a significant lower intensity. No HeI lines are present and OI 7772 is present in weak emission and displays the strongest P-Cyg aborption of all, with a structurated profile, at an overall velocity -790 km/s and FWHM=560 km/s. The Halpha has a FWHM=1560 km/s with a sharp P-Cyg absorption of FWHM=530 km/s placed on its blue wing at velocity of -625 km/s with respect to the emission component, which is rather Guassian in shape. The integrated absolute flux of the Halpha emission component is 9.12E-12 erg/cm2/s. The Halpha/Hbeta flux ratio is 8.8. Overall, TCP J17490276-2324066 appears to be a classical nova, of the FeII type, caught close to maximum brightness, and suffering from a large reddening, possibly amounting to E(B-V)=1.5 mag as supported by the very strong interstellar atomic lines and diffuse interstellar bands, and the large Halpha/Hbeta ratio. TCP J00003597+1757408 (2024/07/11) Andreoli.V and Castellani.F report the classification of TCP J00003597+1757408. We obtained, From Monte Baldo Observatory (OMB) located in Novezzina (Italy), a low resolution spectra (7x600s), by 0.25-m telescope + Alpy600 spectrograph (dispersion 4.9 Ang/pix), on 2024-07-11.007 . The spectrum shows a blue continuum and absorption in H delta (4100 Ang) and H gamma (4340 Ang) while H beta (4861 Ang) and H alpha (6562.8 Ang) are not present in our spectrum, probably filled-up by a disk. All the characteristics are typical of CV stars. We propose the classification of TCP J00003597+1757408 as a CV star. TCP J02055218+1440593 (2024/01/26) Andreoli.V and Castellani.F reports a follow up of TCP J02055218+1440593. 6x300s (clear filter) images were obtained with the 0.4m telescope + Moravian G4 CCD full frame located at Osservatorio Monte Baldo in Novezzina (Italy), date 2024-01-26.875 (limit mag 19.3). A very weak object is present at coordinate 02:05:52.15 +14:40:59.5 in our image with an estimate magn. of 19.1. The luminosity is clearly decreased compared to that taken by XOSS our image can be found on https://photos.app.goo.gl/b1ZBhZffukQKMLiV8 2024aru (2024/01/24) TNS Classification Report No. 16468 Andreoli.V , Castellani.F and Vesentini.F report/s a classification of object: AT 2024aru Type: CV Remarks: Low resolution spectrum was obtained 0.25-m telescope + Alpy600 spectrograph (with dispersion 4.9 Ang/pix) located in Novezzina (Italy) on 2024-01-23.9375. The spectrum shows a blue continuum and a weak absorption of balmer lines expept Halpha (6562.8 Ang) that is no visible in our spectrum. B,V,R photometry was also collected with 0.4m telescope + Moravian G4 CCD full frame located in Novezzina (Italy) at 2024/01/23.9375 with results B=14.441, V=13.866, R=14.278; (B-V) =0.575; (V-R)=-0.414. A probable progenitor was found on ZTF with mag r of 19.6 (mean mag) this means that Δmag ≈ 5. All this feature are typically of a CV stars so we propose to classified TCPJ07593036+0459025 as a CV. The astrometric measurement was also made and giving the coordinates 07:59:30.33 +04:59:03.1 (the png of the spectrum is available on 2023 TNS Astronomical Transient Report No. 194448 Discovery certificate for object 2023yij IAU Designation: AT 2023yij Discoverer internal name: OMB-PNV21 Coordinates (J2000): RA = 00:42:45.870 (10.691125) DEC = +41:21:37.90 (41.360528) Discovery date: 2023-11-23 19:11:12.000 Potential host galaxy: M31. Host redshift: -0.001 Flavio Castellani report the discovery by F.Castellani, R.Belligoli,and V.Andreoli of a PNV (Mag. 19.1R +-0.2 – USNOA2 catalogue) in the host galaxy M31 at Monte Baldo Observatory, Ferrara di Monte Baldo, Verona, Italy (A99), in the course of Italian Supernovae Search Project using a 0.40m f/8 Ritchey-Chretien telescope (+ Moravian G4-9000 KAF CCD unfiltered CCD camera). No stellar source is visible at the position of the transient in our past images including reference image dated 2023-11-22 19:05:27 (AT2023yij) AT2023ylu TCP J20315286+2740166 Andreoli.V ; Ochner.P : Castellani.F, Cazzola.R reports a spectroscopic classification of TCP J20315286+2740166. Low resolution spectra was obteined by 1.22-m tlescope + B&C spectrograph (with dispersion 2.25 Ang/pix) located in Asiago (Italy) on 2023-11-12.788 and with 0.25-m tlescope + Alpy600 spectrograph (with dispersion 4.9 Ang/pix) located in Novezzina (Italy) on 2023-11-12.823, the spectra show emission of Halpha (6562.8 Ang) and [O I] (5577 Ang), absorption of Hbeta, Hdelta, Hgamma, Hepsilon and He I (4471 Ang) and has a blue continuum. Considered d=0.406 kpc from the 3D dust mapping (Green et al 2019) get E(B-V)≈0.00 B,V,R photometry was also collected with 0.4m telescope + Moravian G4 CCD full frame located in Novezzina (Italy) at 2023/11/12.788 with results B=13.961, V=13.466, R= 13.036 , (B-V)0 =0.495 . Gaia DR2 1857057959447151616 is also present in ZTF database at magnitude 17.9 (filter zg) that’s means Δmag ≈ 5 mag (referring to the magnitude of discovery) All this feature are typically of a dwarf nova outburst, so a classification as dwarf nova was proposed. TCP J06333486-2305449 Transient Object Followup Reports Andreoli.V, Vagnozzi.A, Castellani.F and Ochner.P obtained low resolution spectrum at 2023/11/02.022 with 0.5m telescope + MARK III spectrograph (resolution 2.74 Ang/pix ,self-build) located in Stroncone (Italy), Hight resolution spectrum with 1.22m telescope + B&C spectrograph (resolution 0.6 Ang/pix) at 2023/11/01.118 and 2023/11/4.132. Spectra shows a blue continuum, no evidence of Hα (6562.8 Ang) probably filled by accretion disk the other Balmer absorptions are presents. Hβ shows an FWHM of 2639 km/s . Also emission of O I (5577 Ang) and He I (4922 Ang) are clearly present in the low resolution spectrum. Considered d=0.2876 kpc from the 3D dust mapping (Green et al 2019) get E(B-V)≈0.005 B,V,I photometry was also collected with 0.25-m f/3.4 reflector + SBIG ST-10XME (T05 - iTelescope.NET) at 2023/11/02.358 with results B=12.879 ±0.047 , V=12.903 ± 0.033 and I= 12.953 ± 0.058 , (B-V)0 = -0.02 . Also considering the light curve reported by AAVSO which shows a "rapid" variation where 90 minutes pass between one maximum and the next within a slower decline. Gaia DR3 2924954955730613376 is also present in ZTF database at magnitude 19 (filter zr) that’s means Δmag ≈ 6.5 All this feature are compatible of WZ Sge stars so a classification as a dwarf nova WZ Sge type was proposed. (TCP J06333486-2305449) TNS Astronomical Transient Report No. 192558 Discovery certificate for object 2023wnh IAU Designation: AT 2023wnh Discoverer internal name: OMB-TNS01 Coordinates (J2000): RA = 00:43:48.700 (10.952917) DEC = +41:32:43.90 (41.545528) Discovery date: 2023-11-03 19:04:14.000 Potential host galaxy: m31 Transient observed By F.Castellani, R.Belligoli and V.Andreoli, in the course of Italian Supernovae Search Project using a 0.40m f/8 Ritchey-Chretien telescope (+ Moravian G4-9000 KAF CCD unfiltered CCD camera). No stellar source is visible at the position of the transient in our past images including reference image dated 15Th sept 2023. The transient has been already detected by Zwicky Transient Facility as ZTF23abighaj. (AT2023whn) Spectroscopic analysis of the binaries systems Epsilon Herculis and HIP107162 Andreoli.V;Nogara.M3;Grazioli.M.G;Castellani.F; Vagnozzi.A;Penayo.M1;Moltomoli.S;Zampieri.G;Pomari.C Remarks: During the 2022 internship involving a group of high school students at the Monte Baldo Astronomical Observatory (hereafter referred to as OMB) in Ferrara di Monte Baldo, Verona, Italy, the two stellar systems of HIP107162 and Eps Her were observed, and high and low-resolution spectroscopic analysis was conducted. The construction of the radial velocity curve allowed for the determination of the binary systems’ structure, while the low-resolution spectra enabled the identification of present elements and consequently their spectral classification. See more (20230608-ArticoloStage2022) TNS Classification Report No. 14816 classification of object: AT 2023gfj Andreoli.V ; Castellani.F reports the classification of object AT 2023gfj. We obtained, From Monte Baldo Observatory (OMB) located in Novezzina (Italy), low resolution spectra by 0.25-m telescope + Alpy600 spectrograph (dispersion 4.9 Ang/pix) on 2023-04-26.851 (4x300s), on 2023-04-27.828 (3x300s) and V (Jhonson) photometry with 0.4m telescope + Moravian G4 CCD full frame on 2023-04-27.828 . Photometry reduction give V mag 12.8. The spectra show red continuum and TiO molecular bands ( 4760, 4954 ,4956 ,5448 ,5450 ,5847 ,6149 ,6357 ,6714 ,7087 Ang) typically feature of M-type stars. V mag and spectral features are correspondent with the near star ROSS 619 that have a very high proper motion (1069 , -5094) mas/yr in module 5204 mas/yr. If we assume that ROSS 619 is 2023gfj then the distance from the coordinates reported on SIMBAD (Wenger.M et al, 2000) by the coordinates presented on the TNS N°175337 is 2.4’ (144 arcsec) , this distance has been travelled in 27.67 years. This time scale is consistent with our hypothesis. We propose that the transient 2023gfj is ROSS 619 in the new position. TNS Classification Report No.14539 Classification of object: AT2023dez Remarks: Andreoli.V ; Castellani.F report/s a classification of object: AT 2023dez. Low resolution spectrum (6 X 600s) was obtained on 2023-03-17.802 from Osservatorio Monte Baldo located in Novezzina (Italy) by 0.25-m telescope + Alpy600 spectrograph (with dispersion 4.9 Ang/pix). The spectrum shows H-alpha emission (6562.8 Ang), a weak absorpion of H-beta (4861.03) problably filled up by the accretion disk and strong absorpions of the other Balmer lines and He I (4471;4922;5876 Ang). It also shows interstellar NaI D1,D2 (5885,5890 Ang). These features belong to a type Be Herbig star. Furthermore the coordinates are coincident to LS I+56 76, object prensent in the Catalog of galactig OB stars (Reed 2003). We propose the identification for this transient as a Be star. TNS Classification Report No.14508 Classification of object: AT2023cub Remarks: Andreoli.V ; Castellani.F ; Vesentini.F report/s a classification of object: AT 2023cub. Low resolution spectrum (5 X 600s) was obtained by 0.25-m telescope + Alpy600 spectrograph (with dispersion 4.9 Ang/pix) located in Novezzina (Italy) on 2023-03-09.792. The spectrum shows red continuum and absorption of H-alpha (6562.825 Ang), H-Beta (4861.03 Ang), D1,D2 Na doublet (5885;5890 Ang) and Ca I (4302 Ang) ; also the coordinates are coincident to V*520Mon (MAXI J0655-013) and at these coordinates an hard X-ray was detected (Serino et al. ATel #15442). We propose the identification of the transient as a brightness of the X-ray variable. (Classification-cert) (AT2023cub) TNS Classification Report No.14413 Classification of object: AT2023bne Remarks: Flavio Castellani, Claudio Balcon and Vittorio Andreoli reports: We obtained BVRI photometry of PNV J01345297+3047145 (AT 2023bne) with 0.4m telescope + Moravian G4 CCD full frame located in Novezzina (Italy), date 2023/02/11.7868 B=17.11 ; V=17.04 ; R=17.01 ; I=16.84 (Vphot AAVSO photometry tool). Color index B-V=0.07 is similar to cataclysmic variable (CV) Z Cam B-V=0.05 (Bruch 1984) at maximum. We also obtained two low resolution spectra (2x2400s , R=100) by 0.2m telescope on 2023-02-11.772 UT, the spectrum shows a blue continuum with no features above noise level. These characteristics are compatible with those of a CV in outburst. (Classification-cert) (AT2023bne) TNS Astronomical Transient Report No.168720 Discovery certificate for object 2023ps Remarks: F.Castellani, R.Belligoli, V.Andreoli, C.Marangoni, OMB extragalactic nova monitoring by ISSP collaboration reports the discovery of a probable nova in M31. The transient designated also PNV J00424623+4117357. New transient was clearly detected on '2023 1 14,7674' UT using 16 x 300s frames (4800s total) obtained by a Moravian G4-9000 KAF unfiltered CCD with the 0.4m f.8 Ritchey-Chrétien telescope from Monte Baldo "A.Gelodi" Astronomic Observatory, località Novezzina, Ferrara di Monte Baldo, Verona, Italy. The discovery magnitude is 19.3±0.5 mag in the CV band (clear visual). Offset 25" Est e 90" Nord from M31 galactic centre. The new transient is close to Globular Cluster M31GC J004246+411737 (1.78"). (AT2023ps) Spectroscopic Observation of the Dwarf Nova PNV J00215475+5231007 Remarks:V.Andreoli, A.Vagnozzi. Also, weak absorption lines of Hα, Na I, and Mg II are seen. Therefore, my spectrum is consistent with the report on CBAT by V. Andreoli & A. Vagnozzi, confirming their classification as a cataclysmic variable. According to the photometric observations by S. Kiyota, H. Itoh, and the Kyoto U team, this object is likely a WZ Sge-type dwarf nova (vsnet-alert 27305 & 27306). 2022 TNS Astronomical Transient Report No.154172 Discovery certificate for object 2022qpg Remarks: R.Belligoli, F.Castellani, V.Andreoli, C.Marangoni, OMB extragalactic nova monitoring with ISSP collaboration, reports the discovery of a probable nova in M31. Offset 1091E 425N. It should be noted that in the same position a optical transient TSS J004420.7 + 412311 was reported ATel #627; R. Quimby, M. Sellers, P. Hoeflich, J. C. Wheeler (University of Texas), and C. Gerardy (Imperial College) on 12 Oct 2005; 19:30 UT. The transient designated also PNV J00442079+4123111; AT2022qpg A new outburst of the symbiotic star V919 Sgr, again 15 yrs past the previous one ATel #15528; U. Munari (INAF Padova), A. Vagnozzi, A. Maitan, F. Castellani, M. Graziani (ANS Collaboration), P. Ochner, A. Reguitti (Padova Univ.) on 25 Jul 2022; 15:44 V919 Sgr is a bright symbiotic star, of the burning type, which is largely ignored by observers. Its first known outburst in 1991-92 was described by Ivison et al. (1993, A&A 277, 510), with a second one in 2007 reported by Munari et al. (2007, CBET 999). V919 Sgr is currently again in outburst, as also noted by B. Monard in vsnet-alert N. 26878. The three recorded outburst are separated by similar ~15 yrs intervals. (ATel15528)(PDF) TNS Astronomical Transient Report No. 140016 Discovery certificate for object 2022eqj Remarks: F.Castellani, R.Belligoli, V.Andreoli, C.Marangoni, OMB extragalactic nova monitoring with ISSP collaboration, reports the discovery of a probable nova in M31. The coordinates of the new transient are only 0.5 arc/sec from Nova Bryan 1990A/M31N2007-07a The transient designated also PNV J00430406+4117080 ; AT2022eqj TNS Astronomical Transient Report No. 139430 Discovery certificate for object 2022elz Remarks: Flavio Castellani report the discovery by F.Castellani, R.Belligoli, V.Andreoli of a PNV (Mag.19.5R +-0.2 - USNOB1 catalogue) in the host galaxy M81 at Monte Baldo Observatory, Ferrara di Monte Baldo, Verona, Italy (A99), in the course of Italian Supernovae Search Project using a 0.40m f/8 Ritchey-Chretien telescope (+ Moravian G4-9000 KAF CCD unfiltered CCD camera). No stellar source is visible at the position of the transient in our past images including reference image dated 02 March 2022. PNV J09552559+6907558 2021 Nova TCP J20210770+2914093 turns into an FeII-type as it keeps rising in brightness ATel #14816; U. Munari (INAF Padova), S. Moretti, A. Maitan, V. Andreoli (ANS Collaboration) The transient TCP J20210770+2914093 was discovered by K. Itagaki on 2021 Jul 16.492 UT at unfiltered magnitude 12.0, and classified as a nova by Munari et al. (ATel #14793) based on a spectrum taken on July 17.102 UT. This initial spectrum resembled novae of the He/N type, with Balmer, HeI, and NII lines present in emission. However, Munari et al. (ATel #14793) warned that with the nova possibly still progressing toward maximum light, the spectral type could evolve toward the FeII type. This has been indeed what happened and here we report about the evolution of the nova during the last two weeks. Spectroscopic follow-up observations of Nova Herculis 2021 ATel #14718; I. Albanese, A. Farina, V. Andreoli, P. Ochner (UniPd), A. Reguitti (UNAB) We report spectroscopic follow-up observations of Nova Herculis 2021 (TCP J18573095+1653396). It was discovered by Seiji Ueda on 2021-06-12.548 UT and spectroscopically classified as a classical nova by Munari et al. 2021 (ATel #14704). We obtained a low-resolution spectrum with Monte Baldo Observatory 0.25-m Telescope + Alpy 600 spectrograph (380-800 nm, 0.497 nm/px) on 12/06/2021 and 13/06/2021, and a medium resolution spectrum with Asiago 1.22-m 'Galileo' telescope + B&C spectrograph (460-700 nm, resolution 0.25 nm) on 13/06/2021. (ATel14718) (PDF) Photometry and spectroscopy of the 2021 outburst of the symbiotic star YY Her ATel #14464; U. Munari (INAF Padova), P. Ochner (Univ. Padova), S. Dallaporta, G. L. Righetti, M. Graziani, F. Castellani, A. Maitan, S. Moretti, (ANS Collaboration), and N. Masetti (INAF Bologna) The symbiotic star YY Her has just been announced in outburst (ATel #14458), based on unfiltered telephoto lens images taken on March 15.006 UT during the New Milky Way survey for transients. (ATel14464) (PDF) 2020 Nova Cas 2020 (=V1391 Cas) is likely forming dust U. Munari (INAF Padova), D. P.K. Banerjee (PRL, India), F. Castellani, S. Dallaporta, A. Maitan, and A. Vagnozzi (ANS Collaboration) The brightness of the nova has dramatically dropped over the last couple of days with a marked reddening of colors. The presence of a faint and nearby field star, just a few arcsec away from the nova, now requires that the photometry be performed via PSF- fitting. The night values, averaged over PSF-fitting measurements from data that we collected with ANS Collaboration telescopes...(Atel14267) (PDF) Classification of TCP J04291884+4354232 as a classical nova U. Munari (INAF Padova), F. Castellani, S. Dallaporta, V. Andreoli (ANS Collaboration) We have obtained low-resolution spectroscopy of the transient TCP J04291884+4354232 with a 25cm telescope + Alpy600 on Nov 26.05 UT. The spectrum shows broad Balmer emission lines with deep P-Cyg as typical of a nova close to maximum brightness. (Atel14224) (PDF) Spectroscopic confirmation and photometry of the recent nova M31 2020-11c (AT 2020yye) (= OMB-PNV12) (= PNV J00431316+4124562) S. Fabrika, O. Sholukhova, A. Sarkisyan, A, Vinokurov, Yu. Solovyeva (SAO RAS), A. W. Shafter (SDSU), A. Valeev (SAO RAS) We report optical spectroscopic confirmation of the nova M31 2020-11c (PNV J00431313+4124567) announced in ATel #14155. (Atel14217) (PDF) The optical counterpart of the X-ray source 2SXPS J173508.4-292958 is a new, yellow-type symbiotic star. U. Munari (INAF Padova), P. Valisa, S. Dallaporta, A. Vagnozzi, V. Andreoli, F. Castellani (ANS Collaboration) With an assortment of telescopes operated by ANS Collaboration, we have obtained optical spectroscopy (low and high resolution) and BVRI photometry of the optical counterpart of 2SXPS J173508.4-292958, the source recently reported by Heinke et al. (ATel #13648) to have brightened in the X-rays. (Atel13660) (PDF) LAMOST J202629.80+423652.0 is not a symbiotic star - V. Andreoli and U. Munari Abstract. LAMOST J202629.80+423652.0 has been recently classi ed as a new symbiotic star containing a long-period Mira, surrounded by dust (D- type) and displaying in the optical spectra high ionization emission lines, in- cluding the Raman-scattered OVI at 6825 A. We have observed LAMOST J202629.80+423652.0 photometrically in the BVRI bands and spectroscopically over the 3500-8000 A range. (CAOSP Vol.50) (PDF) The OMB-supernova monitoring (ISSP collaboration), R.Belligoli, F.Castellani, C.Marangoni, F.Marziali reports the discovery of a PSN J16393220+6602141 SN2020gpe in NGC6214 by a Moravian G4-9000 KAF unfiltered CCD frames taken on '2020-04-12T03:21:49' UT on the 0.4m f.8 Ritchey-Chrétien telescope. The object observed is located at RA= '16 39 32.19' DEC= '+66 02 14.01' (equinox 2000.0) Offset 2"W 9"S from the center of NGC6214 galaxy (see link to discovery image below). Apparent magnitude 17.0 Clear (err +/- 0,5). (Atel13640) (PDF) We report the independent discovery of a probable nova in M31 on a co-added 810-s R-band CCD frame taken on 2020 Mar. 15.768 UT with the 0.65-m telescope at Ondrejov. The object was independently discovered and first announced by F. Castellani and R. Belligoli and designated as PNV J00424612+4111362 = AT 2020emi. The object was designated by us as M31N 2020-03c and is located at R.A. = 0h42m52s.16, Decl. = +41o13'37".2 (equinox 2000.0), which is 88.4" east and 151.3" south of the center of M31 ... (ATel_13561) (PDF) Remarks: F. Castellani, Verona, Italy reports the discovery by Flavio Castellani, Raffaele Belligoli and Claudio Marangoni, in the course of the ISSP Italian Supernovae Search Project, of an apparent nova in two images taken with a Moravian G4-9000 KAF CCD unfiltered, from Monte Baldo Observatory (Ferrara di Monte Baldo, Verona, Italy), with the 0.4m f.8 Ritchey-Chrétien telescope, obtained on 2020 March 04.7596. The new object is located at RA 00 42 08.56 DEC +41 26 00.8 (equinox 2000.0) Apparent magnitude about 18.0 in host Galaxy M31 Nothing is visible at this position on the reference image taken on 2020-02-28.769... (TNS Astronomical Transient Report No. 63512) 2019 The 2018 eruption and long-term evolution of the new high-mass Herbig Ae/Be object Gaia-18azl = VES 263 MNRAS U. Munari, V. Joshi, D. P. K. Banerjee, K. Cotar, S. Y. Shugarov, R. Jurdana-Sepi, R. Belligoli, A. Bergamini, M. Graziani, G. L. Righetti, A. Vagnozzi and P. Valisa We have been monitoring, at high cadence, the photometric and spectroscopic evolution of VES 263 following the discovery in 2018 of a brightening labelled as event Gaia-18azl. VES 263 is so far a neglected emission-line object discovered in the 1960s on objective prism plates, tentatively classified as a semiregular AGB cool giant by automated analysis of ASASSN light curves. We have discovered that VES 263 is a bona fide massive pre-mainsequence object (∼12 M), of the Herbig AeBe type. (MNRAS 488, 5536–5550 (2019) (PDF) 2018 Liverpool Telescope classification of optical transients AT2018hho and AT2018hhy ATel #12138; S. C. Williams (Lancaster), M. J. Darnley (LJMU), M. W. Healy (LJMU) on 22 Oct 2018; 22:36 UT Credential Certification: Steven Williams (s.williams7@lancaster.ac.uk) A faint continuum is detected in each case, but the S/N is too low for a classification. AT2018hho was observed at 2018-10-16.94 UT. We detect a Hα emission line with FWHM ~ 3100 km/s. We obtained a spectrum of AT2018hhy at 2018-10-17.99 UT, which shows TiO absorption bands on a red continuum, indicating that this object is a red LPV. We also note that there is a variable coincident with the position of AT2018hhy in Macri et al. (2001) and Hartman et al. (2006). (Atel_12138) (PDF) Independent INT/WFC discovery, improved position and IAC80/CAMELOT photometry of AT2018hho (= PNV J00424012+4117273) in M31 ATel #12127; Credential Certification: Ismael Perez-Fournon (ipf@iac.es) We report the independent discovery of a nova candidate in M31 on CCD images taken from 2018 Oct 13.937 to 2018 Oct 14.176 with the Wide Field Camera of the Isaac Newton Telescope. The discovery of this nova candidate was reported to TNS by Raffaele Belligoli, Flavio Castellani and Claudio Marangoni. We also observed AT2018hho with the CAMELOT CCD camera of the IAC80 telescope at Teide Observatory in Tenerife on the same night. (Atel_12127) (PDF) Independent Discovery of PNV J00424012+4117273 and Confirmation of PNV J01334673+3032181 ATel #12113; K. Hornoch (Astronomical Institute, Ondrejov, Czech Republic) on 15 Oct 2018; 07:55 UT Credential Certification: Matt Darnley (M.J.Darnley@ljmu.ac.uk) I report the independent discovery of a probable nova in M31 on a co-added 770-s R-band CCD frame taken on 2018 Oct. 14.740 UT with the 0.65-m telescope at Ondrejov. The object was independently discovered by R. Belligoli et al. (designated as PNV J00424012+4117273 = AT2018hfs) and is located at R.A. = 0h42m40s.11, Decl. = +41o17'26".9 (equinox 2000.0), which is 47.5" west and 78.4" north of the center of M31. (Atel_12113) (PDF) The Mass Accretion Rate of the Young Variable Star GM Cep Authors: Giannini, T.; Munari, U.; Lorenzetti, D.; Antoniucci, S.; Castellani, F.; Dallaporta, D.; Jurdana-Šepić, R. Affiliation: AA(INAF—Osservatorio Astronomico di Roma—Via Frascati, 33—Monte Porzio Catone I-00078, Italy Electronic On-line Article (HTML) - (PDF) The super-soft X-ray and CH/Ba-enhanced symbiotic star StHa 32 is in outburst ATel #11304; U. Munari (INAF Padova), S. Dallaporta, M. Graziani, G. L. Righetti, S. Tomaselli, S. Moretti, A. Maitan, F. Castellani, P. Valisa, L. Baldinelli (ANS Collaboration) on 15 Feb 2018; 11:12 UT Credential Certification: U. Munari (ulisse.munari@oapd.inaf.it) The supersoft X-ray source, Barium-enhanced, metal-deficient and Halo symbiotic star StHa 32 in going into outburst, the first ever recorded to the best of our knowledge.(ATel_11304) Asiago spectroscopic classification of 3 transients The Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) reports the spectroscopic classification of AT 2018eq discovered by R. Belligoli (ISSP) in the direction of M31; PS18bq (AT2018bi) discovered by J. Grzegorzek and Pan-STARRS1 in UGC1791; and AT2018C (= Gaia18aak), a blue hostless transient discovered by Gaia. The observations were performed with the Asiago 1.82 m Copernico Telescope equipped with AFOSC (range 340-820 nm; resolution 1.4 nm).(ATel_11168) 2017 Spectroscopic classification AT 2017jdm as a nova, and likely recurrent eruption of M31N 2007-10b We obtained a spectrum of the transient AT 2017jdm (discovered by F. Castellani, R. Belligoli, C. Marangoni and F. Marziali; see TNS) with the SPRAT spectrograph (resolution R ~ 350; Piascik et al. 2014) on the 2-m Liverpool Telescope (Steele et al. 2004) on 2017 Dec 24.86 UT. (Atel_11088) A sudden brightness decrease of the young pre-MS object GM Cep U. Munari (INAF - Osservatorio Astronomico di Padova, Italy), F. Castellani (ANS Collaboration, Italy), T. Giannini, S. Antoniucci, D. Lorenzetti (INAF - Osservatorio Astronomico di Roma, Monte Porzio, Italy) on 24 Nov 2017; 14:38 UT Credential Certification: Simone Antoniucci (antoniucci@oa-roma.inaf.it) (Atel_11004) Nova ASASSN-17hx fast returning to maximum brightness, now at much larger velocities U. Munari (INAF Padova), P. Ochner (Univ. Padova), F.-J. Hambsch, A. Frigo, F. Castellani, A. Milani, P. Valisa, A. Vagnozzi (ANS Collaboration) on 11 Sep 2017; 21:54 UT Credential Certification: U. Munari (ulisse.munari@oapd.inaf.it) Nova ASASSN-17hx continues its unexpected and rapid re-brightening (ATel #10725), approaching the brightness attained at primary maximum when it peaked at B=9.65, V=8.44, R=7.79, I=7.05 around July 30.1 UT (ATel #10641)... (ATel_10736) "Photometry and spectroscopy of declining Nova ASASSN-17hx, now passing at t_2" U. Munari (INAF Padova), G. Traven (Univ. Ljubljana), F.-J. Hambsch, F. Castellani, A. Frigo, A. Milani, P. Valisa (ANS Collaboration), P. Ochner (Univ. Padova) ASASSN-17hx was discovered (Atel #10524) when still >4 mag below and ~41 days before maximum. Spectral classification and pre-maximum evolution have been reported (Atel #10527, #10558, #10572, #10613), as well as the identification in the VVVX survey of a Ks=16.7 mag star as the likely progenitor of the nova, and recently UV observations and an upper limit to X-ray flux obtained with Swift (Atel 10636) (ATel_10641) "Photometry and spectroscopy of FeII nova ASASSN-17hx, finally passing through maximum" U. Munari (INAF Padova), F.-J. Hambsch, A. Frigo, F. Castellani (ANS Collaboration),G. La Mura (Univ. Padova), G. Traven (Univ. Ljubljana), M. Ozbey Arabaci, T. Saguner (Ataturk Univ.) on 13 Jul 2017; 10:08 UT Credential Certification: U. Munari (ulisse.munari@oapd.inaf.it) More than two weeks past its discovery, nova ASASSN-17hx has finally reached what appears to be its peak optical brightness. Announced as a candidate nova on June 23.7 UT (ATel #10523), we begun daily photometric monitoring of ASASSN-17hx on June 24.07 UT when we measured V=12.39, B-V=+0.72, V-I=+1.19. After a monotonic - although structured - rise toward maximum, peak brightness has been reached at V=10.90, B-V=+0.85 on June 10, followed by a slow decline. (ATel_10572) After 23 years the yellow symbiotic star LT Del is again in outburst U. Munari (INAF Padova), P. Ochner (Univ. Padova), S. Dallaporta and R.Belligoli (ANS Collaboration) The ANS Collaboration photometric and spectroscopic monitoring of symbiotic stars has detected LT Del (= Hen 2467 = PK 06312.1 = StHa 179) in outburst. This is the first recorded outburst since the last one of 19941995, which was discovered by Passuello et al. (1994, IAUC 6065 ) and described by Arkhipova et al. (1995a, ALett 21, 339; 1995b, ALett 21, 391). LT Del is steeply rising in brightness. Last ANS photometric observation on UT (ATel 10361) NOVA 2017-04b (= PNV J09551279+6900093) IN M81 The extended M81 nova monitoring collaboration reports the discovery of a probable nova in M81 on pair of co-added 3900-s and 4200-s unfiltered CCD frames taken on 2017 Apr. 18.799 UT and 18.848 UT, respectively with the 0.4-m telescope at the Monte Baldo Observatory, Verona, Italy (MBO). The object designated PNV J09551279+6900093 is located at R.A. = 9h55m12s.79, Decl. = +69o00'09".3 (equinox 2000.0), which is 109.4" west and 225.8" south of the center of M81 (see link to discovery image below). (see link to discovery image). Atel#10290 NOVA AT2017blf in M81 The M81 nova monitoring collaboration reports the independent discovery of an apparent nova in M81 on a coadded 3510s unfiltered CCD frame taken on 2017 Feb. 24.119 UT with the 0.65m telescope at Ondrejov.The object designated PNV J09563149+6907301 was first announced and designated AT2017blf by F. Castellani et al. (see here) and is located at R.A. = 9h56m31s.49, Decl. = +69o07'30".1 (equinox 2000.0), which is 312.1" east and 215.0" north of the center of M81 (see link to discovery image below). Atel#10133 NOVA AT2017axz in M81 The M81 nova monitoring collaboration reports the independent discovery of an apparent nova in M81 on a co-added 5400-s unfiltered CCD frame taken on 2017 Feb. 19.962 UT with the 0.65-m telescope at Ondrejov (OND). The object designated PNV J09553619+6906210 was first announced and designated AT2017axz by F. Castellani et al. NOVA AT2017axi in M31 Nova M31 2017-02a? (= AT2017axi), TNS discovered 2017/02/18.746 by Raffaele Belligoli et al.(ISSP) Found in M31 at R.A. = 00h42m38s.120, Decl. = +41°14'10".70 Located 3".0 east and 115".0 south of the center of M31 (Discovery image) (ISSP image) Mag 18.3:2/18, Type unknown (References: CBAT TOCP) 2016 The 2016 outburst of the unique symbiotic star MWC 560 ( = V694 Mon), its long-term BVRI evolution and a marked 331 days periodicity U. Munari, S. Dallaporta, F. Castellani, L. Baldinelli, G.L. Righetti, M. Graziani, G. Cherini, A. Maitan, S. Moretti, S. Tomaselli, A. Frigo BVRI photometry obtained in 357 nights distributed between 2005 and 2016. Analysis of the long term photometric evolution and of the record breaking 2016 outburst. Detection of strong periodicities at 331 and 1860 days, and their relation to orbital period. New Astronomy 49, PDF. MASTER Independent Detection: Possible Nova in M31 After our detection we found discovery information at Bishop pages by Emmanuel Conseil (see at TNS https://wis-tns.weizmann.ac.il/object/2016jbx ) Atel#9912 Indipendent and prediscovery nova AT2016jbx by R.Belligoli, F.Castellani, C.Marangoni and F.Marziali on TNS UAI AT2016jbx. Confirmation and Photometry of M31 Transients AT2016jbg and AT2016ize Roughly 2.9' almost directly west of AT2016jbg lies the transient AT2016ize, reported to the IAU-TNS by Belligoli et al. on 2016 December 21.7139 UT with an unfiltered magnitude of 18.5 from observations conducted with ISSP. ATel#9915 NOVA AT2016ize in M31 The object designated PNV J00424659+4116578 was first announced and designated AT2016ize by R. Belligoli et al. (see here) and is located at R.A. = 0h42m46s.59, Decl. = +41o16'57".8 (equinox 2000.0), which is 25.5" east and 49.3" north of the center of M31 (see link to discovery image below). Atel#9896 Congratulations! Your paper is one of the 5 most highly cited papers published in New Astronomy. Dear Dr. Munari, The editors of New Astronomy are delighted to inform you that your paper, BVRI lightcurves of supernovae SN 2011fe in M101, SN 2012aw in M95, and SN 2012cg in NGC 4424, published in 2013 is one of the most highly cited papers during 2014, 2015 and up until June 2016. We would like to take this opportunity to thank you for publishing with us and to congratulate you. See more... The 2016 outburst of the unique symbiotic star MWC 560 ( = V694 Mon), its long-term BVRI evolution and a marked 331 days periodicity U. Munari, S. Dallaporta, F. Castellani, L. Baldinelli, G.L. Righetti, M. Graziani, G. Cherini, A. Maitan, S. Moretti, S. Tomaselli, A. Frigo NewAstronomy_49_43.pdf SUPERNOVA AT2016bry IN UGC 11635 The Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) reports the spectroscopic classification of AT2016bry, discovered by V. Tinella in UGC 11635, and preliminary photometric follow-up. Additional CCD magnitudes for AT2016bry: 2016-04-27.35 | Bj 15.87 +- 0.02 | Vj 15.57 +- 0.01 | Rc15.17 +- 0.01 (R. Belligoli, F. Castellani, Verona, Italy) ATel#9018; (2016) 2015 SUPERNOVA 2015Q IN NGC 3888 = PSN J11473508+5558147 Additional CCD magnitudes for 2015Q: 19.905, 16.3 (R. Belligoli, F. Castellani, and C. Marangoni, Verona, Italy) "The symbiotic binary and super-soft X-ray source AG Dra is going into outburst" U. Munari (INAF Padova-Asiago), G. L. Righetti, U. Sollecchia, F. Castellani (ANS Collaboration) 2014 “The symbiotic star Hen 2-468 is undergoing a rare and bright outburst” U. Munari (INAF-Padova), S. Dallaporta and F. Castellani (ANS Collaboration) "The prototype symbiotic star AX Per is in outburst" U. Munari (INAF Padova-Asiago), S. Dallaporta, G. L. Righetti, F. Castellani, G. Cherini (ANS Collaboration) Study of three 2013 novae: V1830 Aql, V556 Ser and V809 Cep U. Munari, P. Ochner, S. Dallaporta, P. Valisa, M. Graziani, G.L. Righetti, G. Cherini, F. Castellani, G. Cetrulo and A., Englaro NOVA SCORPII 2014 = TCP J17154683-3128303 U. Munari, S. Dallaporta, F. Castellani, R. Belligoli Electronic Telegram No. 3841* NOVA CYGNI 2014 = PNV J20214234+3103296 U. Munari, G. Cetrulo, D. Degano, and F. Castellani Electronic Telegram No. 3842* Optical photometry of the rapidly declining Nova Scorpii 2014 U. Munari (INAF Padova-Asiago), S. Dallaporta, F. Castellani, C. Marangoni (ANS Collaboration) on 1 Apr 2014; 09:05 UT Credential Certification: U. Munari (ulisse.munari@oapd.inaf.it) Nova Scorpii 2014 was discovered as optical transient TCP J17154683-3128303 by Nishiyama and Kabashima, and classified from optical spectra as a nova by Jelinek et al (ATEL #6025). X-ray emission was detected on Swift observations by Kuulkers et al. (ATEL #6015),... (ATel_6034) NOVA CEPHEI 2014 = TCP J20542386+6017077 SUPERNOVA 2014J IN M82 = PSN J09554214+6940260 U. Munari, F. Castellani, R. Belligoli, G. L. Righetti The symbiotic star TX CVn has entered an active state. U. Munari, F. Castellani, P. Valisa, S. Dallaporta, G. Cherini, A. Vagnozzi, G. L. Righetti, R. Belligoli The Metrology of Supernova Lightcurves 223rd American Astronomical Society Meeting Authors: Rust, Bert W.1; Mullen, Katharine M.2 Institutions: 1. NIST, Gaithersburg, MD, United States. 2. UCLA, Los Angeles, CA, United States. 3. ANS Collaboration: U.Munari, Italia 2013 SUPERNOVA 2013ff IN NGC 2748 = PSN J09133888+7628108 Belligoli R, Castellani F. Photometric evolution, orbital modulation and progenitor of Nova Mon 2012. Munari, U., Dallaporta, S., Castellani, F., Valisa, P., Frigo, A., Chomiuk, L., Ribeiro, V.A.R.M. An ongoing active phase for the old symbiotic nova AG Peg Munari, U., Valisa, P., Dallaporta, S., Cherini, G.L. Righetti, G., Castellani, F. ATel 5258 (2013) BVRI lightcurves of supernovae SN 2011fe in M101, SN 2012aw in M95, and SN 2012cg in NGC 4424. Munari, U., Henden, A., Belligoli, R., Castellani, F., Cherini, G., Righetti, G.L., Vagnozzi, A. Nova Cephei 2013 has emerged from dust obscuration U. Munari, P. Ochner, A. Siviero, M. Graziani, S. Dallaporta, G. L. Righetti, G. Cherini, F. Castellani An ongoing active phase for the old symbiotic nova AG Peg Munari, U., Valisa, P., Dallaporta, S., Cherini, G.L. Righetti, G., Castellani, F. ATel 5258 (2013) The symbiotic star YY Her is in outburst Munari, U., Dallaporta S., Castellani F., Belligoli R., Cherini G., Righetti G.L., Graziani M., Valisa P., Milani A. Is Nova Cep 2013 currently forming dust ? Munari, U., Dallaporta, S., Cherini, G., Castellani, F., Cetrulo, G., Valisa, P., Graziani, M. The decline of the super-soft X-ray source in Nova Mon 2012. Page, K.L., Osborne, J.P., Munari, U., Wagner, R.M., Beardmore, A.P., Castellani, F., Dallaporta, S., Shore, S.N., Starrfield, S., Woodward, C.E. ATel 4845 (2013) 2012 SUPERNOVA 2012fm IN UGC 3528 = PSN J06561339+8404502 Belligoli R, Castellani F. ABELL-35 PHENOMENA IN SYMBIOTIC STARS: DISCOVERY OF 1.2 AND 6.4 DAY PERIODS IN VV8 (V471 PER) U. Munari, A. Siviero, E. Tamajo, M. Fiaschi, S. Dallaporta, G. Cherini, A. Frigo, F. Castellani, M. Graziani, S. Moretti and S. Tomaselli The ANS Collaboration Monitoring Program Munari, U., Bacci, S., Baldinelli, L., Castellani, F., Cetrulo, G., Cherini, G., Dallaporta, S., Dallavia, G., Englaro, A., Frigo, A., Graziani, M., Luppi, V., Maitan, A., Marangoni, C., Milani, A., Moretti, S., Moschini, F., Ochner, P., Siviero, A., Righetti, G. L., Tomaselli, S., Tomasoni, S., Vagnozzi, A., Valisa, P. Informational Bulletin on Variable Stars SUPERNOVA 2012aw IN M95 = PSN J10435372+1140177 A. Vagnozzi, F. Castellani 2011 The 2010 nova outburst of the symbiotic Mira V407 Cyg U. Munari, V.H. Joshi, N.M. Ashok, D.P.K. Banerjee, P. Valisa, A. Milani, A. Siviero, S. Dallaporta, F. Castellani Formation of a disk structure in the symbiotic binary AX Per during its 2007-10 precursor-type activity A. Skopal, T. N. Tarasova, Z. Cariková, F. Castellani, G. Cherini, S. Dallaporta, A. Frigo, C. Marangoni, S. Moretti, U. Munari, G. L. Righetti, A. Siviero, S. Tomaselli, A. Vagnozzi, P. Valisa YY HERCULIS U. Munari, Istituto Nazionale di Astrofisica, Padova Astronomical Observatory; A. Siviero Department of Astronomy, University of Padova; G. L. Righetti, F. Castellani, S. Dallaporta, M. Graziani, G. Cherini, S. Moretti, S. Tomaselli, and A. Frigo SUPERNOVA 2011fe IN M101 Magnitude estimates: B. Mikuz and J. Vales, Crni Vrh Observatory, W. Souza, F. Castellani and R. Belligoli, Monte Baldo, G. Masi, J. Carvajal,P. Schmeer, Bischmisheim. 2010 BVRcIc Photometric Evolution and Flickering during the 2010 Outburst of the Recurrent Nova U Scorpii Munari, U., Dallaporta, S., Castellani, F. AX Persei Munari U., Siviero, A., R.L.M. Corradi R.L.M., Valisa P., Cherini G., Castellani F., Dallaporta S. COMET C/2010 G1 (BOATTINI) A. Boattini, R. Ligustri , E. Pettarin, F. Castellani and C. Marangoni, P. Birtwhistle, L. Buzzi, J. E. McGaha CI Cygni U. Munari, (INAF Padova-Asiago, Italy), P. Valisa, A. Milani, G. Cherini, F. Castellani, S. Dallaporta, A. Siviero, A. Frigo (ANS Collaboration) 2009 The 2006-2008 Outburst of AG Draconis Munari, U., Siviero, A., Ochner, P., Wallerstein, G., Castellani, F., Righetti, G., Cherini, G., Valisa, P., Cetrulo, G. AX PERSEI Munari, U., Siviero, A., Dallaporta, S., Cherini, G., Valisa, P., Castellani, F., Frigo, A., Vagnozzi, A., Bacci, S., Righetti, G., Moretti, S., Tomaselli, S. Ongoing meteor work - A Comprehensive List of Meteor Showers Obtained from 10 Years of Observations with the IMO Video Meteor 2008 NOVA SAGITTARII 2008 Munari, U., Siviero, A., Moretti, S., Tomaselli, S., Maitan, A., Baldinelli, L., Castellani, F., Dallaporta, S., Ochner, P. V2468 CYGNI Munari, U., Siviero, A., Valisa, P., Dallaporta, S., Cherini, G., Ochner, P., Castellani, F., Buzzi, L., Brienza, M., Luppi, V. 2008, CBET, 1431 Characterization of the HD 17156 planetary system M. Barbieri, R. Alonso, S. Desidera, A. Sozzetti, A.F. Martinez Fiorenzano, J. M. Almenara, M. Cecconi, R.U.Claudi, D. Charbonneau, M. Endl, V. Granata, R. Gratton, G. Laughlin, B. Loeillet, Amateur Consortium ⋆⋆ E.A.C. observations obtained by: F. Castellani (Mt. BaldoObservatory), B. Gary, J. Gregorio, C. Lopresti, A. Marchini (SienaUniversity Observatory),M. Nicolini (Cavezzo Observatory), R. Papini, C. Vallerani 2007 V2467 Cygni (Nova Cyg 2007) V919 Sgr Munari, U., Siviero, A., Navasardyan H., Castellani, F., Bortolotti M., Valisa, P., Luppi V. 2007, CBET, 999 AG DRACONIS Munari, U., Siviero, A., Castellani, F., Valisa, P., Cherini, G., Bano, I., Englaro, A., Cetrulo, G. The 2006 outburst of the recurrent nova RS Oph U. Munari, A. Siviero, Sostero, G., Guido, E., Dallaporta, S., Moretti, S., Graziani, M., Tomaselli, S., Castellani, F., Ochner, P. in "Evolution and Chemistry of Symbiotic Stars, Binary post-AGB and related Objects", held 29-31 August, 2006 in Wierzba, Mazury Lakes (Poland) |
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