Publikacje

Lajatico astronomical observatory pubblications.

 

Optical and X-ray behaviour of the high mass X-ray transient A0535+26/HDE245770 in February-March 2014

F. Giovannelli (1), G.S. Bisnovatyi-Kogan (2,3), I. Bruni (4), G. Corfini (5), F. Martinelli (5), C. Rossi (6) ((1) INAF – Istituto di Astrofisica e Planetologia Spaziali,Area di Ricerca di Roma (2) Roma,Italy, (2) Space Research Institute,Moscow, Russia, (3) National Research Nuclear University MEPhI, Moscow, Russia, (4) INAF – Osservatorio Astronomico di Bologna Loiano, Italy, (5) Montecatini Val di Cecina Astronomical Centre,Montecatibi, Italy, (6) Dept. of Physics, Roma Sapienza University, Roma, Italy)
(Submitted on 11 Sep 2014)

The optical behaviour of the Be star in the high-mass X-ray transient A0535+26/HDE245770 shows that at periastron the luminosity is typically enhanced by 0.02 to a few tenths magnitude, and the X-ray outburst occurs eight days after the periastron. Indeed, at the periastron an increase of the mass flux occurs. This sort of flush reaches the external part of the temporary accretion disk around the neutron star and moves to the hot central parts of the accretion disk and the neutron star surface. The time necessary for this way is dependent on the turbulent viscosity in the accretion disk, as discussed by Giovannelli, Bisnovatyi-Kogan, and Klepnev (2013) (GBK13). In this paper we will show the behaviour of this system in optical band around the predicted periastron passage on 21st February 2014, by using the GBK13 ephemeris that we used to schedule our spectroscopic and photometric optical observations. Spectroscopic unusual activity detected in the Balmer lines and the enhancement in the emission in B, V, and R bands around the periastron passage, and the subsequent X-ray event definitively demonstrate the existence of about 8 day delay between optical and X-ray flares.

Link to web site:  http://arxiv.org/abs/1409.3434

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. IV: The Fourth Year (2011-2012)

http://arxiv.org/abs/1210.0678     Astronomicalcentre staff in collaborazione con: Mariinsjaya High School, Odessa Ukraine Odessa National Martime University, Odessa Ukraine Scopritori: M.Mogoryan, Natalia Virnina & Fabio Martinelli Scoperta di 7 nuove stelle variabili tra la costellazione di Pegaso e Lacerta. Uno studio di circa un anno, un monitoraggio effettuato con il telescopio da 25cm SC dell’osservatorio astronomico Montecatini Val di Cecina Pisa, e l’osservatorio astronomico I telescope.net.   1° stella variabile, tipo EA, coordinate: 22 46 57.72, +34 05 55.2 Image:         Light curve   1. Secondary minimum: HJD = 2456536.8522.O’Connell effect (O’Connell 1951) is possible. Alternative period is 0d.5549. MinII = 13m.649. _________________________________________________________ 2° stella variabile, tipo EW, coordinate: 22 47 08.02, +34 14 21.6     Light curve         2. Secondary minimum: HJD = 2456534.8598. MinII = 17m.10 ____________________________________________________________   3° stella variabile, tipo EW, coordinate: 22 47 17.68, +34 06 37.2           Light curve       3. Secondary minimum: HJD = 2456535.8633. MinII = 15m.18. ____________________________________________________________     4° stella variabile, tipo EW, coordinate:  22 48 27.69, +34 13 50.9     Light curve           _________________________________________________________       5° stella variabile, tipo EA, coordinate: 22 48 34.85, +34 15 22.0               Light curve         5. Secondary minima: HJD = 2456159.6101, HJD = 2456224.3904, HJD = 2456559.5520. The phase curve is combined of unfiltered observations, collected in 2012 with Mead 10″ (black points); R-filtered observations obtained in 2013 with the same telescope (blue points); and R-filtered observations, made with the T5 telescope of the iTelescope.net observatory (red points).     ____________________________________________________________   6° stella variable, tipo, EB, coordinate: 22 49 47.54, +34 00 55.8               Light curve         6. Primary minima: HJD = 2456535.9370, HJD = 2456542.7177. MinII = 14m.32. O’Connell effect is clearly present. A total eclipse in the primary minimum is possible. The orbital inclination is close to 90°. Another interesting feature is a rather large difference in minima depths: minI – minII = 0m.28. Despite the shape of the light curve and the period, which are typical of EW-type binaries, the components of this binary do not show thermal contact.   ________________________________________________________________   7° stella variabile, tipo, EW, coordinate: 22 50 10.69, +34 04 56.3     Light curve       7. MinII = 14m.97.   Articolo completo sul sito:  http://www.astronet.ru/db/varstars/msg/1297456 Un ringraziamento particolare a chi ha collaborato alle osservazioni, e messa a punto della strumentazione, lo staff di Astronomicalcentre, all’amministrazione comunale, in particolare il Sindaco Sandro Cerri che ha concesso i permessi dell’osservatorio astronomico, e un ringraziamento caloroso all’agriturismo Palareta, Stefano e Babette che hanno concesso il loro terreno, in un posto meraviglioso che ci consente di fare osservazioni a livello professionale. PSN J18185620+2339370 2012 08 08.0625 Reports the discovery by Fabio Martinelli and Riccardo Mancini of an apparent supernova (mag about 16.5) on unfiltered CCD images (limiting mag about 18.0) taken with 0.35-m telescope of the Osservatorio Astronomico Montecatini val di Cecina, Italy, behalf of the Italian Supernovae Search Project (ISSP) on Agu. 08.0625 UT. The new object is located at R.A. = 18h18m56s.2, Decl. = +23d39’37″.0 (equinox 2000.0), which is 11″ east and 17″ nord of the nucleus of NGC 6619. Nothing is visible at this position on Palomar Sky Survey infrared, red, and blue plates.   Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.eduQuesto indirizzo e-mail è protetto dallo spam bot. Abilita Javascript per vederlo. (alternate cbat@iau.orgQuesto indirizzo e-mail è protetto dallo spam bot. Abilita Javascript per vederlo. ) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network SUPERNOVA 2012dz IN NGC 6619 = PSN J18185620+2339370 Fabio Martinelli and Riccardo Mancini report the discovery of an apparent supernova (mag about 16.5) on unfiltered CCD images (limiting mag about 18.0) taken with a 0.35-m telescope of the Osservatorio Astronomico Montecatini val di Cecina, Italy, in the course of the Italian Supernovae Search Project on Aug. 8.0625 UT. The new object is located at R.A. = 18h18m56s.2, Decl. = +23d39’37″.0 (equinox 2000.0), which is 11″ east and 17″ north of the nucleus of NGC 6619. Nothing is visible at this position on Palomar Sky Survey infrared, red, and blue plates. The variable was designated PSN J18185620+2339370 when it was posted at the Central Bureau’s TOCP webpage and is here designated SN 2012dz based on the spectroscopic confirmation reported below. Additional CCD magnitudes for 2012dz: July 21.78, [19.2 (D. Denisenko and V. Lipunov, Sternberg Astronomical Institute at Lomonosov, Moscow State University; MASTER-Kislovodsk images); Aug. 7.615, 16.6 (Denisenko and Lipunov; two unfiltered 60-s images taken with the 0.40-m f/2.5 MASTER Amur robotic telescope + 16-megapixel camera; pre-discovery; position end figures averaged from two exposures are 56s.00, 32″.9); Aug. 8.865, R_c = 16.1 (Massimiliano Martignoni, Magnago, Italy, 25-cm f/10 reflector). A comparison of the Aug. 7 and June 20 MASTER-Amur images is posted at website URL http://master.sai.msu.ru/static/OT/PSNJ18185620+2339370-MASTER-Amur.jpg. L. Tomasella, P. Ochner, A. Pastorello, S. Benetti, E. Cappellaro, M. Turatto, and S. Valenti, Osservatorio Astronomico di Padova, Istituto Nazionale di Astrofisica, report that a spectrogram of PSN J18185620+2339370 = 2012dz, obtained on Aug. 8.88 UT with the Asiago 1.82-m Copernico Telescope (+ AFOSC; range 340-820 nm; resolution 2.4 nm), suggests that this is a normal type-Ia supernova. Adopting for the host galaxy, NGC 6619, a redshift z = 0.016805 (Wegner et al. 2003, A.J. 126, 2268; via NED), comparison with a library of supernovae spectra via GELATO (Harutyuyan et al. 2008, A.Ap. 488, 383) shows that it is a type-Ia event, a few days after B-maximum light. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright       2012 CBAT 2012   August 9 (CBET 3198) Daniel W. E. Green       MSU) Russia Autori Denis Denisenko e Fabio Martinelli http://arxiv.org/abs/1207.6320      Osservazione del transito HAT-P-5 con telescopio da 25 cm focale 1600 camera ccd DTA con sensore KAF1600, no Observation of transit HAT-P-5 with telescope 25 cm focal 1600 mm ccd, camera DTA with KAF 1600 09/07/12

Pubblication of the transit HD 189733  b in collaboration with Czech Astronomical Society . Authors Fabio Martinelli and Giorgio Corfini.

1970-01-02 00:55:39

2012-07-09

                         

 

Pubblication of the transit KOI0135 b in collaboration with Czech Astronomical Society . Authors Fabio Martinelli and Giorgio Corfini.

1970-01-02 00:20:41

2012-06-30

                     

web link:

http://var2.astro.cz/EN/tresca/transit-detail.php?id=1341080951

 

Pubblication of the transit HD 189733 b in collaboration with Czech Astronomical Society . Authors Fabio Martinelli and Giorgio Corfini.

1970-01-02 00:20:41

2012-06-30

web link: http://var2.astro.cz/EN/tresca/transit-detail.php?id=1341080835

 

Pubblication of the transit KOI 0196 b in collaboration with Czech Astronomical Society . Authors Fabio Martinelli and Giorgio Corfini.

1970-01-02 00:10:47

2012-06-18

Pubblication of the transit TRES-3 in collaboration with Czech Astronomical Society . Authors Fabio Martinelli and Giorgio Corfini.

1970-01-02 01:42:37

2012-04-02

                           

Pubblication of obsevation of SN in NGC 5775 in collaboration with ISSP, Italian Supernovae Search Project, Observation by Fabio Martinelli and Fabio Briganti.

                        http://www.rochesterastronomy.org/supernova.html    ——————————————————————————————————-

Pubblication of the transit  Wasp-14  in collaboration with  Czech Astronomical Society  & Luigi Mancini Max Plank Instutute for astronomy Germany.  Authors Fabio Martinelli and Giorgio Corfini.

Telescope Cassegrain 356 mm focal lenth 2500 CCD SBIG ST8XME  KAF1600.

Web link: http://var2.astro.cz/EN/tresca/transit-detail.php?id=1332953052

 —————————————————————————————————–

 

Pubblication of the transit  GJ1214 in collaboration with  Czech Astronomical Society  & Luigi Mancini Max Plank Instutute for astronomy Germany.  Authors Fabio Martinelli and Giorgio Corfini.

Telescope Cassegrain 302 mm focal lenth 2000 CCD SBIG KAF1600.

Web link: http://var2.astro.cz/tresca/transit-detail.php?id=1332519743

——————————————————————————————————-

Exoplanet transit of WASP-43 By Fabio Martinelli and data reduction by Giorgio Corfini Telescope 356 mm focal lenth 2257 mm, CCD camera ST-8XME Baader yellow filter 495nm.

Pubblication by

http://var2.astro.cz/EN/tresca/transit-detail.php?id=1330606862

                   

 

Latest supernovae, discovered SN in NGC 5806

Posted on 23 Januar 2012 by redazione

Discovered a SN by Fabio Briganti and Alessandro Dimai in NGC 5806. The transient, discovered by Fabio Briganti (Santa Croce sull’Arno – PI) in poor seeing condition, with the SC 11″ f/6,3 of the Col Drusciè Observatory, in the cours of Italian Supernovae Search Project, needs a confirmation, because there is only a frame of the suspect. No known minor planets in the field at the time of discovery. Nothing is visible in red and blue plates of Palomar Sky Survey POSS2.

Here http://www.cortinastelle.it/cross/NGC5806_20120122_034439_55_Luminance_2_Maioni.jpg

   you can find the discovery image.

Congratulation to Fabio Briganti and Alessandro Dimai     Up date about the SN in NGC 5806 cause it’s very interesting and bright supernova.

The PTF (ATEL #1964, #3253; http://www.astro.caltech.edu/ptf ) reports the discovery of a new supernova in NGC 5806 (independently discovered by F. Briganti and reported as PSN J14595904+0153251 on Jan 22). The source is located at RA = 14:59:59.08, Dec = +01:53:24.2 (J2000), was first detected by the Palomar 1.2m telescope with an R-band magnitude of about 17 on 2012 Jan 10 (UT) and brightened to about 16.1 mag on Jan 20. PTF did not detect the source prior to 2012 Jan 5. Spectroscopic follow-up was performed with the HET (+LRS) on Jan 14, the INT (+IDS) on Jan 15-18, Gemini N (+GMOS) on Jan 17 and the Palomar 5m (+DBSP) on Jan 18. The spectra show prominent H features as well as He absorption at about 10,000 km/s, consistent with a type IIb classification.   Credential Certification: Christopher J. Stockdale (chris.stockdale@mu.edu)

Subjects: Radio, X-ray, Supernovae

We report the detection of radio emission near the position of the type-IIb supernova PTF2012os (ATEL #3881) with the Karl G. Jansky Very Large Array radio telescope in the DnC configuration: A flux density of 0.44 +/- 0.05 mJy was measured at 5.02 GHz (wavelength 6.0 cm) on 2012 Jan. 22.42 UT. The measured position of the radio emission of R.A. = 14h59m59.s12, Decl. = +01d53m23s.3, equinox 2000.0 is in good agreement with the measured optical position of (ending digits) R.A. = 59.s08, Decl. = 24s.2, equinox 2000.0 (ATEL #3881). Radio observations are continuing. Using 9.4 ks of co-added Swift X-Ray Telescope (XRT) data, obtained on 2012-01-14 (2.0 ks exposure time; PI Kasliwal), 2012-01-16 (2.4 ks; PI Kasliwal), and 2012-01-24 (5.0 ks; PI Immler), no X-ray source is detected at the position of the SN. The PSF, dead-time, and vignetting corrected upper limit to the XRT net count rate is 1.1E-03 cts/s (3-sigma), corresponding to an unabsorbed (0.2-10 keV band) X-ray flux limit of 5.4E-14 erg/cm/cm/s and a luminosity limit of 4.2E39 erg/s for an adopted thermal plasma spectrum with a temperature of kT = 10 keV, a Galactic foreground column density of 4.14E+20 (Dickey & Lockman, 1990, ARAA 28) and a distance of 25.4 Mpc (NED). Swift observations are continuing. The object warrants further study in all wavelength bands.   Credential Certification: Schuyler D. Van Dyk (vandyk@ipac.caltech.edu)

Subjects: Optical, Supernovae, Transient, Variables

Schuyler D. Van Dyk (Spitzer Science Center/Caltech), Avishay Gal-Yam, Iair Arcavi (Weizmann Institute), Mansi M. Kasliwal (OCIW/Princeton), and Assaf Horesh (Caltech), on behalf of the larger PTF collaboration, report their attempt to identify the progenitor of the Type IIb supernova PTF12os, aka PSN J14595904+0153251, in archival Hubble Space Telescope (HST) ACS/WFC F435W, F555W, and F814W images from 2005 March 10 UT (PI: Smartt). We have astrometrically matched a B-band image (with 0.87″ seeing) from 2012 January 18 UT obtained with the IMACS camera on the Magellan Baade 6.5 m telescope at Las Campanas Observatory, Chile, with the ACS F435W image, using 10 fiducial stars in common. The SN position has been located on the ACS image with an uncertainty of 0.57 WFC pixel, or 0.028″. This is within 1 WFC pixel, to the southwest, of a candidate source detected in all three ACS bands. The site of PTF12os lies approximately 2.2″ southeast of the position of the Type II SN 2004dg in this same host galaxy. Preliminary photometry of the ACS images using Dolphot (Dolphin 2000, PASP, 112, 1383) results in a brightness for the object of B=23.30, V=23.04, and I=22.53 (uncertainties are all 0.012 mag or smaller). Assuming the average value of the distance modulus to the host, NGC 5608, from the NASA/IPAC Extragalactic Database (NED), 32.01 mag, and also assuming only the Galactic foreground extinction at V-band from Schlegel, Finkbeiner, & Davis (1998, ApJ, 500, 525), 0.17 mag, this object had V absolute magnitude of -9.1 and absolute colors (B-V)_0=0.21 and (V-I)_0=0.44 (consistent with an early F spectral type). This could be a highly-luminous supergiant star, or, alternatively, a compact star cluster. Evidence exists from the strength of the Na I D lines in follow-up spectra (ATel 3881) that the extinction to the SN could, in fact, be higher, implying that the source is even more luminous and bluer. We tentatively identify this source as a candidate for the progenitor, although given the offset of the SN position from the object’s centroid, the host galaxy distance, and the inferred higher extinction, it is quite possible that the progenitor has not been detected. Higher-resolution imaging is pending for candidate confirmation, and further analysis is ongoing.   Credential Certification: Assaf Horesh (assafh@astro.caltech.edu)    

Subjects: Millimeter, Supernovae

We report a CARMA observation of the type IIb supernova PTF12os (Arcavi et al.; ATEL# 3881). The observation was undertaken on 2012 Jan 14.65 UT. We report a null-detection in the 3-mm band (at a center frequency of 93 GHz) with a 3 sigma upper limit of 0.36 mJy/beam. We thank the CARMA staff for scheduling this target of opportunity.   Pubblicazione della scoperta.

Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
CBAT Director:  Daniel W. E. Green; Hoffman Lab 209; Harvard University;
 20 Oxford St.; Cambridge, MA  02138; U.S.A.
e-mail:
 cbatiau@eps.harvard.edu (alternate
 cbat@iau.org)
URL http://www.cbat.eps.harvard.edu/index.html
Prepared using the Tamkin Foundation Computer Network

SUPERNOVA 2012P IN NGC 5806 = PSN J14595904+0153251
     Alessandro Dimai, Cortina d'Ampezzo, Italy, on behalf of the Italian
Supernovae Search Project (ISSP), reports the discovery by Fabio Briganti
(Santa Croce sull'Arno, Pisa, Italy) of an apparent supernova (mag about 15.0)
on unfiltered CCD images (limiting mag about 16.5) taken with the "Maioni"
0.28-m telescope of the Osservatorio Astronomico del Col Druscie at Cortina
d'Ampezzo, Italy, on Jan. 22.1556 UT.  The new object is located at R.A. =
14h59m59s.12, Decl. = +1d53'24".4 (equinox 2000.0), which is 10" west and 1"
south of the nucleus of NGC 5806.  Nothing is visible at this position on
Palomar Sky Survey infrared, red, and blue plates.  The discovery image is
posted at website URL http://tinyurl.com/7lzoeyv.  The variable was designated
PSN J14595904+0153251 when it was posted at the Central Bureau's TOCP webpage
and is here designated SN 2012P based on the spectroscopic confirmation
reported below.  Additional CCD magnitudes for 2012P (unfiltered unless noted
otherwise):  2011 Dec. 7, [18.0 (ISSP); 2012 Jan. 23.227, 15.2 (Briganti);
23.549, 16.3 (Joseph Brimacombe, Cairns, Australia; remotely using a 51-cm
RCOS telescope + STL11K camera + luminance filter at the New Mexico Skies
Observatory near Mayhill, NM, U.S.A.; position end figures 59s.09, 24".1;
image posted at URL http://www.flickr.com/photos/43846774@N02/6752536997/).
The type-II supernova 2004dg also appeared in NGC 5806 (cf. IAUC 8375).

     L. Borsato and V. Nascimbeni, Dipartimento di Fisica e Astronomia,
Universita di Padova; and S. Benetti, A. Pastorello, S. Valenti, L. Tomasella,
E. Cappellaro, P. Ochner, and M. Turatto, Osservatorio Astronomico di Padova,
Istituto Nazionale di Astrofisica, report that a spectrum (range 360-810 nm;
resolution 2.2 nm) of PSN J14595904+0153251 = SN 2012P was obtained on Jan.
23.17 UT with the Ekar-Copernico 1.82-m telescope (+ AFOSC).  Using a library
of supernova spectra via GELATO (Harutyunyan et al. 2008, A.Ap. 488, 383;
available via https://gelato.tng.iac.es/login.cgi), they found a best match
with typical type-Ib/c supernovae soon after maximum if a redshift of z =
0.004533 (Falco et al. 1999, PASP 111, 438; via NED) is assumed.  From the
minimum of a deep-intense absorption measured at 627.6 nm, an expansion
velocity of about 5100 km/s is deduced for the ejecta if identified with Si
II 635.5-nm (but an expansion velocity of about 14400 km/s if identified
with H-alpha).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
      superseded by text appearing later in the printed IAU Circulars.

                         (C) Copyright 2012 CBAT
2012 January 25                  (CBET 2993)              Daniel W. E. Green

 

DISCOVERY SUPERNOVA IN NGC 7485

 

  Just one mounth we started the astronomical search, and we have the first Supernova discovered by Montecatini val di Cecina astronomical association. During the night of 13th october 2011 the survery for Supernova search with C14 telescope, Bellincioni Beta mount using DTA camera with Kodak KAF1000, Fabio Martinelli get an image of galaxy NGC 7485. During the controll By Riccardo Mancini.

we discovered the SN of Magnitude 17.00.

 

  

 

The pubblication about PSN by IAU, International astronomical union. http://www.cbat.eps.harvard.edu/unconf/followups/J23060280+3406367.htmlA. Dimai, Cortina d’Ampezzo, Italy, reports the discovery by Fabio Martinelli, Riccardo Mancini and Fabio Briganti, on behalf of Italian Supernovae Search Project, of an apparent supernova (see PSN J23060280+3406367), on unfiltered CCD images taken with the 0.35-m telescope of the Montecatini Valdicecina Observatory (Pisa – Italy) on October 14.0299 (at mag about 18.0; limiting mag about 19.0) and 14.9319 UT (mag about 17.6; limiting mag about 19.0). The new object is located at R.A. = 23h06m02s.80, Decl. = +34°06’36”.7 (equinox 2000.0), which is 22″ west and 8″ north of the nucleus of NGC 7485. ISSP images of the same field taken on 2011 Oct. 01 (limiting mag about 19.5) shows nothing at this position, nor do Palomar Sky Survey infrared, red, and blue plates. A confirmation image, taken by A. Dimai with the „Maioni” 0.28 m. telescope of the Col Drusciè Observatory on October 15.9, shows the PSN at mag. +17.0 C. Best Regards Alessandro Dimai We are glad to get this discovered. Montecatini astronomical association.

J231935.0+364705: superhumps evolution

Denis Denisenko d.v.denisenko at gmail.com Fri Oct 7 17:55:49 JST 2011 Fabio Martinelli (Astronomical Centre at Montecatini, Italy) has obtained fifty 160-sec exposures of J2319+3647 covering 2.3 hours interval from 00:58 to 03:18 UT on 2011 Oct. 05. Light curve (unfiltered magnitudes with Red zero point) is uploaded to http://pics.livejournal.com/bigdenru/pic/000adk0k/ I was using R=14.4 as the comparison star and R=14.2 as check star from my 2007 finder chart at http://hea.iki.rssi.ru/~denis/J2319+3647-comps.gif Amplitude of orbital modualtion has decreased to 0.13-0.14m. It was 0.24m during Oct. 01/02 observations by Etienne Morelle. Denis Denisenko P.S. Regarding the new object from vsnet-alert 13736: dwarf nova 1RXS J231935.0+364705 is also a hard ROSAT source (HR1=1.00+/-0.09, HR2=0.47+/-0.16).

     

Observation of the last SN in M101 by our observatory show how is been fast the light curve of the Supernova in M101 Immage by latest supernovae .

http://www.rochesterastronomy.org/sn2011/sn2011fe.html

Pubblication by Coelum magazine about Italian Supernovae Search Project. ISSP Magazine pubblication Italian language only.

Observations and Pubblication during telescopes test and previus the observatory opening.

   

Pre-discovery Immage of SN near NGC 6577 observed 27/06/2011. Immage by Fabio Martinelli, Survey controll by Fabio Briganti. Telescope SC 14″ immage with DTA camera KAF1000 60 sec exp, telescope test Montecatini VdC Astronomical Association SN Discoverde by Fabrizio Ciabattari, S. Donati e G. Fornaciari Italian Supernovae Search Project.

       

SN Immage observed 23/05/2011 in UGC10018 galaxy Telescope C14 celestron  ccd camera DTA KAF1000 60 sec exp By Fabio Martinelli e Mauro Biagetti communicated to Latest Supernovae.   Montecatini VdC Astronomical Association.

  

 

SN Observed 10/05/2011 in UGC9356 Immage by Fabio Martinelli e Fabio Briganti Schmidt cassegrain 14″ telescope.

Supernova observed the night 14/05/2011 in anonymous galaxy By C14 telescope ccd camera KAF100 DTA.

Observed by Fabio Martinelli & Fabio Briganti.

Możliwość komentowania jest wyłączona.