Montecatini astronomical observatory, is an astronomical station made for scientific research and studies. The most of the telescopes are available for astronomy, astrophysic and astrometry observing targets. Observatory geographic info Lat: 43.39° Log: 10.75, S.L.M 600 metres. Supernovae extragalattic search program. The Supernovae search program is completed under our controll, Montecatini Astronomical association has got different telescopes for this kind of search, the main telescope is a Dall Kirkham 16″ F/10, the others are C14 celestron a meade 12″, all the telescopes are on equatorial mounts, and every instrument has got CCD camera unfiltered for SN survey. The survey program has got about 4500 galaxies of the boreal hemisphere, and going untill sourthen declinations, around -30 or -35 cause the dark skies we have from the observatory. This galaxies list is made by a theory of the distance, it’s mean we didn’t put in our list the very far galaxies cause for our instruments is too difficult to discovery a SN. During the clear nights we observe the most of galaxies we can, getting two immages for every galaxy. The exposition time is around 60 sec for every telescope, and the magnitude limit is around 19,50. The morning after we install the immages in a web site, where the Montecatini astronomical members gets the immage for controll. The night after we take picture of the galaxies wich we have doubts and new list. If we have bad weather we ask collaborations to our partners. Montecatini astronomical observatory is member ship of ISSP, Italian Supernovae Search Project. ISSP it’s a program with 4 astronomical observatory, CROSS Col Drusciè – Cortina (Belluno) MOSS Astronomical observatory Montarrenti (Siena), MASACAS Astronomical observatory Monte Agliale (Lucca). The reason why of this collaborations is due of the numbers of the telescopes can monitoring the sky. Every observatory has got list of galaxies must be monitorated, in this way we have the full controll of the sky.
independent discovery supernova in UGC11322
Co-discovery con astrofili cinesi, Zhijian Xu e Xing Gao. Supernova in UGC11322 telescopio C14 celestron con CCD camera DTA KAF1001E
SUPERNOVA 2012ek IN PGC 62237 = PSN J18402884+3607174 Zhijian Xu, Nanjing, Jiangsu, China; and Xing Gao, Urumqi, Xinjiang, >China, report the discovery of a possible supernova (mag approximately 17.9) >on a 40-s unfiltered CCD image (limiting mag about 18.8) taken by Xing Gao >in the course of the Xingming Sky Survey around Aug. 18.810 UT using a >0.36-m f/6.9 Celestron C14 telescope at Mt. Nanshan. The new object is approximately located at R.A. = 18h40m28s.84, Decl. = +36d07’17″.4 (equinox >2000.0; reference stars from USNO-B1.0 catalogue), which is about 13″.6 >west and 12″.2 south of the center of the PGC 62237. Nothing is visible at >this position on a red Digitized Sky Survey plate from 1992 Aug. 20 >(limiting mag about 19.8). The Xingming images are posted at website URL http://www.xjltp.com/XOSS/XM48ZX/XM48ZX.htm. The object was designated PSN >J18402884+3607174 when it was posted at the Central Bureau’s TOCP webpage >and is here designated SN 2012ek based on the spectroscopic confirmation >reported below. Additional CCD magnitudes for 2012ek (unfiltered unless >noted otherwise): 2012 Aug. 7, [19.0 (Xu and Gao); Aug. 19.64, 17.9 (Xu >and Gao; image posted at the following website URL: http://www.flickr.com/photos/75341417@N06/7816496822/in/p hotostream); >Aug. 19.896, 17.8 (Fabio Briganti and Fabio Martinelli, Celestron 14 >telescope; independent discovery in the course of survey of the Italian >Supernovae Search Project); Aug. 20.206, 18.1 (J. 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 28s.92, 16″.6; image posted at http://www.flickr.com/photos/43846774@N02/7824016820/); Aug. 20.62, 17.7 >(Xu and Gao).
M. Turatto, S. Benetti, A. Pastorello, L. Tomasella, M. Fiaschi, P. >Ochner, E. Cappellaro, and S. Valenti, Osservatorio Astronomico di Padova, >Istituto Nazionale di Astrofisica, report that a spectrogram of PSN J18402884+3607174 = SN 2012ek, obtained on Aug. 21.79 UT with the Asiago >1.82-m Copernico Telescope (+ AFOSC; range 340-820 nm; resolution 1.4 nm), >indicates that it is a type-Ib supernova. Adopting for the host galaxy (PGC 62237) a redshift z = 0.028563 (Freudling et al. 1995, A.Ap. Suppl. >112, 429; via NED), comparison with a library of supernovae spectra via >GELATO (Harutyuyan et al. 2008, A.Ap. 488, 383) shows close similarities >of the spectrum of 2012ek to spectra of several type-Ib supernovae one week >after maximum.
NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. > (C) Copyright 2012 CBAT 2012 August 28 (CBET 3212) Michael Rudenko
Discovered supernova in NGC 6619 in the night 08/08/2012 by Fabio Martinelli and Riccardo Mancini.
Imaging with telescope SC da 35 cm C 14 celestron, ccd camera DTA con sensore KAF1001E 50 sec esposition CGE-PRO Celetron mount.
In collaboration with ISSP, Italian supernovae search project.
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.
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
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.
Latest supernovae, discovered SN in NGC 5806
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.
you can find the discovery image.
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 (firstname.lastname@example.org)
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 (email@example.com)
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 (firstname.lastname@example.org)
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: email@example.com (alternate firstname.lastname@example.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