|
|
| Riga 1: |
Riga 1: |
| - | = Alert Notice 512: Nova Sagittarii 2015 No. 2 = PNV J18365700-2855420 =
| + | October 14, 2015 |
| | | | |
| - | Si riporta qui allerta AAVSO per una Nova in Sagittario al limite del visuale,cartine e dati su sito AAVSO come sempre
| + | Riporto qui Alert AAVSO per seconda Nova in Ofiuco |
| - | March 16, 2015
| + | |
| | | | |
| - | Event: Nova Sagittarii 2015 No. 2 = PNV J18365700-2855420
| + | risulta di 12.1 non filtrata al momento della scoperta |
| | | | |
| - | Discovered by: John Seach, Chatsworth Island, NSW, Australia
| + | in V siamo sulla 13 a qualche giorno fa |
| | | | |
| - | Discovery magnitude: 6.0 using DSLR and 50mm f/1.0 lens
| + | fare riferimento au aavso.org alert 531 |
| | | | |
| - | Discovery date: 2015 March 15.634 UT
| + | per le carte sempre su aavso |
| | | | |
| - | Coordinates: R.A. 18 36 56.84 Dec. -28 55 39.8 (2000.0)
| + | i dati sottoporli ad aavso come NOVA OPH 2015 NO. 2 rispettando gli spazi visto che non ha ancora una designazione definitiva |
| | | | |
| - | Spectra: An optical spectrum by S. C. Williams (Liverpool John Moores University) et al. (ATel #7230) obtained 2015 March 16.27 UT using the FRODOspec spectrograph on the Liverpool Telescope at 2015 March 16.27 UT indicates N Sgr 2015 No. 2 is a classical Fe II nova.
| |
| | | | |
| - | J. Powles (PJOC, Latham, ACT, Australia) reports a low-resolution (R=260, 150 l/mm) spectrum obtained by him appears to be that of a Fe II nova shortly after maximum.
| |
| | | | |
| - | Observing recommendations: Observations of all types (visual, CCD, DSLR, spectroscopy) are strongly encouraged as this nova evolves. T. Finzell (Michigan State University) requests ongoing optical coverage in support of radio and x-ray observations being scheduled.
| + | Event: Nova Oph 2015 No. 2 = TCP J17344775-2409042 |
| | | | |
| - | Charts: Charts for Nova Sgr 2015 No. 2 may be created using the AAVSO Variable Star Plotter (VSP) at http://www.aavso.org/vsp. A binocular sequence for this nova is being created. However, comparison stars may be found now using VSP and requesting an 'a' or 'b' scale chart.
| + | Independent discovery by: <br> - Koichi Nishiyama (Kurume, Japan) and Fujio Kabashima (Miyaki, Japan)<br> - Shigehisa Fujikawa (Kan'onji, Kagawa, Japan) |
| | | | |
| - | Observations reported to the AAVSO:
| + | Discovery magnitude:<br> - Nishiyama and Kabashima: 11.8 unfiltered (CCD, using a 135-mm f/4 camera lens (+FLI 09000 camera))<br> - Fujikawa: 12.1 unfiltered (CCD using a MINOLTA F 3.5 f 120mm lens) |
| - | 2015 Mar. 15.802 UT, 5.3 (K. Itagaki, Yamagata, Japan);
| + | |
| - | 16.3131, 5.8 (AAX, A. Amorim, Florianapolis, Brazil);
| + | |
| - | 16.3375, 5.9 (CLUB, L. Camargo da Silva, Brazil);
| + | |
| - | 16.3604, 6.1 (Camargo da Silva);
| + | |
| - | 16.5275, 5.8 R-CCD (E. Guido and N. Howes, 0.61-m f/6.5 astrograph+CCD) of ITelescope network (MPC Code U69, Auberry, CA);
| + | |
| - | 16.74861, 6.0 (PEX, A. Pearce, Nedlands, WA, Australia);
| + | |
| - | 16.77, 6.0 (CMQ, P. Camilleri, Warners Bay, Newcastle, NSW, Australia);
| + | |
| | | | |
| - | Submit observations: Please submit observations to the AAVSO International Database using the name "NOVA SGR 2015 NO. 2". Once a GCVS name has been assigned, please use that name.
| + | Discovery date:<br> - Nishiyama and Kabashima: 2015 October 11.4129 UT<br> - Fujikawa: 2015 Oct 11.41474 UT |
| | | | |
| | + | Coordinates (2000.0): R.A. 17 34 47.75 Dec -24 09 04.2 (Nishiyama and Kabashima, in VSX) |
| | | | |
| | + | Spectra: A low resolution spectrum obtained at Van Vleck Observatory by C. Littlefield (Wesleyan University) and P. Garnavich (Notre Dame) on 2015 October 11.99 UT across an airmass range of 3.6-4.5, which yielded noisy data, indicate the nova to be an Fe II-type classical nova (ATel #8156). Spectra by M. Fujii (Kurashiki, Okayama, Japan) obtained on 2015 October 12.421 UT at Fujii Kurosaki Observatory indicate a highly reddened nova (CBET 4150). His spectrogram is posted at http://otobs.org/FBO/etc/tcp_oph.htm. |
| | | | |
| - | = Allerta osservativa AAVSO nova simbiotica ASAS J174600-2321.3 =
| + | Observing recommendations: This nova is faint, but observations of all types (visual, CCD, DSLR, spectroscopy) as instrumentation permits are strongly encouraged as this nova evolves. |
| | | | |
| - | L'allert AAVSO sotto riportata riguarda la nova simbiotica in questione.La campagna parte da subito fino a fine luglio in visuale e CCD.A febbraio era di mag.12.28 quindi buona anche per il visuale.In CCD filtri V,B e Ic,tenere presente che durante la fase massima in B la stella sarà molto debole.Qualche osservazione per notte e nelle fasi di inizio massino e fine molte di più possibilmente nei vari filtri.Le date non sono precisissime mancando molti dati su questo particolare sistema.Dettagli più precisi sulla nota allegata
| + | Charts: Charts for Nova Oph 2015 No. 2 may be created using the AAVSO Variable Star Plotter (VSP). Be sure to include spaces in the name as shown.<br> |
| | | | |
| - | cartina Vis.
| + | Oct. 7.405, <13.4 (Nishiyama and Kabashima);<br>11.394, 12.0 unfiltered (T. Kojima, Tsumagoi, Gunma-ken, Japan, pre-discovery observation);<br>11.490, 11.7 unfiltered CCD (S. Fujikawa, Kan'onji, Kagawa, Japan, confirming image);<br>11.721, 11.2 CR (G. Masi, remotely using the 17"-f/6.8 robotic unit part of the Virtual Telescope Project facility at Bellatrix Astronomical Observatory,Ceccano, Italy);<br>12.06870 UT, 9.90 I +/-0.07 (S. O'Connor, St. George, Bermuda);<br>12.07110, 11.89 V +/-0.03 (O'Connor);<br>12.07380, 11.70 CV +/-0.04 (O'Connor);<br>12.0900, 13.65 B (S. Kiyota, Kamagaya, Japan, remotely using 0.50-m f/4.5 CDK astrograph + FLI-PL11002M CCD f iTelescope.NET at Mayhill, NM, USA);<br>12.0900, 12.04 V (Kiyota);<br>12.0900, 11.12 Rc (Kiyota);<br>12.0900, 10.09 Ic (Kiyota);<br>13.38560, 11.56 R +/-0.05 (O'Connor);<br>13.407, 12.9 V (T. Yusa, Osaki, Japan, remotely using the 0.43-m f/6.8 astrograph + CCD(FLI Proline 16803)at the iTelescopeNET, Siding Spring, Australia).<br>14.05870, 10.4 I +/-0.1 (O'Connor);<br>14.06100, 13.33 V +/-0.08 (O'Connor);<br>14.06350, 12.82 CV +/-V0.03 (O'Connor);<br>14.06944, <11.2 (S. Aguirre, Hermosillo, Mexico);<br>14.37700, 10.68 I +/-0.05 (O'Connor);<br>14.37840, 12.05 R +/-0.05 (O'Connor);<br>14.37990, 13.32 V +/-0.02 (O'Connor);<br>14.38120, 14.00 TB +/-0.14 (O'Connor);<br>14.38120, 14.87 TB +/-0.04 (O'Connor);<br>14.38250, 13.00 CV +/-0.02 (O'Connor); |
| - | | + | |
| - | [[Image:ASAS J174600-2321.3 visuale.png]]
| + | |
| - | | + | |
| - | cartina CCD
| + | |
| - | | + | |
| - | [[Image:ASAS Jccd.png]]
| + | |
| - | | + | |
| - | <br>
| + | |
| - | | + | |
| - | alert originale: March 5, 2015: The AAVSO is requesting observations of the symbiotic nova candidate ASAS J174600-2321.3 during the predicted upcoming eclipse of this system. Observers are asked to begin observing immediately (2015 March 5), and continue observations through the end of July 2015. Both visual and instrumental observations are encouraged; the object was at V=12.28 on 2015 February 6.764 (OCN; S. O'Connor, Bermuda). Filtered, transformed photometry in B, V, and Ic are especially encouraged, with several observations per night required during the ingress and egress phases. The project is being organized by S. Otero, P. Tisserand, K. Bernhard, and S. Hummerich, and is an extension of the research program discussed in Hummerich et al. (2015, AAVSO preprint (=eJAAVSO) #295, in press).
| + | |
| - | | + | |
| - | The researchers have provided the following discussion of the project:
| + | |
| - | | + | |
| - | "The deeply eclipsing system and likely symbiotic nova ASAS J174600-2321.3
| + | |
| - | | + | |
| - | === RA: 17 46 00.18 , Dec: -23 21 16.4 (J2000.0) ===
| + | |
| - | | + | |
| - | is going to enter an eclipse in mid-March according to the published elements HJD = 2456142 + 1011.5 x E. The eclipse duration is approximately 115 days.
| + | |
| - | | + | |
| - | The system has shown a conspicuous brightening of ~4 magnitudes (V) that started in 1999 and has been in outburst since then. Recent photometry shows the system fluctuating around 12.2 mag (V) as recently as 2014 November 07 (JD 2456969.49068; HMB, J. Hambsch, Mol, Belgium, remotely from Chile). It will go fainter than 16.9 mag (V) at mid-eclipse when the red giant passes in front of the outbursting white dwarf. We might also be seeing semi-regular pulsations from the red giant during eclipse.
| + | |
| - | | + | |
| - | As no observations around mid-eclipse exist after the considerable brightening of the primary star, the exact shape of eclipse is open to conjecture. Thus, no times of second or third contact are given below, although there was a pronounced time of totality during the eclipse that has been covered before the onset of activity in the system (compare Fig. 4, JAAVSO preprint (=eJAAVSO) #295).
| + | |
| - | | + | |
| - | We encourage visual and CCD observations during the eclipse, preferably multicolour photometry to record the colour changes as the red star starts to dominate the total flux of the system. Observations in V, B and Ic would be very valuable (note, though, that the object will be very faint in B during eclipse). During the ingress and egress phases, several observations per night are advisable. During the remainder of the eclipse, one set of observations per night will be adequate due to the long period of the system. Stacking might be advisable to reach the faint magnitudes during the eclipse.
| + | |
| - | | + | |
| - | Observations should start as soon as possible to check on the brightness of the object before the eclipse sets in. Once the event is over, continued photometry with a cadence of one observation per week is encouraged to detect the start of the fading phase of this very slow nova.
| + | |
| - | | + | |
| - | Spectroscopic observations near mid-eclipse would be very desirable, too.
| + | |
| - | | + | |
| - | These are the dates observers should keep in mind:
| + | |
| - | | + | |
| - | === 1st contact: 2015 March 14 (JD 2457096) ===
| + | |
| - | | + | |
| - | === Mid-eclipse: 2015 May 11 (JD 2457153.5) ===
| + | |
| - | | + | |
| - | === 4th contact: 2015 July 07 (JD 2457211) ===
| + | |
| - | | + | |
| - | The start and end of the eclipse may vary so please be patient if the eclipse doesn't start at the predicted date!"
| + | |
| - | | + | |
| - | Charts with sequence may be created using the AAVSO Variable Star Plotter (http://www.aavso.org/vsp).
| + | |
| - | | + | |
| - | Observations should be submitted to the AAVSO International Database using the name ASAS J174600-2321.3.
| + | |
| - | | + | |
| - | This AAVSO Alert Notice was prepared by S. Hummerich and collaborators, with assistance from M. Templeton.
| + | |
| - | | + | |
| - | <br>
| + | |
| - | | + | |
| - | <br>
| + | |
| - | | + | |
| - | = '''Nova Cygni 2014 PNV J20214234+3103296''' =
| + | |
| - | | + | |
| - | Alert osservativa AAVSO N.500 da notizia di una brillante nova nel Cigno al momento della scoperta di magnitudine 10.9 non filtrata quindi alla portata di piccoli strumenti e chi volesse anche visuale.Ogni tipo di osservazione è consigliata anche filtrate vista la natura abbastanza rossastra della stella. Per il momento in mancanza di designazione le osservazioni vanno inviate ad AAVSO con il nome NOVA Cyg 20014
| + | |
| - | | + | |
| - | Da spettri raccolti la stella risulta essere una classica nova di tipi Fe-II vicina al massimo.
| + | |
| - | | + | |
| - | [[Image:Nova Cyg 2014.jpg]]
| + | |
| - | | + | |
| - | foto di campo di Gianluca Masi
| + | |
| - | | + | |
| - | <br> | + | |
| - | | + | |
| - | [[Image:Nova-Cyg2014-chart.jpg]]
| + | |
| - | | + | |
| - | di seguito l'allerta e coordinate
| + | |
| - | | + | |
| - | Event: Nova Cygni 2014 = PNV J20214234+3103296
| + | |
| - | | + | |
| - | Discovered by: Koichi Nishiyama (Kurume, Japan) and Fujio Kabashima (Miyaki, Japan)
| + | |
| - | | + | |
| - | Discovery magnitude: magnitude 10.9 unfiltered CCD, using a 105-mm-f.l. f/4 camera lens (+ SBIG STL6303E camera)
| + | |
| - | | + | |
| - | Discovery date: 2014 Mar. 31.790 UT
| + | |
| - | | + | |
| - | Coordinates: '''R.A. 20 21 42.32, Decl. +31 03 29.4''' (equinox 2000.0) from G. Masi, F. Nocentini, and P. Schmeer, remotely as described below, via CBET 3842
| + | |
| - | | + | |
| - | Spectra: Spectra obtained on 2014 Apr. 1 by U. Munari et al. (Istituto Nazionale di Astrofisica, Padova Astron. Obs., Italy), by A. Arai et al. (Nishi-Harima Astron. Obs., University of Hyogo, Japan), by K. Ayani (Bisei Astron. Obs., Ibara, Okayama, Japan), and by M. Fujii (Fujii Kurosaki Obs., Kurashiki, Okayama, Japan) all indicate a highly reddened classical Fe II-type nova around maximum. See CBET 3842 for spectra details; spectra URLs in Note f.
| + | |
| - | | + | |
| - | Observing recommendations: Observations of all types (visual, CCD, DSLR, spectroscopy) are strongly encouraged in following the evolution of this nova. Filtered observations are preferred if possible due to the reddened nature of this object.
| + | |
| - | | + | |
| - | Charts: Nova Cyg 2014 has been added to the International Variable Star Index (VSX, http://www.aavso.org/vsx). Finder charts with a comparison star sequence may be created using the AAVSO Variable Star Plotter (VSP, http://www.aavso.org/vsp).
| + | |
| - | | + | |
| - | <br> Submit observations: Please submit observations to the AAVSO International Database using the name NOVA CYG 2014. Once a GCVS name has been assigned, please use that name. | + | |
| - | | + | |
| - | <br>
| + | |
| - | | + | |
| - | = Nova Sagittarii 2014 = PNV J18250860-2236024 =
| + | |
| - | | + | |
| - | Spettri a bassa risoluzione della stella hanno rivelato trattarsi di una classica nova FE II-tipo past massimo. Scesa nei giorni scorsi alla 11.5V è risalita alla 9.8V. Osservazioni di qualsiasi tipo anche visuali sono richieste da AAVSO nella loro alert 497 che allego. Le osservazioni inviate al database aavso devono avere come nome della stella NOVA SGR 2014
| + | |
| - | | + | |
| - | February 11, 2014
| + | |
| - | | + | |
| - | 1. Event: Nova Sagittarii 2014 = PNV J18250860-2236024
| + | |
| - | | + | |
| - | Discovered by: Sigeru Furuyama (Tone-machi, Ibaraki-ken, Japan) and reported by S. Nakano (Sumoto, Japan)
| + | |
| - | | + | |
| - | Discovery magnitude: unfiltered CCD magnitude 8.7, using a 200-mm f/2.8 camera lens + BJ-42L camera
| + | |
| - | | + | |
| - | Discovery date: 2014 Jan. 26.857 UT
| + | |
| - | | + | |
| - | Coordinates: R.A. 18 25 08.60 Decl. = -22 36 02.4 (2000.0)
| + | |
| - | | + | |
| - | Spectra: Low-resolution spectra obtained by A. Arai (Nishi-Harima Astronomical Observatory, University of Hyogo, Japan) on 2014 Jan. 30.87 UT indicate that the object is a Fe II-type classical nova past maximum. Spectroscopy details may be found in CBET 3802 (see Note a below).
| + | |
| - | | + | |
| - | Observing recommendations: Nova Sgr 2014, which had faded to 11.5 V, has brightened to visual magnitude 9.8. Observations of all types (visual, CCD, DSLR, spectroscopy) are strongly encouraged in following the evolution of this nova.
| + | |
| - | | + | |
| - | Charts: Charts for Nova Sgr 2014 may be created using the AAVSO Variable Star Plotter (VSP) at http://www.aavso.org/vsp.
| + | |
| - | | + | |
| - | Observations reported to the AAVSO: 2014 Jan. 27.847 UT, 9.6 (T. Noguchi, Katori, Chiba-ken, Japan, confirming observation, CBET 3802); 28.32640, 10.1 (AAX, A. Amorim, Florianopolis, Brazil); 28.48056, 10.2 (SLH, L. Shotter, Uniontown, PA); 28.83889, 10.5 (PEX, A. Pearce, Nedlands, W. Australia); 28.876, 10.19 V (KSI, S. Kiyota, Kamagaya, Japan, CBET 3802); 28.876, 9.72 Rc (Kiyota, CBET 3802); 28.876, 9.15 Ic (Kiyota, CBET 3802); 29.31460, 10.5 (Amorim); 29.39323, 10.585 +/-0.012 V (HMB, J. Hambsch, Mol, Belgium, remotely at San Pedro de Atacama, Chile); 29.39363, 9.223 +/-0.023 I (Hambsch); 30.39456, 10.826 +/-0.014 V (Hambsch); 30.39496, 9.385 +/-0.024 I (Hambsch); 31.30830, 11.0 (Amorim); 31.39523, 10.964 +/-0.014 V (Hambsch); 31.39563, 9.433 +/-0.025 I (Hambsch); Feb. 01.31250, 11.0 (Amorim); 01.39527, 10.981 +/-0.014 V (Hambsch); 01.39565, 9.563 +/-0.026 I (Hambsch); 02.31180, 11.2 (Amorim); 02.39615, 11.379 +/-0.020 V (Hambsch); 02.39656, 9.787 +/-0.042 I (Hambsch); 02.862, 10.7 (K. Kadota, Ageo, Saitama-ken, Japan, CBET 3802); 03.31250, 11.5 (Amorim); 03.39598, 11.513 +/-0.020 V (Hambsch); 03.39639, 10.028 +/-0.048 I (Hambsch); 04.39677, 11.432 +/-0.017 V (Hambsch); 04.39717, 10.239 +/-0.033 I (Hambsch); 06.39971, 10.990 +/-0.016 V (Hambsch); 06.40025, 10.177 +/-0.039 I (Hambsch); 07.39994, 11.172 +/-0.012 V (Hambsch); 07.40035, 10.333 +/-0.028 I (Hambsch); 08.30000, 11.1 (Amorim); 08.83403, 10.9 (Pearce); 09.39966, 10.604 +/-0.012 V (Hambsch); 09.40008, 9.786 +/-0.030 I (Hambsch); 09.82850, 10.8 (Pearce); 10.40196, 10.063 +/-0.010 V (Hambsch); 10.40237, 9.259 +/-0.026 I (Hambsch); 10.85140, 9.8 (Pearce);
| + | |
| - | | + | |
| - | Submit observations: Please submit observations to the AAVSO International Database using the name NOVA SGR 2014. Once a GCVS name has been assigned, please use that name.
| + | |
| - | | + | |
| - | = <br> =
| + | |
i dati sottoporli ad aavso come NOVA OPH 2015 NO. 2 rispettando gli spazi visto che non ha ancora una designazione definitiva
Event: Nova Oph 2015 No. 2 = TCP J17344775-2409042
Coordinates (2000.0): R.A. 17 34 47.75 Dec -24 09 04.2 (Nishiyama and Kabashima, in VSX)
Spectra: A low resolution spectrum obtained at Van Vleck Observatory by C. Littlefield (Wesleyan University) and P. Garnavich (Notre Dame) on 2015 October 11.99 UT across an airmass range of 3.6-4.5, which yielded noisy data, indicate the nova to be an Fe II-type classical nova (ATel #8156). Spectra by M. Fujii (Kurashiki, Okayama, Japan) obtained on 2015 October 12.421 UT at Fujii Kurosaki Observatory indicate a highly reddened nova (CBET 4150). His spectrogram is posted at http://otobs.org/FBO/etc/tcp_oph.htm.
Observing recommendations: This nova is faint, but observations of all types (visual, CCD, DSLR, spectroscopy) as instrumentation permits are strongly encouraged as this nova evolves.
Charts: Charts for Nova Oph 2015 No. 2 may be created using the AAVSO Variable Star Plotter (VSP). Be sure to include spaces in the name as shown.
Oct. 7.405, <13.4 (Nishiyama and Kabashima);
11.394, 12.0 unfiltered (T. Kojima, Tsumagoi, Gunma-ken, Japan, pre-discovery observation);
11.490, 11.7 unfiltered CCD (S. Fujikawa, Kan'onji, Kagawa, Japan, confirming image);
11.721, 11.2 CR (G. Masi, remotely using the 17"-f/6.8 robotic unit part of the Virtual Telescope Project facility at Bellatrix Astronomical Observatory,Ceccano, Italy);
12.06870 UT, 9.90 I +/-0.07 (S. O'Connor, St. George, Bermuda);
12.07110, 11.89 V +/-0.03 (O'Connor);
12.07380, 11.70 CV +/-0.04 (O'Connor);
12.0900, 13.65 B (S. Kiyota, Kamagaya, Japan, remotely using 0.50-m f/4.5 CDK astrograph + FLI-PL11002M CCD f iTelescope.NET at Mayhill, NM, USA);
12.0900, 12.04 V (Kiyota);
12.0900, 11.12 Rc (Kiyota);
12.0900, 10.09 Ic (Kiyota);
13.38560, 11.56 R +/-0.05 (O'Connor);
13.407, 12.9 V (T. Yusa, Osaki, Japan, remotely using the 0.43-m f/6.8 astrograph + CCD(FLI Proline 16803)at the iTelescopeNET, Siding Spring, Australia).
14.05870, 10.4 I +/-0.1 (O'Connor);
14.06100, 13.33 V +/-0.08 (O'Connor);
14.06350, 12.82 CV +/-V0.03 (O'Connor);
14.06944, <11.2 (S. Aguirre, Hermosillo, Mexico);
14.37700, 10.68 I +/-0.05 (O'Connor);
14.37840, 12.05 R +/-0.05 (O'Connor);
14.37990, 13.32 V +/-0.02 (O'Connor);
14.38120, 14.00 TB +/-0.14 (O'Connor);
14.38120, 14.87 TB +/-0.04 (O'Connor);
14.38250, 13.00 CV +/-0.02 (O'Connor);
