ALERT OSSERVATIVI CATACLISMICHE E NOVAE - Cronologia

Marco il 11:48, 15 ott 2015

2015-10-15T11:48:07Z

← Versione meno recente		Versione delle 11:48, 15 ott 2015
Riga 7:		Riga 7:
	in V siamo sulla 13 a qualche giorno fa		in V siamo sulla 13 a qualche giorno fa

-	fare riferimento au aavso.org alert 531	+	fare riferimento ad  www.aavso.org alert 531

	per le carte sempre su aavso		per le carte sempre su aavso
Riga 13:		Riga 13:
	i dati sottoporli ad aavso come NOVA OPH 2015 NO. 2 rispettando gli spazi visto che non ha ancora una designazione definitiva		i dati sottoporli ad aavso come NOVA OPH 2015 NO. 2 rispettando gli spazi visto che non ha ancora una designazione definitiva

-	sono richieste osservazioni di qualsiasi tipo durante la fase di evoluzione della nova	+	sono richieste osservazioni di qualsiasi tipo durante la fase di evoluzione della nova

	<br>		<br>

Marco il 11:47, 15 ott 2015

2015-10-15T11:47:28Z

Marco il 11:45, 15 ott 2015

2015-10-15T11:45:50Z

Mostra cambiamenti

Marco il 14:19, 17 mar 2015

2015-03-17T14:19:42Z

← Versione meno recente		Versione delle 14:19, 17 mar 2015
Riga 1:		Riga 1:
-	= ~~GK Per in outburst~~ =	+	= Alert Notice 512: Nova Sagittarii 2015 No. 2 = PNV J18365700-2855420 =

-	~~L'avviso 399 da~~ AAVSO ~~indica la vecchia~~ Nova ~~(N Per 1901)~~ in ~~outburst.La nova ha degli outbursts ogni 18-24 mesi~~,~~sebbene l'intervallo possa variare leggermente.Difficile prevedere l'intensità dell'outburst corrente poichè l'intensità dei recenti outburst sono variate notevolmente.~~	+	Si riporta qui allerta AAVSO per una Nova in Sagittario al limite del visuale,cartine e dati su sito AAVSO come sempre
		+	March 16, 2015

-	~~L'ultimo outburst è avvenuto esattamente due anni fa,nel marzo 2013,quando ha raggiunto V=12~~.2 ~~per solo 17 giorni.~~	+	Event: Nova Sagittarii 2015 No. 2 = PNV J18365700-2855420

-	~~Il precedente avvenne nel marzo 2010 e raggiunse la V=9.7~~,~~il maggiore dal 1901.~~	+	Discovered by: John Seach, Chatsworth Island, NSW, Australia

-	~~'''Coordinate~~: R.~~A. 03 31 12.01 Dec. +43 54 15.4 (2000~~.0~~)'''<br>~~	+	Discovery magnitude: 6.0 using DSLR and 50mm f/1.0 lens
-	~~avviso AAVSO originale:~~	+

-	GK Per has dwarf nova outbursts about every 18-24 months, although the interval can vary quite a bit. It is difficult to predict how bright this outburst may be; the brightness and duration of recent GK Per outbursts has varied substantially.	+	Discovery date: 2015 March 15.634 UT

-	~~Its last outburst was almost exactly two years ago, in March 2013, when it reached V=12~~.~~2 and was brighter than V=12~~.8 ~~for only 17 days, according to the AAVSO International Database~~ (~~AAVSO Special Notice #343). That outburst is the faintest and shortest on record since July 1978~~.	+	Coordinates: R.A. 18 36 56.84 Dec. -28 55 39.8 (2000.0)

-	~~Its previous outburst was three years earlier, in March 2010, when it reached V=9~~.~~7 and was brighter than V=12~~.~~8 for at least 100 days~~ (the ~~exact number of days~~ is ~~unknown because GK Per returned to minimum during its seasonal gap~~), ~~according~~ to ~~the AAVSO International Database~~. ~~That outburst is the brightest on record since the~~ nova ~~outburst~~ in ~~1901~~. ~~The 2010 outburst brightness~~ may be ~~related to~~ the ~~long interval to the 2013 outburst~~, ~~as well as~~ to the ~~interval between the 2008 and 2010 outbursts~~, ~~which was six months shorter than usual~~. (~~The September 2008 outburst reached V=12~~.1 ~~and was brighter than 12~~.8 ~~for about 30 days~~.)	+	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.
		+
		+	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.
		+
		+	Observations reported to the AAVSO:
		+	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.

-	~~Please monitor GK Per and report your observations to the AAVSO, using the name GK PER.<br>le cartine di campo si possono creare qui   '''http://www.aavso.org/vsp'''~~

-	~~<br>~~

	= Allerta osservativa AAVSO nova simbiotica ASAS J174600-2321.3 =		= Allerta osservativa AAVSO nova simbiotica ASAS J174600-2321.3 =

Marco il 10:54, 13 mar 2015

2015-03-13T10:54:44Z

← Versione meno recente		Versione delle 10:54, 13 mar 2015
Riga 1:		Riga 1:
		+	= GK Per in outburst =
		+
		+	L'avviso 399 da AAVSO indica la vecchia Nova (N Per 1901) in outburst.La nova ha degli outbursts ogni 18-24 mesi,sebbene l'intervallo possa variare leggermente.Difficile prevedere l'intensità dell'outburst corrente poichè l'intensità dei recenti outburst sono variate notevolmente.
		+
		+	L'ultimo outburst è avvenuto esattamente due anni fa,nel marzo 2013,quando ha raggiunto V=12.2 per solo 17 giorni.
		+
		+	Il precedente avvenne nel marzo 2010 e raggiunse la V=9.7,il maggiore dal 1901.
		+
		+	'''Coordinate: R.A. 03 31 12.01 Dec. +43 54 15.4 (2000.0)'''<br>
		+	avviso AAVSO originale:
		+
		+	GK Per has dwarf nova outbursts about every 18-24 months, although the interval can vary quite a bit. It is difficult to predict how bright this outburst may be; the brightness and duration of recent GK Per outbursts has varied substantially.
		+
		+	Its last outburst was almost exactly two years ago, in March 2013, when it reached V=12.2 and was brighter than V=12.8 for only 17 days, according to the AAVSO International Database (AAVSO Special Notice #343). That outburst is the faintest and shortest on record since July 1978.
		+
		+	Its previous outburst was three years earlier, in March 2010, when it reached V=9.7 and was brighter than V=12.8 for at least 100 days (the exact number of days is unknown because GK Per returned to minimum during its seasonal gap), according to the AAVSO International Database. That outburst is the brightest on record since the nova outburst in 1901. The 2010 outburst brightness may be related to the long interval to the 2013 outburst, as well as to the interval between the 2008 and 2010 outbursts, which was six months shorter than usual. (The September 2008 outburst reached V=12.1 and was brighter than 12.8 for about 30 days.)
		+
		+	Please monitor GK Per and report your observations to the AAVSO, using the name GK PER.<br>le cartine di campo si possono creare qui   '''http://www.aavso.org/vsp'''
		+
		+	<br>
		+
	= Allerta osservativa AAVSO nova simbiotica ASAS J174600-2321.3 =		= Allerta osservativa AAVSO nova simbiotica ASAS J174600-2321.3 =

Riga 19:		Riga 40:
	"The deeply eclipsing system and likely symbiotic nova ASAS J174600-2321.3		"The deeply eclipsing system and likely symbiotic nova ASAS J174600-2321.3

-	=== RA: 17 46 00.18 , Dec: -23 21 16.4 (J2000.0) ===	+	=== 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.		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.
Riga 35:		Riga 56:
	These are the dates observers should keep in mind:		These are the dates observers should keep in mind:

-	=== 1st contact: 2015 March 14 (JD 2457096) ===	+	=== 1st contact: 2015 March 14 (JD 2457096) ===

	=== Mid-eclipse: 2015 May 11 (JD 2457153.5) ===		=== Mid-eclipse: 2015 May 11 (JD 2457153.5) ===

Marco il 15:06, 7 mar 2015

2015-03-07T15:06:42Z

← Versione meno recente		Versione delle 15:06, 7 mar 2015
Riga 1:		Riga 1:
		+	= Allerta osservativa AAVSO nova simbiotica ASAS J174600-2321.3 =
		+
		+	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
		+
		+	cartina Vis.
		+
		+	[[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''' =		= '''Nova Cygni 2014  PNV J20214234+3103296''' =

Marco il 11:26, 1 giu 2014

2014-06-01T11:26:45Z

← Versione meno recente		Versione delle 11:26, 1 giu 2014
Riga 33:		Riga 33:
	<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> 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>	+	<br>

	= Nova Sagittarii 2014 = PNV J18250860-2236024 =		= Nova Sagittarii 2014 = PNV J18250860-2236024 =

Marco il 10:24, 9 apr 2014

2014-04-09T10:24:56Z

← Versione meno recente		Versione delle 10:24, 9 apr 2014
Riga 61:		Riga 61:
	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.		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.

-	= ~~GR Ori in super-outburst =~~	+	= <br> =
-		+
-	Rod Stubbings dall'Australia riporta un outburst della sospetta vecchia nova (Nova Ori 1916),stimandola visualmente di magnitudine 13.0 a Febbraio 11.476 UT (JD 2456334.976).Questa osservazione è stata confermata da Stephen Howell (New Zealand),che ha ugualmente riportato la stella a magnitudine 13.0 Febbraio 11.461.Mike Simonsen (AAVSO) fa notare che la sospetta progenitrice di questa stella ha una magnitudine intorno alla 22.8 nella Sloan Digital Sky Survey,suggerendo un ampio outburst di 8-10 magnitudini,e che la stella potrebbe essere una WZ Sge dwarf nova piuttosto che una nova classica o ricorrente.La maggioranza delle osservazioni di questa stella sono visuali e il comportamento degli outburst è poco studiato.Naturalmente si sono notati aumenti di luminosità nei decenni passati.<br>~~Osservazioni di GR Ori,specialmente time series in V sono richieste ed aiuterebbero a comprendere meglio questo oggetto.~~	+
-		+
-	~~GR Ori si trova:<br>R.A. 05 21 34.98 Dec +01 10 10.2 (2000.0)~~	+
-		+
-	~~La sequenza e le stelle di confronto sono state aggiornate e si trovano sul sito AAVSO http://www.aavso.org/vsp~~	+
-		+
-	~~Per chi disponesse di un codice AAVSO le osservazioni vanno inviate come GR Ori~~	+
-		+
-	~~qui la alert AAVSO http://www.aavso.org/aavso-special-notice-334~~	+
-		+
-	~~[[Image:GROriField.jpg]]~~	+
-		+
-	~~22:05, 12 feb 2013 (UTC)~~	+

Marco il 10:12, 9 apr 2014

2014-04-09T10:12:04Z

← Versione meno recente		Versione delle 10:12, 9 apr 2014
Riga 9:		Riga 9:
	foto di campo di Gianluca Masi		foto di campo di Gianluca Masi

-	di seguito l'allerta e coordinate	+	<br>
		+
		+	[[Image:Nova-Cyg2014-chart.jpg]]
		+
		+	di seguito l'allerta e coordinate

	Event: Nova Cygni 2014 = PNV J20214234+3103296		Event: Nova Cygni 2014 = PNV J20214234+3103296

Marco il 09:44, 9 apr 2014

2014-04-09T09:44:17Z

← Versione meno recente		Versione delle 09:44, 9 apr 2014
Riga 9:		Riga 9:
	foto di campo di Gianluca Masi		foto di campo di Gianluca Masi

-	di seguito l'allerta	+	di seguito l'allerta e coordinate

	Event: Nova Cygni 2014 = PNV J20214234+3103296		Event: Nova Cygni 2014 = PNV J20214234+3103296
Riga 19:		Riga 19:
	Discovery date: 2014 Mar. 31.790 UT		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	+	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.		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.

← Versione meno recente		Versione delle 11:47, 15 ott 2015
Riga 1:		Riga 1:
-	October 14, 2015	+	October 14, 2015

-	Riporto qui Alert AAVSO per seconda Nova in Ofiuco	+	Riporto qui Alert AAVSO per seconda Nova in Ofiuco

-	risulta di 12.1 non filtrata al momento della scoperta	+	risulta di 12.1 non filtrata al momento della scoperta

-	in V siamo sulla 13 a qualche giorno fa	+	in V siamo sulla 13 a qualche giorno fa

-	fare riferimento au aavso.org alert 531	+	fare riferimento au aavso.org alert 531

-	per le carte sempre su aavso	+	per le carte sempre su aavso

-	i dati sottoporli ad aavso come NOVA OPH 2015 NO. 2 rispettando gli spazi visto che non ha ancora una designazione definitiva	+	i dati sottoporli ad aavso come NOVA OPH 2015 NO. 2 rispettando gli spazi visto che non ha ancora una designazione definitiva

		+	sono richieste osservazioni di qualsiasi tipo durante la fase di evoluzione della nova

		+	<br>

-	Event: Nova Oph 2015 No. 2 = TCP J17344775-2409042	+	Event: Nova Oph 2015 No. 2 = TCP J17344775-2409042

-	Independent discovery by: <br> - Koichi Nishiyama (Kurume, Japan) and Fujio Kabashima (Miyaki, Japan)<br> - Shigehisa Fujikawa (Kan'onji, Kagawa, Japan)	+	Independent discovery by: <br> - Koichi Nishiyama (Kurume, Japan) and Fujio Kabashima (Miyaki, Japan)<br> - Shigehisa Fujikawa (Kan'onji, Kagawa, Japan)

-	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)	+	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)

-	Discovery date:<br> - Nishiyama and Kabashima: 2015 October 11.4129 UT<br> - Fujikawa: 2015 Oct 11.41474 UT	+	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)	+	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.	+	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.	+	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.<br>		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>

	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);		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);