V2860 Orionis = PNV J06095740+1212255: very fast classical galactic nova

Alert Notice 676: Nova in Orion: N Ori 2019 = PNV J06095740+1212255

Update: Nova Orionis 2019 (PNV J06095740+1212255) has been assigned the name V2860 Orionis, according to E. V. Kazarovets (Institute of Astronomy, Russian Academy of Sciences). Please use V2680 ORI in reporting your observations.  -  Elizabeth O. Waagen, 15 August 2019

14 August 2019

AAVSO Forum threads (scroll to the bottom of a thread for latest posts):

- Novae: https://www.aavso.org/pnv-j060957401212255-possible-nova-94-mag-orion

- Time Sensitive Alerts: https://www.aavso.org/pnv-j060957401212255-possible-nova-94-mag-orion-0

Event:  Nova in Orion: N Ori 2019 = PNV J06095740+1212255

Discovered by: Shigehisa Fujikawa (Kan'onji, Kagawa, Japan)

Discovery magnitude: 9.4 unfiltered CCD (using a Minolta F 3.5 f 120mm lens, limiting mag 13.5)

Discovery date: 2019 August 07.7984 UT

Coordinates (2000.0): R.A. 06 09 57.45   Decl. +12 12 25.2  (from VSX)

Spectra: Spectroscopy obtained by E. Aydi et al. (ATel #13027) on 2019 August 14.44 UT using the Goodman spectrograph on the SOAR telescope indicates that N Ori 2019 is a very fast expanding classical He/N nova, possibly in the post-maximum phase.

Observing recommendations: Observations of all types (visual, CCD, DSLR, PEP, spectroscopy) and multiple bands as instrumentation permits are strongly encouraged as the nova evolves.

Observations reported to the AAVSO (for full list see AAVSO International Database):

2019 Aug. 08.34722 UT, 9.7 (A. Amorim, Florianopolis, Brazil);

08.40833, 9.8 (R. King, Duluth, MN);

08.43204, 10.131 V +/-0.008 (J.-F. Hambsch, remotely from ROAD Observatory, Atacama, Chile, selected dates from 42 obs Aug. 8-14);

08.43238, 7.939 I +/-0.008 (Hambsch);

08.43285, 10.928 B +/-0.011 (Hambsch);

08.7944, 10.17 V (S. Kiyota, Kamagaya, Japan, large error possible due to low altitude; via TOCP);

08.7944, 9.28 Ic (Kiyota, large error possible due to low altitude; via TOCP);

08.796, 10.64 cG (K. Yoshimoto, Yamaguchi-ken, Japan, Nikon D5100 digital camera; via TOCP);

09.09930, 10.7 (W. Kriebel, Schierling/Walkenstetten, Germany);

09.10903, 10.6 V (K. Wenzel, Grossostheim, Germany);

09.12479, 10.728 V +/-0.021 (S. Brincat, San Gwann, Malta, selected from 36 obs Aug. 9-11);

09.12548, 8.690 I +/-0.020 (Brincat);

09.12968, 10.724 V +/-0.016 (Brincat);

09.13031, 8.711 I +/-0.013 (Brincat);

09.34226, 10.1 CCD (no filter given; BRaTS patrol, reported by L. Amaral, Bilac, Brazil; via TOCP);

09.43137, 10.935 V +/-0.009 (Hambsch);

09.43171, 8.517 I +/-0.008 (Hambsch);

09.43218, 11.646 B +/-0.015 (Hambsch);

10.06809, 10.804 V +/-0.0333 (A. Nowak, Bilcza, Poland);

10.07531, 10.781 V +/-0.0462 (Nowak);

10.32986, <9.8 (A. Padilla Filho, Rio de Janerio, Brazil);

10.36528, 11.0 (L. Shotter, Uniontown, PA);

10.41073, 10.732 V +/-0.017 (K. Sokolovsky, Moscow, Russian Fed.);

10.41100, 10.676 V +/-0.012 (Sokolovsky);

10.41125, 10.738 V +/-0.015 (Sokolovsky);

10.43122, 11.162 V +/-0.011 (Hambsch);

10.43156, 8.758 I +/-0.009 (Hambsch);

10.43203, 11.867 B +/-0.017 (Hambsch);

10.788, 10.1 (K. Itagaki (Yamagata, Japan; via TOCP);

11.10764, 10.35 CV (Wenzel);

11.12075, 11.395 V +/-0.014 (Brincat);

11.12125, 9.184 I +/-0.009 (Brincat);

11.12755, 11.312 V +/-0.014 (Brincat);

11.12806, 9.224 I +/-0.009 (Brincat);

11.13435, 11.344 V +/-0.019 (Brincat);

11.13495, 9.247 I +/-0.010 (Brincat);

11.43049, 11.348 V +/-0.012 (Hambsch);

11.43083, 8.909 I +/-0.009 (Hambsch);

11.43128, 12.029 B +/-0.021 (Hambsch);

12.09600, 11.7 (W. Vollmann, Vienna, Austria);

12.38542, 11.4 (Shotter);

12.42998, 11.533 V +/-0.013 (Hambsch);

12.43032, 9.108 I +/-0.010 (Hambsch);

12.43080, 12.133 B +/-0.023 (Hambsch);

13.42988, 11.708 V +/-0.015 (Hambsch);

13.43023, 9.345 I +/-0.011 (Hambsch);

13.43069, 12.355 B +/-0.027 (Hambsch);

14.42924, 12.058 V +/-0.019 (Hambsch);

14.42958, 9.659 I +/-0.014 (Hambsch);

14.43005, 12.557 B +/-0.029 (Hambsch);

Charts: Charts with comparison stars for N Ori 2019 may be created using the AAVSO Variable Star Plotter (VSP).

Submit observations: Please submit observations to the AAVSO International Database using the name N ORI 2019. When a GCVS name is announced in an IAU Circular or CBET, please use that name.

Notes:

a. Designated PNV J06095740+1212255 when posted to the IAU Central Bureau for Astronomical Telegrams Transient Object Confirmation Page (TOCP). Some information in this Alert Notice is taken from the TOCP page.

b. P. Schmeer (Saarbrücken-Bischmisheim, Germany) reports that a blue star (mag. 19) 1" from the reported postion has the following names: USNO-A2.0 0975-02661189 (Bmag. 19.7, Rmag. 19.2), USNO-B1.0 1022-0102056, GSC2.3 N80U009326 (Fmag. 19.24, Bjmag. 20.11), WISE J060957.44+121224.9, IPHAS J060957.45+121225.2; and gives Gaia DR2 position end figures 57.453s 25.15" (equinox J2000.0, epoch 2015.5, Gmag. 19.18).

c. K. Sokolovsky et al. (ATel #13029) report that Swift observations obtained on 2019 August 14.172 UT did not show X-ray emission.

d. Position end figures

- K. Yoshimoto, Yamaguchi-ken, Japan (2019 Aug. 08.796 UT, via CBAT TOCP): 57.41s, 24.9"

e. Images

- K. Itagaki, Yamagata, Japan (2019 Aug. 10.788 UT, via CBAT TOCP): http://k-itagaki.jp/images/PN-Ori.jpg

Congratulations to Shigehisa Fujikawa on his latest discovery!

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.

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AAVSO Alert Notice 675: 

V386 Serpentis – 2nd rescheduling of Hubble Space Telescope observations

2 August 2019

Further to AAVSO Alert Notices 669 and 667, Dr. Paula Szkody (University of Washington) informs us that the HST observations of the cataclysmic variable V386 Ser originally scheduled for June and rescheduled to early August have been rescheduled again for 2019 August 15 or 16 (the exact date and time are not yet known).

It is essential to continue obtaining nightly snapshots in order to know the status of this system from now through the HST observation window. Your patience with these reschedulings is very much appreciated, as are your ongoing crucial observations!

Please continue obtaining nightly snapshots through August 23. They are particularly important from August 4 on, when frequent reports will have to be relayed to the HST scheduling team. Intensive monitoring is requested August 12 through August 17; this period of intensive monitoring may be adjusted when the exact time of the HST observations is known. When the exact time is known, it will be posted to the AAVSO forum thread on this campaign (see above) and this Alert Notice will be updated online. During the period of intensive observations, prompt submission of observations will be critical.

AAVSO observations are essential to know the state of the V386 Ser system in order to ensure that the system is NOT in outburst when observed with HST. AAVSO observations made 24 hours before the HST observing time will be used to make a go/no-go decision; AAVSO data will be used in the analysis of the resulting HST data.

V386 Ser (UGWZ+ZZ/GWLIB = WZ Sge type with a non-radially pulsating white dwarf) is faint at quiescence (V~19.2). It had an outburst in January 2019, and on 2019 August 2.0795 UT it was CV = 17.815 +/-0.063 (F.-J. Hambsch, Mol, Belgium). There is a V=17.757 star to the NW of the variable (178 in the AAVSO comparison star sequence; R.A. 16 10 33.15 Dec. -01 02 14.2); knowing whether the variable is fainter than, comparable to, or brighter than it will be very useful.

If visual observers are unable to detect V836 Ser, please report any "fainter-than" estimates using the magnitude of the faintest comparison star magnitude seen. CCD observers are asked to use filters during observations if available; V is preferred. Detection of the variable itself is not required unless you can reach V=18.4 in reasonable time, but please use sufficient exposure to detect at least the 178 comparison star with a S/N of 10 and report the observation as a "fainter-than" observation. V386 Ser may be as bright as V=10.4 in outburst.

Coordinates (J2000): R.A. 16 10 33.63  Dec. -01 02 23.2

Charts with comparison stars for V386 Ser may be created using the AAVSO Variable Star Plotter (VSP).

Please report all observations to the AAVSO International Database using the name V386 SER.

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.

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AAVSO Alert Notice 674:

UU Aquarii being observed with the Chandra X-ray Observatory on August 3

25 July 2019

AAVSO Forum threads (scroll to the bottom of a thread for latest posts):

– Campaigns and Observing Reports: https://www.aavso.org/six-novalikes-2018-campaign

– Cataclysmic Variables: https://www.aavso.org/six-novalikes-2018-campaign-01

Further to AAVSO Alert Notice 652, Dr. Koji Mukai (NASA Goddard Space Flight Center) informs us that UU Aqr, the last of the nova-like variables in his target list, will be observed with Chandra on 2019 August 3 06:16 UT – 10:10 UT.

Knowing the status of the target is essential for interpreting the X-ray data. Dr. Mukai thanks observers for the observations they have already made of UU Aqr, and asks if more observations (a snapshot every night through August 4, and then every one to two nights) could be made between now and August 13. V filter is optimal. Visual observations are welcome. The CV range of UU Aqr is 12.85 – 15.5 V.

As Dr. Mukai wrote in Alert Notice 652, "We think we know how dwarf novae behave in X-rays, through various campaigns (famously that one on SS Cyg in outburst that Janet Mattei [and AAVSO observers] was heavily involved in, with Pete Wheatley and Chris Mauche, 2003MNRAS.345...49W): they are X-ray bright in optical quiescence, and fainter and softer in X-rays during outburst. In the optical, we think of nova-likes as systems in permanent outburst — but in X-rays, they don’t quite resemble dwarf novae in outburst. In fact, we haven’t seen a clear pattern, when we made X-ray observations of nova-like systems at various optical magnitudes. This Chandra program is part of an effort to look for patterns and to understand their X-ray emission."

UU Aqr is the sixth and final target on the list given in Alert Notice 652 (KQ Mon, V378 Peg, EC 21178-5417, 1SWASP J022916.91-395901.4, LQ Peg, UU Aqr). Once UU Aqr has been observed successfully with Chandra, this campaign will come to a close, and no additional observations of any of the targets will be required.

Coordinates (2000) of UU Aqr: RA  22 09 05.70  Dec -03 46 17.5

Charts with comparison star sequences for UU Aqr may be created using the AAVSO Variable Star Plotter (VSP).

Please submit observations to the AAVSO International Database using the name UU AQR.

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.

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AAVSO Alert Notice 673: 

SS Cygni photometry and spectroscopy requested to complement Transiting Exoplanet Survey Satellite (TESS) monitoring

25 July 2019

AAVSO Forum threads (scroll to the bottom of a thread for latest posts):

– Campaigns and Observing Reports: https://www.aavso.org/ss-cyg-tess-2019

– Cataclysmic Variables: https://www.aavso.org/ss-cyg-tess-2019-01

Dr. Stella Kafka (AAVSO) has requested multicolor photometry and spectra of the dwarf nova SS Cyg to complement monitoring by the TESS satellite taking place now to mid-September.

Dr. Kafka writes: "With more than 100 years of observations in the AAVSO International Database, SS Cyg is one of the best observed dwarf novae – and one of the most rewarding targets in the night sky. SS Cyg will be observed with TESS from mid-July to mid-September. The TESS dataset will provide uninterrupted observations of the target for about 2 months. This is a unique opportunity to complement satellite data with multi-color ground-based photometric observations and small telescope spectra and uniquely capture quiescence behavior and expected outbursts of the system."

Coverage is requested now through September 2019. Filtered photometry (all filters) is requested. Spectroscopy is also requested. Visual observations are welcome to complement the filtered photometry. SS Cyg (V=8.0~12.4) is currently nearly back at minimum following an outburst that occurred on 2019 July 11.

Coordinates for SS Cyg (J2000): RA 21 42 42.79  Dec +43 35 09.9

Finder charts with comparison stars for SS Cyg may be created using the AAVSO Variable Star Plotter (VSP).

Optical observations should be submitted to the AAVSO International Database using the name SS CYG.

For information on submitting spectra to the AAVSO Spectroscopy Database, please see the bottom of the AAVSO Spectroscopy Section webpage (https://www.aavso.org/spectroscopy-observing-section).

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.

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