March 14, 2024
AAVSO Forum threads (scroll to the bottom of a thread for latest posts):
- Time Sensitive Alerts: https://www.aavso.org/n-oph-2024-v-4370-oph-tcp-j-17395720-2627410
- Novae: https://www.aavso.org/node/90814
Please subscribe to these threads if you are observing this nova so you can be updated as to its behavior and any observing campaigns on it. Join in the discussion or ask questions there!
Event: Nova in Ophiuchus: N Oph 2024 = V4370 Oph = TCP J17395720-2627410
Discovered independently by:
- Tadashi Kojima (Tsumagoi, Gunma-ken, Japan)
- Koichi Itagaki (Yamagata, Japan)
- Yuji Nakamura (Kameyama, Mie, Japan)
- Minoru Yamamoto (Okazaki, Aichi, Japan)
- Shigehisa Fujikawa (Kan'onji, Kagawa, Japan)
- Andrew Pearce (Nedlands, Western Australia)
Discovery magnitude:
- Kojima - 11.5 unfiltered CCD with a Canon EOS 6D camera + 200-mm-f.l. f/3.2 lens
- Itagaki - 10.9 unfiltered CCD
- Nakamura - 11.1 unfiltered with a 135-mm-f.l. lens + CMOS camera
- Yamamoto - 11.1 unfiltered CCD with a Canon EOS 6D camera + 180-mm-f.l. lens
- Fujikawa - 10.4 unfiltered with a digital camera + 120-mm-f.l. lens
- Pearce - 10.2 unfiltered CCD with a Canon 800D camera (+ 85-mm-f.l. f/1.2 lens)
Discovery date:
- Kojima - 2024 Mar. 10.775 UT
- Itagaki - Mar. 10.818 UT
- Nakamura - Mar. 10.797 UT
- Yamamoto - Mar. 10.807 UT
- Fujikawa - Mar. 10.825 UT
- Pearce - Mar. 10.772 UT
Coordinates (2000.0): R.A. 17 39 57.00 Decl. -26 27 41.0 (from VSX page for V4370 Oph)
Spectra: Spectra indicating the object to be a classical nova were obtained by M. Uemura and T. Nakaoka (Hiroshima University), who report that spectra obtained on 2024 Mar. 10.84 UT with the Higashi-Hiroshima Astronomical Observatory 1.5-m "Kanata" telescope suggest that TCP J17395720-2627410 is a highly reddened He/N-class nova (https://www.astronomerstelegram.org/?read=16521) (via CBET 5365).
Observing recommendations: Please observe V4370 Oph as it continues to evolve, with observations of all types (visual, CCD/CMOS, DSLR, spectroscopy) and multiple bands as instrumentation permits. Frequency of observation depends on the rate of decline, but Dr. Fred Walter (Stony Brook University) recommends a minimum of one observation per night per band.
For spectroscopy, Dr. Walter recommends spectra in blue to observe He II 4686, H-beta, and the Bowen blend (4640A), in addition to H-alpha. Cadence for spectra depends on how fast the nova continues to evolve, but, he adds, "you can't go wrong with a spectrum every clear night." AAVSO Spectroscopy Section co-leader Lauren Herrington adds: "Slitless spectra would also be valuable; spectra with resolution as low as R=100 are useful to track broad changes in emission as the nova evolves."
Observations reported to the AAVSO:
2024 Feb. 27.816 UT, <13.0 unfiltered (Nakamura, via CBET 5365);
Mar. 06.807 <13.2 unfiltered (Kojima, via CBET 5365);
08.77153, <12.0 (Pearce);
08.772, <12.0 unfiltered (Pearce);
09.771, <12.0 unfiltered (Pearce);
09.77222, <12.0 (Pearce);
09.81, <15 unfiltered (Yamamoto, via CBET 5365);
10.77222, 11.3 (Pearce);
10.784 11.3 unfiltered (Kojima, via CBET 5365);
10.852, 10.4 unfiltered (A. Takao, Kitakyushu, Japan, via CBET 5365);
10.852, 10.9 unfiltered (Fujikawa, via CBET 5365);
11.107, 10.3 V (S. Korotkiy, K. Sokolovsky, S. Ostapenko, V. Belousov, and N. Potapov, apparently in Russia, via CBET 5365);
11.249, 10.3 (A. Amorim, Florianopolis, Brazil);
11.28889, 9.78 TR +/-0.05 (V. Cseh, Debrecen, Hungary);
11.296, 10.34 V (Yoshimoto, via CBET 5365);
11.296, 11.75 B (K. Yoshimoto, Yamaguchi, Japan, remotely at "Deep Sky Chile", via CBET 5365);
11.296, 7.82 I (Yoshimoto, via CBET 5365);
11.32014, 10.2 (Pearce);
11.68419, 12.684 B +/-0.005 (Pearce, remotely using a 0.50-m f/6.8 reflector at Siding Spring, NSW, Australia);
11.68498, 11.033 V +/-0.002 (Pearce, remotely);
11.68575, 9.394 R +/-0.007 (Pearce, remotely);
11.68657, 7.984 I +/-0.022 (Pearce, remotely);
11.77108, 10.837 V +/-0.004 (Pearce, remotely);
11.77108, 12.176 B +/-0.011 (Pearce, remotely);
11.77108, 9.746 TR+/-0.003 (Pearce, remotely);
11.77472, 10.825 V +/-0.005 (Pearce, remotely);
11.77472, 12.273 B +/-0.012 (Pearce, remotely);
11.77472, 9.824 TR+/-0.004 (Pearce, remotely);
11.77708, 11.3 (Pearce);
11.77846, 10.859 V +/-0.005 (Pearce, remotely);
11.77846, 12.253 B +/-0.013 (Pearce, remotely);
11.77846, 9.803 TR +/-0.004 (Pearce, remotely);
12.19792, 11.9 (A. Padilla Filho, Petropolis, Brazil);
12.2895, 12.0: (A Amorim, Florianopolis, Brazil);
12.68929, 13.774 B +/-0.009 (Pearce, remotely);
12.69009, 12.228 V +/-0.003 (Pearce, remotely);
12.69087, 10.228 R +/-0.001 (Pearce, remotely);
12.69162, 8.879 I +/-0.011 (Pearce, remotely);
12.81597, 12.2 (Pearce);
13.39188, 9.564 I +/-0.028 (J.-F. Hambsch, remotely from Atacama, Chile);
13.39204, 10.072 I +/-0.055 (Hambsch, remotely);
13.39249, 12.857 V +/-0.077 (Hambsch, remotely);
13.39284, 14.169 B +/-0.024 (Hambsch, remotely);
13.39323, 14.330 B +/-0.056 (Hambsch, remotely);
13.39358, 10.541 R +/-0.013 (Hambsch, remotely);
13.39380, 10.832 R +/-0.006 (Hambsch, remotely);
13.68946, 14.620 B +/-0.033 (Pearce, remotely);
13.69020, 13.019 V +/-0.005 (Pearce, remotely);
13.69093, 10.642 R +/-0.001 (Pearce, remotely);
13.69169, 9.441 I +/-0.002 (Pearce, remotely);
Charts: Charts with comparison stars for V4370 Oph may be created using the AAVSO Variable Star Plotter (VSP).
Submit observations: Please submit observations using the name V4370 OPH.
- Submit optical observations to the AAVSO International Database using WebObs.
- Submit spectra to the AAVSO Spectroscopy Database (AVSpec).
Notes:
a. Designated TCP J17395720-2627410 when posted by T. Kojima to the IAU Central Bureau for Astronomical Telegrams Transient Object Confirmation Page (TOCP). It was designated TCP J17395699-2627413 when posted by K. Itagaki to the TOCP page.
b. Except for Pearce, discovery information is from IAU CBAT CBET 5365, D. W. E. Green, Ed.
c. A. Pearce reports on Mar. 13 that "further astrometry of the nova as it has faded [shows that] there is no catalogued Gaia DR3 source matching the nova position within the uncertainties. Position is 1.1" away from a Gaia 18.9 G magnitude star (Gaia DR3 4061829569164264576). More accurate end figures are 57.07s, 41.9s. Nothing else is visible on PANSTARRS or DeCAPS images so the progenitor must be fainter than, say, mag 22."
d. Images
- K. Yoshimoto (2024 Mar. 11.296 UT, via CBET 5365): http://orange.zero.jp/k-yoshimoto/TCP_J17395720-2627410_20240311.jpg
e. E. Kazarovets writes that the GCVS name V4370 Oph has been assigned to N Oph 2024 (CBET 5365).
Congratulations to Tadashi Kojima, Koichi Itagaki, Yuji Nakamura, Minoru Yamamoto, Shigehisa Fujikawa, and Andrew Pearce on their independent discoveries!
This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.
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