Nova in Lup: V462 Lup (N Lup 2025 = ASASSN-25cm = AT 2025nlr)
Abstract:
V462 Lup (N Lup 2025 = ASASSN-25cm = AT 2025nlr) was discovered by the ASAS-SN survey (K. Z. Stanek reporting for the ASAS-SN team) on 2025 June 12. 8700 UT, magnitude 8.7 Sloan g. SPECTROSCOPY by Y. Tampo (SAAO) using the SAAO 1-m Lesedi telescope on 2025 June 14.745 UT shows a classical nova (ATel #17228, https://www.astronomerstelegram.org/?read=17228). COORDINATES (J 2000): RA 15 08 03.27 Dec. -40 08 29.6. PROGENITOR: S. Otero (AAVSO) reports the approximate minimum of the nova is 22.3: B, obtained from a MAMA srcj plate. PHOTOMETRY: see Justification. View the light curve via the AAVSO Light Curve Generator (https://www.aavso.org/LCGv2/).
Justification:
The AAVSO requests coverage of this nova with observations of all types (visual, CCD/CMOS, DSLR, PEP, spectroscopy) and in all filters as it evolves. All novae are worthy of as good coverage as possible for as long as possible to support research on novae being carried out now and in the future. Spectroscopy is also encouraged where possible. See sections below for cadence and other observing recommendations. NOTE: E. Kazarovets (Inst. of Astronomy, Moscow) reports assignment of the GCVS name V462 Lup (via CBET 5570, D. W. E. Green, Ed.). PHOTOMETRY (selected from observations submitted to the AAVSO): 2025 Jun. 4.678 UT, <4.7 unfiltered (R. H. McNaught, Coonabarabran, NSW, Australia, using Canon EOS 6D camera (+ 135-mm-f.l. f/2.8 lens, McNaught obs selected from CBET 5570); 5.447, <13.2 (McNaught); 5.477, <12.8 (McNaught); 13.378, 8.0 unfiltered (McNaught); 13.590, 8.2 unfiltered (McNaught); 13.753, 8.2 unfiltered McNaught); 14.1674, 7.9 visual (L. Herrington, Ketchum, OK, USA); 14.2431, 7.8 visual (Herrington); 2025 June 14.304, 7.7 visual (P. Camilleri, Rolleston, NZ); 14.452, 8.1 visual (McNaught); 14.4936, 8.267 TB +/-0.003 (A. Pearce, Nedlands, W. Australia); 14.340, 7.8 unfiltered (McNaught); 14.4937, 8.320 TG +/-0.003 (Pearce); 14.4993, 8.1 visual (Pearce); 14.6994, 7.688 Ic +/-0.123 (M. Odeh, Abu Dhabi, UAE); 14.6996, 8.171 V +/-0.122 (Odeh); 14.6996, 8.267 B +/-0.229 (Odeh); 15.1384, 8.510 V +/-0.004 (F.-J. Hambsch, Mol, Belgium, remotely from Atacama, Chile); 15.1385, 7.279 I +/-0.008 (Hambsch); 15.1387, 8.660 B +/-0.003 (Hambsch); 15.3983, 7.254 V +/-0.011 (R. Axelsen, Kenmore, QLD, Australia); 15.408, 7.2 (McNaught); 15.6236, 7.0 (Pearce); 15.7292, 7.1 (K. Alburaidi, Bukayriyah, Al-Qassim, Saudi Arabia); 15.7631, 6.554 I +/-0.041 (Odeh); 15.7632, 6.902 V +/-0.086 (Odeh); 15.7632, 7.216 B +/-0.086 (Odeh); 15.7847, 6.709 TG +/-0.058 (M. Kolb, Wuppertal, Germany); 15.7873, 7.337 TB +/-0.104 (Kolb); 15.8924, 6.8 (Axelsen); 15.9479, 6.8 (W. de Souza, Sao Paulo, Brazil); 15.9583, 6.7 (J. Aguiar, Campinas, Brazil); 15.9725, 6.8226 CV +/-0.002 (J. Sanchez, Rosario, Argentina); 16.0049, 7.483 TG +/-0.009 (de Souza); 16.0757, 7.2 (P. Diaz, Argentina); 16.1639, 6.4 (Herrington); 16.383, 6.4 (McNaught); 16.4250, 6.4 (Pearce); 16.5701, 6.5 (Pearce); 16.7681, 6.7 (Alburaidi); 16.7738, 6.307 I +/-0.010 (Odeh); 16.7739, 6.693 V +/-0.075 (Odeh); 16.7739, 6.952 B +/-0.014 (Odeh). Download photometric/spectroscopic observations submitted to the AAVSO via the AAVSO Global Search (https://apps.aavso.org/v2/data/search/global/).
Requested Data Types:
Spectroscopy, Photometry
Targets
| Name | Magnitude | Variability Type | Photometry Notes | Spectroscopy Notes |
|---|---|---|---|---|
| N Lup 2025 | 6.80 | N |
Cadence: Custom Precision: 100 |
Cadence: Custom Resolution: 250 Desired SNR: 100 |
Spectroscopy Lines:
He II (4686.0 Å), H-beta (4861.0 Å), H-alpha (6563.0 Å)
Photometry Filters:
B (Johnson), V (Johnson), R (Cousins), I (Cousins), g (Sloan), r (Sloan), i (Sloan), z (Sloan), Other (Please Specify)
Comparison Stars:
Finder charts with comparison stars may be created using the AAVSO Variable Star Plotter (VSP, https://apps.aavso.org/vsp/). An 'AB' scale chart shows comp stars as bright as 5th mag, with one 2nd mag star.
Co-Authorship
Observers are eligible for co-authorship.
Additional Observer Input:
Additional photometry filters and cadence: also TB, TG, TR. Cadence depends on rate of change and other behavior of the nova, but at least one observation per night is recommended. Additional spectroscopy lines and cadence: Bowen blend (4640 A). 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." Former 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."
Additional Submission Location:
Not provided
Notes:
No public notes