Nova in Vulpecula: V615 Vul ( = N Vul 2024 = PNV J19430751+2100204)
Active Dates: Aug. 2, 2024 – Aug. 31, 2025
Abstract:
V615 Vul ( = N Vul 2024 = PNV J19430751+2100204) was discovered on 2024 July 29.832 UT at unfiltered CCD magnitude 11.2 by the New Milky Way (NMW) survey, and reported on behalf of the survey team by K. Sokolovsky (University of Illinois and Sternberg Astronomical Institute), S. Korotkiy, N. Potapov, and S. Ostapenko; images were obtained with a 135-mm-f.l. f/2.0 telephoto lens (IAU CBAT Transient Object Confirmation Page; CBET 5423). It was confirmed as a highly reddened galactic nova by K. Taguchi (ATel #16743) on 2024 July 30.47 UT and by P. Valisa and U. Munari (ATel #16746) on July 30.869 UT. Ongoing photometry and spectroscopy are requested. Coordinates (2000): RA 19 43 07.50 DEC 19 43 07.50 +21 00 21.4 URLs: IAU CBAT TOCP (http://www.cbat.eps.harvard.edu/unconf/followups/J19430751+2100204.html); ATel #16743 ( (https://www.astronomerstelegram.org/?read=16743)); ATel #16746 (https://www.astronomerstelegram.org/?read=16746).
Justification:
Optical coverage of N Vul 2024 as it evolves is needed to build the light curve to be used for reference and analysis; coverage until after the nova returns to minimum is essential for studies of long-term behavior of novae. Spectroscopic coverage contributes to understanding the processes taking place during the evolution of the eruption.
Requested Data Types:
Spectroscopy, Photometry
Targets
| Name | Magnitude | Variability Type | Photometry Notes | Spectroscopy Notes |
|---|---|---|---|---|
| N Vul 2024 | 9.80 | N |
Cadence: Custom Precision: 100 |
Cadence: Custom Resolution: 1000 Desired SNR: 100 |
Spectroscopy Lines:
H-beta (4861.0 Å), H-alpha (6563.0 Å)
Photometry Filters:
B (Johnson), V (Johnson), R (Cousins), I (Cousins)
Comparison Stars:
No comparison stars provided
Co-Authorship
Observers are not eligible for co-authorship.
Additional Observer Input:
Visual observations are welcome. Cadence for photometry is one to multiple times per night as the nova evolves. Please be sure to check your reduced photometry for errors before uploading to the AAVSO. Spectroscopy cadence is also variable, with one spectrum per night suggested; more frequent observations may be warranted, depending on the behavior of the nova. Additional spectroscopy line: Bowen blend (4640 Å). 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:
none
Notes:
Recent observations of V615 Vul submitted to the AAVSO International Database include: 2024 Jul 28.840, <14.5 unfiltered CCD (NMW survey, via CBET 5423); Jul. 29.8317 UT, 11.2 CV +/-0.05 (K. Sokolovsky, Moscow, Russian Fed.); Jul. 29.892, 10.94 CV +/-0.05 (Sokolovsky); Jul. 30.57551, 9.671 V +/-0.051 (A. Pearce, Broadway Nedlands, W. Australia); Jul. 30 - Jul. 31 average mag 9.7 V (639 multicolor/visual observations, 14 observers); Jul. 31 - Aug. 1 average mag 10.1 V (330 multicolor/visual observations, 19 observers); Aug. 1 - Aug. 2 average mag 10.7 V (427 multicolor/visual observations, 14 observers); most recent: 10.975 V +/- 0.02 (C. Cynamon, Mount Airy, MD). See individual observations via the AAVSO Light Curve Generator (https://www.aavso.org/LCGv2/) or AAVSO Data Download tool (https://www.aavso.org/data-download).