Nova in Vulpecula: N Vul 2021 = TCP J20210770+2914093
Abstract:
Discovered by: Koichi Itagaki (Yamagata, Japan, via TOCP); Discovery mag: unfiltered CCD magnitude 12.0 (using 180-mm camera lens + CCD, via TOCP); Discovery date: 2021 July 16.475 UT (via TOCP); Coordinates (2000.0): R.A. 20 21 07.70 Decl. +29 14 09.1 (from VSX page for N Vul 2021); Spectra: Spectroscopy indicating the object to be a nova was obtained by: R. Leadbeater (Wigton, UK) on 2021 Jul. 16.915 UT. His spectrum may be viewed at: https://britastro.org/specdb/data_graph.php?obs_id=10094; U. Munari et al. (ATel #14793) on 2021 Jul. 17.102 UT with the Stroncone 0.50-m telescope and mk.III Astrolight Instrument multi-mode spectrograph. Their spectra indicated an He/N type nova, but they commented that: "Should the nova still rise in brightness, it could cool down to a FeII type by the time of maximum."
Justification:
Please observe N Vul 2021 as it continues to evolve, with observations of all types (visual, CCD, DSLR, PEP, spectroscopy) and multiple bands as instrumentation permits.
Requested Data Types:
Photometry, Spectroscopy
Targets
| Name | Magnitude | Variability Type | Photometry Notes | Spectroscopy Notes |
|---|---|---|---|---|
| V0606 Vul | 9.90 | NA |
Cadence: Custom Precision: 100 mmag |
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 are available via the AAVSO Variable Star Plotter (VSP, https://apps.aavso.org/vsp/).
Co-Authorship
Observers are not eligible for co-authorship.
Additional Observer Input:
Please observe N Vul 2021 as it continues to evolve, with observations of all types (visual, CCD, DSLR, PEP, spectroscopy) and multiple bands as instrumentation permits. Dr. Fred Walter (Stony Brook University) recommends observations every few hours in the early stages as the nova continues to brighten. Frequency of observation once past peak depends on the rate of decline, but should be a minimum of one observation per night per band. For spectroscopy, he 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 evolves, but, he adds, "you can't go wrong with a spectrum every clear night." Notes: a. Designated TCP J20210770+29140930 when posted to the IAU Central Bureau for Astronomical Telegrams Transient Object Confirmation Page (TOCP). b. P. Schmeer (Saarbrücken-Bischmisheim, Germany) reports no previous brightenings had been recorded in the ASAS-SN Sky Patrol data since 2015 February 27. c. P. Schmeer reports the likely progenitor is catalogued as: Gaia EDR3 1861166838700691968 (RA 20 21 07.704 DEC +29 14 09.09, equinox J2000.0, epoch J2016; Gmag. 21.05); SDSS J202107.70+291409.0 (gmag. 22.3, rmag. 21.7, imag. 21.4); Pan-STARRS1 source PSO J202107.703+291409.136 (gmag. 21.85, rmag. 21.29, imag. 21.13. d. Images: K. Itagaki (2021 Jul. 16.475 UT, discovery image, via TOCP): http://k-itagaki.jp/images/2021-Vul.jpg; S. Kiyota (2021 Jul 16.5647 UT, via TOCP): http://meineko.sakura.ne.jp/ccd/TCP_J20210770+2914093.jpg; R. Fidrich (2021 Jul. 16.8995 UT, via TOCP): https://twitter.com/fidusz/status/1416585687558725639
Additional Submission Location:
Not provided
Notes:
Principal Investigator: Dr. Fred Walter; Imported Campaign (Alert Notice #749)