Electronic Telegram No. 3842 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network NOVA CYGNI 2014 = PNV J20214234+3103296 Koichi Nishiyama, Kurume, Japan; and Fujio Kabashima, Miyaki, Japan, report the discovery of a possible nova (mag 10.9) in Cyg on two 40-s unfiltered CCD frames (limiting mag 13.1) taken around Mar. 31.790 UT using a 105-mm-f.l. f/4 camera lens (+ SBIG STL6303E camera). They confirmed the object's presence on five 5-s unfiltered CCD frames (limiting mag 17.6) taken around Mar. 31.820 using a Meade 200R 0.40-m f/9.8 reflector (+ SBIG STL1001E camera). The variable is located at R.A. = 20h21m42s.34, Decl. = +31d03'29".6 (equinox 2000.0). Nothing is visible at this position on their past survey frames taken on Mar. 27.781 (limiting mag 13.4) or on the Digitized Sky Survey, but it is apparently visible at mag 12.4 on a pre-discovery image (limiting mag 13.5) taken on Mar. 30.769 UT. The variable was designated PNV J20214234+3103296 when it was posted at the Central Bureau's TOCP webpage. Additional magnitudes for PNV J20214234+310329: Apr. 1.103 UT, 11.0 (Gianluca Masi, Francesca Nocentini, and Patrick Schmeer; remotely using a 43-cm telescope + CCD near Ceccano, Italy; position end figures 42s.32, 29".4); 1.109, 11.2 (Wolfgang Vollmann, Vienna, Austria; 0.20-m reflector; visual); 2.177, 11.0 (Patrick Schmeer, Bischmisheim, Germany; 0.20-m Schmidt-Cassegrain reflector; visual). Ulisse Munari, Istituto Nazionale di Astrofisica, Padova Astronomical Observatory; and G. Cetrulo, D. Degano, and F. Castellani, "Asiago Novae and Symbiotic Stars" (ANS) collaboration, report that on Apr. 1.060 UT they obtained a medium-resolution spectrogram (range 647-951 nm, dispersion 0.11 nm/pixel) of PNV J20214234+3103296 with the 0.70-m Polse di Cougnes telescope (+ Mark I Multi-Mode Spectrograph). The spectrum has a red slope and is that of a classical nova close to maximum brightness and appreciably reddened. H_alpha, and O I 777.4- and 844.6-nm, are seen in emission, perhaps along with the Ca II. The integrated fluxex of the H_alpha and the O I 777.4- and 844.6-nm emission lines are, respectively, 4.7, 1.0, and 1.5 in units of 10**(-12) erg cm**(-2) s**(-1). O I 777.4-nm presents a P-Cyg profile with a deep P-Cyg absorption that is blue-shifted by -500 km/s from the emission component. The FWHM of the absorption and emission components are 420 and 860 km/s, respectively. The absorption component of the H_alpha P-Cyg profile is less conspicuous and blue-shifted by -480 km/s from the emission component. The FWHM of the absorption and emission components of H_alpha are 350 and 760 km/s, respectively. On Apr. 1.099, they obtained the following photometry for PNV J20214234+3103296: B = 12.28, V = 11.32, R_c = 10.68, I_c = 10.03. The large B-V color supports a significant reddening affecting this nova. Akira Arai, Nishi-Harima Astronomical Observatory, University of Hyogo, reports that a low-dispersion spectrogram (R about 980 at 650 nm) was obtained of the possible nova PNV J20214234+3103296 on Apr. 1.73 UT using the 2-m Nayuta telescope (+ MALLS) at the Nishi-Harima Astronomical Observatory. The spectrum shows emission lines for H-alpha (FWHM about 650 km/s, EW about -3.5 nm), H-beta (EW about -0.8 nm), Fe II multiplets (42, 48, 49, 55, 74), O I (777.3, 844.6 nm), and the Ca II infrared triplet on the continuum emission. P-Cyg profiles are seen with the H-alpha, Fe II lines, and O I lines at about -650 to -550 km/s. These results suggests that the object would be a "Fe II"-type classical nova around maximum. The spectrum is visible via website URL http://tinyurl.com/nnsofud. K. Ayani, Bisei Astronomical Observatory (BAO), Ibara, Okayama, Japan, obtained a low-resolution spectrogram (range 400-800 nm; resolution 0.5 nm at H-alpha) of PNV J20214234+3103296 on Apr. 1.8 UT with the BAO 1-m telescope. The spectrum shows Balmer lines and Fe II lines (multiplets 42 and 49). Most of the lines have P-Cyg profiles. The strongest H-alpha emission has FWHM about 500 km/s, and its absorption bottom is blueshifted by about 600 km/s with respect to the emission peak. The spectrum resembles that of an "Fe II"- type nova. The spectrum is visible via URL http://tinyurl.com/njpf7ap. Ayani also communicates that M. Fujii, Fujii Kurosaki Observatory (FKO), Kurashiki, Okayama, Japan, obtained a low-resolution spectrogram of this variable on Apr. 1.816 UT with 0.4-m telescope at FKO, finding emission lines with P-Cyg profiles of the Balmer series; Fe II (37) 449.1-, 452.0-, 455.6-, 458.4, and 462.9-nm; Fe II (42) 492.4-, 501.8-, and 516.9-nm; Fe II (49) 519.8-, 523.5-, 527.6-, and 531.7-nm; Fe II (74) 614.9-, 624.8-, and 645.6-nm; and O I 777.3-nm. The center of absorption of H-alpha is blueshifted by about 600 km/s with respect to the center of emission. Fujii comments that this appears like a "Fe II"-type nova. His spectrum is posted at website URL http://otobs.org/FBO/etc/pnv_j20214234+3103296.png. NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2014 CBAT 2014 April 2 (CBET 3842) Daniel W. E. Gre