Electronic Telegram No. 3691 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 AQUILAE 2013 = PNV J19023335+0315190 S. Nakano, Sumoto, Japan, reports the discovery by Koichi Itagaki (Teppo-cho, Yamagata, Japan) of a possible nova (mag 13.8) on an unfiltered CCD frame (limiting mag about 15) taken on Oct. 28.443 UT using a 0.21-m f/3 reflector. Itagaki measured mag 13.8 and the following position for the variable from confirming frames taken with a 0.50-m f/6 reflector on Oct. 28.457: R.A. = 19h02m33s.35, Decl. = +3d15'19".0 (equinox 2000.0). Nothing is visible at this position on Itagaki's most recent survey image of the field taken on Oct. 18.463 UT (limiting mag 14.3) using the same survey telescope. The discovery image is posted at http://www.k-itagaki.jp/images/aql-pnv.jpg. The variable was designated PNV J19023335+0315190 when it was posted at the Central Bureau's TOCP webpage. G. Masi, Ceccano, Italy, writes that he inspected red digitized Palomar Sky Survey plates with P. Schmeer and F. Nocentini of the position around the new variable, finding two very close stars of mag about 15 involved with a fainter possible progenitor of mag 20.0-20.5 having osition end figures 33s.38, 18".1 (UCAC-4 reference stars). Additional CCD magnitudes for PNV J19023335+0315190 (unfiltered unless noted otherwise): Oct. 28.782, 13.5 (Masi, Nocentini, and Schmeer; remotely using a 43-cm telescope at Ceccano; position end figures 33s.38, 18".9); 29.111, V = 15.3, R_c = 13.8, I_c = 12.0 (Seiichiro Kiyota, Kamagaya, Japan; remotely with a 0.43-m astrogrph + FLI-PL6303E camera located near Mayhill, NM, USA); 30.723, I = 11.3, R_c = 13.6, V = 15.6, B = 18.1 (A. Oksanen, Hankasalmi Observatory, Finland; 40-cm reflector + SBIG STL-1001E camera; position end figures 33s.38, 19".1; USNO-B1.0 reference stars); Nov. 6.723, 14.1 (Masi, Nocentini, Schmeer). Terry Bohlsen, Armidale, NSW, Australia, reports that spectra taken of PNV J19023335+031590 at low altitude on Oct. 28 with a 28-cm telescope (+ LISA spectrograph using a 24-micron slit; R = 900) show H_alpha emission with a FWHM of 800 km/s, with no other features visible; one of his spectra can be viewed via website URL http://tinyurl.com/mopo6p6. Masi, Schmeer, and Nocentini report that low-resolution spectroscopy on Oct. 28.794 with a 35.6-cm telescope (+ 100 lines/mm grating; dispersion about 3.47 nm/pixel) at Ceccano also shows the H-alpha emission; their follow-up spectra on Oct. 29.722 clearly show that the H-alpha emission at 656.3 nm was much stronger than the previous night, an O I emission at 844.6 nm was also seen -- both emissions confirmed again on Nov. 6.723, when the O I emission was seen to be very strong. Kazuya Ayani, Bisei Astronomical Observatory, reports that M. Fujii (Kurashiki, Okayama, Japan) obtained a spectrogram (resolution R = 650 at H_alpha) of PNV J19023335+0315190 on Oct. 29.426 UT with a 0.4-m telescope at the Fujii Kurosaki Observatory and found an H-alpha emission line with a P-Cyg profile on a continuum, which seems to be highly reddened. The FWHM of H-alpha emission is 750 km/s, and the absorption is blue-shifted by 950 km/s with respect to the emission. An Na D absorption can be seen (equivalent width about 1.5 nm), although it is very noisy. The spectrogram is posted at website URL http://otobs.org/FBO/fko/nova/pnvj19023335+0315190.png. U. Munari, Astronomical observatory of Padova, INAF, writes that a low-resolution spectrum (range 450.0-800.0 nm; 0.23 nm/pixel) of PNV J19023335+0315190 was obtained on Nov. 3.764 UT with the Asiago 1.22-m telescope (+ Boller & Chivens spectrograph). The spectrum is that of a normal nova, of the "Fe II" type, observed close to maximum brightness. The very red flux distribution of the continuum suggests a huge reddening affecting the nova. The strongest emission lines are H_alpha and O I 777.2-nm, which both show P-Cyg profiles (with a FWHM of 1150 km/s for the emission component and the absorption component shifted by -950 km/s with respect to the emission). Fe II emission lines from multiplets number 42, 48, 49, 73, and 74 are clearly visible. Also in emission are [O I] 630.0- and 636.4-nm and the Na I 589.0- and 589.6-nm doublet. The flux ratio between H_alpha and H_beta is 75, confirming a very large reddening affecting the nova. K. Takaki, R. Itoh, Y. Kanda, and K. S. Kawabata, Hiroshima University, obtained a low-resolution optical spectrum (range 450-900 nm) of PNV J19023335+0315190 on Nov. 5.4 UT with the 1.5-m Kanata telescope (+ HOWPol) at the Higashi-Hiroshima Observatory. The spectrum is consistent with a reddened galactic nova at early phase. It shows emission lines of H-alpha and the Ca II infrared triplet, as well as P-Cyg profiles of O I 777.3- and 844.6-nm. The FWHMs of the H-alpha and O I 777.3-nm emission lines are 1200 km/s, and the blueshift of the absorption line of O I 777.3-nm cooresponds to -1100 km/s in radial velocity. Fe II lines in the range 500-600 nm and He I lines at 587.6-, 667.8-, and 706.5 nm are not significant. NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2013 CBAT 2013 November 7 (CBET 3691) Daniel W. E. Green