Nova Aquilae 2013 = PNV J19023335+0315190: spectrum (29 Oct. 2013)

PNV J19023335+0315190: spectrum (29 Oct. 2013)

PNV J19023335+0315190: spectrum (29 Oct. 2013)

Updates (8 Nov. 2013): the Central Bureau for Astronomical Telegrams has just issued the CBET 3691 Circular, announcing this object is now Nova Aquilae 2013. Our early and continued observations made possible to understand the nova nature. Here are some short extracts from CBET 3691: “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 position 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); Nov. 6.723,14.1 (Masi, Nocentini, Schmeer). 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.”

After our very prompt confirmation of this transient, we observed again PNV J19023335+0315190 on 29 Oct. 2013 under much better sky conditions and altitude, in order to capture spectroscopy.

The Celestron C14 robotic unit, equipped with a 100 lines/mm diffraction grating, started collecting spectra early in the evening, with the source higher than 44 deg above the western horizon. Averaging 10, 300-seconds exposures we see very clearly emission at H-alpha. It is clearly stronger than on the discovery night.

In addition, we see emission at the OI (8446) wavelength.

Note that the two peaks between 4000 and 5000 angstroms are stars involved with the spectrum.

Below in a new image showing the transient, obtained on 29 Oct. 2013, 17:30 UT, at mag 13.4R:

Possible Nova PNV J19023335+0315190: 29 Oct. 2013

Possible Nova PNV J19023335+0315190: 29 Oct. 2013

More spectra will be collected in the next days.

Observations were performed by Gianluca Masi, Patrick Schmeer and Francesca Nocentini.

 

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