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Last night's result with my 300/1200 Newton, 6 x 30 minute, Alpy 600 (18 micron slit), ATIK 414 EXm: The reddening is obvious.
I am wondering, what can be the emission at 4922A (used to be He I, but it has emission elsewhere).
Moreover, O I 7772 has prominent P-Cyg profile, though it's blended: Peter

Page opened: http://www.astrosurf.com/aras/Aras_Data ... as2020.htm


Nice to see OI 7772 so prominent, Peter!



François

The H beta and Fe curtain region (LHIRES 600/mm, R=1950)

Peter Somogyi wrote: I am wondering, what can be the emission at 4922A

Hi Peter,

It appears in my spectrum too. The emission peak is at 4924A so could be Fe II 4923.92
There is also Fe II 5316.23 and visible faintly just in your spectrum I think, Fe II 5264.18

(Fe II Line identifications from Visual Spec)

Cheers
Robin

Bonjour Christian,

Difficile ce problème, il n'y a vraiment pas de possibilité à faire un montage pour réussir à collecter l'info de la pollution lumineuse... la double bonnette pourrait résoudre cela ? Comment font les pros qui font des spectres très résolus depuis des observatoires avec pollution lumineuse ? Ils ont peut être 2 spectros cote à coté un pour le spectre l'autre pour la pollution lumineuse ?
Est ce que ça existerait des montages eshel maintenant qu'il y a des très grands capteurs CMOS qui pourraient utiliser une fibre en forme de fente au lieu d'etre un trou ? L'idée serait d'avoir le spectre et juste au dessus ou en dessous le fond de ciel sur quelques pixels pour pouvoir le soustraire ??

Hi Robin,
Thank you for the line identification, so those all 4 peaks in your spectra then Fe II emissions then!
Last night I've made a repeat, same instrument and amount of exposure (6x30 minute) - except that got the star higher: There is a large Balmer EW decrement (similar including H-alpha) and O I 7772 emission, whilst the EW of all the "Fe II curtain" remained similar.
The continuum difference can be an error from my instrument (equatorial mount, off slit guiding sometimes).
Peter

Peter,

I confirm: Fe II (42) multiplet always appears as 3 lines: 4924, 5018 and 5169
It is often the brightest multiplet

François

A list of lines identified in novae (adapted from Williams, 2012): http://www.astronomie-amateur.fr/Docume ... _Novae.pdf

Another spectrum of the nova recorded on 1st August under better conditions than my spectrum on 30th July.
As before LISA (23 micron slit) + C11 SCT + SXVR-H694 (unbinned).
The nova was slightly brighter at V = 12.81. Many Fe II lines now clearly visible.
Flux in H-alpha and H-beta has reduced to 2.7E-12 and 2.2E-13 erg/cm2/sec respectively.
P Cyg absorption still present on H-alpha extending blue-ward to -750 km/s.

David

Nice Fe II crowd, David! - I've just started to report similar...
Here is my progress from last night, with same exposures as before (however, a windy weather): Balmer (and OI 7772) decrease should be because of the 0.5mag brightness increase from 07.30 to 07.31- despite of that, the EW of the Fe II multiplet seems to be increased.
Weather gone bad permanently, please continue!
Peter

The nova has brightened steadily over the past 5 days reaching V = 12.07 on the night of 3rd August. The continuum level of the spectrum has correspondingly increased and there are now P Cyg absorption dips on most of the Fe II emission lines as well as on the H-alpha and H-beta lines. These typically extend to -600 km/s from the emission peak on the blue side. H-alpha and H-beta emission line fluxes have reduced to 2.3E-12 and 1.7E-13 erg/cms2/sec respectively.

David