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PNV J20233073+2046041
Nova near star HD194113 in constellation Delphinus

 

 

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Astronomer Telegram
5322 confirmation of no X-rays from Nova Del 2013
5318 No X-ray detection of Nova Del 2013 with Swift
5314 X-ray detection of Nova Del 2013 with Swift
5312 Continuing spectroscopic observations (3500-8800A) of Nova Del 2013 with the Ondrejov Observatory and the ARAS group
5310 Addendum to ATel 5304
5305 Further X-ray observations of Nova Del 2013 with Swift
5304 After a post-maximum plateau Nova Del 2013 has begun a normal decline
5302 Detection of gamma rays from Nova Delphini 2013
5300 Liverpool Telescope spectral monitoring of Nova Delphini 2013 reveals dramatic changes in the Hydrogen Balmer lines
5298 Initiation of Radio/Millimeter Monitoring of Nova Del 2013
5297 Spectroscopy of the very fast Nova Del 2013, already declining past maximum brightness
5295 BVR photometry and CCD spectroscopy of nova Del 2013
5294 UBVJHKLM photometry of Nova Del 2013
5291 Spectroscopic Observation of Nova Del 2013 with the 2.6m Telescope of the Crimean Astrophysical Observatory
5288 Optical photometry and spectroscopy of Nova Del 2013
5283 No X-rays detected from PNV J20233073+2046041 (= Nova Delphini 2013), 9 hours after discovery
5282 Further spectroscopic observations of Nova Del 2013 = PNV J20233073+2046041 with the Ondrejov Observatory
5279 Spectroscopic Observation of PNV J20233073+2046041 with the Liverpool Telescope
4310 Possible Association of the Gamma-ray Transient Fermi J0639+0548 with Nova Mon 2012
4284 Fermi LAT Detection of a New Galactic Bulge Gamma-ray Transient in the Scorpius Region: Fermi J1750-3243, and its Possible Association with Nova Sco 2012
2487 Fermi LAT Detection of a New Galactic Plane Gamma-ray Transient in the Cygnus Region: Fermi J2102+4542, and its Possible Association with V407 Cyg

CBAT Notes

      So what's the difference between a NOVA and a SUPERNOVA?

Supernovae are catastrophic destructive events caused by a core collapse of a star.
A Classic Nova is  the result of fusion reaction  in the outer layer of a white dwarf star which is slowly stealing material from it neighbor star. If the amount of mass accreted reaches a critical point the white dwarf will explode in a  type I-a supernova.
A nova can occur  repeatedly in the same star.

A listing of Supernovae brighter than 17 Mag. can be found at this site
http://www.rochesterastronomy.org/snimages/

         I will keep this graph updated by getting at least one image a night (weather permitting) till it is no longer visible.
 Note: The smaller the magnitude number the brighter the object.

     If you  are interested in how to convert ADU ( Analog Digital Units) values to  a Magnitude value, check out this link http://www.warren-wilson.edu/~physics/Contemp-Astronomy/starmag/starmag.html. You  will need the ADU and Magnitude numbers for a reference star  in the same field as the primary object as well as the ADU value of the object in question.  I use Nebulosity to get the ADU figures.

(This Page was last changed 06/17/2014)


 

These measurements were taken in the visible light without any color filters using an Orion SSP V2 on a SN8, dark subtracted and flat applied.

 

These images will be updated as I get more data.

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