ICCE

putting the 'New' back into the New Variable star programme.

A programme to examine the variable star discoveries of Mike Collins was first proposed under Gary Poyner's Directorship in March 1989 (see VSSC 83) and formally adopted as the New Variable Star Programme announced in VSSC 85 (September 1989).

In the time since 1989, although the program has attracted some interest and a few observers have followed a selection of the objects, the level of attention that the program has attracted has been significantly less than that of, for example, the ROP.

There have been papers published concerning objects in the program since 1989 which have resulted in a few objects receiving entries in the GCVS. Some of these papers have even included observations from contributing observers to the 'new' Variable star programme, although these participations have been on an individual basis rather than as part of the BAAVSS observational database.

The time is therefore ripe for a re-launch of the 'New' Variable Star Programme with more specific objectives and a revised list of objects.

ICCE stands for Identification, Characterisation, Correction of Erroneous GCVS entry's.

The acronym summarising the objectives of the programme and the progression of objects on to, through and off the programme. If the identity of the object is not uniquely known then the determination of this is the first priority. Where the identity is known the priority will be in determining the character of the object. The objects 'character' includes its range, period of variability and in some cases, with the support of the CCD equipped observers, the investigation of the variability at different wavelengths. Effectively the collection of characterisation information which is sufficient to 'classify' the variable within the GCVS scheme.

Once both unique identity and character (classification) have been established a GCVS entry should follow on publication of the results and the object can be removed from the programme.

For objects where an erroneous GCVS entry is suspected once sufficient data is available to either confirm or correct the GCVS entry which is under suspicion the object can be removed from the programme.

ICCE Programme 2005.

Identity NSV Const J2000 Range Notes Chart
RA   Dec Max Min
TAV 0033 +53 15133 Cas 00 36 +59 40 10.3 11? GCAS TA
V720 Cas   Cas 00 45 +53 26 12.4?? 13.6?? CCD! SR? TA
TAV 0216 +48   And 02 19 +48 14 9.5 [ 13.5 Mira? TA
TAV 0346 +38   Per 03 49 +38 47 10.3 12.2 C Star TA
CC Cam   Cam 04 57 +69 27 10.8 [14.3   TA
NSV2249 2249 Tau 05 35 +23 53 10.5 [16 Mira? Hendon
TAV 0559 +06   Ori 06 02 +06 38 10.9 12.9 SRa? TA
TASV 0626 +34 16874 Aur 06 29 +34 42 9.8 11.9   TA
TAV 0714 +17   Gem 07 17 +17 54 10.5 12.2 CCD! SR? TA
J0712 +296   Gem 07 12 +29 38 11.3 13.8 CCD! LB? TA
TASV 1812 +40 24346 Her 18 14 +40 26 9.5 10.3 360d? TA
NSV10836 10836 Her 18 28 +15 42 11.0 [15.0 Mira? TA
Q1992/076   Her 18 29 +15 16 11.2 [16 Mira? TA
V2303 Oph   Oph 18 38 +11 11 10.8 [16 Mira? TA (BAA)
V335 Vul   Vul 19 23 +24 30 10.1 13.5 C Star TA (BAA)
TAV 1933 +53   Cyg 19 34 +53 53 10.3 12 CCD! TA
TASV 1946 +00 24897 Aql 19 49 +00 30 10 [16 Mira 330d? TA (BAA)
TAV 2034 +61 25186 Cep 20 35 +61 48 9.6 11.2   TA
NSV13806 13806 Cyg 21 36 +32 31 11.1 [16   TA
TASV 2204 +59 25835 Cep 22 06 +59 30 10.1 12.5 SR? TA
NSV14687 14687 Cep 23 44 +71 46 11.9 [14   TA

Comments on the programme objects:

V720 Cas - The identity of this object is not uniquely known, there being three stars within the error circle of the original discovery information. CCD images taken some weeks or months apart should reveal which of three candidates is actually the variable.

NSV2249 - This object has been on the CCD programme for some time. The amplitude range and strong red excess of the variable indicate a Mira type variability, however the identifying a consistent period for the object has proven surprisingly difficult.

TAV 0714 +17 - This object has a low amplitude and strong red colour that make reliable estimation visually difficult.

V2303 Oph - A new BAAVSS chart and sequence for this object is being prepared and will be available shortly.

V335 Vul - A new BAAVSS chart and sequence for this object is being prepared and will be available shortly J0712+296 - This object has a low amplitude and strong red colour that make reliable estimation visually difficult.

TAV 1933 +53 - This object has a low amplitude and strong red colour that make reliable estimation visually difficult.

NSV 24897 (TASV 1946+00) - A new BAAVSS chart and sequence for this object is being prepared and will be available shortly.

Further detailed comments on each of the objects in the programme will appear in future circulars. There are opportunities for VSSC members to contribute to the programme in a number of ways. CCD equipped observers willing to assist in the development of sequences for these objects would be especially valuable at this stage. There are also objects on the programme (as noted above) that would particularly benefit from observation with CCD's.

Visual observations of any of the programme stars would, of course, be appreciated. As data starts to accumulate on these objects there will be opportunities for the more statistically minded to analyse the data for publication.

The intention is to keep the programme small, but dynamic, with new objects being introduced and well studied objects removed on a regular basis.

The current list of potential objects for the programme numbers over 600 it is therefore unlikely that we will run out of work to be done in the foreseeable future!

I should be grateful if anybody who is interested in taking part in the programme could contact me (details below) so that I can keep you informed of chart developments and other changes to the programme.

Observations reports, monthly, would also be welcomed (in TA format (preferred) or BAA format).

Chris Jones
{adress details}
Email cpj@cix.co.uk